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The survey covers of an area covered by the Dark Energy Survey, reaching a depth of 25–30 rms at a spatial resolution of 11–18 arcsec, resulting in a catalogue of 220 000 sources, of which 180 000 are single-component sources. Here we present the catalogue of single-component sources, together with (where available) optical and infrared cross-identifications, classifications, and redshifts. This survey explores a new region of parameter space compared to previous surveys. Specifically, the EMU Pilot Survey has a high density of sources, and also a high sensitivity to low surface brightness emission. These properties result in the detection of types of sources that were rarely seen in or absent from previous surveys. 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Australia</span> </a></li><li class="page-breadcrumbs__item" data-v-3692cf84><span aria-hidden="true" class="breadcrumbs-wrapper__arrow" data-v-3692cf84>></span><a href="/core/journals/publications-of-the-astronomical-society-of-australia/volume/08A6F1C86EBBD90385E0EF1AF9272071" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-3692cf84><span data-v-63dfaf6e>Volume 38</span> </a></li><li class="page-breadcrumbs__item" data-v-3692cf84><span aria-hidden="true" class="breadcrumbs-wrapper__arrow" data-v-3692cf84>></span><span data-v-3692cf84>The Evolutionary Map of the Universe pilot survey</span></li></ul></div></div> <div class="language" data-v-3692cf84><ul class="language-switch" data-v-6b1118dd data-v-3692cf84><li aria-label="English" data-v-6b1118dd><span class="language-option current divider" data-v-6b1118dd>English</span></li><li aria-label="Français" data-v-6b1118dd><span role="button" tabindex="0" href="#" lang="fr" class="language-option" data-v-6b1118dd> Français </span></li></ul></div></div></div></div> <div class="container container__modified" data-v-01274b1d>  <div class="row" data-v-01274b1d><div role="complementary" aria-label="table of content" class="column__left" data-v-01274b1d><div class="col journal-container row" data-v-146270e8 data-v-01274b1d><img src="https://static.cambridge.org/covers/PAS_0_0_0/publications-of-the-astronomical-society-of-australia.jpg" alt="" class="journal__image" data-v-146270e8> <a href="/core/journals/publications-of-the-astronomical-society-of-australia" class="app-link journal__title app-link__text app-link--underlined" data-v-63dfaf6e data-v-146270e8><span class="text" data-v-63dfaf6e>Publications of the Astronomical Society of Australia </span> </a> <hr aria-hidden="true" class="separator default" data-v-7036083a data-v-146270e8></div>  <div id="toc" class="table-of-content" data-v-01274b1d><h2>Article contents</h2> <div id="toc-list-wrapper" class="table-of-content__wrapper"><ul id="toc-list" class="list"><li class="list__item"><a href="#sec0" class="list__item__link"><span class="toc-title">Abstract</span></a></li> <li class="list__item"><a href="#s1" class="list__item__link"> <span><div class="toc-title">Introduction</div></span></a></li><li class="list__item"><a href="#s2" class="list__item__link"> <span><div class="toc-title">Observations</div></span></a></li><li class="list__item"><a href="#s3" class="list__item__link"> <span><div class="toc-title">Pipeline data reduction</div></span></a></li><li class="list__item"><a href="#s4" class="list__item__link"> <span><div class="toc-title">Value-added processing</div></span></a></li><li class="list__item"><a href="#s5" class="list__item__link"> <span><div class="toc-title">Results</div></span></a></li><li class="list__item"><a href="#s6" class="list__item__link"> <span><div class="toc-title">Preliminary science results</div></span></a></li><li class="list__item"><a href="#s7" class="list__item__link"> <span><div class="toc-title">Conclusion</div></span></a></li> <li class="list__item"><a href="#footnotes-list" class="list__item__link"><span class="toc-title">Footnotes</span></a></li> <li class="list__item"><a href="#references-list" class="list__item__link"><span class="toc-title">References</span></a></li></ul></div></div></div> <div class="column__main" data-v-01274b1d><div class="row" data-v-01274b1d><div class="column__main__left" data-v-01274b1d><div id="maincontent" class="col" data-v-862424e6 data-v-01274b1d> <hgroup data-v-862424e6><h1 data-v-862424e6>The Evolutionary Map of the Universe pilot survey</h1> </hgroup>    <div class="row part-of" data-v-862424e6><span class="part-of__label" data-v-862424e6> Part of: </span> <a href="/core/product/identifier/ASKAP/type/BESPOKE_COLLECTION" class="part-of__collection" data-v-f0b31360 data-v-862424e6> Australian SKA Pathfinder </a></div> <div class="row published-date" data-v-862424e6><p data-v-862424e6> Published online by Cambridge University Press: <strong data-v-862424e6>07 September 2021</strong></p></div>   <div class="contributors-details" data-v-99f6eb26 data-v-862424e6><div class="row contributors" data-v-99f6eb26><div class="col" data-v-99f6eb26><div class="row contributor-type" data-v-792406ce data-v-99f6eb26> <div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=Ray%20P.%20Norris&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>Ray P. Norris</span> </a> <a target="_blank" href="https://orcid.org/0000-0002-4597-1906" data-test-orcid="Ray P. Norris" class="app-link contributor-type__contributor__orcid app-link__icon app-link--" data-v-63dfaf6e data-v-792406ce><img src="data:image/svg+xml;base64,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" alt="Open the ORCID record for Ray P. Norris" class="app-icon icon orcid" data-v-d2c09870 data-v-63dfaf6e> <span class="sr-only" data-v-63dfaf6e>[Opens in a new window]</span></a> <span data-v-792406ce>,</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=Joshua%20Marvil&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>Joshua Marvil</span> </a>  <span data-v-792406ce>,</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=J.%20D.%20Collier&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>J. D. Collier</span> </a>  <span data-v-792406ce>,</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=Anna%20D.%20Kapi%C5%84ska&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>Anna D. Kapińska</span> </a>  <span data-v-792406ce>,</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=Andrew%20N.%20O%E2%80%99Brien&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>Andrew N. O’Brien</span> </a>  <span data-v-792406ce>,</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=L.%20Rudnick&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>L. Rudnick</span> </a> <a target="_blank" href="https://orcid.org/0000-0001-5636-7213" data-test-orcid="L. Rudnick" class="app-link contributor-type__contributor__orcid app-link__icon app-link--" data-v-63dfaf6e data-v-792406ce><img src="data:image/svg+xml;base64,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" alt="Open the ORCID record for L. Rudnick" class="app-icon icon orcid" data-v-d2c09870 data-v-63dfaf6e> <span class="sr-only" data-v-63dfaf6e>[Opens in a new window]</span></a> <span data-v-792406ce>,</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=Heinz%20Andernach&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>Heinz Andernach</span> </a>  <span data-v-792406ce>,</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=Jacobo%20Asorey&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>Jacobo Asorey</span> </a>  <span data-v-792406ce>,</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=Michael%20J.%20I.%20Brown&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>Michael J. I. Brown</span> </a>  <span data-v-792406ce> and</span></div><div class="contributor-type__contributor" data-v-792406ce><a href="/core/search?filters%5BauthorTerms%5D=Marcus%20Br%C3%BCggen&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-792406ce><span data-v-63dfaf6e>Marcus Brüggen</span> </a>  <span data-v-792406ce></span></div> <a href="#" class="app-link app-link__text-icon app-link--secondary reverse" data-v-63dfaf6e data-v-792406ce><img src="data:image/svg+xml;base64,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" alt="" class="app-icon icon arrow-down" data-v-d2c09870 data-v-63dfaf6e><span class="text" data-v-63dfaf6e>...Show all authors </span> </a></div> </div> <div class="col-2 collapse-link" data-v-99f6eb26><a href="#authors-details" data-toggle="collapse" aria-expanded="false" aria-controls="authors-details" class="app-link collapsed app-link__text-icon app-link--secondary reverse" data-v-63dfaf6e data-v-99f6eb26><img src="data:image/svg+xml;base64,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" alt="" class="app-icon icon arrow-down" data-v-d2c09870 data-v-63dfaf6e><span class="text" data-v-63dfaf6e>Show author details </span> </a></div></div> <hr aria-hidden="true" class="separator default" data-v-7036083a data-v-99f6eb26> <dl id="authors-details" class="authors-details collapse" data-v-2edb8da6 data-v-99f6eb26><div data-test-author="Ray P. Norris" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Ray P. Norris*</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="Joshua Marvil" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Joshua Marvil</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>National Radio Astronomy Observatory, PO Box 0, Socorro, NM87801, USA</span> </span></div></dd></div><div data-test-author="J. D. Collier" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>J. D. Collier</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>The Inter-University Institute for Data Intensive Astronomy (IDIA), Department of Astronomy, University of Cape Town, Rondebosch, 7701, South Africa</span> </span></div></dd></div><div data-test-author="Anna D. Kapińska" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Anna D. Kapińska</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>National Radio Astronomy Observatory, PO Box 0, Socorro, NM87801, USA</span> </span></div></dd></div><div data-test-author="Andrew N. O’Brien" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Andrew N. O’Brien</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>Department of Physics, University of Wisconsin-Milwaukee, P.O. Box 413, Milwaukee, WI 53201, USA</span> </span></div></dd></div><div data-test-author="L. Rudnick" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>L. Rudnick</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Minnesota Institute for Astrophysics, University of Minnesota, 116 Church St. SE, Minneapolis, MN 55455, USA</span> </span></div></dd></div><div data-test-author="Heinz Andernach" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Heinz Andernach</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Depto. de Astronomía, DCNE, Universidad de Guanajuato, Cjón. de Jalisco s/n, Guanajuato, CP 36023, Mexico</span> </span></div></dd></div><div data-test-author="Jacobo Asorey" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Jacobo Asorey</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Av. Complutense, 40, 28040 Madrid, Spain</span> </span></div></dd></div><div data-test-author="Michael J. I. Brown" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Michael J. I. Brown</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia</span> </span></div></dd></div><div data-test-author="Marcus Brüggen" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Marcus Brüggen</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>University of Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany</span> </span></div></dd></div><div data-test-author="Evan Crawford" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Evan Crawford</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span></div></dd></div><div data-test-author="Jayanne English" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Jayanne English</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Institute of Space and Planetary Astrophysics (ISPA), University of Karachi (UoK), Karachi, Pakistan</span> </span></div></dd></div><div data-test-author="Syed Faisal ur Rahman" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Syed Faisal ur Rahman</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Department of Physics and Astronomy, University of Manitoba, Winnipeg, MB R3T 2N2, Canada</span> </span></div></dd></div><div data-test-author="Miroslav D. Filipović" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Miroslav D. Filipović</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span></div></dd></div><div data-test-author="Yjan Gordon" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Yjan Gordon</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Institute of Space and Planetary Astrophysics (ISPA), University of Karachi (UoK), Karachi, Pakistan</span> </span></div></dd></div><div data-test-author="Gülay Gürkan" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Gülay Gürkan</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, PO Box 1130, Bentley WA 6102, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>Thüringer Landessternwarte, Sternwarte 5, D-07778 Tautenburg, Germany</span> </span></div></dd></div><div data-test-author="Catherine Hale" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Catherine Hale</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, PO Box 1130, Bentley WA 6102, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>School of Physics and Astronomy, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, EH9 3HJ Edinburgh, UK</span> </span></div></dd></div><div data-test-author="Andrew M. Hopkins" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Andrew M. Hopkins</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>Australian Astronomical Optics, Macquarie University, 105 Delhi Rd, North Ryde, NSW 2113, Australia</span> </span></div></dd></div><div data-test-author="Minh T. Huynh" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Minh T. Huynh</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, PO Box 1130, Bentley WA 6102, Australia</span> </span></div></dd></div><div data-test-author="Kim HyeongHan" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Kim HyeongHan</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Yonsei University, Department of Astronomy, Seoul, Republic of Korea</span> </span></div></dd></div><div data-test-author="M. James Jee" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>M. James Jee</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Yonsei University, Department of Astronomy, Seoul, Republic of Korea</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>Department of Physics, University of California, Davis, California, USA</span> </span></div></dd></div><div data-test-author="Bärbel S. Koribalski" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Bärbel S. Koribalski</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="Emil Lenc" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Emil Lenc</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="Kieran Luken" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Kieran Luken</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="David Parkinson" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>David Parkinson</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Korea Astronomy and Space Science Institute, Daejeon 34055, Korea</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>University of Science and Technology, Daejeon 34113, Korea</span> </span></div></dd></div><div data-test-author="Isabella Prandoni" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Isabella Prandoni</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>INAF – Istituto di Radioastronomia, via P. Gobetti 101, 40129 Bologna, Italy</span> </span></div></dd></div><div data-test-author="Wasim Raja" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Wasim Raja</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="Thomas H. Reiprich" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Thomas H. Reiprich</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Argelander Institute for Astronomy (AIfA), University of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany</span> </span></div></dd></div><div data-test-author="Christopher J. Riseley" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Christopher J. Riseley</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, PO Box 1130, Bentley WA 6102, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>INAF – Istituto di Radioastronomia, via P. Gobetti 101, 40129 Bologna, Italy</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>Dipartimento di Fisica e Astronomia, Università degli Studi di Bologna, via P. Gobetti 93/2, 40129 Bologna, Italy</span> </span></div></dd></div><div data-test-author="Stanislav S. Shabala" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Stanislav S. Shabala</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>School of Natural Sciences, University of Tasmania, Private Bag 37, Hobart, TAS 7001, Australia</span> </span></div></dd></div><div data-test-author="Jaimie R. Sheil" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Jaimie R. Sheil</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia</span> </span></div></dd></div><div data-test-author="Tessa Vernstrom" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Tessa Vernstrom</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, PO Box 1130, Bentley WA 6102, Australia</span> </span></div></dd></div><div data-test-author="Matthew T. Whiting" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Matthew T. Whiting</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="James R. Allison" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>James R. Allison</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>Sub-Dept. of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Rd., Oxford, OX1 3RH, UK</span> </span></div></dd></div><div data-test-author="C. S. Anderson" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>C. S. Anderson</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>National Radio Astronomy Observatory, PO Box 0, Socorro, NM87801, USA</span> </span></div></dd></div><div data-test-author="Lewis Ball" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Lewis Ball</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>SKA Observatory, Jodrell Bank, Lower Withington, Macclesfield, Cheshire SK11 9FT, UK</span> </span></div></dd></div><div data-test-author="Martin Bell" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Martin Bell</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>School of Mathematical and Physical Sciences, University of Technology Sydney</span> </span></div></dd></div><div data-test-author="John Bunton" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>John Bunton</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="T. J. Galvin" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>T. J. Galvin</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, PO Box 1130, Bentley WA 6102, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>International Centre for Radio Astronomy Research, Curtin University, Bentley, WA 6102, Australia</span> </span></div></dd></div><div data-test-author="Neeraj Gupta" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Neeraj Gupta</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>IUCAA, Post Bag 4, Ganeshkhind, Pune University Campus,Pune 411 007, India</span> </span></div></dd></div><div data-test-author="Aidan Hotan" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Aidan Hotan</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, PO Box 1130, Bentley WA 6102, Australia</span> </span></div></dd></div><div data-test-author="Colin Jacka" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Colin Jacka</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="Peter J. Macgregor" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Peter J. Macgregor</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia</span> </span><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="Elizabeth K. Mahony" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Elizabeth K. Mahony</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="Umberto Maio" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Umberto Maio</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>INAF - Observatory of Trieste, via G. Tiepolo 11, 34143 Trieste, Italy</span> </span></div></dd></div><div data-test-author="Vanessa Moss" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Vanessa Moss</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div><div data-test-author="M. Pandey-Pommier" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>M. Pandey-Pommier</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>University Claude Bernard Lyon 1, Bâtiment Quai 43 - 2ème étage, 28, avenue Gaston Berger, 69622 Villeurbanne Cedex, France</span> </span></div></dd></div><div data-test-author="Maxim A. Voronkov" class="row author" data-v-2edb8da6><dt class="col-12 col-sm-2 title" data-v-2edb8da6>Maxim A. Voronkov</dt> <dd class="col content d-inline d-sm-flex" data-v-2edb8da6><span class="content__title" data-v-2edb8da6>Affiliation:</span> <div class="d-sm-flex flex-column flex-sm-1 d-inline" data-v-2edb8da6><span data-v-2edb8da6><span data-v-2edb8da6>CSIRO Space & Astronomy, P.O. Box 76, Epping, NSW 1710, Australia</span> </span></div></dd></div> <div class="row" data-v-2edb8da6><dt class="col-sm-2 col-12 title" data-v-2edb8da6> * </dt> <dd class="col content" data-v-2edb8da6><div class="row" data-v-2edb8da6><div class="d-sm-flex d-inline flex-sm-1 flex-sm-wrap" data-v-2edb8da6><div class="d-inline" data-v-2edb8da6><span data-v-2edb8da6><div class="corresp"><span class="label">*</span>Author for correspondence: Ray P. Norris, E-mail: <a href="mailto:raypnorris@gmail.com">raypnorris@gmail.com</a></div></span></div></div></div></dd></div> <hr aria-hidden="true" class="separator default" data-v-7036083a data-v-2edb8da6></dl></div></div> <div id="app-tabs" class="tabs" data-v-1d90c6ce data-v-01274b1d><div id="app-tabs-wrapper" class="tabs__wrapper" data-v-1d90c6ce><div role="navigation" aria-label="tab navigation" class="container" data-v-1d90c6ce><a data-toggle="collapse" href="#appTabs" role="button" aria-expanded="false" aria-controls="appTabs" class="tabs__collapse collapsed d-sm-none d-print-none" data-v-1d90c6ce><span data-v-1d90c6ce></span> <span class="tabs-arrow-up" data-v-1d90c6ce></span> <span class="tabs-arrow-down" data-v-1d90c6ce></span></a> <ul id="appTabs" role="tablist" class="nav nav-tabs tabs__list collapse show" data-v-1d90c6ce><li role="none" class="tabs__tab" data-v-1d90c6ce><a aria-selected="true" href="#article-tab" role="tab" aria-controls="article-tab" tabindex="-1" 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class="toc-arrow-down"></span></a> <ul id="toc-list-mobile" class="list collapse"><li class="list__item"><a href="#sec0" class="list__item__link"><span class="toc-title">Abstract</span></a></li> <li class="list__item"><a href="#s1" class="list__item__link"> <span>Introduction</span></a></li><li class="list__item"><a href="#s2" class="list__item__link"> <span>Observations</span></a></li><li class="list__item"><a href="#s3" class="list__item__link"> <span>Pipeline data reduction</span></a></li><li class="list__item"><a href="#s4" class="list__item__link"> <span>Value-added processing</span></a></li><li class="list__item"><a href="#s5" class="list__item__link"> <span>Results</span></a></li><li class="list__item"><a href="#s6" class="list__item__link"> <span>Preliminary science results</span></a></li><li class="list__item"><a href="#s7" class="list__item__link"> <span>Conclusion</span></a></li> <li class="list__item"><a href="#footnotes-list" class="list__item__link"><span 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href="https://s100.copyright.com/AppDispatchServlet?publisherName=CUP&publication=PAS&title=The%20Evolutionary%20Map%20of%20the%20Universe%20pilot%20survey&publicationDate=07%20September%202021&author=Ray%20P.%20Norris%2C%20Joshua%20Marvil%2C%20J.%20D.%20Collier%2C%20Anna%20D.%20Kapi%C5%84ska%2C%20Andrew%20N.%20O%E2%80%99Brien%2C%20L.%20Rudnick%2C%20Heinz%20Andernach%2C%20Jacobo%20Asorey%2C%20Michael%20J.%20I.%20Brown%2C%20Marcus%20Br%C3%BCggen%2C%20Evan%20Crawford%2C%20Jayanne%20English%2C%20Syed%20Faisal%20ur%20Rahman%2C%20Miroslav%20D.%20Filipovi%C4%87%2C%20Yjan%20Gordon%2C%20G%C3%BClay%20G%C3%BCrkan%2C%20Catherine%20Hale%2C%20Andrew%20M.%20Hopkins%2C%20Minh%20T.%20Huynh%2C%20Kim%20HyeongHan%2C%20M.%20James%20Jee%2C%20B%C3%A4rbel%20S.%20Koribalski%2C%20Emil%20Lenc%2C%20Kieran%20Luken%2C%20David%20Parkinson%2C%20Isabella%20Prandoni%2C%20Wasim%20Raja%2C%20Thomas%20H.%20Reiprich%2C%20Christopher%20J.%20Riseley%2C%20Stanislav%20S.%20Shabala%2C%20Jaimie%20R.%20Sheil%2C%20Tessa%20Vernstrom%2C%20Matthew%20T.%20Whiting%2C%20James%20R.%20Allison%2C%20C.%20S.%20Anderson%2C%20Lewis%20Ball%2C%20Martin%20Bell%2C%20John%20Bunton%2C%20T.%20J.%20Galvin%2C%20Neeraj%20Gupta%2C%20Aidan%20Hotan%2C%20Colin%20Jacka%2C%20Peter%20J.%20Macgregor%2C%20Elizabeth%20K.%20Mahony%2C%20Umberto%20Maio%2C%20Vanessa%20Moss%2C%20M.%20Pandey-Pommier%2C%20Maxim%20A.%20Voronkov©right=%C2%A9%20The%20Author(s)%2C%202021.%20Published%20by%20Cambridge%20University%20Press%20on%20behalf%20of%20the%20Astronomical%20Society%20of%20Australia&contentID=10.1017%2Fpasa.2021.42&startPage=&endPage=&orderBeanReset=True&volumeNum=38&issueNum=&oa=" data-test-id="buttonRightLink" class="app-link rights-link d-print-none app-link__text-icon app-link--accent" data-v-63dfaf6e data-v-92ee52a2 data-v-43a4d572><img src="/core/page-component/img/rights-icon.d4a677c.svg" alt="" class="app-icon icon rights" data-v-d2c09870 data-v-63dfaf6e><span class="text" data-v-63dfaf6e>Rights & Permissions </span> <span class="sr-only" data-v-63dfaf6e>[Opens in a new window]</span></a></div> <hr aria-hidden="true" class="separator default" data-v-7036083a></div> <div class="share-modal-overlay" style="display:none;" data-v-43a4d572></div> <div data-spy="scroll" data-target="#toc" class="scrollspy-content" data-v-43a4d572> <div id="sec0" class="col article-abstract sec" data-v-2fa8b348 data-v-43a4d572><div class="abstract-text-container" data-v-2fa8b348><div lang="en"><h2>Abstract</h2>  <div class="abstract-content"><div class="abstract" data-abstract-type="normal"> <p>We present the data and initial results from the first pilot survey of the Evolutionary Map of the Universe (EMU), observed at 944 MHz with the Australian Square Kilometre Array Pathfinder (ASKAP) telescope. The survey covers <span class="inlineFormula"> <span class="alternatives"> <img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline1.png" /> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $270 \,\mathrm{deg}^2$ </span></span> </span> </span> of an area covered by the Dark Energy Survey, reaching a depth of 25–30 <span class="inlineFormula"> <span class="alternatives"> <img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline2.png" /> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> rms at a spatial resolution of <span class="inlineFormula"> <span class="alternatives"> <img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline3.png" /> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>11–18 arcsec, resulting in a catalogue of <span class="inlineFormula"> <span class="alternatives"> <img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline4.png" /> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>220 000 sources, of which <span class="inlineFormula"> <span class="alternatives"> <img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline5.png" /> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>180 000 are single-component sources. Here we present the catalogue of single-component sources, together with (where available) optical and infrared cross-identifications, classifications, and redshifts. This survey explores a new region of parameter space compared to previous surveys. Specifically, the EMU Pilot Survey has a high density of sources, and also a high sensitivity to low surface brightness emission. These properties result in the detection of types of sources that were rarely seen in or absent from previous surveys. We present some of these new results here.</p> </div></div> <hr aria-hidden="true" class="abstract-divider separator default" data-v-7036083a></div></div>   </div>  <div class="keywords" data-v-86c27100 data-v-43a4d572><h2 data-v-86c27100>Keywords</h2> <div class="row keywords__pills" data-v-86c27100><a href="/core/search?filters[keywords]=Extragalactic astronomy" data-v-f0b31360 data-v-86c27100><span data-v-f0b31360 data-v-86c27100>Extragalactic astronomy</span></a><a href="/core/search?filters[keywords]=Radio astronomy" data-v-f0b31360 data-v-86c27100><span data-v-f0b31360 data-v-86c27100>Radio astronomy</span></a><a href="/core/search?filters[keywords]=Sky surveys" data-v-f0b31360 data-v-86c27100><span data-v-f0b31360 data-v-86c27100>Sky surveys</span></a></div> <hr aria-hidden="true" class="separator default" data-v-7036083a data-v-86c27100></div>  <dl class="article-details" data-v-6e32a161 data-v-43a4d572><div class="row" data-v-6e32a161><dt class="col-12 col-sm-3 col-md-2_5 title" data-v-6e32a161> Type </dt> <dd class="col content" data-v-6e32a161>Research Article</dd></div> <div class="row" data-v-6e32a161><dt class="col-12 col-sm-3 col-md-2_5 title" data-v-6e32a161> Information </dt> <dd class="col content" data-v-6e32a161><div class="content__journal" data-v-6e32a161><a href="/core/journals/publications-of-the-astronomical-society-of-australia" class="app-link app-link__text app-link--underlined" data-v-63dfaf6e data-v-6e32a161><span class="text" data-v-63dfaf6e>Publications of the Astronomical Society of Australia </span> </a> <span data-v-6e32a161> , <a href="/core/journals/publications-of-the-astronomical-society-of-australia/volume/08A6F1C86EBBD90385E0EF1AF9272071" class="app-link app-link__text app-link--underlined" data-v-63dfaf6e data-v-6e32a161><span class="text" data-v-63dfaf6e>Volume 38 </span> </a></span>  <span data-v-6e32a161>, 2021</span>   <span data-v-6e32a161>, e046</span></div> <div class="doi-data" data-v-6e32a161><div data-v-6e32a161>DOI: <a target="_blank" href="https://doi.org/10.1017/pasa.2021.42" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-6e32a161><span class="text" data-v-63dfaf6e>https://doi.org/10.1017/pasa.2021.42 </span> <span class="sr-only" data-v-63dfaf6e>[Opens in a new window]</span></a></div> <a data-target="crossmark" aria-label="Check for updates" href="#" class="crossmark-widget" data-v-6e32a161><img src="/core/page-component/img/crossmark-logo.61d5da3.svg" alt="Check for updates" data-v-6e32a161></a></div>  <div data-v-6e32a161><a target="_blank" href="https://ui.adsabs.harvard.edu/abs/10.1017/pasa.2021.42" class="app-link app-link__text app-link--underlined" data-v-63dfaf6e data-v-6e32a161><span class="text" data-v-63dfaf6e>NASA ADS Abstract Service </span> <span class="sr-only" data-v-63dfaf6e>[Opens in a new window]</span></a></div></dd></div>   <div class="row" data-v-6e32a161><dt class="col-12 col-sm-3 col-md-2_5 title" data-v-6e32a161> Copyright </dt> <dd class="col content" data-v-6e32a161><div data-v-6e32a161> © The Author(s), 2021. Published by Cambridge University Press on behalf of the Astronomical Society of Australia </div></dd></div></dl>  <div id="content-container" class="content-container" data-v-43a4d572><div class="content-box"><div class="article research-article NLM"> <div class="body"> <div class="sec intro" data-magellan-destination="s1" id="s1"> <h2 class="A"><span class="label">1.</span> Introduction</h2> <p class="p"> Large radio surveys provide substantial samples of galaxies for studying cosmology. They also reveal rare but important stages of galaxy evolution and expand the volume of observed parameter space. Before the survey described here took place, about 2.5 million radio sources were known. That figure is about to increase by about two orders of magnitude (Norris <a class="xref bibr" href="#r91"><span class="show-for-sr">Reference Norris</span>2017</a>a), primarily due to using innovative technology in the development of new radio telescopes and upgrading of older radio telescopes. These technological developments will enable several large radio surveys, which are expected to drive a rapid advance in knowledge. <a class="xref fig" href="#f1">Figure 1</a> shows the historical growth of these surveys. </p><section><div class="fig" data-magellan-destination="f1" id="f1"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig1.png?pub-status=live" class="aop-lazy-load-image" width="2250" height="1586" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig1.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 1.</span> The number of known extragalactic radio sources discovered by surveys as a function of time, adapted from Norris (<a class="xref bibr" href="#r91"><span class="show-for-sr">Reference Norris</span>2017</a>a). The symbols indicate the type of telescope used to make the survey, and are fully described in Norris (<a class="xref bibr" href="#r91"><span class="show-for-sr">Reference Norris</span>2017</a>a). The dates and survey size are based on estimates made in 2017, and some later surveys (e.g. RACS McConnell et al. <a class="xref bibr" href="#r81"><span class="show-for-sr">Reference McConnell</span>2020</a>, with 2.8 million sources) are missing from this plot. Survey abbreviations and references are given in Norris (<a class="xref bibr" href="#r91"><span class="show-for-sr">Reference Norris</span>2017</a>a). The shading under the curve is merely to improve readability.</p> </div></div></section> <section><div class="fig" data-magellan-destination="f2" id="f2"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig2.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1005" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig2.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 2.</span> Some of the ASKAP antennas equipped with phased array feeds, located in the Murchison Region of Western Australia. Photo credit: CSIRO</p> </div></div></section> <section><div class="fig" data-magellan-destination="f3" id="f3"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig3.png?pub-status=live" class="aop-lazy-load-image" width="1499" height="855" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig3.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 3.</span> One of the phased array feeds. Each square on the chequerboard is an antenna element connected to two receivers. Photo credit: CSIRO</p> </div></div></section> <p class="p"> One of these new telescopes is the Australian Square Kilometre Array Pathfinder, (ASKAP, Johnston et al. <a class="xref bibr" href="#r60"><span class="show-for-sr">Reference Johnston</span>2007</a>; Johnston et al. <a class="xref bibr" href="#r61"><span class="show-for-sr">Reference Johnston</span>2008</a>; McConnell et al. <a class="xref bibr" href="#r79"><span class="show-for-sr">Reference McConnell</span>2016</a>; Hotan et al. <a class="xref bibr" href="#r54"><span class="show-for-sr">Reference Hotan</span>2021</a>) which consists of 36 12-m antennas spread over a region 6 km in diameter at the Murchison Radio-astronomy Observatory in Western Australia, shown in <a class="xref fig" href="#f2">Figure 2</a>. At the focus of each antenna is an innovative phased-array feed (PAF: Hay et al. <a class="xref bibr" href="#r47"><span class="show-for-sr">Reference Hay, O’Sullivan, Kot, Granet, Lacoste, Ouwehand and Special Publication</span>2006</a>) of 94 dual-polarisation pixels (<a class="xref fig" href="#f3">Figure 3</a>). As a result, ASKAP has an instantaneous field of view up to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline6.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline6.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $30 \,\mathrm{deg}^2$ </span></span> </span> </span>, producing a much higher survey speed than that of previous synthesis arrays. The antennas are a novel three-axis design, with the feed and reflector rotating to ensure a constant position angle of the PAF and sidelobes on the sky.</p> <p class="p"> The first all-sky survey undertaken by ASKAP was the Rapid ASKAP Continuum Survey (McConnell et al. <a class="xref bibr" href="#r81"><span class="show-for-sr">Reference McConnell</span>2020</a>) which surveyed the entire sky south of Declination <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline7.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline7.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $+41^{\circ}$ </span></span> </span> </span> to a median rms of about 250 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline8.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline8.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>. Apart from its astrophysical importance, this survey will also generate a sky model (Hale et al., in preparation) to facilitate the calibration of subsequent deeper observations with ASKAP.</p> <p class="p"> ASKAP will conduct a deep all-sky continuum survey known as the Evolutionary Map of the Universe (EMU: Norris et al. <a class="xref bibr" href="#r94"><span class="show-for-sr">Reference Norris</span>2011</a>). The primary goal of EMU is to make a deep (10–20 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline9.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="75" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline9.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> rms) radio continuum survey of the entire southern sky, extending as far north as <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline10.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline10.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $+30^{\circ}$ </span></span> </span> </span>. EMU is expected to generate a catalogue of as many as 70 million galaxies.</p> <p class="p"> In preparation for the full EMU survey, we conducted the EMU Pilot Survey (EMU-PS) with the goal of testing the planned EMU survey strategy and the processing pipeline. In designing the pilot survey, we adopted the following boundary conditions: </p><ul class="list nomark"> <li class="list-item"> <p class="p"> Declination <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline11.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="48" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline11.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $ < -30 ^{\circ} $ </span></span> </span> </span> (to avoid potentially poor <em class="italic">u</em>,<em class="italic">v</em> coverage near the equator).</p> </li> <li class="list-item"> <p class="p"> Galactic latitude <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline12.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="47" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline12.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $ > +20 ^{\circ} $ </span></span> </span> </span> (to avoid the strong diffuse emission in the Galactic plane).</p> </li> <li class="list-item"> <p class="p"> Sufficiently far from the Sun to avoid solar interference, or night-time observation.</p> </li> <li class="list-item"> <p class="p"> A single area of 240–300 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline13.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="28" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline13.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mathrm{deg}^2$ </span></span> </span> </span>, of 10–12 h observations each on contiguous fields, to form a rectangular area. Cosmological analyses are optimised if the area is as square as possible.</p> </li> <li class="list-item"> <p class="p"> Fields overlapped by a small amount to provide uniform sensitivity.</p> </li> <li class="list-item"> <p class="p"> Frequency band chosen to avoid any radio frequency interference and maximise survey speed, subject to constraints on resolution and confusion.</p> </li> <li class="list-item"> <p class="p"> Field that is well studied at other wavelengths to maximise the scientific value.</p> </li> </ul> <p class="p"> These boundary conditions were satisfied by the survey described in this paper. The survey specifications are given in <a class="xref table" href="#tbl1">Table 1</a>.</p><div class="table-wrap" data-magellan-destination="tbl1" id="tbl1"> <div class="caption"> <p class="p"><span class="label">Table 1.</span> EMU Pilot Survey specifications.</p> </div> <span> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab1.png?pub-status=live" class="aop-lazy-load-image" width="399" height="111" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab1.png" data-zoomable="false"></div> </span> </div> <p class="p"> An area of sky within the Dark Energy Survey (DES: Abbott et al. <a class="xref bibr" href="#r1"><span class="show-for-sr">Reference Abbott</span>2018</a>) was chosen so that we could access the excellent optical photometric data available from DES. EMU and DES have a Memorandum of Understanding that enables data to be shared between the two projects.</p> <p class="p"> The observations were taken and processed in late 2019. It should be emphasised that, at the time of observation, commissioning of the telescope and its processing software were not yet complete, so that there are known telescope issues and processing deficiencies which were not yet addressed. As a result, the images show some artefacts, and the rms noise level is about twice as high as we expect in the final EMU survey. Nevertheless, this is still the largest radio survey ever completed at this depth, and so a great deal of valuable science results are being obtained, some of which are discussed briefly in this paper.</p> <p class="p"> <a class="xref sec" href="#s2">Section 2</a> of this paper describes the observations, and <a class="xref sec" href="#s3">Section 3</a> describes the data reduction. <a class="xref sec" href="#s4">Section 4</a> describes the ‘value-added’ data processing, and <a class="xref sec" href="#s5">Section 5</a> presents the results and data access. <a class="xref sec" href="#s6">Section 6</a> presents some preliminary science results.</p> <div class="sec" data-magellan-destination="s1-1" id="s1-1"> <h3 class="B"><span class="label">1.1.</span> Nomenclature and conventions</h3> <p class="p"> Throughout this paper and in the catalogue, we use source names in the format EMU PS JHHMMSS.S<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline18.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline18.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>DDMMSS and we define spectral index <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline19.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline19.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha$ </span></span> </span> </span> in terms of the relationship between flux density <em class="italic">S</em> and observing frequency <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline20.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="8" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline20.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\nu$ </span></span> </span> </span> as <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline21.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="40" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline21.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S \propto \nu^{\alpha}$ </span></span> </span> </span>.</p> <p class="p"> For consistency among science results derived from EMU-PS data, we encourage the use of a consistent set of cosmological parameters in papers reporting results from EMU-PS. Here we assume a flat <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline22.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline22.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\Lambda$ </span></span> </span> </span>CDM model, with parameter values taken from the mean posterior of the Planck 2018 cosmology, from paper VI (Planck Collaboration et al. 2020), using a combination of Planck data, but with no extra, non-Planck data (e.g. no Baryon Acoustic Oscillation data). This results in the parameter set shown in <a class="xref table" href="#tbl2">Table 2</a>.</p><div class="table-wrap" data-magellan-destination="tbl2" id="tbl2"> <div class="caption"> <p class="p"><span class="label">Table 2.</span> Cosmological parameters used in this paper and adopted for EMU-PS.</p> </div> <span> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab2.png?pub-status=live" class="aop-lazy-load-image" width="416" height="243" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab2.png" data-zoomable="false"></div> </span> </div> </div> </div> <div class="sec other" data-magellan-destination="s2" id="s2"> <h2 class="A"><span class="label">2.</span> Observations</h2> <p class="p"> ASKAP has 36 antennas, all but 6 of which are within a region of 2.3 km diameter, with the outer 6 extending the baselines up to 6.4 km. In all pilot survey observations, as many of the 36 antennas were used as possible. However, in some cases, a few antennas were omitted because of maintenance or hardware issues. The actual number of antennas used is shown in <a class="xref table" href="#tbl3">Table 3</a>. </p><div class="table-wrap" data-magellan-destination="tbl3" id="tbl3"> <div class="caption"> <p class="p"><span class="label">Table 3.</span> EMU pilot observation details.</p> </div> <span> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab3.png?pub-status=live" class="aop-lazy-load-image" width="416" height="265" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab3.png" data-zoomable="false"></div> </span> <div class="table-wrap-foot"> <p class="p"> The position shown is the antenna pointing centre, corresponding to position (0,0) in <a class="xref fig" href="#f4">Figure 4</a>. Columns 5 and 6 show the ASKAP scheduling block identification (SBID) number for the target and calibrator observations.</p> </div> </div> <p class="p"> At the prime focus of each antenna is a phased array feed (PAF), which subtends a solid angle of about <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline42.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline42.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $30 \,\mathrm{deg}^2$ </span></span> </span> </span> of the sky. The PAF consists of 188 single-polarisation dipole receivers. A weighted sum of the outputs of groups of these receivers is used to form 36 dual-polarisation ‘beams’. Individual dipole receivers will, in general, contribute to more than one beam, so that adjacent beams are not completely independent. The 36 beams together cover an area of about <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline43.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="46" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline43.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $30 \,\mathrm{deg}^2$ </span></span> </span> </span> on the sky, which we refer to as a ‘tile’.</p> <p class="p"> There are several ways of arranging the individual beams within the tile. For EMU-PS, we use a hexagonal arrangement of the 36 beams with 6 rows of 6 beams, known as ‘closepack36’ (Hotan et al. <a class="xref bibr" href="#r54"><span class="show-for-sr">Reference Hotan</span>2021</a>), shown in <a class="xref fig" href="#f4">Figure 4</a>. This configuration provides more uniform coverage than the widely used rectangular array known as ‘square_6x6’. The spacing between the beams is known as the ‘pitch’ and is set to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline44.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="24" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline44.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $0.9^{\circ}$ </span></span> </span> </span> for EMU-PS. In some other ASKAP observations, interleaved observations are taken, with the antenna pointing position shifted by half the pitch, to provide better uniformity. However, this is not necessary for the EMU-PS because of the combination of our lower observing frequency and the closepack36 configuration. </p><section><div class="fig" data-magellan-destination="f4" id="f4"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig4.png?pub-status=live" class="aop-lazy-load-image" width="667" height="653" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig4.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 4.</span> The arrangement of the 36 ASKAP beams in the ‘closepack36’ configuration. The beams are numbered from 0 to 35 (diagram adapted from McConnell et al. <a class="xref bibr" href="#r80"><span class="show-for-sr">Reference McConnell</span>2019</a>). The circles shown are for illustration only. For EMU-PS, the actual full width half maximum of each beam is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline45.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="37" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline45.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}1.5^{\circ}$ </span></span> </span> </span> at the band centre, and the pitch spacing is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline46.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="24" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline46.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $0.9^{\circ}$ </span></span> </span> </span>, giving an approximately uniform sensitivity over the field of view.</p> </div></div></section> <p class="p"> The weights of the individual beams are initially calibrated by observing the Sun, placed successively at the centre of each beam, and then adjusting the weights for maximum signal-to-noise ratio. A radiator at the vertex of each antenna (the On-Dish Calibrator, or ODC) enables the gain of each receiver to be monitored, and the weight solution initially obtained from solar observations may be updated if necessary using these ODC measurements.</p> <p class="p"> Before (or sometimes after) the observation of each target, the calibrator source PKS 1934–638 is observed for 200 s at the centre of each of the 36 beams to provide bandpass and gain calibration. This calibration observation takes about 2 h.</p> <p class="p"> The positions of the tiles are chosen using a tiling scheme which will be used for the main EMU survey, shown in <a class="xref fig" href="#f5">Figure 5</a>. At most declinations, the tiles are aligned with lines of constant declination. At the south polar cap (below declination <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline47.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="51" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline47.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-71.81^{\circ}$ </span></span> </span> </span>), they are arranged in a rectangular grid as shown in <a class="xref fig" href="#f5">Figure 5</a>. Using this scheme, the sky south of Declination <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline48.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline48.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $+30^{\circ}$ </span></span> </span> </span> is covered by 1 280 tiles. Overlaps between tiles amount to less than 5% of the total area covered. </p><section><div class="fig" data-magellan-destination="f5" id="f5"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig5.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1502" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig5.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 5.</span> The sky tiling scheme adopted for the EMU-PS. The red rectangles covering the celestial sphere show the tiles planned for the EMU survey, and the orange area indicates the 10 tiles of the EMU-PS. The white strip shows the Galactic plane, and the south celestial pole is at the bottom of the figure.</p> </div></div></section> <section><div class="fig" data-magellan-destination="f6" id="f6"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig6.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="705" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig6.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 6.</span> The location of the EMU Pilot Survey area on the sky within DES DR1, adapted from Abbott et al. (<a class="xref bibr" href="#r1"><span class="show-for-sr">Reference Abbott</span>2018</a>). The diagram is in equatorial coordinates, and the solid line marks the Galactic plane, flanked by two dashed lines showing Galactic latitude <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline49.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline49.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\pm 10 ^{\circ}$ </span></span> </span> </span>.</p> </div></div></section> <p class="p"> The pilot survey was observed with ASKAP in the period from 2019 July 15 to 2019 November 24. In some cases, the initial observations were subsequently found to be faulty, in which case the field was re-observed. <a class="xref table" href="#tbl3">Table 3</a> shows the details of the observations that were used in the final data product.</p> <p class="p"> The survey consists of a 10-h observation of each of the 10 tiles, each accompanied by a calibration observation as described above. No further calibration is performed during the observation. The location of the survey area is shown in <a class="xref fig" href="#f6">Figure 6</a>, and the details of the pointing centres are shown in <a class="xref table" href="#tbl3">Table 3</a> and in <a class="xref fig" href="#f7">Figure 7</a>. </p> </div> <div class="sec other" data-magellan-destination="s3" id="s3"> <h2 class="A"><span class="label">3.</span> Pipeline data reduction</h2> <p class="p"> We process the data using the ASKAPsoft pipeline (Whiting et al. <a class="xref bibr" href="#r125"><span class="show-for-sr">Reference Whiting, Voronkov and Mitchell</span>2017</a>; Whiting <a class="xref bibr" href="#r123"><span class="show-for-sr">Reference Whiting, Ballester, Ibsen, Solar and Shortridge</span>2020</a>; Guzman et al. <a class="xref bibr" href="#r45"><span class="show-for-sr">Reference Guzman</span>2019</a>) with the parameters shown in <a class="xref table" href="#tbl4">Table 4</a>, and using 2-arcsec square pixels. All parameter names, shown in italics in this section, are included in <a class="xref table" href="#tbl4">Table 4</a>. </p><div class="table-wrap" data-magellan-destination="tbl4" id="tbl4"> <div class="caption"> <p class="p"><span class="label">Table 4.</span> EMU pilot processing parameters. The first column shows the parameter name used by ASKAPsoft.</p> </div> <span> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab4.png?pub-status=live" class="aop-lazy-load-image" width="748" height="353" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab4.png" data-zoomable="true"></div> </span> </div><div class="table-wrap" data-magellan-destination="tbl5" id="tbl5"> <div class="caption"> <p class="p"><span class="label">Table 5.</span> Results of tests to measure the optimum robustness.</p> </div> <span> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab5.png?pub-status=live" class="aop-lazy-load-image" width="416" height="199" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab5.png" data-zoomable="false"></div> </span> <div class="table-wrap-foot"> <p class="p"> Tests were conducted at 888 MHz, using a 10-h ASKAP observation on arrays of 33 (for Stokes V, using SB8129 on a field close to UV Ceti) and 35 (for Stokes I, using SB8137 on the GAMA23 field) antennas. Columns 2 and 3 given the major and minor axes of the restoring beam, and columns 4 and 5 gives the measured rms values in (a) a source-free region of the Stokes I image, and (b) the Stokes V image, which is almost source-free. The results have been scaled to a 10-h observation on an array of 36 antennas.</p> </div> </div> <p class="p"> The ASKAP correlator generates 16384 spectral line channels and, for EMU data, we start by averaging these to 288 1-MHz channels to reduce the computational load (i.e. <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline58.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="110" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline58.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $DO\_SPECTRAL\_$ </span></span> </span> </span> <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline59.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="112" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline59.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $ IMAGING = true$ </span></span> </span> </span> and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline60.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="119" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline60.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $DO\_CONTCUBE\_ $ </span></span> </span> </span> <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline61.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="112" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline61.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $ IMAGING = true$ </span></span> </span> </span>)</p> <p class="p"> Weighting and tapering in ASKAPsoft are done using a Wiener filter preconditioning technique, which is computationally more efficient than traditional tapering and weighting. (i.e. <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline62.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="381" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline62.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $ RESTORE\_PRECONDITIONER\_LIST = [Wiener, Gaussian$- </span></span> </span> </span> <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline63.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="39" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline63.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $Taper]$ </span></span> </span> </span>) for the main and alt image respectively</p> <p class="p"> To choose the robustness (Briggs <a class="xref bibr" href="#r16"><span class="show-for-sr">Reference Briggs</span>1995</a>), we conducted tests on part of the GAMA23 field (at about Right Ascension 23:00, Declination <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline64.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline64.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>32:00; Leahy et al. (<a class="xref bibr" href="#r72"><span class="show-for-sr">Reference Leahy</span>2019</a>), Prandoni et al., in preparation), in both Stokes I (total intensity) and Stokes V (circular polarisation) resulting in the values shown in <a class="xref table" href="#tbl5">Table 5</a>. At lower (more negative) values of robustness, the rms increases because the near-uniform weighting discards information. At higher (more positive) values of robustness, corresponding to near-natural weighting, the V rms continues to decrease but the I rms increases presumably because of (a) confusion, (b) poorer <em class="italic">u</em>,<em class="italic">v</em> coverage leading to increased sidelobes, (c) increased radio frequency interference on short baselines. Based on these results, we choose a robustness of 0.0 as an optimum value for the EMU-PS, that is, <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline65.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="335" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline65.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $PRECONDITIONER\_WIENER\_ROBUSTNESS=0.0$ </span></span> </span> </span>. Although robustness +0.5 has a slightly lower rms, it has a significantly increased beam size. No further tapering is used in the main image. </p><section><div class="fig" data-magellan-destination="f7" id="f7"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig7.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1095" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig7.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 7.</span> The arrangement of the ten individual ASKAP tiles on the sky for EMU-PS with their SBID numbers as listed in <a class="xref table" href="#tbl3">Table 3</a>. The rectangles are separated in this diagram for clarity, but there is actually overlapping coverage as illustrated by the greyscale background.</p> </div></div></section> <p class="p"> The non-coplanarity of ASKAP is managed using the w-projection technique (Cornwell et al. <a class="xref bibr" href="#r27"><span class="show-for-sr">Reference Cornwell, Golap and Bhatnagar</span>2008</a>; Rau et al. <a class="xref bibr" href="#r107"><span class="show-for-sr">Reference Rau, Bhatnagar, Voronkov and Cornwell</span>2009</a>), using a total of 557 w-planes (i.e. <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline66.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="196" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline66.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $GRIDDER\_NWPLANES=557$ </span></span> </span> </span>). The data are gridded using multi-frequency synthesis and deconvolved using a multi-frequency multiscale CLEAN, using <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline67.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="109" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline67.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $CLEAN\_SCALES$ </span></span> </span> </span> of [0,6,15,30,45,60] pixels, which gives 6 scales up to 10 times the clean beam size. After initial imaging and cleaning (using 5 major cycles: <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline68.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="212" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline68.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $CLEAN\_NUM\_MAJOR\_CYCLES$ </span></span> </span> </span>, with 400 iterations in each minor cycle, down to a limit of 0.25 mJy), the data are given one iteration of phase selfcal using the output of the previous CLEAN (i.e. <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline69.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="204" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline69.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $SELFCAL\_METHOD=CLEAN$ </span></span> </span> </span>) before the final imaging and cleaning (15 major cycles with up up to 3000 iterations in each minor cycle, with minor cycles triggering a major cycle when they reach a 30% CLEAN limit, to a clean limit of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline70.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="42" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline70.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $30 \,\mu\mathrm{Jy}$ </span></span> </span> </span>, i.e. <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline71.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="251" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline71.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $CLEAN\_THRESHOLD\_MINORCYCLE$ </span></span> </span> </span>). Two images are produced by the pipeline: the main image at full resolution and an alternative (‘alt’) image tapered to a 30-arcsec resolution, which is optimised for faint diffuse emission. The alt image is not used in this paper.</p> <p class="p"> The multi-frequency synthesis imaging uses a Taylor term technique (Rau & Cornwell <a class="xref bibr" href="#r106"><span class="show-for-sr">Reference Rau and Cornwell</span>2011</a>) over the 288-MHz bandwidth to account for the spectral variation of each source. We use two terms in the Taylor expansion, resulting in two planes called TT0 and TT1. The TT0 plane is the zeroth-order term, corresponding to the total intensity of each pixel integrated over the full bandwidth. TT1 is the first-order term and allows the spectral indices at each pixel to be measured as <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline72.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline72.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha$ </span></span> </span> </span> = TT1/TT0.</p> <p class="p"> Primary beam correction is applied to each beam, and beams are combined using a weighted mean down to a cut-off of 20% of the peak (i.e. <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline73.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="154" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline73.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $LINMOSCUTOFF =0.2$ </span></span> </span> </span>) assuming a Gaussian primary beam shape. Future ASKAP surveys will use a beam shape based on holographic measurements, but that was not available for EMU-PS. Using the Gaussian beam approximation increases calibration errors and the rms noise level.</p> <p class="p"> Source extraction uses the ‘ <em class="italic">Selavy</em>’ software tool (Whiting & Humphreys <a class="xref bibr" href="#r124"><span class="show-for-sr">Reference Whiting and Humphreys</span>2012</a>; Whiting et al. <a class="xref bibr" href="#r125"><span class="show-for-sr">Reference Whiting, Voronkov and Mitchell</span>2017</a>) which identifies ‘islands’ of emission higher than three times the local rms in the image, using a flood-fill technique, and then fits Gaussian components to peaks of emission within the islands. Only components and islands greater than five times the local rms are retained.</p> <p class="p"> In the EMU initial public data release (defined in <a class="xref sec" href="#s5-1">Section 5.1</a>), spectral indices for individual components are measured as <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline74.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline74.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha$ </span></span> </span> </span> = TT1/TT0, where TT0 and TT1 are a weighted mean of the Taylor terms over the area of the component, down to a level of five times the local rms noise. However, this technique has been found to be unsatisfactory, so the spectral indices in the initial public data release should be regarded as unreliable. Our alternative technique is discussed below in <a class="xref sec" href="#s4-4">Section 4.4</a> </p> <p class="p"> As a final step within the pipeline, the data from each scheduling block are uploaded to the data archive (but not yet released) and passed through the ASKAP continuum validation package<a class="xref fn" href="#fn1"><span class="show-for-sr">Footnote </span>a</a> using default parameters. This package takes the final image, noise map, and <em class="italic">Selavy</em> catalogue as input and produces metrics and data quality flags based on a number of validation tests<a class="xref fn" href="#fn2"><span class="show-for-sr">Footnote </span>b</a>. The following metrics are used for each of these tests using ASKAP data only: </p><ul class="list nomark"> <li class="list-item"> <p class="p"> Fraction of sources considered resolved, given by the difference in the integrated (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline75.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="20" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline75.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\rm int}$ </span></span> </span> </span>) and peak (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline76.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="28" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline76.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\rm peak}$ </span></span> </span> </span>) flux densities, and local noise <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline77.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline77.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sigma$ </span></span> </span> </span>. We consider a source to be resolved when (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline78.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="237" height="29" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline78.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\rm int} - S_{\rm peak}) / \sqrt{dS_{\rm int}^2 + dS_{\rm peak}^2 + \sigma^2} > 3$ </span></span> </span> </span>, where <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline79.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="28" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline79.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $dS_{\rm int}$ </span></span> </span> </span> and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline80.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="36" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline80.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $dS_{\rm peak}$ </span></span> </span> </span> are the estimated measurement errors in <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline81.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="20" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline81.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\rm int}$ </span></span> </span> </span> and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline82.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="28" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline82.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\rm peak}$ </span></span> </span> </span> </p> </li> <li class="list-item"> <p class="p"> Reduced <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline83.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="16" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline83.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\chi^2$ </span></span> </span> </span> of differential Euclidean source counts</p> </li> <li class="list-item"> <p class="p"> Median RMS value (from <em class="italic">Selavy</em> noise map)</p> </li> <li class="list-item"> <p class="p"> Median in-band spectral index (from <em class="italic">Selavy</em> catalogue, measured from Taylor term images)</p> </li> </ul> <section><div class="fig" data-magellan-destination="f8" id="f8"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig8.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="2298" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig8.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 8.</span> An example validation report for one of the processing runs for SB9325, including the metrics and their flags. A higher-resolution version is available online2.</p> </div></div></section> <p class="p"> The following additional metrics are used with respect to selected point sources, cross-matched to the reference catalogue that provided the most matches, which for the pilot, is SUMSS (Mauch et al. <a class="xref bibr" href="#r78"><span class="show-for-sr">Reference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler</span>2003</a>), which has a resolution of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline84.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline84.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>45 arcsec at an observing frequency of 843 MHz: </p><ul class="list nomark"> <li class="list-item"> <p class="p"> Median absolute deviation (MAD) of the ratio of the flux density of the reference catalogue to the ASKAP flux density, after correcting for the frequency difference assuming <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline85.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="59" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline85.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha = -0.8$ </span></span> </span> </span>,</p> </li> <li class="list-item"> <p class="p"> Flux density ratio uncertainty, calculated from the MAD</p> </li> <li class="list-item"> <p class="p"> Positional offset, given by the median compared to reference catalogue</p> </li> <li class="list-item"> <p class="p"> Positional offset uncertainty, calculated from the MAD</p> </li> </ul> <p class="p"> An example report<a class="xref fn" href="#fn3"><span class="show-for-sr">Footnote </span>c</a> for one of the processing runs for SB9325 is shown in <a class="xref fig" href="#f8">Figure 8</a>, including a summary of the metrics and their flags. Each metric is flagged as good, bad, or uncertain based on selected tolerance values<a class="xref fn" href="#fn4"><span class="show-for-sr">Footnote </span>d</a>. The metrics and flags are associated and archived with the data, and the validation reports are automatically uploaded as a report under project AS101<a class="xref fn" href="#fn5"><span class="show-for-sr">Footnote </span>e</a>. </p> <p class="p"> The final validation process is done by members of the EMU team and includes </p><ul class="list nomark"> <li class="list-item"> <p class="p"> inspecting each of the validation reports described above,</p> </li> <li class="list-item"> <p class="p"> inspecting the images to search for artefacts,</p> </li> <li class="list-item"> <p class="p"> examining quantities such as the variation of restoring beam among the 36 beams used in the mosaic.</p> </li> </ul> <p class="p"> Data deemed to be acceptable are then released to the public domain on the data archive, described in <a class="xref sec" href="#s5-1">Section 5.1</a>. If the data are not found to be acceptable, then the data are removed from the archive and we request a re-observation.</p> </div> <div class="sec other" data-magellan-destination="s4" id="s4"> <h2 class="A"><span class="label">4.</span> Value-added processing</h2> <p class="p"> To mitigate some of the data issues in the initial public data release and to produce a unified image and source catalogue covering the full EMU-PS field, we conduct value-added processing on the initial public data release to generate a value-added data release. This value-added processing also includes some optical and infrared ancillary data, as described below.</p> <div class="sec" data-magellan-destination="s4-1" id="s4-1"> <h3 class="B"><span class="label">4.1.</span> Merging tiles</h3> <p class="p"> The initial public release of the survey data consists of 10 overlapping tiles, each with its own source catalogue. Simply merging these catalogues generates a large number of duplicate sources, which must be reconciled to maximise the information integrity and consistency. This approach also fails to take full advantage of the additional information, such as increased sensitivity, available where tiles overlap.</p> <p class="p"> To overcome these issues, we merged the 10 tiles in the image plane using the ASKAPsoft task <em class="italic">linmos</em>, which performs a weighted average of the data in overlapping regions. The merged data set is shown in <a class="xref fig" href="#f9">Figure 9</a>. We refer to this image, which has a typical spatial resolution of 11–13 arcsec, as the ‘native resolution image’.</p> <p class="p"> </p><section><div class="fig" data-magellan-destination="f9" id="f9"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig9.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1088" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig9.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 9.</span> The resulting native resolution (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline86.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="61" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline86.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $13'' \times 11''$ </span></span> </span> </span>) image of the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline87.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="53" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline87.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $270 \,\mathrm{deg}^2$ </span></span> </span> </span> EMU Pilot Survey, containing about 220 000 radio sources. The rms noise level is 25–30 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline88.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline88.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>, and the peak flux density is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline89.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="90" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline89.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $3.14 \mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section> </div> <div class="sec" data-magellan-destination="s4-2" id="s4-2"> <h3 class="B"><span class="label">4.2.</span> Convolution to a common restoring beam size</h3> <p class="p"> A problem with the native resolution image is that the point spread function (psf) varies from beam to beam over the field, so that both the flux density scale and also the spectral indices vary from beam to beam. To overcome this problem, we created a version of the data in which each PAF beam is individually convolved with a Gaussian kernel to obtain a common circular restoring beam of 18 arcsec FWHM. We then recombined all beams into a weighted average using the ASKAPsoft task <em class="italic">linmos</em>. We refer to this data set as the ‘convolved image’.</p> <p class="p"> We then ran the <em class="italic">Selavy</em> source finder on the convolved image, to produce a catalogue of components and islands. This convolved catalogue has 220 102 components. These ‘convolved’ data are recommended over the ‘native’ data product for the measurements of flux density and spectral index. However, the data products in native resolution are still optimum for studies of morphology, or when the higher resolution is needed.</p> </div> <div class="sec" data-magellan-destination="s4-3" id="s4-3"> <h3 class="B"><span class="label">4.3.</span> Separation of sources into simple and complex</h3> <p class="p"> Many value-added operations, such as measuring spectral index, and cross-identifying to optical/IR catalogues, are far more complex for extended or complex sources than for simple, compact sources. These techniques are still under development for the full EMU survey.</p> <p class="p"> We therefore divided the source catalogue into ‘simple’ and ‘complex’ sources. A sophisticated technique for this separation is still under development, so for the purposes of this paper we used a simple technique in which we defined islands with only one component (specifically, with <em class="italic">has_siblings</em> <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline90.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline90.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>$ </span></span> </span> </span> <em class="italic">0)</em> to be simple, and all other islands are defined to be ‘complex’. This technique results in a catalogue of 178 921 components, so that about 81% of sources in the catalogue are ‘simple’.</p> <p class="p"> Many ‘complex’ sources are classical FRI or FR II sources (Fanaroff & Riley <a class="xref bibr" href="#r37"><span class="show-for-sr">Reference Fanaroff and Riley</span>1974</a>), but our high sensitivity to low surface brightness has also enabled the detection of several peculiar-looking sources that are quite unlike those seen in earlier surveys such as NVSS (Condon et al. <a class="xref bibr" href="#r25"><span class="show-for-sr">Reference Condon, Cotton, Greisen, Yin, Perley, Taylor and Broderick</span>1998</a>) or FIRST (White et al. <a class="xref bibr" href="#r120"><span class="show-for-sr">Reference White, Becker, Helfand and Gregg</span>1997</a>). In <a class="xref sec" href="#s6">Section 6</a>, we discuss a small sample of these peculiar objects, which will be further explored in subsequent papers.</p> <p class="p"> We expect about half of the ‘simple’ sources to be star-forming galaxies (SFGs), with the remaining half to be AGN. It is this simple sample for which we obtain multiwavelength data in this paper.The rest of the value-added processing described here is concerned only with this simple catalogue, and the value-added processing of the complex sources will be described in a future paper (Marvil et al., in preparation).</p> <p class="p"> In <a class="xref table" href="#tbl6">Table 6</a>, we list the numbers of sources remaining at each stage of the value-added processing.</p> </div> <div class="sec" data-magellan-destination="s4-4" id="s4-4"> <h3 class="B"><span class="label">4.4.</span> Spectral indices</h3> <p class="p"> Spectral indices of the simple sources are measured over the 288-MHz bandwidth of ASKAP using the Taylor term technique described above. We measure spectral indices by calculating them from the Taylor terms at the peak pixel of each component, in the convolved data set. Note, as discussed above, that this procedure differs from that in the initial public data release, which we consider to be unreliable.</p><div class="table-wrap" data-magellan-destination="tbl6" id="tbl6"> <div class="caption"> <p class="p"><span class="label">Table 6.</span> Numbers of sources remaining after each stage of the value-added processing.</p> </div> <span> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab6.png?pub-status=live" class="aop-lazy-load-image" width="416" height="199" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab6.png" data-zoomable="false"></div> </span> <div class="table-wrap-foot"> <p class="p"> Asterisked rows are shown for information but are not used in the subsequent selection step. Photometric redshifts are taken from Zou et al. (<a class="xref bibr" href="#r131"><span class="show-for-sr">Reference Zou, Gao, Zhou and Kong</span>2019</a>), Zou et al. (<a class="xref bibr" href="#r132"><span class="show-for-sr">Reference Zou, Gao, Zhou and Kong</span>2020</a>), and Bilicki et al. (<a class="xref bibr" href="#r8"><span class="show-for-sr">Reference Bilicki</span>2016</a>).</p> </div> </div> <p class="p"> We also explored using the third Taylor term, which would measure spectral curvature, but found that very few sources had a measurable spectral curvature in the 288-MHz bandwidth of these observations. More importantly, we found that introducing a third Taylor term increased the uncertainty in the first two Taylor terms without increasing the accuracy, presumably because we are introducing a third free parameter which is primarily driven by noise.</p> <p class="p"> The distribution of the resulting spectral indices as a function of flux density is shown in <a class="xref fig" href="#f10">Figure 10</a>. Based on the noise measured in the TT1 image, the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline91.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="16" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline91.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $1\sigma$ </span></span> </span> </span> spectral index uncertainty of a source with flux density <em class="italic">S</em> mJy is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline92.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="42" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline92.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $0.25 / S$ </span></span> </span> </span>. The spectral index of a 2.5-mJy source, therefore, has a standard error of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline93.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline93.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>0.1, and spectral indices of sources weaker than this will be increasingly uncertain.</p> <p class="p"> </p><section><div class="fig" data-magellan-destination="f10" id="f10"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig10.png?pub-status=live" class="aop-lazy-load-image" width="1833" height="1462" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig10.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 10.</span> The measured spectral index as a function of flux density. The two solid lines show the 3<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline94.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline94.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sigma$ </span></span> </span> </span> uncertainty for a source of spectral index -0.8. Note the excess of sources with a positive spectral index, discussed in <a class="xref sec" href="#s6-13">Section 6.9</a>.</p> </div></div></section> <p class="p"> A histogram of the spectral indices for the 10458 sources with flux density <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline95.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline95.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>$ </span></span> </span> </span> 2.5 mJy is shown in <a class="xref fig" href="#f11">Figure 11</a>. The peak is at a spectral index of –0.7, as expected for surveys of mJy radio sources, with a tail of steeper spectrum sources extending to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline96.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="59" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline96.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha < -1.3$ </span></span> </span> </span>. Such ‘ultra-steep spectrum sources’ are well known in the literature (e.g. Afonso et al. <a class="xref bibr" href="#r2"><span class="show-for-sr">Reference Afonso</span>2011</a>) and can be an indicator of high redshift sources. There is also an unexpected tail of sources with positive spectral indices. Such sources are also well known (e.g. Healey et al. <a class="xref bibr" href="#r48"><span class="show-for-sr">Reference Healey, Romani, Taylor, Sadler, Ricci, Murphy, Ulvestad and Winn</span>2007</a>) but are relatively rare. Here, however, they appear to constitute a significant fraction of EMU-PS sources. This is discussed further in <a class="xref sec" href="#s6-13">Section 6.9</a>. </p><section><div class="fig" data-magellan-destination="f11" id="f11"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig11.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1011" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig11.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 11.</span> A histogram of measured spectral index as a function of flux density, for the 10458 sources with flux density <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline97.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline97.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>$ </span></span> </span> </span> 2.5 mJy.</p> </div></div></section> <section><div class="fig" data-magellan-destination="f12" id="f12"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig12.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1126" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig12.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 12.</span> The fraction of simple radio sources (as listed in <a class="xref table" href="#tbl6">Table 6</a>) matched with a CWISE source as a function of separation, both for unshifted data and for data shifted by one arcmin.</p> </div></div></section> </div> <div class="sec" data-magellan-destination="s4-5" id="s4-5"> <h3 class="B"><span class="label">4.5.</span> Multi-wavelength cross-identifications and redshifts</h3> <p class="p"> For cross-identifying simple sources, we use a simple nearest-neighbour cross-identification algorithm and show below that this gives an acceptable completeness and false-ID rate. Norris et al. (<a class="xref bibr" href="#r93"><span class="show-for-sr">Reference Norris</span>2006</a>) found that cross-matching with 3.6-<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline98.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="11" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline98.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu$ </span></span> </span> </span>m <em class="italic">Spitzer</em> infrared data and then cross-matching the infrared with optical gave a lower false-ID rate than matching radio with optical directly. We therefore adopt this procedure here, and first match the radio against the W1 band (3.4 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline99.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="11" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline99.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu$ </span></span> </span> </span>m) of the CATWISE2020 catalogue (Marocco et al. <a class="xref bibr" href="#r76"><span class="show-for-sr">Reference Marocco</span>2021</a>), hereafter referred to as ‘CWISE’, and then cross-match the CWISE positions against the DES DR1 optical catalogue (Abbott et al. <a class="xref bibr" href="#r1"><span class="show-for-sr">Reference Abbott</span>2018</a>).</p> <p class="p"> We measured the number of cross-matches between the radio and the infrared as a function of separation, and then estimated the false-ID rate by shifting the radio positions by 1 arcmin and then repeating the cross-match. The result is shown in <a class="xref fig" href="#f12">Figure 12</a>. The choice of an optimum search radius depends on the application (i.e., whether the goal depends on maximising the number of cross-matches or minimising the number of false-IDs). In producing the cross-matched catalogue, we include all cross-matches up to a search radius of 10 arcsec so that users can choose their optimum search radius, but for further work herein we limit our analysis to a maximum search radius of 3 arcsec, at which we find an 8% false-ID rate and a 75% total cross-match rate (which includes the false-IDs). The resulting numbers of sources are listed in <a class="xref table" href="#tbl6">Table 6</a>. </p> <p class="p"> Because of the high numbers of faint CWISE sources, we also explored the effect of introducing a cut-off in the CWISE flux densities, so only the brighter sources would be cross-matched to radio sources, but found that had a negligible effect on the false-ID rate, while significantly reducing the number of true IDs, and so no cut-off is used.</p> <p class="p"> To cross-match the CWISE IR positions against DES optical positions, we again explored the false-ID rate and the total-ID rate as a function of search radius, and show the results in <a class="xref fig" href="#f13">Figure 13</a>. As a result, we adopt a search radius of 2 arcsec. The resulting numbers of sources are listed in <a class="xref table" href="#tbl6">Table 6</a>. </p><section><div class="fig" data-magellan-destination="f13" id="f13"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig13.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1134" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig13.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 13.</span> The fraction of radio sources with a CWISE position matched with a DES DR1 source as a function of separation, both for unshifted data and for data shifted by one arcmin.</p> </div></div></section> <p class="p"> There is no major spectroscopic redshift survey covering the EMU-PS field, but a large number of photometric redshifts are available from Bilicki et al. (<a class="xref bibr" href="#r8"><span class="show-for-sr">Reference Bilicki</span>2016</a>) (using their ‘main’ catalogue), and from Zou et al. (<a class="xref bibr" href="#r131"><span class="show-for-sr">Reference Zou, Gao, Zhou and Kong</span>2019</a>; <a class="xref bibr" href="#r132"><span class="show-for-sr">Reference Zou, Gao, Zhou and Kong</span>2020</a>), and we also include those in the catalogue. Throughout the rest of this paper, redshifts given without a citation refer to these redshifts used in the EMU-PS catalogue.</p> </div> <div class="sec" data-magellan-destination="s4-6" id="s4-6"> <h3 class="B"><span class="label">4.6.</span> Astrometric precision</h3> <p class="p"> For each source that was cross-matched with a CWISE catalogue source, we measured the offset in position, as a check on the precision of the positions of the radio components. The result is shown in <a class="xref fig" href="#f14">Figure 14</a>, showing a mean offset of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline100.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline100.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>0.3 arcsec, which is small compared to the 18 arcsec resolution of the convolved data. The positions in the catalogue have not been corrected for this insignificant offset. </p><section><div class="fig" data-magellan-destination="f14" id="f14"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig14.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1467" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig14.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 14.</span> A plot showing the difference in position of radio sources compared to the matching CWISE source in the W1 band, showing a mean offset of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline101.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline101.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>0.3 arcsec, which is small compared to the 18 arcsec resolution of the convolved data. The horizontal axis is Right Ascension and the vertical axis is Declination.</p> </div></div></section> <section><div class="fig" data-magellan-destination="f15" id="f15"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig15.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1083" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig15.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 15.</span> The ratio of peak flux densities between EMU-PS and SUMSS for simple sources with EMU-PS flux densities <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline102.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline102.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>$ </span></span> </span> </span> 6 mJy, and with catalogued positions within 3 arcsec.</p> </div></div></section> </div> <div class="sec" data-magellan-destination="s4-7" id="s4-7"> <h3 class="B"><span class="label">4.7.</span> Flux density accuracy</h3> <p class="p"> To estimate the flux density accuracy, we select EMU-PS sources stronger than 6 mJy (the minimum flux density for sources in the SUMSS (Mauch et al. <a class="xref bibr" href="#r78"><span class="show-for-sr">Reference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler</span>2003</a>) catalogue) and cross-match them to SUMSS sources using a 3-arcsec search radius, which selects about 50% of the SUMSS sources, and tends to exclude the very extended SUMSS sources. We then calculate the ratio of peak fluxes in the EMU-PS and SUMMS catalogues. The result is shown in <a class="xref fig" href="#f15">Figure 15</a>. </p><section><div class="fig" data-magellan-destination="f16" id="f16"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig16.png?pub-status=live" class="aop-lazy-load-image" width="2400" height="1359" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig16.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 16.</span> A typical section of the survey field, covering about <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline103.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="49" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline103.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $0.3 \,\mathrm{deg}^2$ </span></span> </span> </span> (or about one thousandth of the area of the EMU Pilot Survey) which contains about 250 radio sources). On the left is the SUMSS image (Mauch et al. <a class="xref bibr" href="#r78"><span class="show-for-sr">Reference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler</span>2003</a>) and on the right is the EMU-PS image. Prominent in this image is the Giant Radio Galaxy ESO 234-68. The maximum flux density of ESO 234-68 in the EMU-PS image is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline104.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="103" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline104.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $58.8 \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>, and that of the strong source at the bottom of the image (PMN J2045-5135) is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline105.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="86" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline105.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $1.06 \mathrm{Jy beam}^{-1}$ </span></span> </span> </span>. The rms of the EMU-PS image is 25–30 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline106.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline106.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>, and that of the SUMSS image is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline107.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="119" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline107.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}1.25\ \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section> <p class="p"> Ideally, we would convolve the EMU-PS to the 45-arcsec resolution of SUMSS and then repeat the source extraction, but then it would not be matched to the EMU-PS value-added catalogue. Because we have not done this convolution, some SUMSS peak flux densities are boosted by components which are included in the SUMSS beam but not in the EMU-PS beam. This increases the scatter of the ratios so that the measured scatter in the ratio is an overestimate of the uncertainty in the EMU-PS flux density scale.</p> <p class="p"> We note the following features of <a class="xref fig" href="#f15">Figure 15</a>. </p><ul class="list nomark"> <li class="list-item"> <p class="p"> The EMU-PS central frequency of 944-MHz differs from the SUMSS central frequency of 843 MHz, and, assuming a spectral index of –0.8, we expect the peak of the distribution to occur at a ratio of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline108.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="135" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline108.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}(944/843)^{0.8} = 1.09 $ </span></span> </span> </span> as observed.</p> </li> <li class="list-item"> <p class="p"> The histogram is more extended on the right, presumably because of the larger size of the SUMSS beam which will boost the SUMSS peak flux as discussed above.</p> </li> <li class="list-item"> <p class="p"> The left of the histogram is approximately Gaussian with a standard deviation of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline109.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline109.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>0.12.</p> </li> </ul> <p class="p"> We therefore estimate our flux density scale uncertainty for strong sources to have a maximum value of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline110.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="25" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline110.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sigma \sim$ </span></span> </span> </span>12%. To this should be added in quadrature the estimated flux density scale standard error for SUMSS of 3% (Mauch et al. <a class="xref bibr" href="#r78"><span class="show-for-sr">Reference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler</span>2003</a>).</p> <p class="p"> The measured flux density of weaker sources will be degraded by a factor of 1/SNR, where SNR is the local signal-to-noise ratio. As we have rejected sources from the EMU-PS catalogue with SNR<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline111.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline111.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $<$ </span></span> </span> </span>5, this may add an uncertainty of up to 20% (to be added in quadrature) to the quoted flux densities of weak sources.</p> </div> </div> <div class="sec results" data-magellan-destination="s5" id="s5"> <h2 class="A"><span class="label">5.</span> Results</h2> <div class="sec" data-magellan-destination="s5-1" id="s5-1"> <h3 class="B"><span class="label">5.1.</span> Data summary and access</h3> <p class="p"> The EMU-PS has produced an image of about <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline112.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="53" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline112.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $270 \,\mathrm{deg}^2$ </span></span> </span> </span> of the radio sky at 944 MHz, with a spatial resolution of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline113.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline113.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>11–13 arcsec and an rms sensitivity of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline114.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline114.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>25–30 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline115.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="75" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline115.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>.</p> <p class="p"> A problem with large surveys is that it is difficult to convey the scale and depth of the image in a journal paper. <a class="xref fig" href="#f9">Figure 9</a> shows the entire native resolution image, and <a class="xref fig" href="#f16">Figure 16</a> shows a random section of it, which covers about one thousandth of the area of the EMU-PS. An interactive interface to the image of the entire survey field in HiPS format is available on <a class="uri" href="http://emu-survey.org">http://emu-survey.org</a>.</p> <p class="p"> After observing, processing, and validation by the EMU survey team, the data from each observation are placed on the CSIRO ASKAP Science Data Archive (CASDA) data server and made available to the public as described below. These data consist of all the data from each day’s observations, known as a ‘tile’, including images and tables of extracted components and islands. We call this catalogue the EMU Pilot Initial Public Data Release. The validation metrics and flags are associated with each tile and are fully queryable via table access protocol (TAP).</p> <p class="p"> The data are then processed by merging tiles into a common image covering the whole field of the EMU-PS. The resulting data release of this image is called the ‘native’ value-added data release.</p> <p class="p"> As described in <a class="xref sec" href="#s4">Section 4</a>, we then smooth the native resolution image to a constant resolution of 18 arcsec, perform source extraction, and separate the resulting catalogue of 220 102 components into simple, single, components (81%), and more complex sources (19%). We also perform cross-identifications of the simple sources with other available multiwavelength products.</p> <p class="p"> We call this science-ready data set the ‘Convolved’ data set. The resulting image for an area of sky covering an object of interest is shown in <a class="xref fig" href="#f17">Figure 17</a>, which shows the three data products: the initial public data release, the added-value ‘native’ data release with 11–13 arcsec resolution, and the added-value ‘convolved’ data release with 18 arcsec resolution. </p><section><div class="fig" data-magellan-destination="f17" id="f17"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig17.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="3680" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig17.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 17.</span> A sample of the final image, showing the three data products on a region, covered by three tiles, containing two of the ‘Odd Radio Circles’(Norris et al. <a class="xref bibr" href="#r95"><span class="show-for-sr">Reference Norris</span>2021</a>): (a) the initial public data release from a single tile (SB9351) (resolution 11 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline116.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline116.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\times$ </span></span> </span> </span> 13 arcsec, rms = <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline117.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="93" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline117.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $40 \,\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>, (b) the added-value ‘native’ data release with 11<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline118.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline118.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\times$ </span></span> </span> </span>13 arcsec resolution, from the merged tiles, rms = 25 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline119.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="75" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline119.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>, and (c) the added-value ‘convolved’ data release with 18 arcsec resolution, rms = 25 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline120.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline120.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>. The peak flux density in this image is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline121.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="99" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline121.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $4.6\ \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section> <p class="p"> All three data products from the EMU-PS (the initial public data release, the added-value ‘native’ data release with 11–13 arcsec resolution, and the added-value ‘convolved’ data release with 18 arcsec resolution) are released via the CASDA data server described below. The initial public data release is currently available in the public domain, but the two added-value data releases are available only to EMU members for a proprietary period of 1 year from the date of publication of this paper, after which they will be released into the public domain. However, EMU is an open collaboration, and other astronomers are welcome to join the project, and access the proprietary data, provided they agree to the EMU data and publication policies.</p> <p class="p"> The EMU-PS initial public release data in the CASDA are open to the public domain. To download data from CASDA, users need to obtain a CASS Online Proposal Applications and Links (OPAL) account<a class="xref fn" href="#fn6"><span class="show-for-sr">Footnote </span>f</a>.</p> <p class="p"> CASDA is described in detail by Chapman et al. (<a class="xref bibr" href="#r23"><span class="show-for-sr">Reference Chapman, Dempsey, Miller, Heywood, Pritchard, Sangster, Whiting, Dart, Lorente, Shortridge and Wayth</span>2017</a>) and Huynh et al. (<a class="xref bibr" href="#r55"><span class="show-for-sr">Reference Huynh, Dempsey, Whiting, Ophel, Ballester, Ibsen, Solar and Shortridge</span>2020</a>). In brief, CASDA is implemented across two data centres, the Pawsey Supercomputing Centre in Perth and the CSIRO data centre in Canberra. So-called ‘backend’ functions such as deposit, storage, and data access are implemented at Pawsey, while the ‘frontend’ functions such as the user interface and authentication are implemented at the CSIRO data centre.</p> <p class="p"> The simplest way to access the data is via the CASDA web user interface. From the CASDA webpage<a class="xref fn" href="#fn7"><span class="show-for-sr">Footnote </span>g</a>, select ‘Access CASDA via the Data Access Portal’, to be taken to the Observation Search user interface. EMU-PS data can be obtained by searching for ‘Released’ data under project code AS101. EMU-PS data have Digital Object Identifiers (DOIs) which provide a persistent resolvable link to the data. <a class="xref table" href="#tbl7">Table 7</a> gives the DOI for each data product discussed in this paper. The DOI links to the collection page; from there click on ‘files’ and select the files to download. </p> <p class="p"> CASDA also implements several Virtual Observatory services to maximise the usability and interoperability of ASKAP data products and allow for automated scripted access. For example, the TAP can be used to search for EMU-PS observations under project code AS101, using an application such as TOPCAT (Taylor <a class="xref bibr" href="#r116"><span class="show-for-sr">Reference Taylor, Shopbell, Britton and Ebert</span>2005</a>) or Aladin (Boch & Fernique <a class="xref bibr" href="#r9"><span class="show-for-sr">Reference Boch, Fernique, Manset and Forshay</span>2014</a>; Bonnarel et al. <a class="xref bibr" href="#r14"><span class="show-for-sr">Reference Bonnarel</span>2000</a>). A CASDA module has recently been added to the Python astropy astroquery<a class="xref fn" href="#fn8"><span class="show-for-sr">Footnote </span>h</a> package. Using this Python API, the EMU-PS images can be accessed and downloaded with a cone search of the EMU-PS pointings.</p> <p class="p"> All public data (tables and images, and <em class="italic">u</em>,<em class="italic">v</em> data) are available from CASDA (see <a class="xref table" href="#tbl7">Table 7</a>) and a listing of all ASKAP observations is on the Observation Management Portal (OMP)<a class="xref fn" href="#fn9"><span class="show-for-sr">Footnote </span>i</a>. OMP allows the user to select observations by several parameters including date, SBID (listed in <a class="xref table" href="#tbl3">Table 3</a>), or project name (AS101 for EMU).</p> </div> <div class="sec" data-magellan-destination="s5-2" id="s5-2"> <h3 class="B"><span class="label">5.2.</span> Sensitivity to compact sources</h3> <p class="p"> The EMU-PS survey reaches a typical sensitivity of 25–30 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline122.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline122.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> rms. This is about a factor of two above the calculated thermal noise sensitivity (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline123.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline123.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>13 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline124.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline124.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>), which we tentatively attribute to the following causes. </p><ul class="list nomark"> <li class="list-item"> <p class="p"> Timing errors in the correlator cause a significant fraction of data (30–50%) to be flagged, resulting in a loss of data. Work is in progress to identify and eliminate the cause of this problem.</p> </li> <li class="list-item"> <p class="p"> The data calibration processes are in a preliminary state. By the time of the final EMU survey, we expect to have developed a sky model which will be used to calibrate the data and remove strong sources prior to cleaning.</p> </li> <li class="list-item"> <p class="p"> A dynamic range problem, which is currently being addressed, causes diffraction patterns around strong sources.</p><div class="table-wrap" data-magellan-destination="tbl7" id="tbl7"> <div class="caption"> <p class="p"><span class="label">Table 7.</span> Available data products, including Digital Object Identifiers (DOIs) that can be used to access the data described in this paper.</p> </div> <span> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab7.png?pub-status=live" class="aop-lazy-load-image" width="499" height="155" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab7.png" data-zoomable="false"></div> </span> <div class="table-wrap-foot"> <p class="p"> Notes:</p> <p class="p"> •The initial public data release is immediately available, but the value-added releases are available only to members of the EMU collaboration for 1 year from the data of publication of this paper, after which they become public.</p> <p class="p"> •All catalogues contain island and component information, and, for the added-value catalogue, cross-identifications and redshifts, where available.</p> <p class="p"> •TT0 and TT1 refer to Taylor Term 0 image (total power) and Taylor Term 1 image (TT0 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline125.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline125.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\times$ </span></span> </span> </span> spectral index)</p> </div> </div> <section><div class="fig" data-magellan-destination="f18" id="f18"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig18.png?pub-status=live" class="aop-lazy-load-image" width="3000" height="1067" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig18.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 18.</span> The sensitivity of EMU-PS as a function of spatial scale. The plot was made using visibility data from a single beam and pointing of an interleaved observation (2-h observation, 288-MHz bandwidth, scaled to the EMU-PS observing frequency of 944 MHz) which was filled with Gaussian noise and various uv tapers were applied to shape the beam size. We then measured the image noise (effectively the sensitivity at the scale associated with the uv taper). The two plots show the same result over different ranges of spatial scale.</p> </div></div></section> </li> <li class="list-item"> <p class="p"> The primary beam correction assumes a Gaussian profile across each PAF beam. This is being replaced by a profile based on holographic measurements which will be beam-specific.</p> </li> <li class="list-item"> <p class="p"> The lack of direction-dependent calibration, which we hope to address in the future.</p> </li> </ul> <p class="p"> After correcting these errors, and including a confusion noise of about 9 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline126.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline126.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>, we expect the full EMU survey (conducted at a centre frequency of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline127.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline127.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>944 MHz) can potentially reach an rms of about 17.5 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline128.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline128.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div> <div class="sec" data-magellan-destination="s5-3" id="s5-3"> <h3 class="B"><span class="label">5.3.</span> Sensitivity to extended emission</h3> <p class="p"> As well as its high sensitivity to compact sources, the survey also has high sensitivity to extended low surface brightness emission, because of the large number of short spacings in the ASKAP array.</p> <p class="p"> In <a class="xref fig" href="#f18">Figure 18</a>, we show a plot of the sensitivity of EMU-PS as a function of spatial scale, obtained by running simulated observations with different tapers, producing different beam sizes.</p> <p class="p"> The sensitivity of 25–30 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline129.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="75" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline129.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> at the native resolution of 11–13 arcsec is almost unchanged at the convolved resolution of 18 arcsec and continues at a similar level beyond the 45-arcsec resolution of SUMSS (Mauch et al. <a class="xref bibr" href="#r78"><span class="show-for-sr">Reference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler</span>2003</a>), which has a median rms sensitivity of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline130.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="102" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline130.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $1.27 \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>. The effect of this high sensitivity to low surface brightness emission is demonstrated in <a class="xref sec" href="#s6">Section 6</a>.</p> </div> <div class="sec" data-magellan-destination="s5-4" id="s5-4"> <h3 class="B"><span class="label">5.4.</span> Source counts and confusion</h3> <p class="p"> <a class="xref fig" href="#f19">Figure 19</a> shows the differential source counts normalised to a non-evolving Euclidean model (n <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline131.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline131.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\propto S^{2.5}$ </span></span> </span> </span>) obtained from the EMU-PS catalogue (black symbols), rescaled from 943.5 MHz to 1.4 GHz by assuming <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline132.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="60" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline132.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha=-0.7$ </span></span> </span> </span>. Two counts’ determinations are shown: one referring to the <em class="italic">island</em> catalogue, where components of complex sources are merged together (filled diamonds) and one referring to simple sources only (empty diamonds). The source counts are corrected for both Eddington bias (Eddington <a class="xref bibr" href="#r34"><span class="show-for-sr">Reference Eddington</span>1913</a>; Eddington <a class="xref bibr" href="#r35"><span class="show-for-sr">Reference Eddington</span>1940</a>) and resolution bias (i.e. the incompleteness introduced by the fact that a larger source of a given total flux density will drop below the signal-to-noise threshold of a survey more easily than a smaller source of the same total flux density). This is done following standard recipes in the literature (see e.g. Prandoni et al. 2001; <a class="xref bibr" href="#r103"><span class="show-for-sr">Reference Prandoni, Guglielmino, Morganti, Vaccari, Maini, Röttgering, Jarvis and Garrett</span>2018</a>; Mandal et al. <a class="xref bibr" href="#r75"><span class="show-for-sr">Reference Mandal</span>2021</a>).</p> <p class="p"> </p><section><div class="fig" data-magellan-destination="f19" id="f19"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig19.png?pub-status=live" class="aop-lazy-load-image" width="1190" height="864" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig19.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 19.</span> Normalised differential source counts derived from the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline133.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="54" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline133.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $270\ \mathrm{deg}^2$ </span></span> </span> </span> EMU-PS survey for the <em class="italic">island</em> catalogue (black filled diamonds) and for simple sources only (black empty diamonds). The counts have been rescaled from 943.5 MHz to 1.4 GHz by assuming <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline134.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="60" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline134.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha=-0.7$ </span></span> </span> </span>. Also shown for comparison are the counts derived from 1.4 GHz <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline135.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline135.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>$ </span></span> </span> </span> degree-scale surveys (symbols and colours as indicated in the figure). Vertical bars represent Poissonian errors on the normalised counts. Systematic errors due to incompleteness corrections and spectral index assumptions are approximately included in the size of the plotted symbols. The result of the <em class="italic">P</em>(<em class="italic">D</em>) analysis performed by (Vernstrom et al. <a class="xref bibr" href="#r119"><span class="show-for-sr">Reference Vernstrom</span>2014</a>, rescaled from 3 to 1.4 GHz by assuming <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline136.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline136.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha $ </span></span> </span> </span> = <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline137.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline137.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>0.7) is indicated in dark green. The black solid line represents the predicted counts from 200 sq. degr. of the S3-SEX simulations (Wilman et al. <a class="xref bibr" href="#r127"><span class="show-for-sr">Reference Wilman</span>2008</a>). The light blue and yellow shaded areas illustrate the predicted cosmic variance effects for survey coverages of 5 and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline138.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline138.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $10\ \mathrm{deg}^2$ </span></span> </span> </span>, respectively (obtained by splitting the S3-SEX simulation in 40 5-<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline139.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="28" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline139.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mathrm{deg}^2$ </span></span> </span> </span> and 20 10-<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline140.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="27" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline140.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mathrm{deg}^2$ </span></span> </span> </span> fields, respectively). The <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline141.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="46" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline141.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $25\ \mathrm{deg}^2$ </span></span> </span> </span> medium tier of the more recent T-RECS simulations (Bonaldi et al. <a class="xref bibr" href="#r12"><span class="show-for-sr">Reference Bonaldi, Bonato, Galluzzi, Harrison, Massardi, Kay, De Zotti and Brown</span>2019</a>) is represented by the purple shaded area. Finally, the Mancuso et al. (<a class="xref bibr" href="#r74"><span class="show-for-sr">Reference Mancuso</span>2017</a>) radio source evolutionary model is shown by the light green line.</p> </div></div></section> <p class="p"> <a class="xref fig" href="#f19">Figure 19</a> shows for comparison some of the widest-area samples available to date at 1.4 GHz. This includes sub-mJy surveys covering <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline142.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="53" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline142.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>1\ \mathrm{deg}^2$ </span></span> </span> </span> regions, like PDF (Hopkins et al. <a class="xref bibr" href="#r53"><span class="show-for-sr">Reference Hopkins, Afonso, Chan, Cram, Georgakakis and Mobasher</span>2003</a>), VLA-COSMOS (Bondi et al. <a class="xref bibr" href="#r13"><span class="show-for-sr">Reference Bondi, Ciliegi, Schinnerer, Smolčić, Jahnke, Carilli and Zamorani</span>2008</a>) and the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline143.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="39" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline143.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $6\ \mathrm{deg}^2$ </span></span> </span> </span> Westerbork mosaic covering the Lockman Hole region (LHW: Prandoni et al. <a class="xref bibr" href="#r103"><span class="show-for-sr">Reference Prandoni, Guglielmino, Morganti, Vaccari, Maini, Röttgering, Jarvis and Garrett</span>2018</a>), as well as shallower (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline144.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="21" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline144.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $> 1$ </span></span> </span> </span> mJy) but larger (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline145.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="15" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline145.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\gg$ </span></span> </span> </span>10 sq. degr.) surveys like ATESP (Prandoni et al. <a class="xref bibr" href="#r101"><span class="show-for-sr">Reference Prandoni, Gregorini, Parma, de Ruiter, Vettolani, Wieringa and Ekers</span>2001</a>), SDSS Stripe 82 (Heywood et al. <a class="xref bibr" href="#r52"><span class="show-for-sr">Reference Heywood</span>2016</a>) and FIRST (White et al. <a class="xref bibr" href="#r120"><span class="show-for-sr">Reference White, Becker, Helfand and Gregg</span>1997</a>). Also shown are simulated source counts derived by combining evolutionary models of either classical radio loud (RL) AGN or radio source populations dominating the sub-mJy radio sky, namely SFGs and low-luminosity AGN (LLAGN). In particular, we show the 1.4-GHz counts derived from the recent modelling of Mancuso et al. (<a class="xref bibr" href="#r74"><span class="show-for-sr">Reference Mancuso</span>2017</a>), light green solid line, the T-RECS <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline146.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="46" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline146.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $25\ \mathrm{deg}^2$ </span></span> </span> </span> medium tier simulation (Bonaldi et al. <a class="xref bibr" href="#r12"><span class="show-for-sr">Reference Bonaldi, Bonato, Galluzzi, Harrison, Massardi, Kay, De Zotti and Brown</span>2019</a>), as well as different realisations obtained from the S3-SEX simulated catalogue (Wilman et al. <a class="xref bibr" href="#r127"><span class="show-for-sr">Reference Wilman</span>2008</a>): <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline147.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="79" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline147.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $1\times 200\ \mathrm{deg}^2$ </span></span> </span> </span> (black solid line), <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline148.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="79" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline148.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $20\times 10\ \mathrm{deg}^2$ </span></span> </span> </span> regions (yellow shaded area) and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline149.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="72" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline149.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $40\times 5\ \mathrm{deg}^2$ </span></span> </span> </span> regions (light blue shaded area).</p> <p class="p"> <a class="xref fig" href="#f19">Figure 19</a> clearly shows that the source counts derived from the EMU-PS <em class="italic">island</em> catalogue nicely match previous counts and are in good agreement with the most recent models/simulations (Mancuso et al. <a class="xref bibr" href="#r74"><span class="show-for-sr">Reference Mancuso</span>2017</a>; Bonaldi et al. <a class="xref bibr" href="#r12"><span class="show-for-sr">Reference Bonaldi, Bonato, Galluzzi, Harrison, Massardi, Kay, De Zotti and Brown</span>2019</a>). Even more interestingly they provide very robust statistics all the way from <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline150.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="60" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline150.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}0.1\,\textrm{mJy}$ </span></span> </span> </span> to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline151.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="22" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline151.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>1$ </span></span> </span> </span> Jy, something which could only be achieved in the past by combining deeper (but smaller) surveys with larger (but shallower) surveys. Finally, it is interesting to note that the counts derived from simple sources only (black empty diamonds) fall well below the full counts (black filled diamonds) at bright fluxes. This is not surprising as we expect a large contribution from multi-component RL AGN at flux densities <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline152.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="25" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline152.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\gg 1$ </span></span> </span> </span> mJy. On the other hand, no significant difference is observed at sub-mJy fluxes, confirming that this flux regime is dominated by SFG and LLAGN.</p> <div class="sec" data-magellan-destination="s5-4-1" id="s5-4-1"> <h4 class="C"><span class="label">5.4.1.</span> Source Confusion</h4> <p class="p"> We estimate the source confusion noise, and instrumental noise using the probability of deflection, or <em class="italic">P</em>(<em class="italic">D</em>) technique (Scheuer <a class="xref bibr" href="#r112"><span class="show-for-sr">Reference Scheuer</span>1957</a>). The <em class="italic">P</em>(<em class="italic">D</em>) distribution of an image is the distribution of pixel intensities (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline153.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="64" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline153.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>) which depends on the underlying source count, shape of the beam, and the instrumental noise (see Vernstrom et al. <a class="xref bibr" href="#r119"><span class="show-for-sr">Reference Vernstrom</span>2014</a>, for a detailed description of the method).</p> <p class="p"> The <em class="italic">P</em>(<em class="italic">D</em>) method assumes a Gaussian distribution for the instrumental noise and can therefore be affected by imaging artefacts, such as those found around bright sources. We computed the histogram of pixel intensities for the pilot survey image by selecting regions of pixels devoid of any image artefacts, as well as any complex diffuse or extended emission. Rather than a full source count fitting analysis, which is beyond the scope of this paper, we take the deep <em class="italic">P</em>(<em class="italic">D</em>) source counts derived in Vernstrom et al. (<a class="xref bibr" href="#r119"><span class="show-for-sr">Reference Vernstrom</span>2014</a>) and scale it to a frequency of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline154.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="24" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline154.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $944\,$ </span></span> </span> </span>MHz using <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline155.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="60" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline155.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha =-0.7$ </span></span> </span> </span>. We take the average beam sizes from the individual beams and find <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline156.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="59" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline156.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $B_{\rm maj}=12\,$ </span></span> </span> </span> arcsec and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline157.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="61" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline157.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $B_{\rm min}=10\,$ </span></span> </span> </span> arcsec, while using an image of the ‘dirty’ synthesised beam for sources below the clean limit (approximated at <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline158.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="149" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline158.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\rm clean}=200\, \mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>). We use an average instrumental noise value of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline159.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="122" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline159.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sigma=23\, \mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>. The image <em class="italic">P</em>(<em class="italic">D</em>), noise distribution, and model <em class="italic">P</em>(<em class="italic">D</em>) can be seen in <a class="xref fig" href="#f20">Figure 20</a>.</p> <p class="p"> </p><section><div class="fig" data-magellan-destination="f20" id="f20"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig20.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1499" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig20.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 20.</span> The EMU-PS preliminary <em class="italic">P</em>(<em class="italic">D</em>) distributions. The solid black line is the probability distribution made from sections of the pilot away from bright sources. The upper right inset shows bright flux density tail of the <em class="italic">P</em>(<em class="italic">D</em>) distributions. The blue dot-dashed line shows a Gaussian noise distribution of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline160.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="118" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline160.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sigma= 23 \mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>. The red dashed line shows the predicted or model <em class="italic">P</em>(<em class="italic">D</em>) generated from the source count shown in the lower right inset.</p> </div></div></section> <p class="p"> Without any additional fitting or changes to the parameters or source count, we find very good agreement between the image and model <em class="italic">P</em>(<em class="italic">D</em>) distributions. The noise-free model <em class="italic">P</em>(<em class="italic">D</em>) provides an estimate of the confusion noise in the field of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline161.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="132" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline161.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sigma_{\rm conf}=5\, \mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>. This quick test shows through independent means that the instrumental noise estimate of 20 to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline162.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="92" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline162.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $25\, \mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> is accurate. Furthermore, the fact that the scaled source count model provides a good match to the image is a confirmation of accurate source flux densities in the pilot data, and that confusion noise is not a significant factor for our scientific investigations, even when considering the dirty beam sidelobe confusion noise. At the same time, the observations of P(D) are sensitive enough to probe far below the source populations that we can directly detect.</p> </div> </div> </div> <div class="sec other" data-magellan-destination="s6" id="s6"> <h2 class="A"><span class="label">6.</span> Preliminary science results</h2> <div class="sec" data-magellan-destination="s6-1" id="s6-1"> <h3 class="B"><span class="label">6.1.</span> Peculiar radio sources</h3> <p class="p"> Many unusual radio sources are found in the EMU-PS.</p> <p class="p"> The source PKS 2130-538, shown in <a class="xref fig" href="#f21">Figure 21</a>, has been previously identified as a complex source (e.g. Ekers <a class="xref bibr" href="#r36"><span class="show-for-sr">Reference Ekers</span>1970</a>; Schilizzi & McAdam <a class="xref bibr" href="#r113"><span class="show-for-sr">Reference Schilizzi and McAdam</span>1975</a>; Jones & McAdam <a class="xref bibr" href="#r62"><span class="show-for-sr">Reference Jones and McAdam</span>1992</a>), and as two radio galaxies (G4Jy 1704 and G4Jy 1705) in the G4Jy Sample (White et al. <a class="xref bibr" href="#r122"><span class="show-for-sr">Reference White</span>2020</a>b; White et al. <a class="xref bibr" href="#r121"><span class="show-for-sr">Reference White</span>2020</a>a). However, no previous image shows the wealth of detail and low surface brightness emission seen in <a class="xref fig" href="#f21">Figure 21</a>. It consists of the radio lobes of two host galaxies, one of which (‘Host 1’: 2MASX J21341775-5338101) is the bright galaxy at the centre of the curved northern radio bridge, at a redshift of 0.0781. This is the brightest galaxy of the cluster Abell 3785. The other host galaxy (‘Host 2’: 2MASX J21340666-5334186) is the bright galaxy near the southeast end, at a redshift of 0.0763. </p><section><div class="fig" data-magellan-destination="f21" id="f21"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig21.png?pub-status=live" class="aop-lazy-load-image" width="3666" height="1395" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig21.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 21.</span> A peculiar radio source found in the EMU Pilot Survey, consisting of a group of distorted radio components, collectively known as PKS 2130–538, and nicknamed ‘the dancing ghosts’. The two host galaxies (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline163.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="61" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline163.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z \sim 0.077$ </span></span> </span> </span>) are seen at the centre of the narrow jets (shown with numbers in the figure to indicate their putative host) which expand into diffuse lobes, probably bent by interactions. On the left is the total intensity greyscale image (shown in turquoise), superimposed on a background of the DES optical image, assembled from the r, g, and i images. On the right is the total intensity image of PKS 2130-538, colour-coded by spectral index. The unconventional colour scheme was constructed using sequential colours on the ‘colour wheel’ (e.g. Itten <a class="xref bibr" href="#r58"><span class="show-for-sr">Reference Itten</span>1970</a>). The colours were fixed in luminosity, that is, fixed to be constant in luminosity-chroma-hue colour space (Ferrand <a class="xref bibr" href="#r38"><span class="show-for-sr">Reference Ferrand</span>2019</a>). In this way, the brightness level on the image represents only the total intensity values. The colour bar indicates the spectral index at a single fixed intensity. Since the spectral index map in this colour scheme was multiplied by the total intensity map, darker versions of colours are associated with fainter regions in the data. The peak flux density in this image is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline164.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="102" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline164.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $103\ \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section> <p class="p"> The spectral index image helps to isolate the contributions from these two hosts. In the north, there is a very flat spectrum region (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline165.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="35" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline165.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha \sim 0$ </span></span> </span> </span>) at the position of Host 1, connecting to relatively flat <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline166.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="90" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline166.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha \sim -0.4{-}0.5$ </span></span> </span> </span> jets (‘1’). These then connect to the large bright regions of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline167.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="92" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline167.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha \sim -0.6{-}0.7$ </span></span> </span> </span>, steepening sharply down the tails to the south to at least -1.5, beyond which the spectra become more uncertain. All of this is consistent with the behaviour of bent-tail galaxies. In the eastern half, there is a dramatic change in spectral index at the position of the emission associated with the second host; it has its own flat core and steeper lobe/tail structures. Although the overall emission comes from two distinct hosts, it is unclear whether there is an interaction between them, or merely a superposition. An additional curiosity is the thin stream of emission ‘3’ extending eastward from the NE bright region; it has a median spectral index of -2.1, and both its dynamical origins and particle history do not fit naturally into existing radio galaxy models.</p> <p class="p"> The source PMN J2041-5256, shown in <a class="xref fig" href="#f22">Figure 22</a>, is a double-lobed radio AGN, associated with the host galaxy WISEA J204112.05-525737.7 at a redshift of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline168.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="59" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline168.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z=0.048$ </span></span> </span> </span>. Previous radio data (Mauch et al. <a class="xref bibr" href="#r78"><span class="show-for-sr">Reference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler</span>2003</a>; Gregory et al. <a class="xref bibr" href="#r44"><span class="show-for-sr">Reference Gregory, Vavasour, Scott and Condon</span>1994</a>) show only an indistinct extended source corresponding to the nucleus. Its jets (shown with numbers in the figure to indicate their putative host) are presumably being bent by intracluster winds, but the morphology is much more complex than normal bent-tail galaxies. The eastern jet (‘2’) is bifurcated, while the western jet (‘1’) breaks down into a number of blobs, accompanied by a large diffuse area of emission to the west of the source. One possibility is that its relative motion with respect to the intracluster medium (ICM) has a large component along the line of sight; the bifurcated tail and western diffuse extensions would then be more typical of structures seen in bent-tail galaxies, but seen here in projection. If the direction of motion were <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline169.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline169.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>20 degrees from the line of sight, the entire source length would be <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline170.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline170.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>750 kpc, among the larger bent-tail sources. </p> <p class="p"> <a class="xref fig" href="#f23">Figure 23</a> shows two diffuse clouds of radio emission whose origin is unclear. The most likely hypothesis is that they represent the remnants of a classical double-lobed radio galaxy in which the central engine has switched off, leaving a remnant radio galaxy. We refer to this object as the ‘Smoking Gun.’</p> <p class="p"> A tentative identification of the host (marked A in <a class="xref fig" href="#f23">Figure 23</a>) is the galaxy WISEA J204837.65–491115.2, at a redshift of 0.10 (Bilicki et al. <a class="xref bibr" href="#r8"><span class="show-for-sr">Reference Bilicki</span>2016</a>) and which is detected as a <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline171.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="50" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline171.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $260 \,\mu\mathrm{Jy}$ </span></span> </span> </span> unresolved source in the ASKAP image. At that redshift, the largest angular size across the lobes is 530 kpc, which is not unusual for double-lobed radio galaxies. An alternative identification (marked B in <a class="xref fig" href="#f23">Figure 23</a>) of the host is an isolated unresolved <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline172.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="49" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline172.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $200 \,\mu\mathrm{Jy}$ </span></span> </span> </span> radio source which appears to be coincident with the galaxy DES J204835.43-491137.5, at <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline173.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="61" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline173.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z=0.937$ </span></span> </span> </span> (Zhou et al. <a class="xref bibr" href="#r129"><span class="show-for-sr">Reference Zhou</span>2021</a>). If the ‘Smoking Gun’ were actually at this redshift, then the source’s large inferred radio size (2.25 Mpc) would make it a member of the rare class of ‘Giant Radio Galaxies’ (see <a class="xref sec" href="#s6-4">Section 6.4</a>) and it would also be very luminous (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline174.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="64" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline174.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}4 \times 10^{23}$ </span></span> </span> </span> W/Hz). This seems unlikely for a fading remnant, and so we think A, at a redshift of 0.1, is more likely to be the host galaxy. We note that the northern lobe is unusually circular and resembles the Odd Radio Circles (ORCs) shown in <a class="xref fig" href="#f17">Figure 17</a>, except that the ORCs don’t show a continuous rise of their surface brightness towards their centres.</p><section><div class="fig" data-magellan-destination="f22" id="f22"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig22.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1296" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig22.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 22.</span> Another peculiar radio source found in the EMU Pilot Survey: a double-lobed radio AGN, known as PMN J2041–5256, with a curious ‘double’ bent tail. The radio data from EMU-PS has been ‘stretched’ to show the faint emission, and then coloured turquoise, and adjusted to emphasise the double tail. DES g-, r-, and i-band data are combined to form the background, which is combined with the radio data using a layer mask in GIMP. Embedded in the tails are several radio sources that may be unrelated to the tailed galaxy. The peak flux density in this image is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline175.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="107" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline175.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $58.3\ \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section><section><div class="fig" data-magellan-destination="f23" id="f23"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig23.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1542" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig23.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 23.</span> The ‘Smoking Gun’ Galaxy EMU PS J204835.0–491137 consists of the two diffuse radio clouds seen in this image. These are presumably the remnants of a classical double-lobed radio galaxy in which the central engine has switched off. The labels A and B indicate two possible host galaxies, discussed in the text. The peak flux density in this image is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline176.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="106" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline176.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $0.87\ \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section> <p class="p"> Such remnant radio galaxies have previously been reported (e.g. Brienza et al. <a class="xref bibr" href="#r15"><span class="show-for-sr">Reference Brienza</span>2017</a>; Mahatma et al. <a class="xref bibr" href="#r73"><span class="show-for-sr">Reference Mahatma</span>2018</a>; Saripalli et al. <a class="xref bibr" href="#r111"><span class="show-for-sr">Reference Saripalli, Subrahmanyan, Thorat, Ekers, Hunstead, Johnston and Sadler</span>2012</a>), but these new observations probe a lower level of surface brightness than earlier studies. Another remnant radio galaxy imaged by ASKAP has also been recently reported (Quici et al. <a class="xref bibr" href="#r105"><span class="show-for-sr">Reference Quici</span>2021</a>). However, none of the previously reported remnant radio galaxies has a circular lobe resembling that in <a class="xref fig" href="#f23">Figure 23</a>.</p> <p class="p"> <a class="xref fig" href="#f24">Figure 24</a> shows the radio source EMU PS J210700.0<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline177.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline177.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>501128 (also detected as SUMSS J210704<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline178.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline178.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>501206). It appears similar in some ways to PKS 2130-538 shown above (<a class="xref fig" href="#f21">Figure 21</a>) with two bright patches and diffuse tails, presumably blown to the east by relative motion through an external medium. However, there is no obvious host galaxy between the lobes, only a scattering of faint DES galaxies. Instead, the bright southern lobe is coincident with the quasar WISEA J210703.75<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline179.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline179.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>501207.7 at a redshift of 0.197 (Monroe et al. <a class="xref bibr" href="#r85"><span class="show-for-sr">Reference Monroe, Prochaska, Tejos, Worseck, Hennawi, Schmidt, Tumlinson and Shen</span>2016</a>), also detected in the Second ROSAT all-sky survey (Boller et al. <a class="xref bibr" href="#r11"><span class="show-for-sr">Reference Boller, Freyberg, Trümper, Haberl, Voges and Nandra</span>2016</a>). This raises the possibility that the two ‘lobes’ are two independent tailed radio galaxies with very similar morphologies. An apparent overdensity of galaxies visible in both DES and WISE is embedded in the faint southern emission. However, there is no cataloged cluster near this location, and we found photometric redshifts (Zou et al. <a class="xref bibr" href="#r131"><span class="show-for-sr">Reference Zou, Gao, Zhou and Kong</span>2019</a>) for only three galaxies within the source confines that would be consistent with the quasar redshift, so there is no evidence for a cluster.</p><section><div class="fig" data-magellan-destination="f24" id="f24"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig24.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1431" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig24.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 24.</span> EMU PS J210700.0–501128.8 is an ambiguous case, appearing at first to be a double-lobed source with material blown to the east. But with no host between the bright patches, and the southern bright component coincident with a quasar, marked with an ‘X’, these may be two independent sources with serendipitously similar appearances The peak flux density in this image is <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline180.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="105" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline180.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $11.6\ \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section> </div> <div class="sec" data-magellan-destination="s6-2" id="s6-2"> <h3 class="B"><span class="label">6.2.</span> Odd radio circles</h3> <p class="p"> It has been predicted that, because EMU would observe a previously inaccessible part of observational parameter space, it would probably make unexpected discoveries (Norris <a class="xref bibr" href="#r92"><span class="show-for-sr">Reference Norris</span>2017</a>b). Nevertheless, we were surprised to find an apparently new class of object appearing in the EMU-PS, consisting of circles of radio emission, typically one arcmin across, with no optical or infrared counterpart (Norris et al. <a class="xref bibr" href="#r95"><span class="show-for-sr">Reference Norris</span>2021</a>). The first of these ORCs to be identified is shown in <a class="xref fig" href="#f25">Figure 25</a>, and another example is shown in <a class="xref fig" href="#f17">Figure 17</a>. We do not yet understand the nature of these objects, nor whether they are a single class of object or multiple classes. Since discovering them in EMU-PS, we have subsequently observed them with several other telescopes to confirm their reality and have been able to rule out some potential explanations such as supernova remnants or starburst rings. We have also found more examples in other ASKAP fields (e.g. Koribalski et al. <a class="xref bibr" href="#r68"><span class="show-for-sr">Reference Koribalski, Norris, Andernach, Rudnick, Shabala, Filipovic and Lenc</span>2021</a>). Several ORCs have a galaxy at the centre, typically at a redshift of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline181.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline181.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>0.3 in the currently known examples. Potential explanations are that these central galaxies may be the origins of spherical shock waves which we see in projection as a ring, or else that we are seeing end-on radio lobes.</p> <p class="p"> </p><section><div class="fig" data-magellan-destination="f25" id="f25"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig25.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1427" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig25.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 25.</span> An image of the first ‘Odd Radio Circle’, or ORC, found in EMU-PS (Norris et al. <a class="xref bibr" href="#r95"><span class="show-for-sr">Reference Norris</span>2021</a>). It has no optical counterpart to the diffuse ring, or to other diffuse structure, but has a galaxy at its centre which may be the origin of the ring. The image is based on EMU-PS data at native resolution but enhanced to show faint features as described in Norris et al. (<a class="xref bibr" href="#r95"><span class="show-for-sr">Reference Norris</span>2021</a>), particularly the internal structure or “spokes” of the ORC. Radio data are shown in green, and DES optical data are shown in turquoise, magenta, yellow and red, and mainly appear in this image as white.</p> </div></div></section> </div> <div class="sec" data-magellan-destination="s6-3" id="s6-3"> <h3 class="B"><span class="label">6.3.</span> Nearby galaxies</h3> <p class="p"> The design of ASKAP was largely driven by its two largest survey science projects: the EMU continuum survey (Norris et al. <a class="xref bibr" href="#r94"><span class="show-for-sr">Reference Norris</span>2011</a>) and the WALLABY spectral line survey (Koribalski et al. <a class="xref bibr" href="#r67"><span class="show-for-sr">Reference Koribalski</span>2020</a>) with the latter aiming to map neutral hydrogen (H <span class="sc">i</span>) over the entire extragalactic sky in the declination range from <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline182.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="32" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline182.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-90^{\circ}$ </span></span> </span> </span> to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline183.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline183.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $+30^{\circ}$ </span></span> </span> </span> to a redshift of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline184.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline184.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>0.26. WALLABY will generate H <span class="sc">i</span> image cubes at <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline185.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline185.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>30 arcsec resolution and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline186.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="193" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline186.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}1.6\ \mathrm{mJy\ beam}^{-1}\ \mathrm{per}\ 4\,\mathrm{km\,s}^{-1}$ </span></span> </span> </span> channel sensitivity and is expected to detect around half a million galaxies with a mean redshift of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline187.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline187.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>0.05 (Koribalski et al. <a class="xref bibr" href="#r67"><span class="show-for-sr">Reference Koribalski</span>2020</a>).</p> <p class="p"> The relationship between the integrated radio continuum emission of SFGs, unattenuated by interstellar dust, and their star formation rate (SFR) has been extensively studied, (e.g. Condon <a class="xref bibr" href="#r24"><span class="show-for-sr">Reference Condon</span>1992</a>; Tabatabaei et al. <a class="xref bibr" href="#r115"><span class="show-for-sr">Reference Tabatabaei</span>2017</a>; Davies et al. <a class="xref bibr" href="#r31"><span class="show-for-sr">Reference Davies</span>2017</a>), and the broad correlation is well documented, (e.g. Condon et al. <a class="xref bibr" href="#r26"><span class="show-for-sr">Reference Condon, Cotton and Broderick</span>2002</a>; Murphy <a class="xref bibr" href="#r86"><span class="show-for-sr">Reference Murphy</span>2009</a>; Murphy et al. <a class="xref bibr" href="#r88"><span class="show-for-sr">Reference Murphy</span>2011</a>; Molnár et al. <a class="xref bibr" href="#r84"><span class="show-for-sr">Reference Molnár</span>2021</a>). However, the detailed correlations and the underlying mechanisms are still the subject of much debate (e.g. Heesen et al. <a class="xref bibr" href="#r49"><span class="show-for-sr">Reference Heesen, Brinks, Leroy, Heald, Braun, Bigiel and Beck</span>2014</a>). Furthermore, the relationship between the atomic neutral hydrogen gas content of galaxies (for <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline188.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="44" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline188.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z < 0.2$ </span></span> </span> </span>, where individual galaxy detections are feasible) and their SFR requires further investigation (e.g. Wong et al. <a class="xref bibr" href="#r128"><span class="show-for-sr">Reference Wong, Meurer, Zheng, Heckman, Thilker and Zwaan</span>2016</a>; Bera et al. <a class="xref bibr" href="#r7"><span class="show-for-sr">Reference Bera, Kanekar, Chengalur and Bagla</span>2019</a>).</p> <p class="p"> Our most extensive knowledge of the southern sky in neutral hydrogen currently comes from the low-resolution H <span class="sc">i</span> Parkes All Sky Survey (HIPASS; Barnes et al. <a class="xref bibr" href="#r5"><span class="show-for-sr">Reference Barnes</span>2001</a>) which covers the sky from <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline189.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="32" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline189.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-90^{\circ}$ </span></span> </span> </span> to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline190.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline190.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $+25^{\circ}$ </span></span> </span> </span>. HIPASS produced a catalogue of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline191.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline191.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>5000 galaxies out to a redshift of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline192.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="53" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline192.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z = 0.04$ </span></span> </span> </span> (Koribalski et al. <a class="xref bibr" href="#r66"><span class="show-for-sr">Reference Koribalski</span>2004</a>; Meyer et al. <a class="xref bibr" href="#r82"><span class="show-for-sr">Reference Meyer</span>2004</a>). Corresponding 20-cm radio continuum maps (CHIPASS) were created by Calabretta et al. (<a class="xref bibr" href="#r22"><span class="show-for-sr">Reference Calabretta, Staveley-Smith and Barnes</span>2014</a>). ASKAP delivers a 90-fold (for EMU) or 30-fold (for WALLABY) improvement in angular resolution compared to the HIPASS single-dish beam of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline193.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline193.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>15.5 arcmin.</p> <p class="p"> The survey characteristics of EMU and WALLABY imply that we expect nearly all of the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline194.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline194.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>5000 catalogued HIPASS galaxies to be detected by EMU, and to be well resolved by both EMU and WALLABY. Therefore, the combination of EMU radio continuum and WALLABY H <span class="sc">i</span> spectral line measurements of nearby galaxies, combined with other multi-wavelength data, offers the opportunity to study the relationships between star formation, radio continuum emission, and H <span class="sc">i</span> emission in great detail. Here we start to explore this field using the EMU-PS observations of a small sample of nearby galaxies which have been detected in HIPASS.</p> <p class="p"> Of the 89 catalogued HIPASS sources in the EMU-PS area, 63 are clearly detected by EMU-PS in the radio continuum. We expect most of the remaining HIPASS sources to be detected in the full sensitivity main EMU survey. A selection of these galaxies is shown in <a class="xref fig" href="#f26">Figures 26</a> and <a class="xref fig" href="#f27">27</a>. While no WALLABY H <span class="sc">i</span> data currently exist for this field, high-resolution ATCA H <span class="sc">i</span> images are available for some of the galaxies.</p> <p class="p"> </p><section><div class="fig" data-magellan-destination="f26" id="f26"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig26.png?pub-status=live" class="aop-lazy-load-image" width="3000" height="3734" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig26.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 26.</span> A selection of ASKAP-detected nearby galaxies in the EMU-PS. Optical DSS2 <em class="italic">R</em>-band images are overlaid with ASKAP radio continuum contours. The contour levels are –0.09, 0.09 (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline195.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="30" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline195.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}3 \sigma$ </span></span> </span> </span>), 0.18, 0.36, 0.75, 1.5, 3.0, 7.5, 15.0, and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline196.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="94" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline196.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $30\ \mathrm{mJy\,beam}^{-1}$ </span></span> </span> </span>. The convolved 18 arcsec beam is shown in the bottom left corner of each panel. The galaxy name and heliocentric velocity (all but one, ESO233-IG004, from HIPASS) are also displayed. The velocity of ESO233-IG004 is taken from Jones et al. (<a class="xref bibr" href="#r64"><span class="show-for-sr">Reference Jones</span>2009</a>).</p> </div></div></section> <p class="p"> The most interesting galaxy in <a class="xref fig" href="#f26">Figure 26</a> is the edge-on spiral NGC 7090. Using the ATCA, Heesen et al. (2016; <a class="xref bibr" href="#r51"><span class="show-for-sr">Reference Heesen</span>2018</a>) obtained detailed radio continuum maps, finding a radio halo with polarised emission up to 6 kpc above the disc correlating with extraplanar H<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline197.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="9" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline197.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha$ </span></span> </span> </span> emission. ATCA H <span class="sc">i</span> images (Dahlem et al. <a class="xref bibr" href="#r30"><span class="show-for-sr">Reference Dahlem, Ehle, Ryder, Vlajić and Haynes</span>2005</a>) reveal an asymmetric, slightly disturbed disc matching the stellar extent. Another galaxy of interest is the nearly face-on spiral NGC 7125 (see <a class="xref fig" href="#f27">Figure 27</a>), which forms an interacting pair with its northern companion NGC 7126, separated by six arcmin (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline198.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline198.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>80 kpc). ATCA H <span class="sc">i</span> maps (Nordgren et al. <a class="xref bibr" href="#r90"><span class="show-for-sr">Reference Nordgren, Chengalur, Salpeter and Terzian</span>1997</a>) show a large gas envelope encompassing both galaxies. Once detailed H <span class="sc">i</span> spectral line and radio continuum maps are available for large numbers of nearby resolved galaxies, the local and global SFRs and efficiencies can be analysed as a function of H <span class="sc">i</span> column density and environment (e.g. Koribalski & López-Sánchez <a class="xref bibr" href="#r65"><span class="show-for-sr">Reference Koribalski and López-Sánchez</span>2009</a>; Wong et al. <a class="xref bibr" href="#r128"><span class="show-for-sr">Reference Wong, Meurer, Zheng, Heckman, Thilker and Zwaan</span>2016</a>).</p> </div> <div class="sec" data-magellan-destination="s6-4" id="s6-4"> <h3 class="B"><span class="label">6.4.</span> Giant Radio Galaxies</h3> <p class="p"> Giant Radio Galaxies (GRGs) were originally defined as Radio Galaxies (RGs) whose projected linear size was greater than 1 Mpc for a Hubble constant of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline199.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="144" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline199.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mathrm{H}_0=50\,\mathrm{km\,s}^{-1}\,\mathrm{Mpc}^{-1}$ </span></span> </span> </span> (e.g. Ishwara-Chandra & Saikia <a class="xref bibr" href="#r57"><span class="show-for-sr">Reference Ishwara-Chandra and Saikia</span>1999</a>). However, based on the currently accepted value of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline200.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="143" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline200.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mathrm{H}_0 \sim 70\,\mathrm{km\,s}^{-1}\,\mathrm{Mpc}^{-1}$ </span></span> </span> </span>, RGs larger than 0.7 Mpc are now also considered GRGs. In the compilation of GRGs by Kużmicz et al. (<a class="xref bibr" href="#r69"><span class="show-for-sr">Reference Kużmicz, Jamrozy, Bronarska, Janda-Boczar and Saikia</span>2018</a>), the EMU-PS area contains only a single GRG, namely PKS 2014<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline201.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline201.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>558, first mentioned as a GRG by Jones & McAdam (<a class="xref bibr" href="#r62"><span class="show-for-sr">Reference Jones and McAdam</span>1992</a>) and recently studied in detail by Cotton et al. (<a class="xref bibr" href="#r28"><span class="show-for-sr">Reference Cotton</span>2020</a>).</p> <p class="p"> In a recent ASKAP observation covering <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline202.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline202.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $30 \,\mathrm{deg}^2$ </span></span> </span> </span> centred on the Abell 3391/3395 galaxy cluster pair, and of comparable depth and angular resolution as the EMU-PS, Brüggen et al. (<a class="xref bibr" href="#r18"><span class="show-for-sr">Reference Brüggen</span>2021</a>) found the surface density of GRGs <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline203.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="11" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline203.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\gtrsim$ </span></span> </span> </span>1 Mpc to be <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline204.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="69" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline204.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}0.8\,\mathrm{deg}^{-2}$ </span></span> </span> </span>, and that of GRGs <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline205.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="35" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline205.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\gtrsim0.7$ </span></span> </span> </span> Mpc to be at least <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline206.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="69" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline206.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}1.7\,\mathrm{deg}^{-2}$ </span></span> </span> </span>, suggesting that the EMU-PS should contain <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline207.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline207.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>200 and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline208.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline208.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>460 such GRGs, respectively.</p> <p class="p"> From a preliminary visual inspection of the EMU-PS area, biased towards sources of larger angular size and featuring a radio nucleus, we found <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline209.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline209.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>120 GRGs larger than 1 Mpc and a similar number with sizes between 0.7 and 1 Mpc. We visually cross-identified these with the DES images and catalogues (Abbott et al. <a class="xref bibr" href="#r1"><span class="show-for-sr">Reference Abbott</span>2018</a>) and estimated linear sizes based on photometric redshifts (Bilicki et al. <a class="xref bibr" href="#r8"><span class="show-for-sr">Reference Bilicki</span>2016</a>; Drlica-Wagner et al. <a class="xref bibr" href="#r32"><span class="show-for-sr">Reference Drlica-Wagner</span>2018</a>; Zou et al. <a class="xref bibr" href="#r131"><span class="show-for-sr">Reference Zou, Gao, Zhou and Kong</span>2019</a>). The number of GRGs in EMU-PS is likely to increase with a more thorough visual inspection, the results of which will be reported by Andernach et al. (in prep.).</p> <div class="sec" data-magellan-destination="s6-4-1" id="s6-4-1"> <h4 class="C"><span class="label">6.4.1.</span> The Giant Radio Galaxy EMU PS J205139.8–570434</h4> <p class="p"> The GRG EMU PS J205139.8–570434 (hereafter GRG J2051–5704), shown in <a class="xref fig" href="#f28">Figure 28</a>, is hosted by 2MASX J20513976–5704334 at <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline210.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="76" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline210.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z_{sp}=0.0602$ </span></span> </span> </span> (Jones et al. <a class="xref bibr" href="#r64"><span class="show-for-sr">Reference Jones</span>2009</a>) and its radio emission can be traced over a largest angular size <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline211.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="39" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline211.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}22.1$ </span></span> </span> </span> arcmin and thus a linear projected size of 1.53 Mpc. It has an FR I radio morphology whose jets are oriented roughly north-south, feature several wiggles, and terminate in diffuse lobes at both extremes of the source. The strong (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline212.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="84" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline212.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mathrm{S}_{944}=2.12\,\mathrm{Jy}$ </span></span> </span> </span>) source 3.1 arcmin due E, surrounded by diffraction rings, is the well-studied galaxy IC 5063 at <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline213.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="84" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline213.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z_{sp} =0.01135$ </span></span> </span> </span>.</p> <p class="p"> The central region of the new GRG can be recognised in the SUMSS (Bock et al. <a class="xref bibr" href="#r10"><span class="show-for-sr">Reference Bock, Large and Sadler</span>1999</a>) images and was even detected at mm wavelengths by the South Pole Telescope (Mocanu et al. <a class="xref bibr" href="#r83"><span class="show-for-sr">Reference Mocanu</span>2013</a>). However, the full extended structure shown here has not been previously detected, despite extensive imaging of the neighbouring source IC 5063 (Murphy et al. <a class="xref bibr" href="#r87"><span class="show-for-sr">Reference Murphy</span>2010</a> and references therein), probably because of the brightness sensitivity and dynamic range limitations.</p> <p class="p"> The host galaxy of GRG J2051–5704 is the brightest galaxy of cluster 400d J2051–5704 (aka MCXC J2051.6–5704, Burenin et al. <a class="xref bibr" href="#r21"><span class="show-for-sr">Reference Burenin, Vikhlinin, Hornstrup, Ebeling, Quintana and Mescheryakov</span>2007</a>; Piffaretti et al. <a class="xref bibr" href="#r98"><span class="show-for-sr">Reference Piffaretti, Arnaud, Pratt, Pointecouteau and Melin</span>2011</a>) at a redshift of 0.0599. The radio morphology is reminiscent of archetypal FR I sources such as 3C 31 and Hydra A, with wiggles consistent with either the presence of jet instabilities due to interaction with the surrounding gas, or jet precession (e.g. Nawaz et al. <a class="xref bibr" href="#r89"><span class="show-for-sr">Reference Nawaz, Bicknell, Wagner, Sutherland and McNamara</span>2016</a>). While FR I type sources are rare among GRGs larger than 1 Mpc, a recent LOFAR image showed that the GRG 3C 31 also had an extent <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline214.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="57" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline214.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>\ 1\,\mathrm{Mpc}$ </span></span> </span> </span> (Heesen et al. <a class="xref bibr" href="#r51"><span class="show-for-sr">Reference Heesen</span>2018</a>).</p> <p class="p"> It is likely that more of these very large GRGs will be detected with next-generation radio telescopes such as ASKAP thanks to the combination of good angular resolution necessary to reveal the inner jet structure and identify the host, as well as high sensitivity to the low surface brightness features such as the outer tails or lobes. We note that Turner et al. (<a class="xref bibr" href="#r117"><span class="show-for-sr">Reference Turner, Rogers, Shabala and Krause</span>2018</a>) showed from simulations that more sensitive, or lower frequency, observations will reveal FR I galaxies to be much larger than previously thought.</p><section><div class="fig" data-magellan-destination="f27" id="f27"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig27.png?pub-status=live" class="aop-lazy-load-image" width="1499" height="1370" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig27.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 27.</span> DES-DR1 optical composite image of the nearby face-on spiral galaxy NGC 7125 overlaid with contours from the EMU-PS. The contour levels are: 0.1, 0.25, 0.5, 1.0, 1.3, 1.6, 2.0, and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline215.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="99" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline215.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $2.4\ \mathrm{mJy\,beam}^{-1}$ </span></span> </span> </span>. NGC 7125 and its neighbour NGC 7216 form an interacting galaxy pair (HIPASS J2149–60) with a large pool of hydrogen gas for star formation.</p> </div></div></section> </div> </div> <div class="sec" data-magellan-destination="s6-6" id="s6-6"> <h3 class="B"><span class="label">6.5.</span> Radio counterparts to 6dF galaxies</h3> <p class="p"> EMU and the EMU-PS overlap the 6dF Galaxy Survey (6dFGS; Jones et al. <a class="xref bibr" href="#r63"><span class="show-for-sr">Reference Jones</span>2004</a>; <a class="xref bibr" href="#r64"><span class="show-for-sr">Reference Jones</span>2009</a>), a spectroscopic survey of most of the southern sky containing 125 071 galaxy redshifts with a median redshift of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline216.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="34" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline216.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $0.053$ </span></span> </span> </span>. While a variety of selection criteria were used for 6dFGS, most 6dFGS galaxies are brighter than <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline217.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="64" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline217.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $K=12.65$ </span></span> </span> </span> and have redshifts of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline218.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="52" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline218.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z<0.15$ </span></span> </span> </span>. In the EMU-PS region, there are 2506 6dFGS galaxies and, as we discuss below, a large fraction of these galaxies are detected by the EMU-PS.</p> <p class="p"> We measured the flux density of each 6dFGS galaxy using the pixel in the radio continuum maps corresponding to each galaxy’s position. This will underestimate the total flux density of spatially resolved galaxies, and aperture bias is relevant as the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline219.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="62" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline219.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $13^{\prime\prime}\times 11^{\prime\prime}$ </span></span> </span> </span> EMU-PS beam and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline220.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="25" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline220.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $6.7^{\prime\prime}$ </span></span> </span> </span> 6dFGS spectroscopic fibre correspond to less than <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline221.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline221.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $3.4\,{\rm kpc}$ </span></span> </span> </span> and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline222.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="47" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline222.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $2.0\,{\rm kpc,}$ </span></span> </span> </span> respectively, for galaxies within <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline223.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="47" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline223.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $60\,{\rm Mpc}$ </span></span> </span> </span> of Earth. Despite these limitations, our preliminary measurements allow us to quantify the fraction of 6dFGS galaxies that are radio sources and allows us to push fainter than blind radio source catalogues. Of the 2506 6dFGS galaxies in the EMU-PS region, 1887 (75%) have a flux density greater than 75 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline224.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline224.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>, corresponding to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline225.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="32" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline225.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\gtrsim 3\sigma$ </span></span> </span> </span>. As SFGs and passive galaxies have different distributions of radio continuum luminosities, we roughly split these two populations using the presence and absence of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline226.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="21" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline226.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\rm H\alpha}$ </span></span> </span> </span>, measured from the 6dFGS spectra (Jones et al. <a class="xref bibr" href="#r63"><span class="show-for-sr">Reference Jones</span>2004</a>; <a class="xref bibr" href="#r64"><span class="show-for-sr">Reference Jones</span>2009</a>). To quantify noise and source confusion, we also measure flux density at positions offset by 100 pixels (200 arcsec, so well outside the relevant galaxy).</p> <p class="p"> In <a class="xref fig" href="#f29">Figure 29</a>, we present the histogram of EMU-PS flux densities of 6dFGS galaxies with <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline227.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="21" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline227.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\rm H\alpha}$ </span></span> </span> </span> and with <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline228.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="64" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline228.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $K<12.65$ </span></span> </span> </span>, along with the histogram of flux densities measured at offset positions. Roughly half of the SFGs are fainter than <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline229.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="36" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline229.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $1\,{\rm mJy}$ </span></span> </span> </span> and would not have been detected by previous generations of wide-field radio continuum surveys. Almost all 6dFGS galaxies with detectable <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline230.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="21" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline230.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\rm H\alpha}$ </span></span> </span> </span> emission and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline231.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="64" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline231.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $K<12.65$ </span></span> </span> </span> in the EMU-PS area are detected, with just 17 of the 623 galaxies having flux densities below <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline232.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="42" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline232.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $75\,{\rm \mu Jy}$ </span></span> </span> </span>. For comparison, at the 623 offset positions there are just 22 flux density measurements brighter than 75 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline233.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="75" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline233.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> (corresponding to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline234.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="31" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline234.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\gtrsim 3\sigma$ </span></span> </span> </span>) and only 8 flux density measurements brighter than 125 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline235.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="75" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline235.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> (corresponding to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline236.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="31" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline236.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\gtrsim 5 \sigma$ </span></span> </span> </span>). </p> <p class="p"> The radio continuum flux densities of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline237.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline237.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $K<12$ </span></span> </span> </span> galaxies with and without <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline238.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="21" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline238.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\rm H\alpha}$ </span></span> </span> </span> emission is presented in <a class="xref fig" href="#f30">Figure 30</a>. Most <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline239.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline239.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $K<12$ </span></span> </span> </span> SFGs are detected by EMU-PS, and a significant fraction of passive galaxies are also detected. While the lowest mass passive galaxies are often undetected by EMU-PS, all but one of the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline240.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="69" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline240.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $M_K<-26$ </span></span> </span> </span> passive galaxies has a positive radio continuum flux density, presumably resulting from AGNs. This is consistent with Brown et al. (<a class="xref bibr" href="#r17"><span class="show-for-sr">Reference Brown, Jannuzi, Floyd and Mould</span>2011</a>) and Sabater et al. (<a class="xref bibr" href="#r110"><span class="show-for-sr">Reference Sabater</span>2019</a>), who have concluded that all massive elliptical galaxies are radio continuum sources, using NVSS and LOFAR, respectively. When complete, EMU will detect thousands of nearby <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline241.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="70" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline241.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $M_K<-26$ </span></span> </span> </span> elliptical galaxies, enabling characterisation of the radio luminosities of these objects and the AGNs they host.</p><section><div class="fig" data-magellan-destination="f28" id="f28"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig28.png?pub-status=live" class="aop-lazy-load-image" width="3208" height="1851" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig28.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 28.</span> (Left) The Giant Radio Galaxy (GRG) EMU PS J205139.8–570434, with radio (at native resolution) shown in greyscale, overlaid on the DES DR1 colour image. The GRG consists of the roughly north-south jet and the two diffuse plumes above and below it. The strong source to the east, surrounded by diffraction rings, is the well-studied galaxy IC 5063. (Right) A contour diagram of the central part of the GRG at 18 arcsec resolution, overlaid on the DES DR1 colour image. Contour levels are 3, 7, 12, and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline242.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="94" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline242.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $18\ \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section> </div> <div class="sec" data-magellan-destination="s6-7" id="s6-7"> <h3 class="B"><span class="label">6.6.</span> Comparison with Gaia</h3> <p class="p"> The Gaia project (Gaia Collaboration et al. 2016) has measured the parallax and proper motion of over a billion stars, and as a byproduct has also identified a number of quasars and compact galaxies (Bailer-Jones et al. <a class="xref bibr" href="#r4"><span class="show-for-sr">Reference Bailer-Jones, Fouesneau and Andrae</span>2019</a>). To produce a catalogue of candidate radio-loud quasars, we therefore cross-match the DES counterparts to EMU radio sources against the Gaia EDR3 catalogue (Gaia Collaboration et al. 2021). We use the same technique as in earlier cross-matches in this paper, resulting in a plot of cross-matches as a function of search radius for shifted and unshifted data, shown in <a class="xref fig" href="#f31">Figure 31</a>. As a result of this test, we choose a cross-match radius of 0.2 arcsec, resulting in 14 174 cross-matches in the unshifted data, and 14 cross-matches in the shifted data, indicating a false-ID rate of 0.1%.</p> <p class="p"> To explore the infrared properties of this sample of Gaia-selected sources, we need to use the WISE W3 band, which is absent from the CWISE catalogue, and so we must match our sources against the AllWISE catalogue (Cutri et al. <a class="xref bibr" href="#r29"><span class="show-for-sr">Reference Cutri</span>2021</a>). We therefore cross-match the list of 14 174 sources, using a search radius of 1 arcsec, against the AllWISE catalogue, resulting in a catalogue of 11 142 sources with WISE W1, W2, and W3 flux densities. These sources are shown in <a class="xref fig" href="#f32">Figure 32</a>, colour-coded by their proper motion.</p> <p class="p"> The sources with the lowest proper motions lie in the region identified by Jarrett et al. (<a class="xref bibr" href="#r59"><span class="show-for-sr">Reference Jarrett</span>2017</a>) as being dominated by quasars, while a higher level of proper motion is seen in the region dominated by galaxies. This effect was also noted by Bailer-Jones et al. (<a class="xref bibr" href="#r4"><span class="show-for-sr">Reference Bailer-Jones, Fouesneau and Andrae</span>2019</a>) who explained it as extended galaxies not having well-defined centroids, causing the measured Gaia position to vary, resulting in an apparent proper motion. The group with the highest proper motion (coded as yellow) lie in the region designated as stars, confirming that these DES sources are indeed stars. However, most, if not all, of these ‘stars’ are probably false IDs and do not correspond to radio sources.</p> <p class="p"> Of the 11 142 galaxies with W1, W2, and W3 flux densities, 2604 have W1-W2 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline243.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline243.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>$ </span></span> </span> </span>0.8, and we refer to these as quasar candidates. To estimate the false-ID rate, we repeated the above selection process after shifting the declination by 1 arcmin, and this resulted in 2312 sources with W1, W2, and W3 flux densities, of which 503 have W1-W2 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline244.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="8" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline244.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $>$ </span></span> </span> </span>0.8. We therefore expect that 81% of our quasar candidates are radio-loud quasars, assuming that no other types of source fall in that part of the WISE colour diagram.</p> <p class="p"> The combination of the Gaia selection and the WISE colour selection has, therefore, yielded a catalogue of 2312 radio-loud quasar candidates, of which about 81% are true radio-loud quasars. Using the same technique on the entire EMU survey will yield a catalogue of about 230 000 radio-loud quasar candidates, representing a significant increase in the number of known radio-loud quasars.</p> </div> <div class="sec" data-magellan-destination="s6-8" id="s6-8"> <h3 class="B"><span class="label">6.7.</span> Clusters of galaxies</h3> <p class="p"> Galaxy clusters represent some of the largest gravitationally bound structures in the universe, and radio emission provides an insight into their formation and evolution. They evolve and grow through a variety of processes including passive accretion of gas, consumption of small galaxy groups, and violent merger events which can deposit vast amounts of energy (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline245.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="39" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline245.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}10^{64}$ </span></span> </span> </span> erg, e.g. Ferrari et al. <a class="xref bibr" href="#r39"><span class="show-for-sr">Reference Ferrari, Govoni, Schindler, Bykov and Rephaeli</span>2008</a>) into the ICM.</p> <p class="p"> Many merging galaxy clusters host vast and enigmatic radio continuum sources. These diffuse radio sources are broadly classified into two categories: radio relics (or cluster radio shocks) and radio halos (see van Weeren et al. <a class="xref bibr" href="#r133"><span class="show-for-sr">Reference van Weeren, de Gasperin, Akamatsu, Brüggen, Feretti, Kang, Stroe and Zandanel</span>2019</a>, for a recent review). To date, some <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline246.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="27" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline246.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}70$ </span></span> </span> </span> clusters are known to host radio relics, and some <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline247.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="28" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline247.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}65$ </span></span> </span> </span> clusters are known to host radio halos<a class="xref fn" href="#fn10"><span class="show-for-sr">Footnote </span>j</a>.</p> <p class="p"> Radio relics are highly extended (typically <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline248.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="19" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline248.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}1$ </span></span> </span> </span> Mpc), highly polarised, diffuse synchrotron sources that lie towards the periphery of galaxy clusters. They often exhibit curved morphologies and filamentary sub-structures and are thought to be powered by shocks which generate relativistic electrons through a form of diffusive shock acceleration.</p> <p class="p"> Radio halos, on the other hand, are largely amorphous, unpolarised diffuse synchrotron sources that are centrally located in merging galaxy clusters, and roughly follow the distribution of the thermal plasma in the ICM (as traced by X-ray emission).The most commonly accepted scenario is that radio halos are powered by turbulence injected in the ICM during cluster merger events, although there are alternatives based on collisions between cosmic ray protons (CRp) and thermal protons from the ICM (for a review, see Brunetti & Jones <a class="xref bibr" href="#r19"><span class="show-for-sr">Reference Brunetti and Jones</span>2014</a>). On smaller scales (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline249.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="34" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline249.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\lesssim0.5$ </span></span> </span> </span> Mpc), ‘mini-halos’ are relatively small diffuse radio sources that are generally co-located with powerful, radio-loud, brightest cluster galaxies (BCGs) in relaxed clusters. One theoretical explanation for mini-halos is that ‘core-sloshing’ in the ICM from minor or off-axis mergers produces small-scale turbulence which can then provide sufficient energy for re-acceleration of the relativistic electrons.</p> <p class="p"> For relics, halos, and mini-halos, the shape of the synchrotron emitting spectrum provides a diagnostic for these relativistic particle (re-)acceleration processes. Historically, our understanding of the relevant physics has been limited by (i) the generally relatively poor quality of low-frequency radio data, (ii) missing short spacings, leading to loss of highly-extended radio emission, and (iii) narrow bandwidths, limiting the spectral shape measurements. By circumventing these limitations with the EMU survey, the sample of clusters suitable for study can be increased by at least two orders of magnitude.</p> <p class="p"> There are already <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline250.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline250.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>20 known X-ray detected galaxy clusters in the EMU-PS area. All show compact or moderately extended radio sources that are likely associated with AGN. The eROSITA survey (Predehl et al. <a class="xref bibr" href="#r104"><span class="show-for-sr">Reference Predehl</span>2021</a>) will provide many more X-ray clusters for radio investigation. The first eROSITA all-sky survey (eRASS1) will find as many as <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline251.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="107" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline251.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $1.5\ \mathrm{clusters/\,deg}^2$ </span></span> </span> </span>; more than <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline252.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="97" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline252.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $3\ \mathrm{clusters/\,deg}^2$ </span></span> </span> </span> are expected after all eight all-sky surveys are completed (e.g., Pillepich et al. <a class="xref bibr" href="#r99"><span class="show-for-sr">Reference Pillepich, Reiprich, Porciani, Borm and Merloni</span>2018</a>). Hence, we expect as many as 400 X-ray-detected clusters will soon be available in the EMU-PS area alone, and more than 10 000 AGN.</p> <p class="p"> Early EMU/eROSITA results on the Abell 3391/95 galaxy cluster system (Reiprich et al. <a class="xref bibr" href="#r108"><span class="show-for-sr">Reference Reiprich</span>2021</a>; Brüggen et al. <a class="xref bibr" href="#r18"><span class="show-for-sr">Reference Brüggen</span>2021</a>) have already helped constrain physical processes in the merger. We show two additional examples of diffuse radio sources detected in the EMU-PS area in <a class="xref fig" href="#f33">Figures 33</a> and <a class="xref fig" href="#f34">34</a>.</p><section><div class="fig" data-magellan-destination="f29" id="f29"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig29.png?pub-status=live" class="aop-lazy-load-image" width="1499" height="970" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig29.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 29.</span> The histogram of EMU-PS flux densities for 6dFGS galaxies with <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline253.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="21" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline253.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\rm H\alpha}$ </span></span> </span> </span> emission and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline254.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="64" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline254.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $K<12.65$ </span></span> </span> </span>, along with the corresponding histogram of flux densities measured at offset positions. Just 17 of the 623 6dFGS galaxies with detectable <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline255.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="21" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline255.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\rm H\alpha}$ </span></span> </span> </span> emission have radio flux densities below 75 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline256.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline256.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>.</p> </div></div></section><section><div class="fig" data-magellan-destination="f30" id="f30"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig30.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="983" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig30.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 30.</span> The EMU-PS flux densities of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline257.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline257.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $K<12$ </span></span> </span> </span> galaxies with and without <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline258.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="21" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline258.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\rm H\alpha}$ </span></span> </span> </span> emission as a function of absolute magnitude. The dashed line shows <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline259.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="42" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline259.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $75\,{\rm \mu Jy}$ </span></span> </span> </span>, roughly corresponding to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline260.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="17" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline260.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $3\sigma$ </span></span> </span> </span>. Almost all star-forming galaxies are detected by the EMU-PS. While low mass passive galaxies can have no detectable radio continuum emission, all but one <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline261.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="70" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline261.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $M_K<-26$ </span></span> </span> </span> passive galaxy has a positive radio continuum flux density.</p> </div></div></section><section><div class="fig" data-magellan-destination="f31" id="f31"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig31.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1039" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig31.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 31.</span> The number of cross-matches between DES counterparts to EMU-PS sources, and Gaia sources, for unshifted data (blue), and data shifted by one arcmin (orange).</p> </div></div></section><section><div class="fig" data-magellan-destination="f32" id="f32"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig32.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1090" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig32.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 32.</span> The AllWISE colour-colour plot for EMU-PS sources cross-matched with Gaia, colour-coded according to their measured proper motion. The dashed lines divide the graph into the regions identified by Jarrett et al. (<a class="xref bibr" href="#r59"><span class="show-for-sr">Reference Jarrett</span>2017</a>).</p> </div></div></section><section><div class="fig" data-magellan-destination="f33" id="f33"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig33.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1276" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig33.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 33.</span> Multi-wavelength composite image of SPT-CL J2023<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline262.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline262.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>5535. Contours denote the EMU-PS surface brightness at 944 MHz at 18 arcsec resolution, at <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline263.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="66" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline263.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $3\sigma_{\rm{rms}} \times 2^{n}$ </span></span> </span> </span> where <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline264.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="91" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline264.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $n=0, 1, 2, 3, 4$ </span></span> </span> </span> and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline265.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="71" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline265.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sigma_{rms}=\sim25$ </span></span> </span> </span> <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline266.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline266.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>. Background colourmap shows a composite <em class="italic">g</em>, <em class="italic">r</em>, and <em class="italic">i</em> image from DECam. X-ray emission from <em class="italic">Chandra</em> is also overlaid in red. New diffuse radio sources identified by HyeongHan et al. (<a class="xref bibr" href="#r56"><span class="show-for-sr">Reference HyeongHan</span>2020</a>) are also indicated.</p> </div></div></section> <p class="p"> </p><section><div class="fig" data-magellan-destination="f34" id="f34"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig34.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1301" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig34.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 34.</span> Multi-wavelength composite image of the cluster SPT-CL J2032<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline267.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline267.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>5627. Colour map and contours are the same as <a class="xref fig" href="#f33">Figure 33</a>, but with <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline268.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="32" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline268.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $25\,\mathrm{ks}$ </span></span> </span> </span> XMM- <em class="italic">Newton</em> surface brightness shown in red. It appears that the cluster hosts one of the rare class of double-radio relics with the northern (A and B) and southern (C) relics as indicated.</p> </div></div></section> <p class="p"> Other cluster catalogues will similarly provide important targets for EMU-PS and the full EMU Survey. For example, Aguena et al. (<a class="xref bibr" href="#r3"><span class="show-for-sr">Reference Aguena</span>2021</a>) provide the WaZP catalogue of 60542 clusters from the DES<a class="xref fn" href="#fn11"><span class="show-for-sr">Footnote </span>k</a>. About 30 of their BCGs are coincident with extended RGs in the EMU-PS and will be discussed by Andernach et al. (in preparation).</p> <div class="sec" data-magellan-destination="s6-8-1" id="s6-8-1"> <h4 class="C"><span class="label">6.7.1.</span> SPT-CL J2023-5535</h4> <p class="p"> <a class="xref fig" href="#f33">Figure 33</a> presents the radio halo and relic in the massive merging galaxy cluster, SPT-CL J2023<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline269.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline269.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>5535 (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline270.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="52" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline270.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z=0.23$ </span></span> </span> </span>), reported by HyeongHan et al. (<a class="xref bibr" href="#r56"><span class="show-for-sr">Reference HyeongHan</span>2020</a>). Their weak-lensing analysis has revealed significant substructure in this massive (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline271.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="191" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline271.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $M_{200}=1.04\pm0.36\times 10^{15}\,M_{\odot}$ </span></span> </span> </span>) cluster, which comprises three subclusters.</p> <p class="p"> The merger event between the eastern and central subclusters appears to have generated a <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline272.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="31" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline272.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}0.5$ </span></span> </span> </span> Mpc radio relic on the western edge of the central subcluster. The results presented by HyeongHan et al. (<a class="xref bibr" href="#r56"><span class="show-for-sr">Reference HyeongHan</span>2020</a>) show an unusually flat spectral index <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline273.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="125" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline273.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha_{\rm{int}}=-0.76 \pm 0.06$ </span></span> </span> </span>, which may indicate that this relic is powered by the re-acceleration of fossil electrons, perhaps originally seeded by a nearby (photometric) cluster member AGN. Follow-up observations at other radio frequencies will be required to confirm this flat spectrum.</p> </div> <div class="sec" data-magellan-destination="s6-8-2" id="s6-8-2"> <h4 class="C"><span class="label">6.7.2.</span> SPT-CL J2032-5627</h4> <p class="p"> <a class="xref fig" href="#f34">Figure 34</a> shows a rare class of a possible double-radio relic with an elongation of X-ray emission in the massive (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline274.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="173" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline274.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $M_{500}=4.77^{+0.71}_{-0.63}\times 10^{14}\,M_{\odot}$ </span></span> </span> </span>; Bulbul et al. <a class="xref bibr" href="#r20"><span class="show-for-sr">Reference Bulbul</span>2019</a>) cluster SPT-CL J2032<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline275.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline275.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>5627 (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline276.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="52" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline276.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $z=0.28$ </span></span> </span> </span>). The north-western (sources A & B) and south-eastern (source C) all exhibit steep radio spectra (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline277.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="80" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline277.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha_{\rm{int}} = -1.75$ </span></span> </span> </span>, <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline278.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="79" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline278.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha_{\rm{int}} = -1.69$ </span></span> </span> </span>, and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline279.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="81" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline279.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha_{\rm{int}} =-1.46$ </span></span> </span> </span>, respectively).</p><section><div class="fig" data-magellan-destination="f35" id="f35"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig35.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1425" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig35.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 35.</span> Radio contours overlaid on a multi-wavelength (irg) composite image of 6dFGS g2212485-614658 from DES. The radio image was made from the EMU-PS native resolution data by subtracting four unresolved sources and then convolving to a resolution of 18 arcsec. Contours are at 75, 150, 300, and 600 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline280.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline280.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>. The subtracted sources were at 22:12:48.64 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline281.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline281.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>61:46:58.5 (14.9 mJy), 22:12:43.04 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline282.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline282.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>61:46:50.1 (0.3 mJy), 22:12:51.19 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline283.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline283.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>61:46:15.5 (0.2 mJy), 22:12:37.17 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline284.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline284.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>61:47:24.5 (0.1 mJy)</p> </div></div></section> <p class="p"> The highly asymmetric X-ray surface brightness profile and large projected separation between the radio relics in this cluster suggest that the merger event is occurring close to the plane of the sky. Curiously, no evidence of a shock has been found in the X-ray surface brightness. However, the presence of a cold front towards the leading edge to the south-east of the cluster may suggest that the lack of a shock detection is due to the relatively shallow depth (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline285.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="32" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline285.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $25\,\mathrm{ks}$ </span></span> </span> </span>) of the existing XMM- <em class="italic">Newton</em> observations. See also Duchesne et al. (<a class="xref bibr" href="#r33"><span class="show-for-sr">Reference Duchesne, Johnston-Hollitt, Bartalucci, Hodgson and Pratt</span>2021</a>) for further discussion of SPT-CL J2032<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline286.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="10" height="2" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline286.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $-$ </span></span> </span> </span>5627.</p> </div> <div class="sec" data-magellan-destination="s6-8-3" id="s6-8-3"> <h4 class="C"><span class="label">6.7.3.</span> A Mini-Halo in a poor cluster</h4> <p class="p"> <a class="xref fig" href="#f35">Figure 35</a> shows a very low surface brightness structure, much fainter (50<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline287.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="75" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline287.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span>) than the embedded compact 14.8<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline288.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="67" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline288.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\pm0.07\,\textrm{mJy}$ </span></span> </span> </span> source associated with 6dFGS g2212485-614658 at a redshift of z=0.054. The low surface brightness emission was found using the multi-resolution filtering technique of Rudnick (<a class="xref bibr" href="#r109"><span class="show-for-sr">Reference Rudnick</span>2002</a>), using a filter box size of 34 arcsec which removes the emission from compact components. It has a total extent of 150 arcsec (160 kpc) and a total flux density of 5<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline289.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline289.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\pm$ </span></span> </span> </span>0.5 mJy, corresponding to a luminosity of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline290.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="67" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline290.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\approx 3\times10^{22}$ </span></span> </span> </span> W/Hz. No substructure is apparent. </p> <p class="p"> The diffuse structure could be the dying remains of a radio galaxy, faded to a luminosity comparable to the faintest AGN or to typical SFGs (Mauch & Sadler <a class="xref bibr" href="#r77"><span class="show-for-sr">Reference Mauch and Sadler</span>2007</a>). The lack of radio structure, however, suggests that it could also be an underluminous mini-halo, an option we briefly explore here.</p> <p class="p"> There is no catalogued cluster associated with 6dFGS g2212485-614658, although there are five galaxies with a similar redshift listed in Vizier, out to a separation of 17 arcmin (1 Mpc). This, and the presence of many smaller galaxies embedded in the 6dFGS g2212485-614658 envelope (<a class="xref fig" href="#f35">Figure 35</a>) suggest that this could be a poor cluster or group.</p> <p class="p"> The radio and extended (as opposed to AGN) X-ray luminosities of mini-halo systems are well correlated (Giacintucci et al. <a class="xref bibr" href="#r42"><span class="show-for-sr">Reference Giacintucci, Markevitch, Cassano, Venturi, Clarke, Kale and Cuciti</span>2019</a>). For this system, we determined upper limits to the bolometric (0.2–2 keV) X-ray emission using both RASS and XMM Slew archives, yielding limits in the range 1.4–2.4<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline291.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="114" height="17" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline291.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\times10^{-13}\ \mathrm{erg/s/cm}^2$ </span></span> </span> </span>. At mid-range, the inferred luminosity upper limit of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline292.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="25" height="13" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline292.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $10^{42}$ </span></span> </span> </span> erg/s is two orders of magnitude lower than that of the mini-halo clusters summarised in Giacintucci et al. (<a class="xref bibr" href="#r42"><span class="show-for-sr">Reference Giacintucci, Markevitch, Cassano, Venturi, Clarke, Kale and Cuciti</span>2019</a>) and than the value expected from the radio-X-ray correlation.</p> <p class="p"> Probing mini-halo-like structures in these poor-cluster, low X-ray luminosity type systems is important for understanding the physical mechanisms which form and continue to power the radio emission. We do not know whether the current observed radio-X-ray correlation is influenced by X-ray selection effects, or whether the correlation breaks down at very low cluster masses.</p> <p class="p"> The sensitivity of EMU to very low surface brightness emission such as presented here will provide a powerful tool for exploring the connection between compact and extended AGN emissions and pure cluster/group particle acceleration processes in mini-halos.</p> </div> </div> <div class="sec" data-magellan-destination="s6-12" id="s6-12"> <h3 class="B"><span class="label">6.8.</span> Cosmology</h3> <p class="p"> The spatial distribution of radio sources is a tracer of the underlying matter distribution and can be used to probe the formation conditions of radio galaxies, as well as the underlying fundamental ingredients and physics of the universe. As these continuum sources are not easy to localise in redshift, we use measurements of angular clustering for the EMU-PS.</p> <p class="p"> Here, we use the Landy & Szalay (<a class="xref bibr" href="#r71"><span class="show-for-sr">Reference Landy and Szalay</span>1993</a>) estimator, which is defined as: </p><div data-mathjax-status="alt-graphic" class="disp-formula" data-magellan-destination="disp1" id="disp1"> <span class="label">(1)</span> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_eqn1.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="232" height="37" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_eqn1.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> \begin{equation} w_{\mathrm{LS}}(\theta) = \frac{DD(\theta) + RR(\theta) - 2DR(\theta)}{RR(\theta)},\end{equation} </span></span> </span> </div><p class="p continuation">where <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline293.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="42" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline293.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $DD(\theta)$ </span></span> </span> </span> is the number of observed galaxy pairs at distance between <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline294.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="8" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline294.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\theta$ </span></span> </span> </span> and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline295.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="43" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline295.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\theta+d\theta$ </span></span> </span> </span>, <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline296.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="37" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline296.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $RR(\theta)$ </span></span> </span> </span> is the number of random galaxies pairs at this separation, and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline297.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="40" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline297.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $DR(\theta)$ </span></span> </span> </span> is the number of observed random pairs. We apply this statistic to the pilot survey catalogue, using the island data catalogue as the data vector (<em class="italic">D</em>), and generated random catalogues (<em class="italic">R</em>), normalising the number over all angles such the angular correlation function <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline298.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="29" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline298.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $w(\theta)$ </span></span> </span> </span> functions as a probability excess or decrement relative to an entirely random distribution of galaxies on the sky.</p> <p class="p"> The random catalogue (<em class="italic">R</em>) is generated using the method used in Hale et al. (<a class="xref bibr" href="#r46"><span class="show-for-sr">Reference Hale, Jarvis, Delvecchio, Hatfield, Novak, Smolčić and Zamorani</span>2018</a>) and Siewert et al. (<a class="xref bibr" href="#r114"><span class="show-for-sr">Reference Siewert</span>2020</a>) where random positions for simulated sources are generated across the EMU-PS field of view and for each simulated source a flux density is randomly assigned to the source using flux densities from the SKADS simulation (Wilman et al. <a class="xref bibr" href="#r127"><span class="show-for-sr">Reference Wilman</span>2008</a>)<a class="xref fn" href="#fn12"><span class="show-for-sr">Footnote </span>l</a>. We assign noise to the flux density of the simulated source by sampling from a Gaussian distribution with spread given by the RMS at the random source location. A source remains within the random catalogue provided the simulated source peak flux density (where we assume the random sources are unresolved) added to the noise would be detectable at <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline300.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline300.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\geq 5 \times$ </span></span> </span> </span> the RMS at the simulated source position. </p><section><div class="fig" data-magellan-destination="f36" id="f36"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig36.png?pub-status=live" class="aop-lazy-load-image" width="1499" height="1097" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig36.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 36.</span> The number of sources in the EMU-PS with a flux density greater than some limit (<em class="italic">S</em>), as a function of that limit, compared to scaled predictions from the SKADS and T-RECS simulated catalogues. The dashed black vertical line gives the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline301.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="48" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline301.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $500\mu\mathrm{Jy}$ </span></span> </span> </span> limit we assume for the clustering analysis presented in this paper. There is some discretisation of the prediction for the larger flux density limits, due to a scaling of some small integer value for the original prediction that was made for a much smaller value.</p> </div></div></section> <p class="p"> The robustness of this approach to generate the randoms is checked by comparing the fluxes of the simulated catalogues to the island catalogue of the EMU-PS. We selected both AGN and SFG galaxies from SKADS and T-RECS (Bonaldi et al. <a class="xref bibr" href="#r12"><span class="show-for-sr">Reference Bonaldi, Bonato, Galluzzi, Harrison, Massardi, Kay, De Zotti and Brown</span>2019</a>) simulations. In <a class="xref fig" href="#f36">Figure 36</a>, we compare the number counts for different flux density cuts <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline302.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="48" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline302.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $N(>S)$ </span></span> </span> </span> between the EMU-PS island catalogue and the number counts from both simulated radio catalogues at 1 GHz.</p> <p class="p"> In order to calculate the expected <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline303.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="42" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline303.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $w_{\mathrm LS}(\theta)$ </span></span> </span> </span> distribution, we must know the redshift distribution <em class="italic">N</em>(<em class="italic">z</em>) of the sources. For the analysis here, the SKADS and T-RECS simulations are used for <em class="italic">N</em>(<em class="italic">z</em>) and are shown in <a class="xref fig" href="#f37">Figure 37</a>. There is good agreement in the redshift distribution between these two catalogues, and this consistency indicates that we are accurately modelling <em class="italic">N</em>(<em class="italic">z</em>) and choosing the SKADS catalogue should not introduce a significant error. Using the <em class="italic">N</em>(<em class="italic">z</em>) distribution estimated from SKADS, we compute the theoretical expectation for the clustering statistics at the flux density cut of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline304.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="47" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline304.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $500 \mu\mathrm{Jy}$ </span></span> </span> </span>.</p> <p class="p"> </p><section><div class="fig" data-magellan-destination="f37" id="f37"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig37.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1096" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig37.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 37.</span> The predicted number of sources in the EMU Pilot Survey as a function of redshift, generated by scaling the predictions from the SKADS and T-RECS simulated catalogues. This assumes a flux density limit of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline305.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="48" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline305.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $500\mu\mathrm{Jy}$ </span></span> </span> </span> </p> </div></div></section> <p class="p"> The measured angular correlation function <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline306.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="29" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline306.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $w(\theta)$ </span></span> </span> </span> is shown in <a class="xref fig" href="#f38">Figure 38</a>, estimating the errors from boostrap resampling the data and random simulated data 100 times. We also show the predicted angular correlation function, assuming a cosmological model with values fixed at the values listed in <a class="xref table" href="#tbl2">Table 2</a>, with a number distribution and bias model from SKADS. We show that the theoretical prediction, with no tuning of free parameters, is a reasonable fit to the data in the angular range <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline307.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="92" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline307.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $0.1^{\circ} < \theta < 10^{\circ}$ </span></span> </span> </span>. There is somewhat of a discrepancy at small scales (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline308.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="51" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline308.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\theta < 0.1^{\circ}$ </span></span> </span> </span>), which is probably generated by the multiple components that can be generated by the same radio galaxy, but which here are being treated as independent tracers of the cosmological density field. A more complete analysis, including calibration of the effect of multi-component sources on the angular correlation function on small scales, is planned for future work.</p> <p class="p"> </p><section><div class="fig" data-magellan-destination="f38" id="f38"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig38.png?pub-status=live" class="aop-lazy-load-image" width="1500" height="1112" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig38.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 38.</span> The measured angular correlation function (ACF) <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline309.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="30" height="15" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline309.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $w(\theta)$ </span></span> </span> </span> as a function of angular separation with one-sigma error bar computed from bootstrap re-sampling from 100 bootstraps. The correlation function is measured from the integrated flux-corrected EMU-PS island catalogue, using all sources above a flux density limit of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline310.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="47" height="14" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline310.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $500\mu\mathrm{Jy}$ </span></span> </span> </span>. The blue curve is the theoretical prediction for the correlation function, assuming the Planck 2018 best fit cosmology and a SKADS model for the number distribution with redshift and the bias. No fitting of the cosmological or bias parameters was performed to change the prediction curve. As negative values cannot be shown on a log scale, in bins where the ACF becomes negative, we show (in red) the value of (-ACF) instead.</p> </div></div></section> </div> <div class="sec" data-magellan-destination="s6-13" id="s6-13"> <h3 class="B"><span class="label">6.9.</span> The excess of flat spectral index sources</h3> <p class="p"> To investigate the skew towards flatter and inverted spectral indices shown in <a class="xref fig" href="#f10">Figures 10</a> and <a class="xref fig" href="#f11">11</a>, we compare the spectral index distributions for a sample of clearly resolved and unresolved components from the EMU-PS. The unresolved population contains radio cores and therefore includes flat-spectrum radio quasars (Urry & Padovani <a class="xref bibr" href="#r118"><span class="show-for-sr">Reference Urry and Padovani</span>1995</a>) and peaked-spectrum sources (O’Dea & Saikia <a class="xref bibr" href="#r97"><span class="show-for-sr">Reference O’Dea and Saikia</span>2021</a>). At the observing frequency of EMU-PS (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline311.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="50" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline311.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\nu \sim 900\,$ </span></span> </span> </span>MHz), the radio spectra of Gigahertz Peaked-Spectrum sources tend to have shallow spectral index values as EMU-PS is observing close to their turnover frequency (O’Dea <a class="xref bibr" href="#r96"><span class="show-for-sr">Reference O’Dea</span>1998</a>). For this comparison, we define each source to be resolved or unresolved using the component size after deconvolution from the beam, <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline312.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="11" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline312.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\Psi$ </span></span> </span> </span>, considering components with <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline313.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="80" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline313.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\Psi < 2\,\mathrm{arcsec}$ </span></span> </span> </span> to be unresolved and components with <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline314.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="87" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline314.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\Psi > 20\,\mathrm{arcsec}$ </span></span> </span> </span> to be resolved. </p><section><div class="fig" data-magellan-destination="f39" id="f39"> <div class="figure-thumb"><img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig39.png?pub-status=live" class="aop-lazy-load-image" width="667" height="732" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig39.png" data-zoomable="true"></div> <div class="caption"><p class="p"> </p><p class="p"><span class="label">Figure 39.</span> The spectral index distributions for unresolved (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline315.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline315.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\Psi < 2''$ </span></span> </span> </span>, blue) and resolved (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline316.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="52" height="12" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline316.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\Psi > 20''$ </span></span> </span> </span>, red) EMU components. The three panels show different minimum brightness levels, corresponding to <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline317.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="135" height="19" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline317.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\text{peak}} > 1\,\mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>, <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline318.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="134" height="19" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline318.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\text{peak}} > 3\,\mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>, and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline319.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="142" height="19" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline319.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\text{peak}} > 10\,\mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span> from top to bottom. The legend in each panel denotes the number of components contributing to each distribution shown. Each plot is normalised to the area under the curve.</p> </div></div></section> <p class="p"> In <a class="xref fig" href="#f39">Figure 39</a>, we show the spectral index distributions for the resolved and unresolved EMU components at three levels of minimum peak brightness: <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline320.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="134" height="19" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline320.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\text{peak}} > 1\, \mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>, <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline321.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="135" height="19" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline321.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\text{peak}} > 3\,\mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>, and <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline322.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="141" height="19" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline322.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\text{peak}} > 10\,\mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>. Resolved components have symmetric distributions around a peak of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline323.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="60" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline323.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha \sim -0.7$ </span></span> </span> </span>. However, while the spectral index distribution for the unresolved population is comparable to the resolved population at steep negative spectral indices (<span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline324.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="60" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline324.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha < -0.7$ </span></span> </span> </span>), the distributions differ at flatter spectral indices. At <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline325.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="60" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline325.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\alpha > -0.7$ </span></span> </span> </span>, the unresolved population dominates over the resolved population at all three brightness levels. Due to the large scatter in the spectral index distribution at sub-mJy levels (<a class="xref fig" href="#f10">Figure 10</a>), we have only performed this analysis on EMU components with <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline326.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="134" height="19" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline326.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S_{\text{peak}}>1\,\mathrm{mJy\ beam}^{-1}$ </span></span> </span> </span>. Future EMU data, where potential issues in the spectral index calibration at lower signal to noise are better understood, will present the opportunity to study the spectral index distributions of fainter resolved and unresolved components. Such an analysis, particularly for the full EMU survey, will enable tests of the potential flattening of the spectral index distribution for radio sources with <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline327.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="45" height="16" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline327.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $S \lesssim 0.5\,$ </span></span> </span> </span> mJy (Prandoni et al. <a class="xref bibr" href="#r102"><span class="show-for-sr">Reference Prandoni, Parma, Wieringa, de Ruiter, Gregorini, Mignano, Vettolani and Ekers</span>2006</a>; Whittam et al. <a class="xref bibr" href="#r126"><span class="show-for-sr">Reference Whittam</span>2013</a>). </p> <p class="p"> The different spectral index distributions of resolved and unresolved components we observe with the EMU-PS are consistent with what is seen with higher angular resolution and higher frequency observations. Recently, Gordon et al. (<a class="xref bibr" href="#r43"><span class="show-for-sr">Reference Gordon</span>2021</a>) demonstrated the <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline328.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="43" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline328.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $1.4 - 3\,$ </span></span> </span> </span>GHz spectral index distributions for point-like radio components are skewed to flatter values than well-resolved components using observations from the Faint Images of the Radio Sky at Twenty cm survey (FIRST; <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline329.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="47" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline329.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\nu \sim 1.4\,$ </span></span> </span> </span>GHz, Becker et al. <a class="xref bibr" href="#r6"><span class="show-for-sr">Reference Becker, White and Helfand</span>1995</a>) and the Very Large Array Sky Survey (VLASS, <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline330.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="33" height="11" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline330.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\nu \sim 3\,$ </span></span> </span> </span>GHz, Lacy et al. <a class="xref bibr" href="#r70"><span class="show-for-sr">Reference Lacy</span>2020</a>). Further comparisons between EMU and radio observations in other bands, such as those from VLASS and the Australia Telescope Large Area Survey (ATLAS, <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline331.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="55" height="10" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline331.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $1.4 - 2.3\,$ </span></span> </span> </span>GHz, Zinn et al. <a class="xref bibr" href="#r130"><span class="show-for-sr">Reference Zinn, Middelberg, Norris, Hales, Mao and Randall</span>2012</a>), may help quantify the fractions of peaked-spectrum sources with different turnover frequencies, and this will be the focus of a follow-up work.</p> </div> </div> <div class="sec conclusions" data-magellan-destination="s7" id="s7"> <h2 class="A"><span class="label">7.</span> Conclusion</h2> <p class="p"> We have presented the first pilot survey of EMU, using the ASKAP telescope.</p> <p class="p"> The resulting images reach an rms sensitivity of about 25–30 <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline332.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="74" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline332.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> rms at a spatial resolution of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline333.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline333.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>11–18 arcsec and result in a catalogue of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline334.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline334.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>220 000 sources, of which <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline335.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="12" height="4" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline335.png" data-zoomable="false"> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> $\sim$ </span></span> </span> </span>180 000 are compact. We have presented the catalogue of compact sources, together with optical and infrared cross-identifications and redshifts. We have also shown some preliminary science results, on both these compact sources and on diffuse sources, which will be discussed in more detail in subsequent papers.</p> <p class="p"> The results presented here testify to the outstanding observational characteristics of ASKAP, including its high survey speed and unprecedented sensitivity to low surface brightness emission. Nevertheless, at the time of the pilot survey, several aspects of ASKAP correlator operation, calibration, and data processing were incomplete. We therefore expect future results from ASKAP, including the main EMU survey, to have even better sensitivity and dynamic range than the results presented in this paper.</p> </div> </div> <div class="back"> <div class="ack"> <h2 class="A"> Acknowledgements</h2> <p class="p"> We thank an anonymous referee for valuable feedback on an earlier iteration of this paper. The Australian SKA Pathfinder is part of the Australia Telescope National Facility which is managed by CSIRO. Operation of ASKAP is funded by the Australian Government with support from the National Collaborative Research Infrastructure Strategy. Establishment of the Murchison Radio-astronomy Observatory was funded by the Australian Government and the Government of Western Australia. ASKAP uses advanced supercomputing resources at the Pawsey Supercomputing Centre. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. This work makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. It also makes use of data from the European Space Agency (ESA) mission Gaia, and we acknowledge the institutions listed on <a class="uri" href="https://gea.esac.esa.int/archive/documentation/GEDR3/Miscellaneous/sec_acknowl/">https://gea.esac.esa.int/archive/documentation/GEDR3/Miscellaneous/sec/_acknowl/</a> It also uses public archival data from the DES and we acknowledge the institutions listed on <a class="uri" href="https://www.darkenergysurvey.org/the-des-project/data-access/">https://www.darkenergysurvey.org/the-des-project/</a> <a class="uri" href="https://www.darkenergysurvey.org/the-des-project/data-access/">data-access/.</a> This research has made use of the ‘Aladin sky atlas’ developed at CDS, Strasbourg Observatory, France (Boch & Fernique <a class="xref bibr" href="#r9"><span class="show-for-sr">Reference Boch, Fernique, Manset and Forshay</span>2014</a>). This research uses services or data provided by the Astro Data Lab at NSF’s National Optical-Infrared Astronomy Research Laboratory. NOIRLab is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. Partial support for LR comes from US National Science Foundation Grant AST 17-14205 to the University of Minnesota. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. CLH acknowledges support from the Leverhulme Trust through an Early Career Research Fellowship. IP acknowledges support from CSIRO under its Distinguished Research Visitor Programme, and from INAF through the SKA/CTA PRIN “FORECaST” and the PRIN MAIN STREAM “SAuROS” projects. MJJ acknowledges support from the National Research Foundation of Korea under the program nos. 2017R1A2B2004644 and 2017R1A4A1015178. CJR acknowledges financial support from the ERC Starting Grant ‘DRANOEL’, number 714245. HA benefited from grant CIIC 174/2021 of Universidad de Guanajuato.</p> </div> </div> </div></div> <hr aria-hidden="true" class="list-divider separator default" data-v-7036083a> <div id="footnotes-list" class="circle-list"><h2>Footnotes</h2> <div data-type="fulltextNote" id="fn1" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">a</sup> </span> <a class="uri" href="https://confluence.csiro.au/display/askapsst/Continuum+Validation">https://confluence.csiro.au/display/askapsst/Continuum+Validation</a> </p> </div></div></div><div data-type="fulltextNote" id="fn2" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">b</sup> </span> <a class="uri" href="https://confluence.csiro.au/display/askapsst/Continuum+validation+metrics">https://confluence.csiro.au/display/askapsst/Continuum+validation+metrics</a> </p> </div></div></div><div data-type="fulltextNote" id="fn3" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">c</sup> </span> Reports are available from <a class="uri" href="https://www.atnf.csiro.au/research/ASKAP/ASKAP-validation/commissioning/AS101/SB9325/validation_image.i.SB9325.cont.taylor.0.restored__askapops_2019-09-03-101300/">https://www.atnf.csiro.au/research/ASKAP/ASKAP-</a> <a class="uri" href="https://www.atnf.csiro.au/research/ASKAP/ASKAP-validation/commissioning/AS101/SB9325/validation_image.i.SB9325.cont.taylor.0.restored__askapops_2019-09-03-101300/">validation/commissioning/AS101/SB9325/validation_image.i.SB9325.cont.taylor.0.restored_</a> <a class="uri" href="https://www.atnf.csiro.au/research/ASKAP/ASKAP-validation/commissioning/AS101/SB9325/validation_image.i.SB9325.cont.taylor.0.restored__askapops_2019-09-03-101300/">askapops_2019-09-03-101300/</a> </p> </div></div></div><div data-type="fulltextNote" id="fn4" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">d</sup> </span> The metrics are described in detail in <a class="uri" href="https://confluence.csiro.au/display/askapsst/Continuum+validation+metrics">https://confluence.csiro.au/display/</a> <a class="uri" href="https://confluence.csiro.au/display/askapsst/Continuum+validation+metrics">askapsst/Continuum+validation+metrics</a> </p> </div></div></div><div data-type="fulltextNote" id="fn5" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">e</sup> </span> <a class="uri" href="https://www.atnf.csiro.au/research/ASKAP/ASKAP-validation/commissioning/AS101/">https://www.atnf.csiro.au/research/ASKAP/ASKAP-validation/commissioning/AS101/</a> </p> </div></div></div><div data-type="fulltextNote" id="fn6" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">f</sup> </span> <a class="uri" href="https://opal.atnf.csiro.au/">https://opal.atnf.csiro.au/</a> </p> </div></div></div><div data-type="fulltextNote" id="fn7" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">g</sup> </span> <a class="uri" href="https://casda.csiro.au">https://casda.csiro.au</a> </p> </div></div></div><div data-type="fulltextNote" id="fn8" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">h</sup> </span> <a class="uri" href="https://astroquery.readthedocs.io">https://astroquery.readthedocs.io</a> </p> </div></div></div><div data-type="fulltextNote" id="fn9" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">i</sup> </span> <a class="uri" href="https://apps.atnf.csiro.au/OMP/index.jsp">https://apps.atnf.csiro.au/OMP/index.jsp</a> </p> </div></div></div><div data-type="fulltextNote" id="fn10" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">j</sup> </span> An up-to-date database of these sources is maintained at <a class="uri" href="https://GalaxyClusters.com">GalaxyClusters.com</a>.</p> </div></div></div><div data-type="fulltextNote" id="fn11" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">k</sup> </span> <a class="uri" href="https://www.linea.gov.br/catalogs/wazp/">https://www.linea.gov.br/catalogs/wazp/</a> </p> </div></div></div><div data-type="fulltextNote" id="fn12" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div class="circle-list__item__grouped"><div class="circle-list__item__grouped__content"> <p class="p"><span class="label"> <sup class="sup">l</sup> </span> We use the SKADS 1.4 GHz flux scaled to 944 MHz assuming a spectral index of -0.8. We also apply a minimum flux density cut on the 944 MHz converted SKADS flux of <span data-mathjax-status="alt-graphic" class="inline-formula"> <span class="alternatives"> <img data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline299.png?pub-status=live" class="aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off" width="102" height="18" data-original-image="/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline299.png" data-zoomable="false" /> <span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on"> ${\sim}30 \mu\mathrm{Jy\ beam}^{-1}$ </span></span> </span> </span> </p> </div></div></div></div> <hr aria-hidden="true" class="list-divider separator default" data-v-7036083a> <div id="references-list" class="circle-list"><h2>References</h2> <div id="ref1" aria-flowto="reference-1-content reference-1-button" class="circle-list__item"> <div class="circle-list__item__indicator"></div> <div aria-hidden="true" data-test-hidden="true" class="circle-list__item__number"> </div> <div class="circle-list__item__grouped"><div id="reference-1-content" class="circle-list__item__grouped__content"><span class="string-name"><span class="surname">Abbott</span>, <span class="given-names">T. 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The symbols indicate the type of telescope used to make the survey, and are fully described in Norris (2017a). The dates and survey size are based on estimates made in 2017, and some later surveys (e.g. RACS McConnell et al. 2020, with 2.8 million sources) are missing from this plot. Survey abbreviations and references are given in Norris (2017a). The shading under the curve is merely to improve readability.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 1" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-17464-mediumThumb-S1323358021000424_fig2.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-55270-optimisedImage-S1323358021000424_fig2.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 2.</span> <span data-v-241a4b23><span class="p">Some of the ASKAP antennas equipped with phased array feeds, located in the Murchison Region of Western Australia. Photo credit: CSIRO</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 2" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-80652-mediumThumb-S1323358021000424_fig3.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-72019-optimisedImage-S1323358021000424_fig3.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 3.</span> <span data-v-241a4b23><span class="p">One of the phased array feeds. Each square on the chequerboard is an antenna element connected to two receivers. Photo credit: CSIRO</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 3" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab1.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab1.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Table 1.</span> <span data-v-241a4b23><span class="p">EMU Pilot Survey specifications.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 4" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab2.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab2.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Table 2.</span> <span data-v-241a4b23><span class="p">Cosmological parameters used in this paper and adopted for EMU-PS.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 5" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab3.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab3.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Table 3.</span> <span data-v-241a4b23><span class="p">EMU pilot observation details.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 6" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig4.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig4.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 4.</span> <span data-v-241a4b23><span class="p">The arrangement of the 36 ASKAP beams in the ‘closepack36’ configuration. The beams are numbered from 0 to 35 (diagram adapted from McConnell et al. 2019). The circles shown are for illustration only. For EMU-PS, the actual full width half maximum of each beam is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline45.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">${\sim}1.5^{\circ}$</span></span></span> at the band centre, and the pitch spacing is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline46.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$0.9^{\circ}$</span></span></span>, giving an approximately uniform sensitivity over the field of view.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 7" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-18841-mediumThumb-S1323358021000424_fig5.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-77890-optimisedImage-S1323358021000424_fig5.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 5.</span> <span data-v-241a4b23><span class="p">The sky tiling scheme adopted for the EMU-PS. The red rectangles covering the celestial sphere show the tiles planned for the EMU survey, and the orange area indicates the 10 tiles of the EMU-PS. The white strip shows the Galactic plane, and the south celestial pole is at the bottom of the figure.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 8" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig6.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig6.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 6.</span> <span data-v-241a4b23><span class="p">The location of the EMU Pilot Survey area on the sky within DES DR1, adapted from Abbott et al. (2018). The diagram is in equatorial coordinates, and the solid line marks the Galactic plane, flanked by two dashed lines showing Galactic latitude <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline49.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\pm 10 ^{\circ}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 9" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab4.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab4.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Table 4.</span> <span data-v-241a4b23><span class="p">EMU pilot processing parameters. The first column shows the parameter name used by ASKAPsoft.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 10" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab5.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab5.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Table 5.</span> <span data-v-241a4b23><span class="p">Results of tests to measure the optimum robustness.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 11" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig7.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig7.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 7.</span> <span data-v-241a4b23><span class="p">The arrangement of the ten individual ASKAP tiles on the sky for EMU-PS with their SBID numbers as listed in Table 3. The rectangles are separated in this diagram for clarity, but there is actually overlapping coverage as illustrated by the greyscale background.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 12" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig8.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig8.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 8.</span> <span data-v-241a4b23><span class="p">An example validation report for one of the processing runs for SB9325, including the metrics and their flags. A higher-resolution version is available online2.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 13" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig9.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig9.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 9.</span> <span data-v-241a4b23><span class="p">The resulting native resolution (<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline86.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$13'' \times 11''$</span></span></span>) image of the <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline87.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$270 \,\mathrm{deg}^2$</span></span></span> EMU Pilot Survey, containing about 220 000 radio sources. The rms noise level is 25–30 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline88.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mu\mathrm{Jy\ beam}^{-1}$</span></span></span>, and the peak flux density is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline89.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$3.14 \mathrm{Jy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 14" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab6.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab6.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Table 6.</span> <span data-v-241a4b23><span class="p">Numbers of sources remaining after each stage of the value-added processing.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 15" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig10.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig10.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 10.</span> <span data-v-241a4b23><span class="p">The measured spectral index as a function of flux density. The two solid lines show the 3<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline94.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\sigma$</span></span></span> uncertainty for a source of spectral index -0.8. Note the excess of sources with a positive spectral index, discussed in Section 6.9.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 16" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig11.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig11.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 11.</span> <span data-v-241a4b23><span class="p">A histogram of measured spectral index as a function of flux density, for the 10458 sources with flux density <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline97.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$>$</span></span></span> 2.5 mJy.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 17" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig12.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig12.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 12.</span> <span data-v-241a4b23><span class="p">The fraction of simple radio sources (as listed in Table 6) matched with a CWISE source as a function of separation, both for unshifted data and for data shifted by one arcmin.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 18" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig13.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig13.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 13.</span> <span data-v-241a4b23><span class="p">The fraction of radio sources with a CWISE position matched with a DES DR1 source as a function of separation, both for unshifted data and for data shifted by one arcmin.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 19" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig14.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig14.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 14.</span> <span data-v-241a4b23><span class="p">A plot showing the difference in position of radio sources compared to the matching CWISE source in the W1 band, showing a mean offset of <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline101.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\sim$</span></span></span>0.3 arcsec, which is small compared to the 18 arcsec resolution of the convolved data. The horizontal axis is Right Ascension and the vertical axis is Declination.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 20" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig15.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig15.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 15.</span> <span data-v-241a4b23><span class="p">The ratio of peak flux densities between EMU-PS and SUMSS for simple sources with EMU-PS flux densities <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline102.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$>$</span></span></span> 6 mJy, and with catalogued positions within 3 arcsec.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 21" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-27981-mediumThumb-S1323358021000424_fig16.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-87086-optimisedImage-S1323358021000424_fig16.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 16.</span> <span data-v-241a4b23><span class="p">A typical section of the survey field, covering about <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline103.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$0.3 \,\mathrm{deg}^2$</span></span></span> (or about one thousandth of the area of the EMU Pilot Survey) which contains about 250 radio sources). On the left is the SUMSS image (Mauch et al. 2003) and on the right is the EMU-PS image. Prominent in this image is the Giant Radio Galaxy ESO 234-68. The maximum flux density of ESO 234-68 in the EMU-PS image is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline104.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$58.8 \mathrm{mJy\ beam}^{-1}$</span></span></span>, and that of the strong source at the bottom of the image (PMN J2045-5135) is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline105.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$1.06 \mathrm{Jy beam}^{-1}$</span></span></span>. The rms of the EMU-PS image is 25–30 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline106.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mu\mathrm{Jy\ beam}^{-1}$</span></span></span>, and that of the SUMSS image is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline107.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">${\sim}1.25\ \mathrm{mJy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 22" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-25420-mediumThumb-S1323358021000424_fig17.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-70959-optimisedImage-S1323358021000424_fig17.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 17.</span> <span data-v-241a4b23><span class="p">A sample of the final image, showing the three data products on a region, covered by three tiles, containing two of the ‘Odd Radio Circles’(Norris et al. 2021): (a) the initial public data release from a single tile (SB9351) (resolution 11 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline116.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\times$</span></span></span> 13 arcsec, rms = <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline117.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$40 \,\mu\mathrm{Jy\ beam}^{-1}$</span></span></span>, (b) the added-value ‘native’ data release with 11<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline118.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\times$</span></span></span>13 arcsec resolution, from the merged tiles, rms = 25 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline119.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mu\mathrm{Jy\ beam}^{-1}$</span></span></span>, and (c) the added-value ‘convolved’ data release with 18 arcsec resolution, rms = 25 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline120.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mu\mathrm{Jy\ beam}^{-1}$</span></span></span>. The peak flux density in this image is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline121.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$4.6\ \mathrm{mJy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 23" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab7.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab7.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Table 7.</span> <span data-v-241a4b23><span class="p">Available data products, including Digital Object Identifiers (DOIs) that can be used to access the data described in this paper.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 24" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig18.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig18.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 18.</span> <span data-v-241a4b23><span class="p">The sensitivity of EMU-PS as a function of spatial scale. The plot was made using visibility data from a single beam and pointing of an interleaved observation (2-h observation, 288-MHz bandwidth, scaled to the EMU-PS observing frequency of 944 MHz) which was filled with Gaussian noise and various uv tapers were applied to shape the beam size. We then measured the image noise (effectively the sensitivity at the scale associated with the uv taper). The two plots show the same result over different ranges of spatial scale.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 25" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig19.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig19.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 19.</span> <span data-v-241a4b23><span class="p">Normalised differential source counts derived from the <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline133.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$270\ \mathrm{deg}^2$</span></span></span> EMU-PS survey for the <span class="italic">island</span> catalogue (black filled diamonds) and for simple sources only (black empty diamonds). The counts have been rescaled from 943.5 MHz to 1.4 GHz by assuming <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline134.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\alpha=-0.7$</span></span></span>. Also shown for comparison are the counts derived from 1.4 GHz <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline135.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$>$</span></span></span> degree-scale surveys (symbols and colours as indicated in the figure). Vertical bars represent Poissonian errors on the normalised counts. Systematic errors due to incompleteness corrections and spectral index assumptions are approximately included in the size of the plotted symbols. The result of the <span class="italic">P</span>(<span class="italic">D</span>) analysis performed by (Vernstrom et al. 2014, rescaled from 3 to 1.4 GHz by assuming <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline136.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\alpha $</span></span></span> = <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline137.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$-$</span></span></span>0.7) is indicated in dark green. The black solid line represents the predicted counts from 200 sq. degr. of the S3-SEX simulations (Wilman et al. 2008). The light blue and yellow shaded areas illustrate the predicted cosmic variance effects for survey coverages of 5 and <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline138.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$10\ \mathrm{deg}^2$</span></span></span>, respectively (obtained by splitting the S3-SEX simulation in 40 5-<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline139.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mathrm{deg}^2$</span></span></span> and 20 10-<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline140.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mathrm{deg}^2$</span></span></span> fields, respectively). The <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline141.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$25\ \mathrm{deg}^2$</span></span></span> medium tier of the more recent T-RECS simulations (Bonaldi et al. 2019) is represented by the purple shaded area. Finally, the Mancuso et al. (2017) radio source evolutionary model is shown by the light green line.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 26" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig20.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig20.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 20.</span> <span data-v-241a4b23><span class="p">The EMU-PS preliminary <span class="italic">P</span>(<span class="italic">D</span>) distributions. The solid black line is the probability distribution made from sections of the pilot away from bright sources. The upper right inset shows bright flux density tail of the <span class="italic">P</span>(<span class="italic">D</span>) distributions. The blue dot-dashed line shows a Gaussian noise distribution of <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline160.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\sigma= 23 \mu\mathrm{Jy\ beam}^{-1}$</span></span></span>. The red dashed line shows the predicted or model <span class="italic">P</span>(<span class="italic">D</span>) generated from the source count shown in the lower right inset.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 27" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-80985-mediumThumb-S1323358021000424_fig21.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-15185-optimisedImage-S1323358021000424_fig21.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 21.</span> <span data-v-241a4b23><span class="p">A peculiar radio source found in the EMU Pilot Survey, consisting of a group of distorted radio components, collectively known as PKS 2130–538, and nicknamed ‘the dancing ghosts’. The two host galaxies (<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline163.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$z \sim 0.077$</span></span></span>) are seen at the centre of the narrow jets (shown with numbers in the figure to indicate their putative host) which expand into diffuse lobes, probably bent by interactions. On the left is the total intensity greyscale image (shown in turquoise), superimposed on a background of the DES optical image, assembled from the r, g, and i images. On the right is the total intensity image of PKS 2130-538, colour-coded by spectral index. The unconventional colour scheme was constructed using sequential colours on the ‘colour wheel’ (e.g. Itten 1970). The colours were fixed in luminosity, that is, fixed to be constant in luminosity-chroma-hue colour space (Ferrand 2019). In this way, the brightness level on the image represents only the total intensity values. The colour bar indicates the spectral index at a single fixed intensity. Since the spectral index map in this colour scheme was multiplied by the total intensity map, darker versions of colours are associated with fainter regions in the data. The peak flux density in this image is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline164.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$103\ \mathrm{mJy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 28" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-88490-mediumThumb-S1323358021000424_fig22.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-13700-optimisedImage-S1323358021000424_fig22.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 22.</span> <span data-v-241a4b23><span class="p">Another peculiar radio source found in the EMU Pilot Survey: a double-lobed radio AGN, known as PMN J2041–5256, with a curious ‘double’ bent tail. The radio data from EMU-PS has been ‘stretched’ to show the faint emission, and then coloured turquoise, and adjusted to emphasise the double tail. DES g-, r-, and i-band data are combined to form the background, which is combined with the radio data using a layer mask in GIMP. Embedded in the tails are several radio sources that may be unrelated to the tailed galaxy. The peak flux density in this image is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline175.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$58.3\ \mathrm{mJy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 29" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig23.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig23.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 23.</span> <span data-v-241a4b23><span class="p">The ‘Smoking Gun’ Galaxy EMU PS J204835.0–491137 consists of the two diffuse radio clouds seen in this image. These are presumably the remnants of a classical double-lobed radio galaxy in which the central engine has switched off. The labels A and B indicate two possible host galaxies, discussed in the text. The peak flux density in this image is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline176.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$0.87\ \mathrm{mJy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 30" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig24.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig24.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 24.</span> <span data-v-241a4b23><span class="p">EMU PS J210700.0–501128.8 is an ambiguous case, appearing at first to be a double-lobed source with material blown to the east. But with no host between the bright patches, and the southern bright component coincident with a quasar, marked with an ‘X’, these may be two independent sources with serendipitously similar appearances The peak flux density in this image is <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline180.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$11.6\ \mathrm{mJy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 31" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-62673-mediumThumb-S1323358021000424_fig25.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-49417-optimisedImage-S1323358021000424_fig25.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 25.</span> <span data-v-241a4b23><span class="p">An image of the first ‘Odd Radio Circle’, or ORC, found in EMU-PS (Norris et al. 2021). It has no optical counterpart to the diffuse ring, or to other diffuse structure, but has a galaxy at its centre which may be the origin of the ring. The image is based on EMU-PS data at native resolution but enhanced to show faint features as described in Norris et al. (2021), particularly the internal structure or “spokes” of the ORC. Radio data are shown in green, and DES optical data are shown in turquoise, magenta, yellow and red, and mainly appear in this image as white.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 32" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-77883-mediumThumb-S1323358021000424_fig26.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-91916-optimisedImage-S1323358021000424_fig26.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 26.</span> <span data-v-241a4b23><span class="p">A selection of ASKAP-detected nearby galaxies in the EMU-PS. Optical DSS2 <span class="italic">R</span>-band images are overlaid with ASKAP radio continuum contours. The contour levels are –0.09, 0.09 (<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline195.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">${\sim}3 \sigma$</span></span></span>), 0.18, 0.36, 0.75, 1.5, 3.0, 7.5, 15.0, and <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline196.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$30\ \mathrm{mJy\,beam}^{-1}$</span></span></span>. The convolved 18 arcsec beam is shown in the bottom left corner of each panel. The galaxy name and heliocentric velocity (all but one, ESO233-IG004, from HIPASS) are also displayed. The velocity of ESO233-IG004 is taken from Jones et al. (2009).</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 33" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-80083-mediumThumb-S1323358021000424_fig27.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-72933-optimisedImage-S1323358021000424_fig27.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 27.</span> <span data-v-241a4b23><span class="p">DES-DR1 optical composite image of the nearby face-on spiral galaxy NGC 7125 overlaid with contours from the EMU-PS. The contour levels are: 0.1, 0.25, 0.5, 1.0, 1.3, 1.6, 2.0, and <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline215.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$2.4\ \mathrm{mJy\,beam}^{-1}$</span></span></span>. NGC 7125 and its neighbour NGC 7216 form an interacting galaxy pair (HIPASS J2149–60) with a large pool of hydrogen gas for star formation.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 34" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-45019-mediumThumb-S1323358021000424_fig28.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-06142-optimisedImage-S1323358021000424_fig28.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 28.</span> <span data-v-241a4b23><span class="p">(Left) The Giant Radio Galaxy (GRG) EMU PS J205139.8–570434, with radio (at native resolution) shown in greyscale, overlaid on the DES DR1 colour image. The GRG consists of the roughly north-south jet and the two diffuse plumes above and below it. The strong source to the east, surrounded by diffraction rings, is the well-studied galaxy IC 5063. (Right) A contour diagram of the central part of the GRG at 18 arcsec resolution, overlaid on the DES DR1 colour image. Contour levels are 3, 7, 12, and <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline242.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$18\ \mathrm{mJy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 35" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig29.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig29.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 29.</span> <span data-v-241a4b23><span class="p">The histogram of EMU-PS flux densities for 6dFGS galaxies with <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline253.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">${\rm H\alpha}$</span></span></span> emission and <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline254.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$K<12.65$</span></span></span>, along with the corresponding histogram of flux densities measured at offset positions. Just 17 of the 623 6dFGS galaxies with detectable <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline255.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">${\rm H\alpha}$</span></span></span> emission have radio flux densities below 75 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline256.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mu\mathrm{Jy\ beam}^{-1}$</span></span></span>.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 36" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig30.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig30.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 30.</span> <span data-v-241a4b23><span class="p">The EMU-PS flux densities of <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline257.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$K<12$</span></span></span> galaxies with and without <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline258.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">${\rm H\alpha}$</span></span></span> emission as a function of absolute magnitude. The dashed line shows <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline259.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$75\,{\rm \mu Jy}$</span></span></span>, roughly corresponding to <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline260.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$3\sigma$</span></span></span>. Almost all star-forming galaxies are detected by the EMU-PS. While low mass passive galaxies can have no detectable radio continuum emission, all but one <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline261.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$M_K<-26$</span></span></span> passive galaxy has a positive radio continuum flux density.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 37" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig31.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig31.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 31.</span> <span data-v-241a4b23><span class="p">The number of cross-matches between DES counterparts to EMU-PS sources, and Gaia sources, for unshifted data (blue), and data shifted by one arcmin (orange).</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 38" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig32.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig32.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 32.</span> <span data-v-241a4b23><span class="p">The AllWISE colour-colour plot for EMU-PS sources cross-matched with Gaia, colour-coded according to their measured proper motion. The dashed lines divide the graph into the regions identified by Jarrett et al. (2017).</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 39" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-85763-mediumThumb-S1323358021000424_fig33.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-63763-optimisedImage-S1323358021000424_fig33.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 33.</span> <span data-v-241a4b23><span class="p">Multi-wavelength composite image of SPT-CL J2023<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline262.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$-$</span></span></span>5535. Contours denote the EMU-PS surface brightness at 944 MHz at 18 arcsec resolution, at <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline263.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$3\sigma_{\rm{rms}} \times 2^{n}$</span></span></span> where <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline264.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$n=0, 1, 2, 3, 4$</span></span></span> and <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline265.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\sigma_{rms}=\sim25$</span></span></span><span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline266.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mu\mathrm{Jy\ beam}^{-1}$</span></span></span>. Background colourmap shows a composite <span class="italic">g</span>, <span class="italic">r</span>, and <span class="italic">i</span> image from DECam. X-ray emission from <span class="italic">Chandra</span> is also overlaid in red. New diffuse radio sources identified by HyeongHan et al. (2020) are also indicated.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 40" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-42254-mediumThumb-S1323358021000424_fig34.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-40250-optimisedImage-S1323358021000424_fig34.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 34.</span> <span data-v-241a4b23><span class="p">Multi-wavelength composite image of the cluster SPT-CL J2032<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline267.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$-$</span></span></span>5627. Colour map and contours are the same as Figure 33, but with <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline268.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$25\,\mathrm{ks}$</span></span></span> XMM- <span class="italic">Newton</span> surface brightness shown in red. It appears that the cluster hosts one of the rare class of double-radio relics with the northern (A and B) and southern (C) relics as indicated.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 41" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-60188-mediumThumb-S1323358021000424_fig35.jpg" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary-alt:20210906095333-28830-optimisedImage-S1323358021000424_fig35.jpg" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 35.</span> <span data-v-241a4b23><span class="p">Radio contours overlaid on a multi-wavelength (irg) composite image of 6dFGS g2212485-614658 from DES. The radio image was made from the EMU-PS native resolution data by subtracting four unresolved sources and then convolving to a resolution of 18 arcsec. Contours are at 75, 150, 300, and 600 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline280.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\mu\mathrm{Jy\ beam}^{-1}$</span></span></span>. The subtracted sources were at 22:12:48.64 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline281.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$-$</span></span></span>61:46:58.5 (14.9 mJy), 22:12:43.04 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline282.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$-$</span></span></span>61:46:50.1 (0.3 mJy), 22:12:51.19 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline283.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$-$</span></span></span>61:46:15.5 (0.2 mJy), 22:12:37.17 <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline284.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$-$</span></span></span>61:47:24.5 (0.1 mJy)</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 42" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig36.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig36.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 36.</span> <span data-v-241a4b23><span class="p">The number of sources in the EMU-PS with a flux density greater than some limit (<span class="italic">S</span>), as a function of that limit, compared to scaled predictions from the SKADS and T-RECS simulated catalogues. The dashed black vertical line gives the <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline301.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$500\mu\mathrm{Jy}$</span></span></span> limit we assume for the clustering analysis presented in this paper. There is some discretisation of the prediction for the larger flux density limits, due to a scaling of some small integer value for the original prediction that was made for a much smaller value.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 43" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig37.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig37.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 37.</span> <span data-v-241a4b23><span class="p">The predicted number of sources in the EMU Pilot Survey as a function of redshift, generated by scaling the predictions from the SKADS and T-RECS simulated catalogues. This assumes a flux density limit of <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline305.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$500\mu\mathrm{Jy}$</span></span></span></span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 44" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig38.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig38.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 38.</span> <span data-v-241a4b23><span class="p">The measured angular correlation function (ACF) <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline309.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$w(\theta)$</span></span></span> as a function of angular separation with one-sigma error bar computed from bootstrap re-sampling from 100 bootstraps. The correlation function is measured from the integrated flux-corrected EMU-PS island catalogue, using all sources above a flux density limit of <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline310.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$500\mu\mathrm{Jy}$</span></span></span>. The blue curve is the theoretical prediction for the correlation function, assuming the Planck 2018 best fit cosmology and a SKADS model for the number distribution with redshift and the bias. No fitting of the cosmological or bias parameters was performed to change the prediction curve. As negative values cannot be shown on a log scale, in bins where the ACF becomes negative, we show (in red) the value of (-ACF) instead.</span></span></p></div> </div></div> <hr aria-hidden="true" class="separator dashed" data-v-7036083a data-v-241a4b23></div><div data-v-241a4b23><div class="figures__item" data-v-241a4b23><div class="figures__item__image-box" data-v-241a4b23><button class="figures__ref" data-v-241a4b23> View in content </button> <img src="data:image/gif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==" alt="Figure 45" data-zoomable="true" data-src="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig39.png" data-enlarged-image="https://static.cambridge.org/binary/version/id/urn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig39.png" class="graphic" data-v-241a4b23></div> <div data-v-241a4b23><div class="caption" data-v-241a4b23><p data-v-241a4b23><span class="label" data-v-241a4b23>Figure 39.</span> <span data-v-241a4b23><span class="p">The spectral index distributions for unresolved (<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline315.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\Psi < 2''$</span></span></span>, blue) and resolved (<span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline316.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$\Psi > 20''$</span></span></span>, red) EMU components. The three panels show different minimum brightness levels, corresponding to <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline317.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$S_{\text{peak}} > 1\,\mathrm{mJy\ beam}^{-1}$</span></span></span>, <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline318.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$S_{\text{peak}} > 3\,\mathrm{mJy\ beam}^{-1}$</span></span></span>, and <span class="alternatives"><img class="inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off" data-mimesubtype="png" data-type="" src="${staticDomain}/content/id/urn:cambridge.org:id:article:S1323358021000424/resource/name/S1323358021000424_inline319.png?pub-status=live" /><span class="mathjax-tex-wrapper" data-mathjax-type="texmath"><span class="tex-math mathjax-tex-math mathjax-on">$S_{\text{peak}} > 10\,\mathrm{mJy\ beam}^{-1}$</span></span></span> from top to bottom. The legend in each panel denotes the number of components contributing to each distribution shown. Each plot is normalised to the area under the curve.</span></span></p></div> </div></div> </div></div>    <div id="addendum-tab" class="addendums tab-pane" data-v-0947a2a3><h2 class="addendums__header" data-v-0947a2a3> An addendum has been issued for this article: </h2> <div class="container-fluid" data-v-0947a2a3><div class="row addendums__articles-box" data-v-0947a2a3><div class="article-card col-sm-6" data-v-a97137fe data-v-0947a2a3><p class="article-title" data-v-a97137fe><a href="/core/product/E1EA0E6492F5AC02B9D448923634EAA0" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>The Evolutionary Map of the Universe Pilot Survey – ADDENDUM </span> </a></p> <div class="authors" data-v-a97137fe><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Ray%20P.%20Norris&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Ray P. Norris </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Joshua%20Marvil&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Joshua Marvil </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=J.%20D.%20Collier&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>J. D. Collier </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Anna%20D.%20Kapi%C5%84ska&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Anna D. Kapińska </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Andrew%20N.%20O%E2%80%99Brien&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Andrew N. O’Brien </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=L.%20Rudnick&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>L. Rudnick </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Heinz%20Andernach&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Heinz Andernach </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Jacobo%20Asorey&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Jacobo Asorey </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Michael%20J.%20I.%20Brown&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Michael J. I. Brown </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Marcus%20Br%C3%BCggen&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Marcus Brüggen </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Evan%20Crawford&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Evan Crawford </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Jayanne%20English&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Jayanne English </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Syed%20Faisal%20ur%20Rahman&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Syed Faisal ur Rahman </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Miroslav%20D.%20Filipovi%C4%87&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Miroslav D. Filipović </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Yjan%20Gordon&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Yjan Gordon </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=G%C3%BClay%20G%C3%BCrkan&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Gülay Gürkan </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Catherine%20Hale&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Catherine Hale </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Andrew%20M.%20Hopkins&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Andrew M. Hopkins </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Minh%20T.%20Huynh&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Minh T. Huynh </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Kim%20HyeongHan&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Kim HyeongHan </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=M.%20James%20Jee&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>M. James Jee </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=B%C3%A4rbel%20S.%20Koribalski&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Bärbel S. Koribalski </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Emil%20Lenc&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Emil Lenc </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Kieran%20Luken&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Kieran Luken </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=David%20Parkinson&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>David Parkinson </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Isabella%20Prandoni&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Isabella Prandoni </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Wasim%20Raja&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Wasim Raja </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Thomas%20H.%20Reiprich&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Thomas H. Reiprich </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Christopher%20J.%20Riseley&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Christopher J. Riseley </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Stanislav%20S.%20Shabala&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Stanislav S. Shabala </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Jaimie%20R.%20Sheil&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Jaimie R. Sheil </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Tessa%20Vernstrom&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Tessa Vernstrom </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Matthew%20T.%20Whiting&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Matthew T. Whiting </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=James%20R.%20Allison&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>James R. Allison </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=C.%20S.%20Anderson&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>C. S. Anderson </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Lewis%20Ball&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Lewis Ball </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Martin%20Bell&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Martin Bell </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=John%20Bunton&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>John Bunton </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=T.%20J.%20Galvin&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>T. J. Galvin </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Neeraj%20Gupta&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Neeraj Gupta </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Aidan%20Hotan&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Aidan Hotan </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Colin%20Jacka&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Colin Jacka </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Peter%20J.%20Macgregor&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Peter J. Macgregor </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Elizabeth%20K.%20Mahony&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Elizabeth K. Mahony </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Umberto%20Maio&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Umberto Maio </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Vanessa%20Moss&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Vanessa Moss </span> </a><span data-v-a97137fe>,</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=M.%20Pandey-Pommier&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>M. Pandey-Pommier </span> </a><span data-v-a97137fe> and</span> </span><span data-v-a97137fe><a href="/core/search?filters%5BauthorTerms%5D=Maxim%20A.%20Voronkov&eventCode=SE-AU" class="app-link app-link__text app-link--accent" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Maxim A. Voronkov </span> </a><span data-v-a97137fe></span> </span></div> <div data-v-a97137fe><a href="/core/product/EA97E060D413517C6C4433BED25DDCA9" class="app-link app-link__text app-link--underlined" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Publications of the Astronomical Society of Australia </span> </a><span data-v-a97137fe>,</span> <a href="/core/product/0DF0382C08DE7EF5FF05BE7D545D6C1B" class="app-link app-link__text app-link--underlined" data-v-63dfaf6e data-v-a97137fe><span class="text" data-v-63dfaf6e>Volume 39 </span> </a> </div></div></div></div></div>     <div id="metrics-tab" publication-date="07 September 2021" class="metrics tab-pane" data-v-c41a0c86><div class="app-loader" data-v-c41a0c86></div></div></div></div> </div> <div role="complementary" aria-label="related contents" class="column__main__right" data-v-01274b1d><div class="access-block row access-status" data-v-5fad35b8 data-v-01274b1d><span class="has-access" data-v-5fad35b8><img 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Jee",nameStyle:c,affiliations:[{text:A},{text:bt}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bu,searchUrl:bv,orcidUrl:c},{givenNames:bw,surname:bx,nameStyle:c,affiliations:[{text:i},{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:by,searchUrl:bz,orcidUrl:c},{givenNames:bA,surname:bB,nameStyle:c,affiliations:[{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bC,searchUrl:bD,orcidUrl:"https:\u002F\u002Forcid.org\u002F0000-0002-9994-1593"},{givenNames:bE,surname:bF,nameStyle:c,affiliations:[{text:i},{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bG,searchUrl:bH,orcidUrl:c},{givenNames:bI,surname:bJ,nameStyle:c,affiliations:[{text:bK},{text:bL}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bM,searchUrl:bN,orcidUrl:"https:\u002F\u002Forcid.org\u002F0000-0002-7464-2351"},{givenNames:bO,surname:bP,nameStyle:c,affiliations:[{text:B}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bQ,searchUrl:bR,orcidUrl:c},{givenNames:bS,surname:bT,nameStyle:c,affiliations:[{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bU,searchUrl:bV,orcidUrl:c},{givenNames:bW,surname:bX,nameStyle:c,affiliations:[{text:bY}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bZ,searchUrl:b_,orcidUrl:c},{givenNames:b$,surname:ca,nameStyle:c,affiliations:[{text:k},{text:B},{text:cb}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cc,searchUrl:cd,orcidUrl:c},{givenNames:ce,surname:cf,nameStyle:c,affiliations:[{text:cg}],isCorresponding:b,notes:a,isAnonymous:b,fullName:ch,searchUrl:ci,orcidUrl:c},{givenNames:cj,surname:ck,nameStyle:c,affiliations:[{text:y}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cl,searchUrl:cm,orcidUrl:c},{givenNames:cn,surname:co,nameStyle:c,affiliations:[{text:k}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cp,searchUrl:cq,orcidUrl:c},{givenNames:cr,surname:cs,nameStyle:c,affiliations:[{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:ct,searchUrl:cu,orcidUrl:c},{givenNames:cv,surname:cw,nameStyle:c,affiliations:[{text:h},{text:"Sub-Dept. of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Rd., Oxford, OX1 3RH, UK"}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cx,searchUrl:cy,orcidUrl:c},{givenNames:cz,surname:cA,nameStyle:c,affiliations:[{text:h},{text:r}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cB,searchUrl:cC,orcidUrl:"https:\u002F\u002Forcid.org\u002F0000-0002-6243-7879"},{givenNames:cD,surname:cE,nameStyle:c,affiliations:[{text:h},{text:"SKA Observatory, Jodrell Bank, Lower Withington, Macclesfield, Cheshire SK11 9FT, UK"}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cF,searchUrl:cG,orcidUrl:c},{givenNames:cH,surname:cI,nameStyle:c,affiliations:[{text:h},{text:cJ}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cK,searchUrl:cL,orcidUrl:c},{givenNames:cM,surname:cN,nameStyle:c,affiliations:[{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cO,searchUrl:cP,orcidUrl:c},{givenNames:cQ,surname:cR,nameStyle:c,affiliations:[{text:i},{text:k},{text:cS}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cT,searchUrl:cU,orcidUrl:c},{givenNames:cV,surname:cW,nameStyle:c,affiliations:[{text:h},{text:"IUCAA, Post Bag 4, Ganeshkhind, Pune University Campus,Pune 411 007, India"}],isCorresponding:b,notes:a,isAnonymous:b,fullName:cX,searchUrl:cY,orcidUrl:c},{givenNames:cZ,surname:c_,nameStyle:c,affiliations:[{text:k}],isCorresponding:b,notes:a,isAnonymous:b,fullName:c$,searchUrl:da,orcidUrl:"https:\u002F\u002Forcid.org\u002F0000-0001-7464-8801"},{givenNames:db,surname:dc,nameStyle:c,affiliations:[{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:dd,searchUrl:de,orcidUrl:c},{givenNames:df,surname:dg,nameStyle:c,affiliations:[{text:i},{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:dh,searchUrl:di,orcidUrl:"https:\u002F\u002Forcid.org\u002F0000-0003-1584-5930"},{givenNames:dj,surname:dk,nameStyle:c,affiliations:[{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:dl,searchUrl:dm,orcidUrl:c},{givenNames:dn,surname:do0,nameStyle:c,affiliations:[{text:dp}],isCorresponding:b,notes:a,isAnonymous:b,fullName:dq,searchUrl:dr,orcidUrl:c},{givenNames:ds,surname:dt,nameStyle:c,affiliations:[{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:du,searchUrl:dv,orcidUrl:c},{givenNames:F,surname:dw,nameStyle:c,affiliations:[{text:dx}],isCorresponding:b,notes:a,isAnonymous:b,fullName:dy,searchUrl:dz,orcidUrl:c},{givenNames:dA,surname:dB,nameStyle:c,affiliations:[{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:dC,searchUrl:dD,orcidUrl:c}]},translators:{contributors:[],label:"Translated by"}},collections:[{link:"\u002Fcore\u002Fproduct\u002Fidentifier\u002FASKAP\u002Ftype\u002FBESPOKE_COLLECTION",id:"ASKAP",title:"Australian SKA Pathfinder"}],publishedDate:"07 September 2021",keywords:[{url:"\u002Fcore\u002Fsearch?filters[keywords]=Extragalactic astronomy",name:"Extragalactic astronomy"},{url:"\u002Fcore\u002Fsearch?filters[keywords]=Radio astronomy",name:"Radio astronomy"},{url:"\u002Fcore\u002Fsearch?filters[keywords]=Sky surveys",name:"Sky surveys"}],openPracticeBadges:[],doi:{url:"https:\u002F\u002Fdoi.org\u002F10.1017\u002Fpasa.2021.42",value:"10.1017\u002Fpasa.2021.42"},copyright:{statement:["© The Author(s), 2021. Published by Cambridge University Press on behalf of the Astronomical Society of Australia"],holder:["Astronomical Society of Australia"],year:[2021]},creativeCommons:c,acceptedManuscript:b,type:"research-article",typeDescription:"Research Article",eNumber:"e046",commentsCount:dE,topicsAndSubtopics:c},journal:{id:dF,title:t,titleSlug:dG,mnemonic:"PAS",titleHistory:[],isFirstView:b,journalSlug:dG,isCompanion:b,parentCompanionJournalName:t,associatedParentCollection:c,paymentInfo:{prices:{"£":{price:26,sku:C,skuNew:u,currency:"£"},"€":{price:31,sku:C,skuNew:u,currency:"€"},US$:{price:36,sku:C,skuNew:u,currency:"US$"},AU$:{price:51,sku:C,skuNew:u,currency:"AU$"}}},url:dH,firstViewUrl:"\u002Fcore\u002Fjournals\u002Fpublications-of-the-astronomical-society-of-australia\u002Ffirstview",coverUrl:"https:\u002F\u002Fstatic.cambridge.org\u002Fcovers\u002FPAS_0_0_0\u002Fpublications-of-the-astronomical-society-of-australia.jpg",submitMaterialsUrl:"\u002Fcore\u002Fjournals\u002Fpublications-of-the-astronomical-society-of-australia\u002Finformation\u002Fauthor-instructions\u002Fsubmitting-your-materials",hasHistory:b,latestTitle:t,latestId:dF,hasPastTitle:b,volume:{id:"08A6F1C86EBBD90385E0EF1AF9272071",number:"38",title:dI,publishedDate:j,printPublishTimestamp:1609459200000,url:dJ}},abstract:{textAbstracts:[{title:"Abstract",content:"\u003Cdiv class=\"abstract\" data-abstract-type=\"normal\"\u003E\n\n\u003Cp\u003EWe present the data and initial results from the first pilot survey of the Evolutionary Map of the Universe (EMU), observed at 944 MHz with the Australian Square Kilometre Array Pathfinder (ASKAP) telescope. The survey covers \u003Cspan class=\"inlineFormula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline1.png\" \u002F\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$270 \\,\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E of an area covered by the Dark Energy Survey, reaching a depth of 25–30 \u003Cspan class=\"inlineFormula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline2.png\" \u002F\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E rms at a spatial resolution of \u003Cspan class=\"inlineFormula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline3.png\" \u002F\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E11–18 arcsec, resulting in a catalogue of \u003Cspan class=\"inlineFormula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline4.png\" \u002F\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E220 000 sources, of which \u003Cspan class=\"inlineFormula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline5.png\" \u002F\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E180 000 are single-component sources. Here we present the catalogue of single-component sources, together with (where available) optical and infrared cross-identifications, classifications, and redshifts. This survey explores a new region of parameter space compared to previous surveys. Specifically, the EMU Pilot Survey has a high density of sources, and also a high sensitivity to low surface brightness emission. These properties result in the detection of types of sources that were rarely seen in or absent from previous surveys. We present some of these new results here.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E",lang:dK}]},content:{html:"\u003Cdiv class=\"article research-article NLM\"\u003E\n\n\u003Cdiv class=\"body\"\u003E\n\u003Cdiv class=\"sec intro\" data-magellan-destination=\"s1\" id=\"s1\"\u003E\n\n\u003Ch2 class=\"A\"\u003E\u003Cspan class=\"label\"\u003E1.\u003C\u002Fspan\u003E Introduction\u003C\u002Fh2\u003E\n\u003Cp class=\"p\"\u003E Large radio surveys provide substantial samples of galaxies for studying cosmology. They also reveal rare but important stages of galaxy evolution and expand the volume of observed parameter space. Before the survey described here took place, about 2.5 million radio sources were known. That figure is about to increase by about two orders of magnitude (Norris \u003Ca class=\"xref bibr\" href=\"#r91\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003Ea), primarily due to using innovative technology in the development of new radio telescopes and upgrading of older radio telescopes. These technological developments will enable several large radio surveys, which are expected to drive a rapid advance in knowledge. \u003Ca class=\"xref fig\" href=\"#f1\"\u003EFigure 1\u003C\u002Fa\u003E shows the historical growth of these surveys.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f1\" id=\"f1\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig1.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"2250\" height=\"1586\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig1.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 1.\u003C\u002Fspan\u003E The number of known extragalactic radio sources discovered by surveys as a function of time, adapted from Norris (\u003Ca class=\"xref bibr\" href=\"#r91\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003Ea). The symbols indicate the type of telescope used to make the survey, and are fully described in Norris (\u003Ca class=\"xref bibr\" href=\"#r91\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003Ea). The dates and survey size are based on estimates made in 2017, and some later surveys (e.g. RACS McConnell et al. \u003Ca class=\"xref bibr\" href=\"#r81\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference McConnell\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E, with 2.8 million sources) are missing from this plot. Survey abbreviations and references are given in Norris (\u003Ca class=\"xref bibr\" href=\"#r91\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003Ea). The shading under the curve is merely to improve readability.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f2\" id=\"f2\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig2.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1005\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig2.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 2.\u003C\u002Fspan\u003E Some of the ASKAP antennas equipped with phased array feeds, located in the Murchison Region of Western Australia. Photo credit: CSIRO\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f3\" id=\"f3\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig3.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1499\" height=\"855\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig3.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 3.\u003C\u002Fspan\u003E One of the phased array feeds. Each square on the chequerboard is an antenna element connected to two receivers. Photo credit: CSIRO\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E One of these new telescopes is the Australian Square Kilometre Array Pathfinder, (ASKAP, Johnston et al. \u003Ca class=\"xref bibr\" href=\"#r60\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Johnston\u003C\u002Fspan\u003E2007\u003C\u002Fa\u003E; Johnston et al. \u003Ca class=\"xref bibr\" href=\"#r61\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Johnston\u003C\u002Fspan\u003E2008\u003C\u002Fa\u003E; McConnell et al. \u003Ca class=\"xref bibr\" href=\"#r79\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference McConnell\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E; Hotan et al. \u003Ca class=\"xref bibr\" href=\"#r54\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Hotan\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E) which consists of 36 12-m antennas spread over a region 6 km in diameter at the Murchison Radio-astronomy Observatory in Western Australia, shown in \u003Ca class=\"xref fig\" href=\"#f2\"\u003EFigure 2\u003C\u002Fa\u003E. At the focus of each antenna is an innovative phased-array feed (PAF: Hay et al. \u003Ca class=\"xref bibr\" href=\"#r47\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Hay, O’Sullivan, Kot, Granet, Lacoste, Ouwehand and Special Publication\u003C\u002Fspan\u003E2006\u003C\u002Fa\u003E) of 94 dual-polarisation pixels (\u003Ca class=\"xref fig\" href=\"#f3\"\u003EFigure 3\u003C\u002Fa\u003E). As a result, ASKAP has an instantaneous field of view up to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline6.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline6.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$30 \\,\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, producing a much higher survey speed than that of previous synthesis arrays. The antennas are a novel three-axis design, with the feed and reflector rotating to ensure a constant position angle of the PAF and sidelobes on the sky.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The first all-sky survey undertaken by ASKAP was the Rapid ASKAP Continuum Survey (McConnell et al. \u003Ca class=\"xref bibr\" href=\"#r81\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference McConnell\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E) which surveyed the entire sky south of Declination \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline7.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline7.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$+41^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E to a median rms of about 250 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline8.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline8.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Apart from its astrophysical importance, this survey will also generate a sky model (Hale et al., in preparation) to facilitate the calibration of subsequent deeper observations with ASKAP.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E ASKAP will conduct a deep all-sky continuum survey known as the Evolutionary Map of the Universe (EMU: Norris et al. \u003Ca class=\"xref bibr\" href=\"#r94\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2011\u003C\u002Fa\u003E). The primary goal of EMU is to make a deep (10–20 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline9.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"75\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline9.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E rms) radio continuum survey of the entire southern sky, extending as far north as \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline10.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline10.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$+30^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. EMU is expected to generate a catalogue of as many as 70 million galaxies.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E In preparation for the full EMU survey, we conducted the EMU Pilot Survey (EMU-PS) with the goal of testing the planned EMU survey strategy and the processing pipeline. In designing the pilot survey, we adopted the following boundary conditions:\n\u003C\u002Fp\u003E\u003Cul class=\"list nomark\"\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Declination \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline11.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"48\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline11.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$ < -30 ^{\\circ} $\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (to avoid potentially poor \u003Cem class=\"italic\"\u003Eu\u003C\u002Fem\u003E,\u003Cem class=\"italic\"\u003Ev\u003C\u002Fem\u003E coverage near the equator).\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Galactic latitude \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline12.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"47\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline12.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$ > +20 ^{\\circ} $\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (to avoid the strong diffuse emission in the Galactic plane).\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Sufficiently far from the Sun to avoid solar interference, or night-time observation.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E A single area of 240–300 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline13.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"28\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline13.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, of 10–12 h observations each on contiguous fields, to form a rectangular area. Cosmological analyses are optimised if the area is as square as possible.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Fields overlapped by a small amount to provide uniform sensitivity.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Frequency band chosen to avoid any radio frequency interference and maximise survey speed, subject to constraints on resolution and confusion.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Field that is well studied at other wavelengths to maximise the scientific value.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003C\u002Ful\u003E\n\n\u003Cp class=\"p\"\u003E These boundary conditions were satisfied by the survey described in this paper. The survey specifications are given in \u003Ca class=\"xref table\" href=\"#tbl1\"\u003ETable 1\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\u003Cdiv class=\"table-wrap\" data-magellan-destination=\"tbl1\" id=\"tbl1\"\u003E\n\n\u003Cdiv class=\"caption\"\u003E\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003ETable 1.\u003C\u002Fspan\u003E EMU Pilot Survey specifications.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cspan\u003E\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab1.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"399\" height=\"111\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab1.png\" data-zoomable=\"false\"\u003E\u003C\u002Fdiv\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fdiv\u003E\n\u003Cp class=\"p\"\u003E An area of sky within the Dark Energy Survey (DES: Abbott et al. \u003Ca class=\"xref bibr\" href=\"#r1\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Abbott\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E) was chosen so that we could access the excellent optical photometric data available from DES. EMU and DES have a Memorandum of Understanding that enables data to be shared between the two projects.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The observations were taken and processed in late 2019. It should be emphasised that, at the time of observation, commissioning of the telescope and its processing software were not yet complete, so that there are known telescope issues and processing deficiencies which were not yet addressed. As a result, the images show some artefacts, and the rms noise level is about twice as high as we expect in the final EMU survey. Nevertheless, this is still the largest radio survey ever completed at this depth, and so a great deal of valuable science results are being obtained, some of which are discussed briefly in this paper.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref sec\" href=\"#s2\"\u003ESection 2\u003C\u002Fa\u003E of this paper describes the observations, and \u003Ca class=\"xref sec\" href=\"#s3\"\u003ESection 3\u003C\u002Fa\u003E describes the data reduction. \u003Ca class=\"xref sec\" href=\"#s4\"\u003ESection 4\u003C\u002Fa\u003E describes the ‘value-added’ data processing, and \u003Ca class=\"xref sec\" href=\"#s5\"\u003ESection 5\u003C\u002Fa\u003E presents the results and data access. \u003Ca class=\"xref sec\" href=\"#s6\"\u003ESection 6\u003C\u002Fa\u003E presents some preliminary science results.\u003C\u002Fp\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s1-1\" id=\"s1-1\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E1.1.\u003C\u002Fspan\u003E Nomenclature and conventions\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E Throughout this paper and in the catalogue, we use source names in the format EMU PS JHHMMSS.S\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline18.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline18.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003EDDMMSS and we define spectral index \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline19.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline19.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E in terms of the relationship between flux density \u003Cem class=\"italic\"\u003ES\u003C\u002Fem\u003E and observing frequency \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline20.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"8\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline20.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\nu$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E as \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline21.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"40\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline21.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S \\propto \\nu^{\\alpha}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E For consistency among science results derived from EMU-PS data, we encourage the use of a consistent set of cosmological parameters in papers reporting results from EMU-PS. Here we assume a flat \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline22.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline22.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\Lambda$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003ECDM model, with parameter values taken from the mean posterior of the Planck 2018 cosmology, from paper VI (Planck Collaboration et al. 2020), using a combination of Planck data, but with no extra, non-Planck data (e.g. no Baryon Acoustic Oscillation data). This results in the parameter set shown in \u003Ca class=\"xref table\" href=\"#tbl2\"\u003ETable 2\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\u003Cdiv class=\"table-wrap\" data-magellan-destination=\"tbl2\" id=\"tbl2\"\u003E\n\n\u003Cdiv class=\"caption\"\u003E\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003ETable 2.\u003C\u002Fspan\u003E Cosmological parameters used in this paper and adopted for EMU-PS.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cspan\u003E\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab2.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"416\" height=\"243\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab2.png\" data-zoomable=\"false\"\u003E\u003C\u002Fdiv\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fdiv\u003E\n\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec other\" data-magellan-destination=\"s2\" id=\"s2\"\u003E\n\n\u003Ch2 class=\"A\"\u003E\u003Cspan class=\"label\"\u003E2.\u003C\u002Fspan\u003E Observations\u003C\u002Fh2\u003E\n\u003Cp class=\"p\"\u003E ASKAP has 36 antennas, all but 6 of which are within a region of 2.3 km diameter, with the outer 6 extending the baselines up to 6.4 km. In all pilot survey observations, as many of the 36 antennas were used as possible. However, in some cases, a few antennas were omitted because of maintenance or hardware issues. The actual number of antennas used is shown in \u003Ca class=\"xref table\" href=\"#tbl3\"\u003ETable 3\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\u003Cdiv class=\"table-wrap\" data-magellan-destination=\"tbl3\" id=\"tbl3\"\u003E\n\n\u003Cdiv class=\"caption\"\u003E\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003ETable 3.\u003C\u002Fspan\u003E EMU pilot observation details.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cspan\u003E\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab3.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"416\" height=\"265\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab3.png\" data-zoomable=\"false\"\u003E\u003C\u002Fdiv\u003E\n\u003C\u002Fspan\u003E\n\u003Cdiv class=\"table-wrap-foot\"\u003E\n\u003Cp class=\"p\"\u003E The position shown is the antenna pointing centre, corresponding to position (0,0) in \u003Ca class=\"xref fig\" href=\"#f4\"\u003EFigure 4\u003C\u002Fa\u003E. Columns 5 and 6 show the ASKAP scheduling block identification (SBID) number for the target and calibrator observations.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\n\u003Cp class=\"p\"\u003E At the prime focus of each antenna is a phased array feed (PAF), which subtends a solid angle of about \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline42.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline42.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$30 \\,\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E of the sky. The PAF consists of 188 single-polarisation dipole receivers. A weighted sum of the outputs of groups of these receivers is used to form 36 dual-polarisation ‘beams’. Individual dipole receivers will, in general, contribute to more than one beam, so that adjacent beams are not completely independent. The 36 beams together cover an area of about \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline43.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"46\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline43.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$30 \\,\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E on the sky, which we refer to as a ‘tile’.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E There are several ways of arranging the individual beams within the tile. For EMU-PS, we use a hexagonal arrangement of the 36 beams with 6 rows of 6 beams, known as ‘closepack36’ (Hotan et al. \u003Ca class=\"xref bibr\" href=\"#r54\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Hotan\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E), shown in \u003Ca class=\"xref fig\" href=\"#f4\"\u003EFigure 4\u003C\u002Fa\u003E. This configuration provides more uniform coverage than the widely used rectangular array known as ‘square_6x6’. The spacing between the beams is known as the ‘pitch’ and is set to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline44.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"24\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline44.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$0.9^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E for EMU-PS. In some other ASKAP observations, interleaved observations are taken, with the antenna pointing position shifted by half the pitch, to provide better uniformity. However, this is not necessary for the EMU-PS because of the combination of our lower observing frequency and the closepack36 configuration.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f4\" id=\"f4\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig4.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"667\" height=\"653\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig4.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 4.\u003C\u002Fspan\u003E The arrangement of the 36 ASKAP beams in the ‘closepack36’ configuration. The beams are numbered from 0 to 35 (diagram adapted from McConnell et al. \u003Ca class=\"xref bibr\" href=\"#r80\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference McConnell\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E). The circles shown are for illustration only. For EMU-PS, the actual full width half maximum of each beam is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline45.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"37\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline45.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}1.5^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E at the band centre, and the pitch spacing is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline46.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"24\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline46.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$0.9^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, giving an approximately uniform sensitivity over the field of view.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E The weights of the individual beams are initially calibrated by observing the Sun, placed successively at the centre of each beam, and then adjusting the weights for maximum signal-to-noise ratio. A radiator at the vertex of each antenna (the On-Dish Calibrator, or ODC) enables the gain of each receiver to be monitored, and the weight solution initially obtained from solar observations may be updated if necessary using these ODC measurements.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Before (or sometimes after) the observation of each target, the calibrator source PKS 1934–638 is observed for 200 s at the centre of each of the 36 beams to provide bandpass and gain calibration. This calibration observation takes about 2 h.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The positions of the tiles are chosen using a tiling scheme which will be used for the main EMU survey, shown in \u003Ca class=\"xref fig\" href=\"#f5\"\u003EFigure 5\u003C\u002Fa\u003E. At most declinations, the tiles are aligned with lines of constant declination. At the south polar cap (below declination \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline47.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"51\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline47.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-71.81^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E), they are arranged in a rectangular grid as shown in \u003Ca class=\"xref fig\" href=\"#f5\"\u003EFigure 5\u003C\u002Fa\u003E. Using this scheme, the sky south of Declination \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline48.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline48.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$+30^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E is covered by 1 280 tiles. Overlaps between tiles amount to less than 5% of the total area covered.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f5\" id=\"f5\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig5.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1502\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig5.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 5.\u003C\u002Fspan\u003E The sky tiling scheme adopted for the EMU-PS. The red rectangles covering the celestial sphere show the tiles planned for the EMU survey, and the orange area indicates the 10 tiles of the EMU-PS. The white strip shows the Galactic plane, and the south celestial pole is at the bottom of the figure.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f6\" id=\"f6\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig6.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"705\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig6.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 6.\u003C\u002Fspan\u003E The location of the EMU Pilot Survey area on the sky within DES DR1, adapted from Abbott et al. (\u003Ca class=\"xref bibr\" href=\"#r1\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Abbott\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E). The diagram is in equatorial coordinates, and the solid line marks the Galactic plane, flanked by two dashed lines showing Galactic latitude \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline49.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline49.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\pm 10 ^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E The pilot survey was observed with ASKAP in the period from 2019 July 15 to 2019 November 24. In some cases, the initial observations were subsequently found to be faulty, in which case the field was re-observed. \u003Ca class=\"xref table\" href=\"#tbl3\"\u003ETable 3\u003C\u002Fa\u003E shows the details of the observations that were used in the final data product.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The survey consists of a 10-h observation of each of the 10 tiles, each accompanied by a calibration observation as described above. No further calibration is performed during the observation. The location of the survey area is shown in \u003Ca class=\"xref fig\" href=\"#f6\"\u003EFigure 6\u003C\u002Fa\u003E, and the details of the pointing centres are shown in \u003Ca class=\"xref table\" href=\"#tbl3\"\u003ETable 3\u003C\u002Fa\u003E and in \u003Ca class=\"xref fig\" href=\"#f7\"\u003EFigure 7\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec other\" data-magellan-destination=\"s3\" id=\"s3\"\u003E\n\n\u003Ch2 class=\"A\"\u003E\u003Cspan class=\"label\"\u003E3.\u003C\u002Fspan\u003E Pipeline data reduction\u003C\u002Fh2\u003E\n\u003Cp class=\"p\"\u003E We process the data using the ASKAPsoft pipeline (Whiting et al. \u003Ca class=\"xref bibr\" href=\"#r125\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Whiting, Voronkov and Mitchell\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E; Whiting \u003Ca class=\"xref bibr\" href=\"#r123\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Whiting, Ballester, Ibsen, Solar and Shortridge\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E; Guzman et al. \u003Ca class=\"xref bibr\" href=\"#r45\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Guzman\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E) with the parameters shown in \u003Ca class=\"xref table\" href=\"#tbl4\"\u003ETable 4\u003C\u002Fa\u003E, and using 2-arcsec square pixels. All parameter names, shown in italics in this section, are included in \u003Ca class=\"xref table\" href=\"#tbl4\"\u003ETable 4\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\u003Cdiv class=\"table-wrap\" data-magellan-destination=\"tbl4\" id=\"tbl4\"\u003E\n\n\u003Cdiv class=\"caption\"\u003E\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003ETable 4.\u003C\u002Fspan\u003E EMU pilot processing parameters. The first column shows the parameter name used by ASKAPsoft.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cspan\u003E\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab4.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"748\" height=\"353\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab4.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fdiv\u003E\u003Cdiv class=\"table-wrap\" data-magellan-destination=\"tbl5\" id=\"tbl5\"\u003E\n\n\u003Cdiv class=\"caption\"\u003E\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003ETable 5.\u003C\u002Fspan\u003E Results of tests to measure the optimum robustness.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cspan\u003E\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab5.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"416\" height=\"199\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab5.png\" data-zoomable=\"false\"\u003E\u003C\u002Fdiv\u003E\n\u003C\u002Fspan\u003E\n\u003Cdiv class=\"table-wrap-foot\"\u003E\n\u003Cp class=\"p\"\u003E Tests were conducted at 888 MHz, using a 10-h ASKAP observation on arrays of 33 (for Stokes V, using SB8129 on a field close to UV Ceti) and 35 (for Stokes I, using SB8137 on the GAMA23 field) antennas. Columns 2 and 3 given the major and minor axes of the restoring beam, and columns 4 and 5 gives the measured rms values in (a) a source-free region of the Stokes I image, and (b) the Stokes V image, which is almost source-free. The results have been scaled to a 10-h observation on an array of 36 antennas.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cp class=\"p\"\u003E The ASKAP correlator generates 16384 spectral line channels and, for EMU data, we start by averaging these to 288 1-MHz channels to reduce the computational load (i.e. \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline58.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"110\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline58.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$DO\\_SPECTRAL\\_$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline59.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"112\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline59.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$ IMAGING = true$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline60.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"119\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline60.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$DO\\_CONTCUBE\\_ $\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline61.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"112\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline61.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$ IMAGING = true$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E)\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Weighting and tapering in ASKAPsoft are done using a Wiener filter preconditioning technique, which is computationally more efficient than traditional tapering and weighting. (i.e. \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline62.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"381\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline62.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$ RESTORE\\_PRECONDITIONER\\_LIST = [Wiener, Gaussian$-\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline63.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"39\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline63.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$Taper]$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) for the main and alt image respectively\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E To choose the robustness (Briggs \u003Ca class=\"xref bibr\" href=\"#r16\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Briggs\u003C\u002Fspan\u003E1995\u003C\u002Fa\u003E), we conducted tests on part of the GAMA23 field (at about Right Ascension 23:00, Declination \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline64.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline64.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E32:00; Leahy et al. (\u003Ca class=\"xref bibr\" href=\"#r72\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Leahy\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E), Prandoni et al., in preparation), in both Stokes I (total intensity) and Stokes V (circular polarisation) resulting in the values shown in \u003Ca class=\"xref table\" href=\"#tbl5\"\u003ETable 5\u003C\u002Fa\u003E. At lower (more negative) values of robustness, the rms increases because the near-uniform weighting discards information. At higher (more positive) values of robustness, corresponding to near-natural weighting, the V rms continues to decrease but the I rms increases presumably because of (a) confusion, (b) poorer \u003Cem class=\"italic\"\u003Eu\u003C\u002Fem\u003E,\u003Cem class=\"italic\"\u003Ev\u003C\u002Fem\u003E coverage leading to increased sidelobes, (c) increased radio frequency interference on short baselines. Based on these results, we choose a robustness of 0.0 as an optimum value for the EMU-PS, that is, \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline65.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"335\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline65.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$PRECONDITIONER\\_WIENER\\_ROBUSTNESS=0.0$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Although robustness +0.5 has a slightly lower rms, it has a significantly increased beam size. No further tapering is used in the main image.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f7\" id=\"f7\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig7.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1095\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig7.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 7.\u003C\u002Fspan\u003E The arrangement of the ten individual ASKAP tiles on the sky for EMU-PS with their SBID numbers as listed in \u003Ca class=\"xref table\" href=\"#tbl3\"\u003ETable 3\u003C\u002Fa\u003E. The rectangles are separated in this diagram for clarity, but there is actually overlapping coverage as illustrated by the greyscale background.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E The non-coplanarity of ASKAP is managed using the w-projection technique (Cornwell et al. \u003Ca class=\"xref bibr\" href=\"#r27\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Cornwell, Golap and Bhatnagar\u003C\u002Fspan\u003E2008\u003C\u002Fa\u003E; Rau et al. \u003Ca class=\"xref bibr\" href=\"#r107\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Rau, Bhatnagar, Voronkov and Cornwell\u003C\u002Fspan\u003E2009\u003C\u002Fa\u003E), using a total of 557 w-planes (i.e. \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline66.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"196\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline66.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$GRIDDER\\_NWPLANES=557$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E). The data are gridded using multi-frequency synthesis and deconvolved using a multi-frequency multiscale CLEAN, using \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline67.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"109\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline67.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$CLEAN\\_SCALES$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E of [0,6,15,30,45,60] pixels, which gives 6 scales up to 10 times the clean beam size. After initial imaging and cleaning (using 5 major cycles: \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline68.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"212\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline68.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$CLEAN\\_NUM\\_MAJOR\\_CYCLES$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, with 400 iterations in each minor cycle, down to a limit of 0.25 mJy), the data are given one iteration of phase selfcal using the output of the previous CLEAN (i.e. \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline69.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"204\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline69.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$SELFCAL\\_METHOD=CLEAN$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) before the final imaging and cleaning (15 major cycles with up up to 3000 iterations in each minor cycle, with minor cycles triggering a major cycle when they reach a 30% CLEAN limit, to a clean limit of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline70.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"42\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline70.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$30 \\,\\mu\\mathrm{Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, i.e. \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline71.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"251\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline71.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$CLEAN\\_THRESHOLD\\_MINORCYCLE$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E). Two images are produced by the pipeline: the main image at full resolution and an alternative (‘alt’) image tapered to a 30-arcsec resolution, which is optimised for faint diffuse emission. The alt image is not used in this paper.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The multi-frequency synthesis imaging uses a Taylor term technique (Rau & Cornwell \u003Ca class=\"xref bibr\" href=\"#r106\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Rau and Cornwell\u003C\u002Fspan\u003E2011\u003C\u002Fa\u003E) over the 288-MHz bandwidth to account for the spectral variation of each source. We use two terms in the Taylor expansion, resulting in two planes called TT0 and TT1. The TT0 plane is the zeroth-order term, corresponding to the total intensity of each pixel integrated over the full bandwidth. TT1 is the first-order term and allows the spectral indices at each pixel to be measured as \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline72.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline72.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E = TT1\u002FTT0.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Primary beam correction is applied to each beam, and beams are combined using a weighted mean down to a cut-off of 20% of the peak (i.e. \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline73.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"154\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline73.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$LINMOSCUTOFF =0.2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) assuming a Gaussian primary beam shape. Future ASKAP surveys will use a beam shape based on holographic measurements, but that was not available for EMU-PS. Using the Gaussian beam approximation increases calibration errors and the rms noise level.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Source extraction uses the ‘ \u003Cem class=\"italic\"\u003ESelavy\u003C\u002Fem\u003E’ software tool (Whiting & Humphreys \u003Ca class=\"xref bibr\" href=\"#r124\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Whiting and Humphreys\u003C\u002Fspan\u003E2012\u003C\u002Fa\u003E; Whiting et al. \u003Ca class=\"xref bibr\" href=\"#r125\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Whiting, Voronkov and Mitchell\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E) which identifies ‘islands’ of emission higher than three times the local rms in the image, using a flood-fill technique, and then fits Gaussian components to peaks of emission within the islands. Only components and islands greater than five times the local rms are retained.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E In the EMU initial public data release (defined in \u003Ca class=\"xref sec\" href=\"#s5-1\"\u003ESection 5.1\u003C\u002Fa\u003E), spectral indices for individual components are measured as \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline74.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline74.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E = TT1\u002FTT0, where TT0 and TT1 are a weighted mean of the Taylor terms over the area of the component, down to a level of five times the local rms noise. However, this technique has been found to be unsatisfactory, so the spectral indices in the initial public data release should be regarded as unreliable. Our alternative technique is discussed below in \u003Ca class=\"xref sec\" href=\"#s4-4\"\u003ESection 4.4\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E As a final step within the pipeline, the data from each scheduling block are uploaded to the data archive (but not yet released) and passed through the ASKAP continuum validation package\u003Ca class=\"xref fn\" href=\"#fn1\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Ea\u003C\u002Fa\u003E using default parameters. This package takes the final image, noise map, and \u003Cem class=\"italic\"\u003ESelavy\u003C\u002Fem\u003E catalogue as input and produces metrics and data quality flags based on a number of validation tests\u003Ca class=\"xref fn\" href=\"#fn2\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Eb\u003C\u002Fa\u003E. The following metrics are used for each of these tests using ASKAP data only:\n\u003C\u002Fp\u003E\u003Cul class=\"list nomark\"\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Fraction of sources considered resolved, given by the difference in the integrated (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline75.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"20\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline75.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\rm int}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) and peak (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline76.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"28\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline76.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\rm peak}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) flux densities, and local noise \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline77.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline77.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sigma$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. We consider a source to be resolved when (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline78.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"237\" height=\"29\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline78.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\rm int} - S_{\\rm peak}) \u002F \\sqrt{dS_{\\rm int}^2 + dS_{\\rm peak}^2 + \\sigma^2} > 3$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, where \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline79.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"28\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline79.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$dS_{\\rm int}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline80.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"36\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline80.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$dS_{\\rm peak}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E are the estimated measurement errors in \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline81.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"20\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline81.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\rm int}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline82.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"28\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline82.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\rm peak}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Reduced \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline83.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"16\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline83.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\chi^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E of differential Euclidean source counts\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Median RMS value (from \u003Cem class=\"italic\"\u003ESelavy\u003C\u002Fem\u003E noise map)\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Median in-band spectral index (from \u003Cem class=\"italic\"\u003ESelavy\u003C\u002Fem\u003E catalogue, measured from Taylor term images)\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003C\u002Ful\u003E\n\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f8\" id=\"f8\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig8.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"2298\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig8.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 8.\u003C\u002Fspan\u003E An example validation report for one of the processing runs for SB9325, including the metrics and their flags. A higher-resolution version is available online2.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E The following additional metrics are used with respect to selected point sources, cross-matched to the reference catalogue that provided the most matches, which for the pilot, is SUMSS (Mauch et al. \u003Ca class=\"xref bibr\" href=\"#r78\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler\u003C\u002Fspan\u003E2003\u003C\u002Fa\u003E), which has a resolution of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline84.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline84.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E45 arcsec at an observing frequency of 843 MHz:\n\u003C\u002Fp\u003E\u003Cul class=\"list nomark\"\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Median absolute deviation (MAD) of the ratio of the flux density of the reference catalogue to the ASKAP flux density, after correcting for the frequency difference assuming \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline85.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"59\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline85.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha = -0.8$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E,\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Flux density ratio uncertainty, calculated from the MAD\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Positional offset, given by the median compared to reference catalogue\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Positional offset uncertainty, calculated from the MAD\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003C\u002Ful\u003E\n\n\u003Cp class=\"p\"\u003E An example report\u003Ca class=\"xref fn\" href=\"#fn3\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Ec\u003C\u002Fa\u003E for one of the processing runs for SB9325 is shown in \u003Ca class=\"xref fig\" href=\"#f8\"\u003EFigure 8\u003C\u002Fa\u003E, including a summary of the metrics and their flags. Each metric is flagged as good, bad, or uncertain based on selected tolerance values\u003Ca class=\"xref fn\" href=\"#fn4\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Ed\u003C\u002Fa\u003E. The metrics and flags are associated and archived with the data, and the validation reports are automatically uploaded as a report under project AS101\u003Ca class=\"xref fn\" href=\"#fn5\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Ee\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The final validation process is done by members of the EMU team and includes\n\u003C\u002Fp\u003E\u003Cul class=\"list nomark\"\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E inspecting each of the validation reports described above,\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E inspecting the images to search for artefacts,\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E examining quantities such as the variation of restoring beam among the 36 beams used in the mosaic.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003C\u002Ful\u003E\n\n\u003Cp class=\"p\"\u003E Data deemed to be acceptable are then released to the public domain on the data archive, described in \u003Ca class=\"xref sec\" href=\"#s5-1\"\u003ESection 5.1\u003C\u002Fa\u003E. If the data are not found to be acceptable, then the data are removed from the archive and we request a re-observation.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec other\" data-magellan-destination=\"s4\" id=\"s4\"\u003E\n\n\u003Ch2 class=\"A\"\u003E\u003Cspan class=\"label\"\u003E4.\u003C\u002Fspan\u003E Value-added processing\u003C\u002Fh2\u003E\n\u003Cp class=\"p\"\u003E To mitigate some of the data issues in the initial public data release and to produce a unified image and source catalogue covering the full EMU-PS field, we conduct value-added processing on the initial public data release to generate a value-added data release. This value-added processing also includes some optical and infrared ancillary data, as described below.\u003C\u002Fp\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s4-1\" id=\"s4-1\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E4.1.\u003C\u002Fspan\u003E Merging tiles\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E The initial public release of the survey data consists of 10 overlapping tiles, each with its own source catalogue. Simply merging these catalogues generates a large number of duplicate sources, which must be reconciled to maximise the information integrity and consistency. This approach also fails to take full advantage of the additional information, such as increased sensitivity, available where tiles overlap.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E To overcome these issues, we merged the 10 tiles in the image plane using the ASKAPsoft task \u003Cem class=\"italic\"\u003Elinmos\u003C\u002Fem\u003E, which performs a weighted average of the data in overlapping regions. The merged data set is shown in \u003Ca class=\"xref fig\" href=\"#f9\"\u003EFigure 9\u003C\u002Fa\u003E. We refer to this image, which has a typical spatial resolution of 11–13 arcsec, as the ‘native resolution image’.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f9\" id=\"f9\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig9.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1088\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig9.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 9.\u003C\u002Fspan\u003E The resulting native resolution (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline86.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"61\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline86.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$13'' \\times 11''$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) image of the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline87.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"53\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline87.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$270 \\,\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E EMU Pilot Survey, containing about 220 000 radio sources. The rms noise level is 25–30 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline88.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline88.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, and the peak flux density is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline89.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"90\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline89.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$3.14 \\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s4-2\" id=\"s4-2\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E4.2.\u003C\u002Fspan\u003E Convolution to a common restoring beam size\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E A problem with the native resolution image is that the point spread function (psf) varies from beam to beam over the field, so that both the flux density scale and also the spectral indices vary from beam to beam. To overcome this problem, we created a version of the data in which each PAF beam is individually convolved with a Gaussian kernel to obtain a common circular restoring beam of 18 arcsec FWHM. We then recombined all beams into a weighted average using the ASKAPsoft task \u003Cem class=\"italic\"\u003Elinmos\u003C\u002Fem\u003E. We refer to this data set as the ‘convolved image’.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E We then ran the \u003Cem class=\"italic\"\u003ESelavy\u003C\u002Fem\u003E source finder on the convolved image, to produce a catalogue of components and islands. This convolved catalogue has 220 102 components. These ‘convolved’ data are recommended over the ‘native’ data product for the measurements of flux density and spectral index. However, the data products in native resolution are still optimum for studies of morphology, or when the higher resolution is needed.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s4-3\" id=\"s4-3\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E4.3.\u003C\u002Fspan\u003E Separation of sources into simple and complex\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E Many value-added operations, such as measuring spectral index, and cross-identifying to optical\u002FIR catalogues, are far more complex for extended or complex sources than for simple, compact sources. These techniques are still under development for the full EMU survey.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E We therefore divided the source catalogue into ‘simple’ and ‘complex’ sources. A sophisticated technique for this separation is still under development, so for the purposes of this paper we used a simple technique in which we defined islands with only one component (specifically, with \u003Cem class=\"italic\"\u003Ehas_siblings\u003C\u002Fem\u003E \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline90.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline90.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E \u003Cem class=\"italic\"\u003E0)\u003C\u002Fem\u003E to be simple, and all other islands are defined to be ‘complex’. This technique results in a catalogue of 178 921 components, so that about 81% of sources in the catalogue are ‘simple’.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Many ‘complex’ sources are classical FRI or FR II sources (Fanaroff & Riley \u003Ca class=\"xref bibr\" href=\"#r37\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Fanaroff and Riley\u003C\u002Fspan\u003E1974\u003C\u002Fa\u003E), but our high sensitivity to low surface brightness has also enabled the detection of several peculiar-looking sources that are quite unlike those seen in earlier surveys such as NVSS (Condon et al. \u003Ca class=\"xref bibr\" href=\"#r25\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Condon, Cotton, Greisen, Yin, Perley, Taylor and Broderick\u003C\u002Fspan\u003E1998\u003C\u002Fa\u003E) or FIRST (White et al. \u003Ca class=\"xref bibr\" href=\"#r120\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference White, Becker, Helfand and Gregg\u003C\u002Fspan\u003E1997\u003C\u002Fa\u003E). In \u003Ca class=\"xref sec\" href=\"#s6\"\u003ESection 6\u003C\u002Fa\u003E, we discuss a small sample of these peculiar objects, which will be further explored in subsequent papers.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E We expect about half of the ‘simple’ sources to be star-forming galaxies (SFGs), with the remaining half to be AGN. It is this simple sample for which we obtain multiwavelength data in this paper.The rest of the value-added processing described here is concerned only with this simple catalogue, and the value-added processing of the complex sources will be described in a future paper (Marvil et al., in preparation).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E In \u003Ca class=\"xref table\" href=\"#tbl6\"\u003ETable 6\u003C\u002Fa\u003E, we list the numbers of sources remaining at each stage of the value-added processing.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s4-4\" id=\"s4-4\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E4.4.\u003C\u002Fspan\u003E Spectral indices\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E Spectral indices of the simple sources are measured over the 288-MHz bandwidth of ASKAP using the Taylor term technique described above. We measure spectral indices by calculating them from the Taylor terms at the peak pixel of each component, in the convolved data set. Note, as discussed above, that this procedure differs from that in the initial public data release, which we consider to be unreliable.\u003C\u002Fp\u003E\u003Cdiv class=\"table-wrap\" data-magellan-destination=\"tbl6\" id=\"tbl6\"\u003E\n\n\u003Cdiv class=\"caption\"\u003E\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003ETable 6.\u003C\u002Fspan\u003E Numbers of sources remaining after each stage of the value-added processing.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cspan\u003E\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab6.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"416\" height=\"199\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab6.png\" data-zoomable=\"false\"\u003E\u003C\u002Fdiv\u003E\n\u003C\u002Fspan\u003E\n\u003Cdiv class=\"table-wrap-foot\"\u003E\n\u003Cp class=\"p\"\u003E Asterisked rows are shown for information but are not used in the subsequent selection step. Photometric redshifts are taken from Zou et al. (\u003Ca class=\"xref bibr\" href=\"#r131\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Zou, Gao, Zhou and Kong\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E), Zou et al. (\u003Ca class=\"xref bibr\" href=\"#r132\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Zou, Gao, Zhou and Kong\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E), and Bilicki et al. (\u003Ca class=\"xref bibr\" href=\"#r8\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bilicki\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cp class=\"p\"\u003E We also explored using the third Taylor term, which would measure spectral curvature, but found that very few sources had a measurable spectral curvature in the 288-MHz bandwidth of these observations. More importantly, we found that introducing a third Taylor term increased the uncertainty in the first two Taylor terms without increasing the accuracy, presumably because we are introducing a third free parameter which is primarily driven by noise.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The distribution of the resulting spectral indices as a function of flux density is shown in \u003Ca class=\"xref fig\" href=\"#f10\"\u003EFigure 10\u003C\u002Fa\u003E. Based on the noise measured in the TT1 image, the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline91.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"16\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline91.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$1\\sigma$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E spectral index uncertainty of a source with flux density \u003Cem class=\"italic\"\u003ES\u003C\u002Fem\u003E mJy is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline92.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"42\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline92.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$0.25 \u002F S$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The spectral index of a 2.5-mJy source, therefore, has a standard error of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline93.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline93.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.1, and spectral indices of sources weaker than this will be increasingly uncertain.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f10\" id=\"f10\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig10.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1833\" height=\"1462\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig10.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 10.\u003C\u002Fspan\u003E The measured spectral index as a function of flux density. The two solid lines show the 3\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline94.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline94.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sigma$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E uncertainty for a source of spectral index -0.8. Note the excess of sources with a positive spectral index, discussed in \u003Ca class=\"xref sec\" href=\"#s6-13\"\u003ESection 6.9\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E A histogram of the spectral indices for the 10458 sources with flux density \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline95.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline95.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E 2.5 mJy is shown in \u003Ca class=\"xref fig\" href=\"#f11\"\u003EFigure 11\u003C\u002Fa\u003E. The peak is at a spectral index of –0.7, as expected for surveys of mJy radio sources, with a tail of steeper spectrum sources extending to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline96.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"59\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline96.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha < -1.3$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Such ‘ultra-steep spectrum sources’ are well known in the literature (e.g. Afonso et al. \u003Ca class=\"xref bibr\" href=\"#r2\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Afonso\u003C\u002Fspan\u003E2011\u003C\u002Fa\u003E) and can be an indicator of high redshift sources. There is also an unexpected tail of sources with positive spectral indices. Such sources are also well known (e.g. Healey et al. \u003Ca class=\"xref bibr\" href=\"#r48\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Healey, Romani, Taylor, Sadler, Ricci, Murphy, Ulvestad and Winn\u003C\u002Fspan\u003E2007\u003C\u002Fa\u003E) but are relatively rare. Here, however, they appear to constitute a significant fraction of EMU-PS sources. This is discussed further in \u003Ca class=\"xref sec\" href=\"#s6-13\"\u003ESection 6.9\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f11\" id=\"f11\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig11.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1011\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig11.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 11.\u003C\u002Fspan\u003E A histogram of measured spectral index as a function of flux density, for the 10458 sources with flux density \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline97.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline97.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E 2.5 mJy.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f12\" id=\"f12\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig12.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1126\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig12.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 12.\u003C\u002Fspan\u003E The fraction of simple radio sources (as listed in \u003Ca class=\"xref table\" href=\"#tbl6\"\u003ETable 6\u003C\u002Fa\u003E) matched with a CWISE source as a function of separation, both for unshifted data and for data shifted by one arcmin.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s4-5\" id=\"s4-5\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E4.5.\u003C\u002Fspan\u003E Multi-wavelength cross-identifications and redshifts\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E For cross-identifying simple sources, we use a simple nearest-neighbour cross-identification algorithm and show below that this gives an acceptable completeness and false-ID rate. Norris et al. (\u003Ca class=\"xref bibr\" href=\"#r93\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2006\u003C\u002Fa\u003E) found that cross-matching with 3.6-\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline98.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"11\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline98.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003Em \u003Cem class=\"italic\"\u003ESpitzer\u003C\u002Fem\u003E infrared data and then cross-matching the infrared with optical gave a lower false-ID rate than matching radio with optical directly. We therefore adopt this procedure here, and first match the radio against the W1 band (3.4 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline99.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"11\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline99.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003Em) of the CATWISE2020 catalogue (Marocco et al. \u003Ca class=\"xref bibr\" href=\"#r76\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Marocco\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E), hereafter referred to as ‘CWISE’, and then cross-match the CWISE positions against the DES DR1 optical catalogue (Abbott et al. \u003Ca class=\"xref bibr\" href=\"#r1\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Abbott\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E We measured the number of cross-matches between the radio and the infrared as a function of separation, and then estimated the false-ID rate by shifting the radio positions by 1 arcmin and then repeating the cross-match. The result is shown in \u003Ca class=\"xref fig\" href=\"#f12\"\u003EFigure 12\u003C\u002Fa\u003E. The choice of an optimum search radius depends on the application (i.e., whether the goal depends on maximising the number of cross-matches or minimising the number of false-IDs). In producing the cross-matched catalogue, we include all cross-matches up to a search radius of 10 arcsec so that users can choose their optimum search radius, but for further work herein we limit our analysis to a maximum search radius of 3 arcsec, at which we find an 8% false-ID rate and a 75% total cross-match rate (which includes the false-IDs). The resulting numbers of sources are listed in \u003Ca class=\"xref table\" href=\"#tbl6\"\u003ETable 6\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Because of the high numbers of faint CWISE sources, we also explored the effect of introducing a cut-off in the CWISE flux densities, so only the brighter sources would be cross-matched to radio sources, but found that had a negligible effect on the false-ID rate, while significantly reducing the number of true IDs, and so no cut-off is used.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E To cross-match the CWISE IR positions against DES optical positions, we again explored the false-ID rate and the total-ID rate as a function of search radius, and show the results in \u003Ca class=\"xref fig\" href=\"#f13\"\u003EFigure 13\u003C\u002Fa\u003E. As a result, we adopt a search radius of 2 arcsec. The resulting numbers of sources are listed in \u003Ca class=\"xref table\" href=\"#tbl6\"\u003ETable 6\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f13\" id=\"f13\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig13.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1134\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig13.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 13.\u003C\u002Fspan\u003E The fraction of radio sources with a CWISE position matched with a DES DR1 source as a function of separation, both for unshifted data and for data shifted by one arcmin.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E There is no major spectroscopic redshift survey covering the EMU-PS field, but a large number of photometric redshifts are available from Bilicki et al. (\u003Ca class=\"xref bibr\" href=\"#r8\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bilicki\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E) (using their ‘main’ catalogue), and from Zou et al. (\u003Ca class=\"xref bibr\" href=\"#r131\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Zou, Gao, Zhou and Kong\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E; \u003Ca class=\"xref bibr\" href=\"#r132\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Zou, Gao, Zhou and Kong\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E), and we also include those in the catalogue. Throughout the rest of this paper, redshifts given without a citation refer to these redshifts used in the EMU-PS catalogue.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s4-6\" id=\"s4-6\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E4.6.\u003C\u002Fspan\u003E Astrometric precision\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E For each source that was cross-matched with a CWISE catalogue source, we measured the offset in position, as a check on the precision of the positions of the radio components. The result is shown in \u003Ca class=\"xref fig\" href=\"#f14\"\u003EFigure 14\u003C\u002Fa\u003E, showing a mean offset of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline100.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline100.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.3 arcsec, which is small compared to the 18 arcsec resolution of the convolved data. The positions in the catalogue have not been corrected for this insignificant offset.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f14\" id=\"f14\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig14.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1467\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig14.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 14.\u003C\u002Fspan\u003E A plot showing the difference in position of radio sources compared to the matching CWISE source in the W1 band, showing a mean offset of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline101.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline101.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.3 arcsec, which is small compared to the 18 arcsec resolution of the convolved data. The horizontal axis is Right Ascension and the vertical axis is Declination.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f15\" id=\"f15\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig15.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1083\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig15.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 15.\u003C\u002Fspan\u003E The ratio of peak flux densities between EMU-PS and SUMSS for simple sources with EMU-PS flux densities \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline102.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline102.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E 6 mJy, and with catalogued positions within 3 arcsec.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s4-7\" id=\"s4-7\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E4.7.\u003C\u002Fspan\u003E Flux density accuracy\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E To estimate the flux density accuracy, we select EMU-PS sources stronger than 6 mJy (the minimum flux density for sources in the SUMSS (Mauch et al. \u003Ca class=\"xref bibr\" href=\"#r78\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler\u003C\u002Fspan\u003E2003\u003C\u002Fa\u003E) catalogue) and cross-match them to SUMSS sources using a 3-arcsec search radius, which selects about 50% of the SUMSS sources, and tends to exclude the very extended SUMSS sources. We then calculate the ratio of peak fluxes in the EMU-PS and SUMMS catalogues. The result is shown in \u003Ca class=\"xref fig\" href=\"#f15\"\u003EFigure 15\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f16\" id=\"f16\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig16.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"2400\" height=\"1359\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig16.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 16.\u003C\u002Fspan\u003E A typical section of the survey field, covering about \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline103.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"49\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline103.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$0.3 \\,\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (or about one thousandth of the area of the EMU Pilot Survey) which contains about 250 radio sources). On the left is the SUMSS image (Mauch et al. \u003Ca class=\"xref bibr\" href=\"#r78\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler\u003C\u002Fspan\u003E2003\u003C\u002Fa\u003E) and on the right is the EMU-PS image. Prominent in this image is the Giant Radio Galaxy ESO 234-68. The maximum flux density of ESO 234-68 in the EMU-PS image is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline104.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"103\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline104.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$58.8 \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, and that of the strong source at the bottom of the image (PMN J2045-5135) is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline105.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"86\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline105.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$1.06 \\mathrm{Jy beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The rms of the EMU-PS image is 25–30 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline106.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline106.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, and that of the SUMSS image is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline107.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"119\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline107.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}1.25\\ \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E Ideally, we would convolve the EMU-PS to the 45-arcsec resolution of SUMSS and then repeat the source extraction, but then it would not be matched to the EMU-PS value-added catalogue. Because we have not done this convolution, some SUMSS peak flux densities are boosted by components which are included in the SUMSS beam but not in the EMU-PS beam. This increases the scatter of the ratios so that the measured scatter in the ratio is an overestimate of the uncertainty in the EMU-PS flux density scale.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E We note the following features of \u003Ca class=\"xref fig\" href=\"#f15\"\u003EFigure 15\u003C\u002Fa\u003E.\n\u003C\u002Fp\u003E\u003Cul class=\"list nomark\"\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E The EMU-PS central frequency of 944-MHz differs from the SUMSS central frequency of 843 MHz, and, assuming a spectral index of –0.8, we expect the peak of the distribution to occur at a ratio of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline108.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"135\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline108.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}(944\u002F843)^{0.8} = 1.09 $\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E as observed.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E The histogram is more extended on the right, presumably because of the larger size of the SUMSS beam which will boost the SUMSS peak flux as discussed above.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E The left of the histogram is approximately Gaussian with a standard deviation of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline109.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline109.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.12.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003C\u002Ful\u003E\n\n\u003Cp class=\"p\"\u003E We therefore estimate our flux density scale uncertainty for strong sources to have a maximum value of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline110.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"25\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline110.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sigma \\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E12%. To this should be added in quadrature the estimated flux density scale standard error for SUMSS of 3% (Mauch et al. \u003Ca class=\"xref bibr\" href=\"#r78\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler\u003C\u002Fspan\u003E2003\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The measured flux density of weaker sources will be degraded by a factor of 1\u002FSNR, where SNR is the local signal-to-noise ratio. As we have rejected sources from the EMU-PS catalogue with SNR\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline111.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline111.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$<$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E5, this may add an uncertainty of up to 20% (to be added in quadrature) to the quoted flux densities of weak sources.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec results\" data-magellan-destination=\"s5\" id=\"s5\"\u003E\n\n\u003Ch2 class=\"A\"\u003E\u003Cspan class=\"label\"\u003E5.\u003C\u002Fspan\u003E Results\u003C\u002Fh2\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s5-1\" id=\"s5-1\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E5.1.\u003C\u002Fspan\u003E Data summary and access\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E The EMU-PS has produced an image of about \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline112.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"53\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline112.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$270 \\,\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E of the radio sky at 944 MHz, with a spatial resolution of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline113.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline113.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E11–13 arcsec and an rms sensitivity of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline114.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline114.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E25–30 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline115.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"75\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline115.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E A problem with large surveys is that it is difficult to convey the scale and depth of the image in a journal paper. \u003Ca class=\"xref fig\" href=\"#f9\"\u003EFigure 9\u003C\u002Fa\u003E shows the entire native resolution image, and \u003Ca class=\"xref fig\" href=\"#f16\"\u003EFigure 16\u003C\u002Fa\u003E shows a random section of it, which covers about one thousandth of the area of the EMU-PS. An interactive interface to the image of the entire survey field in HiPS format is available on \u003Ca class=\"uri\" href=\"http:\u002F\u002Femu-survey.org\"\u003Ehttp:\u002F\u002Femu-survey.org\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E After observing, processing, and validation by the EMU survey team, the data from each observation are placed on the CSIRO ASKAP Science Data Archive (CASDA) data server and made available to the public as described below. These data consist of all the data from each day’s observations, known as a ‘tile’, including images and tables of extracted components and islands. We call this catalogue the EMU Pilot Initial Public Data Release. The validation metrics and flags are associated with each tile and are fully queryable via table access protocol (TAP).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The data are then processed by merging tiles into a common image covering the whole field of the EMU-PS. The resulting data release of this image is called the ‘native’ value-added data release.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E As described in \u003Ca class=\"xref sec\" href=\"#s4\"\u003ESection 4\u003C\u002Fa\u003E, we then smooth the native resolution image to a constant resolution of 18 arcsec, perform source extraction, and separate the resulting catalogue of 220 102 components into simple, single, components (81%), and more complex sources (19%). We also perform cross-identifications of the simple sources with other available multiwavelength products.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E We call this science-ready data set the ‘Convolved’ data set. The resulting image for an area of sky covering an object of interest is shown in \u003Ca class=\"xref fig\" href=\"#f17\"\u003EFigure 17\u003C\u002Fa\u003E, which shows the three data products: the initial public data release, the added-value ‘native’ data release with 11–13 arcsec resolution, and the added-value ‘convolved’ data release with 18 arcsec resolution.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f17\" id=\"f17\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig17.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"3680\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig17.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 17.\u003C\u002Fspan\u003E A sample of the final image, showing the three data products on a region, covered by three tiles, containing two of the ‘Odd Radio Circles’(Norris et al. \u003Ca class=\"xref bibr\" href=\"#r95\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E): (a) the initial public data release from a single tile (SB9351) (resolution 11 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline116.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline116.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\times$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E 13 arcsec, rms = \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline117.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"93\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline117.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$40 \\,\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, (b) the added-value ‘native’ data release with 11\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline118.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline118.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\times$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E13 arcsec resolution, from the merged tiles, rms = 25 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline119.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"75\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline119.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, and (c) the added-value ‘convolved’ data release with 18 arcsec resolution, rms = 25 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline120.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline120.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The peak flux density in this image is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline121.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"99\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline121.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$4.6\\ \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E All three data products from the EMU-PS (the initial public data release, the added-value ‘native’ data release with 11–13 arcsec resolution, and the added-value ‘convolved’ data release with 18 arcsec resolution) are released via the CASDA data server described below. The initial public data release is currently available in the public domain, but the two added-value data releases are available only to EMU members for a proprietary period of 1 year from the date of publication of this paper, after which they will be released into the public domain. However, EMU is an open collaboration, and other astronomers are welcome to join the project, and access the proprietary data, provided they agree to the EMU data and publication policies.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The EMU-PS initial public release data in the CASDA are open to the public domain. To download data from CASDA, users need to obtain a CASS Online Proposal Applications and Links (OPAL) account\u003Ca class=\"xref fn\" href=\"#fn6\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Ef\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E CASDA is described in detail by Chapman et al. (\u003Ca class=\"xref bibr\" href=\"#r23\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Chapman, Dempsey, Miller, Heywood, Pritchard, Sangster, Whiting, Dart, Lorente, Shortridge and Wayth\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E) and Huynh et al. (\u003Ca class=\"xref bibr\" href=\"#r55\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Huynh, Dempsey, Whiting, Ophel, Ballester, Ibsen, Solar and Shortridge\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E). In brief, CASDA is implemented across two data centres, the Pawsey Supercomputing Centre in Perth and the CSIRO data centre in Canberra. So-called ‘backend’ functions such as deposit, storage, and data access are implemented at Pawsey, while the ‘frontend’ functions such as the user interface and authentication are implemented at the CSIRO data centre.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The simplest way to access the data is via the CASDA web user interface. From the CASDA webpage\u003Ca class=\"xref fn\" href=\"#fn7\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Eg\u003C\u002Fa\u003E, select ‘Access CASDA via the Data Access Portal’, to be taken to the Observation Search user interface. EMU-PS data can be obtained by searching for ‘Released’ data under project code AS101. EMU-PS data have Digital Object Identifiers (DOIs) which provide a persistent resolvable link to the data. \u003Ca class=\"xref table\" href=\"#tbl7\"\u003ETable 7\u003C\u002Fa\u003E gives the DOI for each data product discussed in this paper. The DOI links to the collection page; from there click on ‘files’ and select the files to download.\n\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E CASDA also implements several Virtual Observatory services to maximise the usability and interoperability of ASKAP data products and allow for automated scripted access. For example, the TAP can be used to search for EMU-PS observations under project code AS101, using an application such as TOPCAT (Taylor \u003Ca class=\"xref bibr\" href=\"#r116\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Taylor, Shopbell, Britton and Ebert\u003C\u002Fspan\u003E2005\u003C\u002Fa\u003E) or Aladin (Boch & Fernique \u003Ca class=\"xref bibr\" href=\"#r9\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Boch, Fernique, Manset and Forshay\u003C\u002Fspan\u003E2014\u003C\u002Fa\u003E; Bonnarel et al. \u003Ca class=\"xref bibr\" href=\"#r14\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bonnarel\u003C\u002Fspan\u003E2000\u003C\u002Fa\u003E). A CASDA module has recently been added to the Python astropy astroquery\u003Ca class=\"xref fn\" href=\"#fn8\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Eh\u003C\u002Fa\u003E package. Using this Python API, the EMU-PS images can be accessed and downloaded with a cone search of the EMU-PS pointings.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E All public data (tables and images, and \u003Cem class=\"italic\"\u003Eu\u003C\u002Fem\u003E,\u003Cem class=\"italic\"\u003Ev\u003C\u002Fem\u003E data) are available from CASDA (see \u003Ca class=\"xref table\" href=\"#tbl7\"\u003ETable 7\u003C\u002Fa\u003E) and a listing of all ASKAP observations is on the Observation Management Portal (OMP)\u003Ca class=\"xref fn\" href=\"#fn9\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Ei\u003C\u002Fa\u003E. OMP allows the user to select observations by several parameters including date, SBID (listed in \u003Ca class=\"xref table\" href=\"#tbl3\"\u003ETable 3\u003C\u002Fa\u003E), or project name (AS101 for EMU).\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s5-2\" id=\"s5-2\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E5.2.\u003C\u002Fspan\u003E Sensitivity to compact sources\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E The EMU-PS survey reaches a typical sensitivity of 25–30 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline122.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline122.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E rms. This is about a factor of two above the calculated thermal noise sensitivity (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline123.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline123.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E13 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline124.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline124.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E), which we tentatively attribute to the following causes.\n\u003C\u002Fp\u003E\u003Cul class=\"list nomark\"\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E Timing errors in the correlator cause a significant fraction of data (30–50%) to be flagged, resulting in a loss of data. Work is in progress to identify and eliminate the cause of this problem.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E The data calibration processes are in a preliminary state. By the time of the final EMU survey, we expect to have developed a sky model which will be used to calibrate the data and remove strong sources prior to cleaning.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E A dynamic range problem, which is currently being addressed, causes diffraction patterns around strong sources.\u003C\u002Fp\u003E\u003Cdiv class=\"table-wrap\" data-magellan-destination=\"tbl7\" id=\"tbl7\"\u003E\n\n\u003Cdiv class=\"caption\"\u003E\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003ETable 7.\u003C\u002Fspan\u003E Available data products, including Digital Object Identifiers (DOIs) that can be used to access the data described in this paper.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cspan\u003E\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab7.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"499\" height=\"155\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_tab7.png\" data-zoomable=\"false\"\u003E\u003C\u002Fdiv\u003E\n\u003C\u002Fspan\u003E\n\u003Cdiv class=\"table-wrap-foot\"\u003E\n\u003Cp class=\"p\"\u003E Notes:\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E •The initial public data release is immediately available, but the value-added releases are available only to members of the EMU collaboration for 1 year from the data of publication of this paper, after which they become public.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E •All catalogues contain island and component information, and, for the added-value catalogue, cross-identifications and redshifts, where available.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E •TT0 and TT1 refer to Taylor Term 0 image (total power) and Taylor Term 1 image (TT0 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline125.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline125.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\times$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E spectral index)\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f18\" id=\"f18\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig18.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"3000\" height=\"1067\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig18.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 18.\u003C\u002Fspan\u003E The sensitivity of EMU-PS as a function of spatial scale. The plot was made using visibility data from a single beam and pointing of an interleaved observation (2-h observation, 288-MHz bandwidth, scaled to the EMU-PS observing frequency of 944 MHz) which was filled with Gaussian noise and various uv tapers were applied to shape the beam size. We then measured the image noise (effectively the sensitivity at the scale associated with the uv taper). The two plots show the same result over different ranges of spatial scale.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E The primary beam correction assumes a Gaussian profile across each PAF beam. This is being replaced by a profile based on holographic measurements which will be beam-specific.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003Cli class=\"list-item\"\u003E\n\u003Cp class=\"p\"\u003E The lack of direction-dependent calibration, which we hope to address in the future.\u003C\u002Fp\u003E\n\u003C\u002Fli\u003E\n\u003C\u002Ful\u003E\n\n\u003Cp class=\"p\"\u003E After correcting these errors, and including a confusion noise of about 9 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline126.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline126.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, we expect the full EMU survey (conducted at a centre frequency of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline127.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline127.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E944 MHz) can potentially reach an rms of about 17.5 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline128.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline128.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s5-3\" id=\"s5-3\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E5.3.\u003C\u002Fspan\u003E Sensitivity to extended emission\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E As well as its high sensitivity to compact sources, the survey also has high sensitivity to extended low surface brightness emission, because of the large number of short spacings in the ASKAP array.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E In \u003Ca class=\"xref fig\" href=\"#f18\"\u003EFigure 18\u003C\u002Fa\u003E, we show a plot of the sensitivity of EMU-PS as a function of spatial scale, obtained by running simulated observations with different tapers, producing different beam sizes.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The sensitivity of 25–30 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline129.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"75\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline129.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E at the native resolution of 11–13 arcsec is almost unchanged at the convolved resolution of 18 arcsec and continues at a similar level beyond the 45-arcsec resolution of SUMSS (Mauch et al. \u003Ca class=\"xref bibr\" href=\"#r78\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler\u003C\u002Fspan\u003E2003\u003C\u002Fa\u003E), which has a median rms sensitivity of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline130.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"102\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline130.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$1.27 \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The effect of this high sensitivity to low surface brightness emission is demonstrated in \u003Ca class=\"xref sec\" href=\"#s6\"\u003ESection 6\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s5-4\" id=\"s5-4\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E5.4.\u003C\u002Fspan\u003E Source counts and confusion\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref fig\" href=\"#f19\"\u003EFigure 19\u003C\u002Fa\u003E shows the differential source counts normalised to a non-evolving Euclidean model (n \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline131.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline131.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\propto S^{2.5}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) obtained from the EMU-PS catalogue (black symbols), rescaled from 943.5 MHz to 1.4 GHz by assuming \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline132.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"60\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline132.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha=-0.7$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Two counts’ determinations are shown: one referring to the \u003Cem class=\"italic\"\u003Eisland\u003C\u002Fem\u003E catalogue, where components of complex sources are merged together (filled diamonds) and one referring to simple sources only (empty diamonds). The source counts are corrected for both Eddington bias (Eddington \u003Ca class=\"xref bibr\" href=\"#r34\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Eddington\u003C\u002Fspan\u003E1913\u003C\u002Fa\u003E; Eddington \u003Ca class=\"xref bibr\" href=\"#r35\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Eddington\u003C\u002Fspan\u003E1940\u003C\u002Fa\u003E) and resolution bias (i.e. the incompleteness introduced by the fact that a larger source of a given total flux density will drop below the signal-to-noise threshold of a survey more easily than a smaller source of the same total flux density). This is done following standard recipes in the literature (see e.g. Prandoni et al. 2001; \u003Ca class=\"xref bibr\" href=\"#r103\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Prandoni, Guglielmino, Morganti, Vaccari, Maini, Röttgering, Jarvis and Garrett\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E; Mandal et al. \u003Ca class=\"xref bibr\" href=\"#r75\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mandal\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f19\" id=\"f19\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig19.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1190\" height=\"864\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig19.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 19.\u003C\u002Fspan\u003E Normalised differential source counts derived from the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline133.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"54\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline133.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$270\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E EMU-PS survey for the \u003Cem class=\"italic\"\u003Eisland\u003C\u002Fem\u003E catalogue (black filled diamonds) and for simple sources only (black empty diamonds). The counts have been rescaled from 943.5 MHz to 1.4 GHz by assuming \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline134.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"60\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline134.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha=-0.7$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Also shown for comparison are the counts derived from 1.4 GHz \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline135.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline135.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E degree-scale surveys (symbols and colours as indicated in the figure). Vertical bars represent Poissonian errors on the normalised counts. Systematic errors due to incompleteness corrections and spectral index assumptions are approximately included in the size of the plotted symbols. The result of the \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) analysis performed by (Vernstrom et al. \u003Ca class=\"xref bibr\" href=\"#r119\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Vernstrom\u003C\u002Fspan\u003E2014\u003C\u002Fa\u003E, rescaled from 3 to 1.4 GHz by assuming \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline136.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline136.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha $\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E = \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline137.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline137.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.7) is indicated in dark green. The black solid line represents the predicted counts from 200 sq. degr. of the S3-SEX simulations (Wilman et al. \u003Ca class=\"xref bibr\" href=\"#r127\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Wilman\u003C\u002Fspan\u003E2008\u003C\u002Fa\u003E). The light blue and yellow shaded areas illustrate the predicted cosmic variance effects for survey coverages of 5 and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline138.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline138.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$10\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, respectively (obtained by splitting the S3-SEX simulation in 40 5-\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline139.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"28\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline139.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and 20 10-\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline140.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"27\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline140.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E fields, respectively). The \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline141.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"46\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline141.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$25\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E medium tier of the more recent T-RECS simulations (Bonaldi et al. \u003Ca class=\"xref bibr\" href=\"#r12\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bonaldi, Bonato, Galluzzi, Harrison, Massardi, Kay, De Zotti and Brown\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E) is represented by the purple shaded area. Finally, the Mancuso et al. (\u003Ca class=\"xref bibr\" href=\"#r74\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mancuso\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E) radio source evolutionary model is shown by the light green line.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref fig\" href=\"#f19\"\u003EFigure 19\u003C\u002Fa\u003E shows for comparison some of the widest-area samples available to date at 1.4 GHz. This includes sub-mJy surveys covering \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline142.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"53\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline142.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>1\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E regions, like PDF (Hopkins et al. \u003Ca class=\"xref bibr\" href=\"#r53\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Hopkins, Afonso, Chan, Cram, Georgakakis and Mobasher\u003C\u002Fspan\u003E2003\u003C\u002Fa\u003E), VLA-COSMOS (Bondi et al. \u003Ca class=\"xref bibr\" href=\"#r13\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bondi, Ciliegi, Schinnerer, Smolčić, Jahnke, Carilli and Zamorani\u003C\u002Fspan\u003E2008\u003C\u002Fa\u003E) and the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline143.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"39\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline143.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$6\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E Westerbork mosaic covering the Lockman Hole region (LHW: Prandoni et al. \u003Ca class=\"xref bibr\" href=\"#r103\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Prandoni, Guglielmino, Morganti, Vaccari, Maini, Röttgering, Jarvis and Garrett\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E), as well as shallower (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline144.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"21\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline144.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$> 1$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E mJy) but larger (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline145.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"15\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline145.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\gg$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E10 sq. degr.) surveys like ATESP (Prandoni et al. \u003Ca class=\"xref bibr\" href=\"#r101\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Prandoni, Gregorini, Parma, de Ruiter, Vettolani, Wieringa and Ekers\u003C\u002Fspan\u003E2001\u003C\u002Fa\u003E), SDSS Stripe 82 (Heywood et al. \u003Ca class=\"xref bibr\" href=\"#r52\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Heywood\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E) and FIRST (White et al. \u003Ca class=\"xref bibr\" href=\"#r120\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference White, Becker, Helfand and Gregg\u003C\u002Fspan\u003E1997\u003C\u002Fa\u003E). Also shown are simulated source counts derived by combining evolutionary models of either classical radio loud (RL) AGN or radio source populations dominating the sub-mJy radio sky, namely SFGs and low-luminosity AGN (LLAGN). In particular, we show the 1.4-GHz counts derived from the recent modelling of Mancuso et al. (\u003Ca class=\"xref bibr\" href=\"#r74\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mancuso\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E), light green solid line, the T-RECS \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline146.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"46\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline146.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$25\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E medium tier simulation (Bonaldi et al. \u003Ca class=\"xref bibr\" href=\"#r12\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bonaldi, Bonato, Galluzzi, Harrison, Massardi, Kay, De Zotti and Brown\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E), as well as different realisations obtained from the S3-SEX simulated catalogue (Wilman et al. \u003Ca class=\"xref bibr\" href=\"#r127\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Wilman\u003C\u002Fspan\u003E2008\u003C\u002Fa\u003E): \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline147.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"79\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline147.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$1\\times 200\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (black solid line), \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline148.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"79\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline148.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$20\\times 10\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E regions (yellow shaded area) and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline149.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"72\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline149.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$40\\times 5\\ \\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E regions (light blue shaded area).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref fig\" href=\"#f19\"\u003EFigure 19\u003C\u002Fa\u003E clearly shows that the source counts derived from the EMU-PS \u003Cem class=\"italic\"\u003Eisland\u003C\u002Fem\u003E catalogue nicely match previous counts and are in good agreement with the most recent models\u002Fsimulations (Mancuso et al. \u003Ca class=\"xref bibr\" href=\"#r74\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mancuso\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E; Bonaldi et al. \u003Ca class=\"xref bibr\" href=\"#r12\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bonaldi, Bonato, Galluzzi, Harrison, Massardi, Kay, De Zotti and Brown\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E). Even more interestingly they provide very robust statistics all the way from \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline150.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"60\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline150.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}0.1\\,\\textrm{mJy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline151.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"22\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline151.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>1$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E Jy, something which could only be achieved in the past by combining deeper (but smaller) surveys with larger (but shallower) surveys. Finally, it is interesting to note that the counts derived from simple sources only (black empty diamonds) fall well below the full counts (black filled diamonds) at bright fluxes. This is not surprising as we expect a large contribution from multi-component RL AGN at flux densities \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline152.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"25\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline152.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\gg 1$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E mJy. On the other hand, no significant difference is observed at sub-mJy fluxes, confirming that this flux regime is dominated by SFG and LLAGN.\u003C\u002Fp\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s5-4-1\" id=\"s5-4-1\"\u003E\n \u003Ch4 class=\"C\"\u003E\u003Cspan class=\"label\"\u003E5.4.1.\u003C\u002Fspan\u003E Source Confusion\u003C\u002Fh4\u003E\n\u003Cp class=\"p\"\u003E We estimate the source confusion noise, and instrumental noise using the probability of deflection, or \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) technique (Scheuer \u003Ca class=\"xref bibr\" href=\"#r112\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Scheuer\u003C\u002Fspan\u003E1957\u003C\u002Fa\u003E). The \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) distribution of an image is the distribution of pixel intensities (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline153.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"64\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline153.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) which depends on the underlying source count, shape of the beam, and the instrumental noise (see Vernstrom et al. \u003Ca class=\"xref bibr\" href=\"#r119\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Vernstrom\u003C\u002Fspan\u003E2014\u003C\u002Fa\u003E, for a detailed description of the method).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) method assumes a Gaussian distribution for the instrumental noise and can therefore be affected by imaging artefacts, such as those found around bright sources. We computed the histogram of pixel intensities for the pilot survey image by selecting regions of pixels devoid of any image artefacts, as well as any complex diffuse or extended emission. Rather than a full source count fitting analysis, which is beyond the scope of this paper, we take the deep \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) source counts derived in Vernstrom et al. (\u003Ca class=\"xref bibr\" href=\"#r119\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Vernstrom\u003C\u002Fspan\u003E2014\u003C\u002Fa\u003E) and scale it to a frequency of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline154.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"24\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline154.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$944\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003EMHz using \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline155.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"60\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline155.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha =-0.7$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. We take the average beam sizes from the individual beams and find \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline156.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"59\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline156.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$B_{\\rm maj}=12\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E arcsec and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline157.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"61\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline157.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$B_{\\rm min}=10\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E arcsec, while using an image of the ‘dirty’ synthesised beam for sources below the clean limit (approximated at \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline158.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"149\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline158.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\rm clean}=200\\, \\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E). We use an average instrumental noise value of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline159.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"122\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline159.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sigma=23\\, \\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The image \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E), noise distribution, and model \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) can be seen in \u003Ca class=\"xref fig\" href=\"#f20\"\u003EFigure 20\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f20\" id=\"f20\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig20.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1499\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig20.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 20.\u003C\u002Fspan\u003E The EMU-PS preliminary \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) distributions. The solid black line is the probability distribution made from sections of the pilot away from bright sources. The upper right inset shows bright flux density tail of the \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) distributions. The blue dot-dashed line shows a Gaussian noise distribution of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline160.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"118\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline160.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sigma= 23 \\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The red dashed line shows the predicted or model \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) generated from the source count shown in the lower right inset.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E Without any additional fitting or changes to the parameters or source count, we find very good agreement between the image and model \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) distributions. The noise-free model \u003Cem class=\"italic\"\u003EP\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E) provides an estimate of the confusion noise in the field of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline161.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"132\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline161.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sigma_{\\rm conf}=5\\, \\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. This quick test shows through independent means that the instrumental noise estimate of 20 to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline162.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"92\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline162.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$25\\, \\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E is accurate. Furthermore, the fact that the scaled source count model provides a good match to the image is a confirmation of accurate source flux densities in the pilot data, and that confusion noise is not a significant factor for our scientific investigations, even when considering the dirty beam sidelobe confusion noise. At the same time, the observations of P(D) are sensitive enough to probe far below the source populations that we can directly detect.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec other\" data-magellan-destination=\"s6\" id=\"s6\"\u003E\n\n\u003Ch2 class=\"A\"\u003E\u003Cspan class=\"label\"\u003E6.\u003C\u002Fspan\u003E Preliminary science results\u003C\u002Fh2\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-1\" id=\"s6-1\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.1.\u003C\u002Fspan\u003E Peculiar radio sources\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E Many unusual radio sources are found in the EMU-PS.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The source PKS 2130-538, shown in \u003Ca class=\"xref fig\" href=\"#f21\"\u003EFigure 21\u003C\u002Fa\u003E, has been previously identified as a complex source (e.g. Ekers \u003Ca class=\"xref bibr\" href=\"#r36\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Ekers\u003C\u002Fspan\u003E1970\u003C\u002Fa\u003E; Schilizzi & McAdam \u003Ca class=\"xref bibr\" href=\"#r113\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Schilizzi and McAdam\u003C\u002Fspan\u003E1975\u003C\u002Fa\u003E; Jones & McAdam \u003Ca class=\"xref bibr\" href=\"#r62\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jones and McAdam\u003C\u002Fspan\u003E1992\u003C\u002Fa\u003E), and as two radio galaxies (G4Jy 1704 and G4Jy 1705) in the G4Jy Sample (White et al. \u003Ca class=\"xref bibr\" href=\"#r122\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference White\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003Eb; White et al. \u003Ca class=\"xref bibr\" href=\"#r121\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference White\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003Ea). However, no previous image shows the wealth of detail and low surface brightness emission seen in \u003Ca class=\"xref fig\" href=\"#f21\"\u003EFigure 21\u003C\u002Fa\u003E. It consists of the radio lobes of two host galaxies, one of which (‘Host 1’: 2MASX J21341775-5338101) is the bright galaxy at the centre of the curved northern radio bridge, at a redshift of 0.0781. This is the brightest galaxy of the cluster Abell 3785. The other host galaxy (‘Host 2’: 2MASX J21340666-5334186) is the bright galaxy near the southeast end, at a redshift of 0.0763.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f21\" id=\"f21\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig21.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"3666\" height=\"1395\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig21.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 21.\u003C\u002Fspan\u003E A peculiar radio source found in the EMU Pilot Survey, consisting of a group of distorted radio components, collectively known as PKS 2130–538, and nicknamed ‘the dancing ghosts’. The two host galaxies (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline163.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"61\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline163.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z \\sim 0.077$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) are seen at the centre of the narrow jets (shown with numbers in the figure to indicate their putative host) which expand into diffuse lobes, probably bent by interactions. On the left is the total intensity greyscale image (shown in turquoise), superimposed on a background of the DES optical image, assembled from the r, g, and i images. On the right is the total intensity image of PKS 2130-538, colour-coded by spectral index. The unconventional colour scheme was constructed using sequential colours on the ‘colour wheel’ (e.g. Itten \u003Ca class=\"xref bibr\" href=\"#r58\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Itten\u003C\u002Fspan\u003E1970\u003C\u002Fa\u003E). The colours were fixed in luminosity, that is, fixed to be constant in luminosity-chroma-hue colour space (Ferrand \u003Ca class=\"xref bibr\" href=\"#r38\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Ferrand\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E). In this way, the brightness level on the image represents only the total intensity values. The colour bar indicates the spectral index at a single fixed intensity. Since the spectral index map in this colour scheme was multiplied by the total intensity map, darker versions of colours are associated with fainter regions in the data. The peak flux density in this image is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline164.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"102\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline164.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$103\\ \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E The spectral index image helps to isolate the contributions from these two hosts. In the north, there is a very flat spectrum region (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline165.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"35\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline165.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha \\sim 0$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) at the position of Host 1, connecting to relatively flat \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline166.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"90\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline166.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha \\sim -0.4{-}0.5$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E jets (‘1’). These then connect to the large bright regions of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline167.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"92\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline167.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha \\sim -0.6{-}0.7$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, steepening sharply down the tails to the south to at least -1.5, beyond which the spectra become more uncertain. All of this is consistent with the behaviour of bent-tail galaxies. In the eastern half, there is a dramatic change in spectral index at the position of the emission associated with the second host; it has its own flat core and steeper lobe\u002Ftail structures. Although the overall emission comes from two distinct hosts, it is unclear whether there is an interaction between them, or merely a superposition. An additional curiosity is the thin stream of emission ‘3’ extending eastward from the NE bright region; it has a median spectral index of -2.1, and both its dynamical origins and particle history do not fit naturally into existing radio galaxy models.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The source PMN J2041-5256, shown in \u003Ca class=\"xref fig\" href=\"#f22\"\u003EFigure 22\u003C\u002Fa\u003E, is a double-lobed radio AGN, associated with the host galaxy WISEA J204112.05-525737.7 at a redshift of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline168.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"59\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline168.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z=0.048$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Previous radio data (Mauch et al. \u003Ca class=\"xref bibr\" href=\"#r78\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mauch, Murphy, Buttery, Curran, Hunstead, Piestrzynski, Robertson and Sadler\u003C\u002Fspan\u003E2003\u003C\u002Fa\u003E; Gregory et al. \u003Ca class=\"xref bibr\" href=\"#r44\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Gregory, Vavasour, Scott and Condon\u003C\u002Fspan\u003E1994\u003C\u002Fa\u003E) show only an indistinct extended source corresponding to the nucleus. Its jets (shown with numbers in the figure to indicate their putative host) are presumably being bent by intracluster winds, but the morphology is much more complex than normal bent-tail galaxies. The eastern jet (‘2’) is bifurcated, while the western jet (‘1’) breaks down into a number of blobs, accompanied by a large diffuse area of emission to the west of the source. One possibility is that its relative motion with respect to the intracluster medium (ICM) has a large component along the line of sight; the bifurcated tail and western diffuse extensions would then be more typical of structures seen in bent-tail galaxies, but seen here in projection. If the direction of motion were \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline169.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline169.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E20 degrees from the line of sight, the entire source length would be \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline170.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline170.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E750 kpc, among the larger bent-tail sources.\n\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref fig\" href=\"#f23\"\u003EFigure 23\u003C\u002Fa\u003E shows two diffuse clouds of radio emission whose origin is unclear. The most likely hypothesis is that they represent the remnants of a classical double-lobed radio galaxy in which the central engine has switched off, leaving a remnant radio galaxy. We refer to this object as the ‘Smoking Gun.’\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E A tentative identification of the host (marked A in \u003Ca class=\"xref fig\" href=\"#f23\"\u003EFigure 23\u003C\u002Fa\u003E) is the galaxy WISEA J204837.65–491115.2, at a redshift of 0.10 (Bilicki et al. \u003Ca class=\"xref bibr\" href=\"#r8\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bilicki\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E) and which is detected as a \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline171.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"50\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline171.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$260 \\,\\mu\\mathrm{Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E unresolved source in the ASKAP image. At that redshift, the largest angular size across the lobes is 530 kpc, which is not unusual for double-lobed radio galaxies. An alternative identification (marked B in \u003Ca class=\"xref fig\" href=\"#f23\"\u003EFigure 23\u003C\u002Fa\u003E) of the host is an isolated unresolved \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline172.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"49\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline172.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$200 \\,\\mu\\mathrm{Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E radio source which appears to be coincident with the galaxy DES J204835.43-491137.5, at \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline173.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"61\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline173.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z=0.937$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (Zhou et al. \u003Ca class=\"xref bibr\" href=\"#r129\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Zhou\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E). If the ‘Smoking Gun’ were actually at this redshift, then the source’s large inferred radio size (2.25 Mpc) would make it a member of the rare class of ‘Giant Radio Galaxies’ (see \u003Ca class=\"xref sec\" href=\"#s6-4\"\u003ESection 6.4\u003C\u002Fa\u003E) and it would also be very luminous (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline174.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"64\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline174.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}4 \\times 10^{23}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E W\u002FHz). This seems unlikely for a fading remnant, and so we think A, at a redshift of 0.1, is more likely to be the host galaxy. We note that the northern lobe is unusually circular and resembles the Odd Radio Circles (ORCs) shown in \u003Ca class=\"xref fig\" href=\"#f17\"\u003EFigure 17\u003C\u002Fa\u003E, except that the ORCs don’t show a continuous rise of their surface brightness towards their centres.\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f22\" id=\"f22\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig22.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1296\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig22.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 22.\u003C\u002Fspan\u003E Another peculiar radio source found in the EMU Pilot Survey: a double-lobed radio AGN, known as PMN J2041–5256, with a curious ‘double’ bent tail. The radio data from EMU-PS has been ‘stretched’ to show the faint emission, and then coloured turquoise, and adjusted to emphasise the double tail. DES g-, r-, and i-band data are combined to form the background, which is combined with the radio data using a layer mask in GIMP. Embedded in the tails are several radio sources that may be unrelated to the tailed galaxy. The peak flux density in this image is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline175.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"107\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline175.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$58.3\\ \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f23\" id=\"f23\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig23.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1542\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig23.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 23.\u003C\u002Fspan\u003E The ‘Smoking Gun’ Galaxy EMU PS J204835.0–491137 consists of the two diffuse radio clouds seen in this image. These are presumably the remnants of a classical double-lobed radio galaxy in which the central engine has switched off. The labels A and B indicate two possible host galaxies, discussed in the text. The peak flux density in this image is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline176.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"106\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline176.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$0.87\\ \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E Such remnant radio galaxies have previously been reported (e.g. Brienza et al. \u003Ca class=\"xref bibr\" href=\"#r15\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Brienza\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E; Mahatma et al. \u003Ca class=\"xref bibr\" href=\"#r73\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mahatma\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E; Saripalli et al. \u003Ca class=\"xref bibr\" href=\"#r111\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Saripalli, Subrahmanyan, Thorat, Ekers, Hunstead, Johnston and Sadler\u003C\u002Fspan\u003E2012\u003C\u002Fa\u003E), but these new observations probe a lower level of surface brightness than earlier studies. Another remnant radio galaxy imaged by ASKAP has also been recently reported (Quici et al. \u003Ca class=\"xref bibr\" href=\"#r105\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Quici\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E). However, none of the previously reported remnant radio galaxies has a circular lobe resembling that in \u003Ca class=\"xref fig\" href=\"#f23\"\u003EFigure 23\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref fig\" href=\"#f24\"\u003EFigure 24\u003C\u002Fa\u003E shows the radio source EMU PS J210700.0\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline177.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline177.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E501128 (also detected as SUMSS J210704\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline178.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline178.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E501206). It appears similar in some ways to PKS 2130-538 shown above (\u003Ca class=\"xref fig\" href=\"#f21\"\u003EFigure 21\u003C\u002Fa\u003E) with two bright patches and diffuse tails, presumably blown to the east by relative motion through an external medium. However, there is no obvious host galaxy between the lobes, only a scattering of faint DES galaxies. Instead, the bright southern lobe is coincident with the quasar WISEA J210703.75\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline179.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline179.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E501207.7 at a redshift of 0.197 (Monroe et al. \u003Ca class=\"xref bibr\" href=\"#r85\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Monroe, Prochaska, Tejos, Worseck, Hennawi, Schmidt, Tumlinson and Shen\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E), also detected in the Second ROSAT all-sky survey (Boller et al. \u003Ca class=\"xref bibr\" href=\"#r11\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Boller, Freyberg, Trümper, Haberl, Voges and Nandra\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E). This raises the possibility that the two ‘lobes’ are two independent tailed radio galaxies with very similar morphologies. An apparent overdensity of galaxies visible in both DES and WISE is embedded in the faint southern emission. However, there is no cataloged cluster near this location, and we found photometric redshifts (Zou et al. \u003Ca class=\"xref bibr\" href=\"#r131\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Zou, Gao, Zhou and Kong\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E) for only three galaxies within the source confines that would be consistent with the quasar redshift, so there is no evidence for a cluster.\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f24\" id=\"f24\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig24.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1431\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig24.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 24.\u003C\u002Fspan\u003E EMU PS J210700.0–501128.8 is an ambiguous case, appearing at first to be a double-lobed source with material blown to the east. But with no host between the bright patches, and the southern bright component coincident with a quasar, marked with an ‘X’, these may be two independent sources with serendipitously similar appearances The peak flux density in this image is \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline180.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"105\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline180.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$11.6\\ \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-2\" id=\"s6-2\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.2.\u003C\u002Fspan\u003E Odd radio circles\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E It has been predicted that, because EMU would observe a previously inaccessible part of observational parameter space, it would probably make unexpected discoveries (Norris \u003Ca class=\"xref bibr\" href=\"#r92\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003Eb). Nevertheless, we were surprised to find an apparently new class of object appearing in the EMU-PS, consisting of circles of radio emission, typically one arcmin across, with no optical or infrared counterpart (Norris et al. \u003Ca class=\"xref bibr\" href=\"#r95\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E). The first of these ORCs to be identified is shown in \u003Ca class=\"xref fig\" href=\"#f25\"\u003EFigure 25\u003C\u002Fa\u003E, and another example is shown in \u003Ca class=\"xref fig\" href=\"#f17\"\u003EFigure 17\u003C\u002Fa\u003E. We do not yet understand the nature of these objects, nor whether they are a single class of object or multiple classes. Since discovering them in EMU-PS, we have subsequently observed them with several other telescopes to confirm their reality and have been able to rule out some potential explanations such as supernova remnants or starburst rings. We have also found more examples in other ASKAP fields (e.g. Koribalski et al. \u003Ca class=\"xref bibr\" href=\"#r68\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Koribalski, Norris, Andernach, Rudnick, Shabala, Filipovic and Lenc\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E). Several ORCs have a galaxy at the centre, typically at a redshift of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline181.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline181.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.3 in the currently known examples. Potential explanations are that these central galaxies may be the origins of spherical shock waves which we see in projection as a ring, or else that we are seeing end-on radio lobes.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f25\" id=\"f25\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig25.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1427\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig25.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 25.\u003C\u002Fspan\u003E An image of the first ‘Odd Radio Circle’, or ORC, found in EMU-PS (Norris et al. \u003Ca class=\"xref bibr\" href=\"#r95\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E). It has no optical counterpart to the diffuse ring, or to other diffuse structure, but has a galaxy at its centre which may be the origin of the ring. The image is based on EMU-PS data at native resolution but enhanced to show faint features as described in Norris et al. (\u003Ca class=\"xref bibr\" href=\"#r95\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E), particularly the internal structure or “spokes” of the ORC. Radio data are shown in green, and DES optical data are shown in turquoise, magenta, yellow and red, and mainly appear in this image as white.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-3\" id=\"s6-3\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.3.\u003C\u002Fspan\u003E Nearby galaxies\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E The design of ASKAP was largely driven by its two largest survey science projects: the EMU continuum survey (Norris et al. \u003Ca class=\"xref bibr\" href=\"#r94\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Norris\u003C\u002Fspan\u003E2011\u003C\u002Fa\u003E) and the WALLABY spectral line survey (Koribalski et al. \u003Ca class=\"xref bibr\" href=\"#r67\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Koribalski\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E) with the latter aiming to map neutral hydrogen (H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E) over the entire extragalactic sky in the declination range from \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline182.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"32\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline182.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-90^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline183.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline183.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$+30^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E to a redshift of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline184.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline184.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.26. WALLABY will generate H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E image cubes at \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline185.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline185.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E30 arcsec resolution and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline186.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"193\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline186.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}1.6\\ \\mathrm{mJy\\ beam}^{-1}\\ \\mathrm{per}\\ 4\\,\\mathrm{km\\,s}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E channel sensitivity and is expected to detect around half a million galaxies with a mean redshift of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline187.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline187.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.05 (Koribalski et al. \u003Ca class=\"xref bibr\" href=\"#r67\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Koribalski\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The relationship between the integrated radio continuum emission of SFGs, unattenuated by interstellar dust, and their star formation rate (SFR) has been extensively studied, (e.g. Condon \u003Ca class=\"xref bibr\" href=\"#r24\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Condon\u003C\u002Fspan\u003E1992\u003C\u002Fa\u003E; Tabatabaei et al. \u003Ca class=\"xref bibr\" href=\"#r115\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Tabatabaei\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E; Davies et al. \u003Ca class=\"xref bibr\" href=\"#r31\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Davies\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E), and the broad correlation is well documented, (e.g. Condon et al. \u003Ca class=\"xref bibr\" href=\"#r26\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Condon, Cotton and Broderick\u003C\u002Fspan\u003E2002\u003C\u002Fa\u003E; Murphy \u003Ca class=\"xref bibr\" href=\"#r86\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Murphy\u003C\u002Fspan\u003E2009\u003C\u002Fa\u003E; Murphy et al. \u003Ca class=\"xref bibr\" href=\"#r88\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Murphy\u003C\u002Fspan\u003E2011\u003C\u002Fa\u003E; Molnár et al. \u003Ca class=\"xref bibr\" href=\"#r84\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Molnár\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E). However, the detailed correlations and the underlying mechanisms are still the subject of much debate (e.g. Heesen et al. \u003Ca class=\"xref bibr\" href=\"#r49\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Heesen, Brinks, Leroy, Heald, Braun, Bigiel and Beck\u003C\u002Fspan\u003E2014\u003C\u002Fa\u003E). Furthermore, the relationship between the atomic neutral hydrogen gas content of galaxies (for \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline188.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"44\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline188.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z < 0.2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, where individual galaxy detections are feasible) and their SFR requires further investigation (e.g. Wong et al. \u003Ca class=\"xref bibr\" href=\"#r128\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Wong, Meurer, Zheng, Heckman, Thilker and Zwaan\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E; Bera et al. \u003Ca class=\"xref bibr\" href=\"#r7\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bera, Kanekar, Chengalur and Bagla\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Our most extensive knowledge of the southern sky in neutral hydrogen currently comes from the low-resolution H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E Parkes All Sky Survey (HIPASS; Barnes et al. \u003Ca class=\"xref bibr\" href=\"#r5\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Barnes\u003C\u002Fspan\u003E2001\u003C\u002Fa\u003E) which covers the sky from \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline189.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"32\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline189.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-90^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline190.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline190.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$+25^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. HIPASS produced a catalogue of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline191.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline191.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E5000 galaxies out to a redshift of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline192.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"53\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline192.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z = 0.04$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (Koribalski et al. \u003Ca class=\"xref bibr\" href=\"#r66\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Koribalski\u003C\u002Fspan\u003E2004\u003C\u002Fa\u003E; Meyer et al. \u003Ca class=\"xref bibr\" href=\"#r82\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Meyer\u003C\u002Fspan\u003E2004\u003C\u002Fa\u003E). Corresponding 20-cm radio continuum maps (CHIPASS) were created by Calabretta et al. (\u003Ca class=\"xref bibr\" href=\"#r22\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Calabretta, Staveley-Smith and Barnes\u003C\u002Fspan\u003E2014\u003C\u002Fa\u003E). ASKAP delivers a 90-fold (for EMU) or 30-fold (for WALLABY) improvement in angular resolution compared to the HIPASS single-dish beam of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline193.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline193.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E15.5 arcmin.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The survey characteristics of EMU and WALLABY imply that we expect nearly all of the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline194.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline194.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E5000 catalogued HIPASS galaxies to be detected by EMU, and to be well resolved by both EMU and WALLABY. Therefore, the combination of EMU radio continuum and WALLABY H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E spectral line measurements of nearby galaxies, combined with other multi-wavelength data, offers the opportunity to study the relationships between star formation, radio continuum emission, and H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E emission in great detail. Here we start to explore this field using the EMU-PS observations of a small sample of nearby galaxies which have been detected in HIPASS.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Of the 89 catalogued HIPASS sources in the EMU-PS area, 63 are clearly detected by EMU-PS in the radio continuum. We expect most of the remaining HIPASS sources to be detected in the full sensitivity main EMU survey. A selection of these galaxies is shown in \u003Ca class=\"xref fig\" href=\"#f26\"\u003EFigures 26\u003C\u002Fa\u003E and \u003Ca class=\"xref fig\" href=\"#f27\"\u003E27\u003C\u002Fa\u003E. While no WALLABY H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E data currently exist for this field, high-resolution ATCA H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E images are available for some of the galaxies.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f26\" id=\"f26\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig26.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"3000\" height=\"3734\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig26.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 26.\u003C\u002Fspan\u003E A selection of ASKAP-detected nearby galaxies in the EMU-PS. Optical DSS2 \u003Cem class=\"italic\"\u003ER\u003C\u002Fem\u003E-band images are overlaid with ASKAP radio continuum contours. The contour levels are –0.09, 0.09 (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline195.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"30\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline195.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}3 \\sigma$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E), 0.18, 0.36, 0.75, 1.5, 3.0, 7.5, 15.0, and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline196.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"94\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline196.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$30\\ \\mathrm{mJy\\,beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The convolved 18 arcsec beam is shown in the bottom left corner of each panel. The galaxy name and heliocentric velocity (all but one, ESO233-IG004, from HIPASS) are also displayed. The velocity of ESO233-IG004 is taken from Jones et al. (\u003Ca class=\"xref bibr\" href=\"#r64\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jones\u003C\u002Fspan\u003E2009\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E The most interesting galaxy in \u003Ca class=\"xref fig\" href=\"#f26\"\u003EFigure 26\u003C\u002Fa\u003E is the edge-on spiral NGC 7090. Using the ATCA, Heesen et al. (2016; \u003Ca class=\"xref bibr\" href=\"#r51\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Heesen\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E) obtained detailed radio continuum maps, finding a radio halo with polarised emission up to 6 kpc above the disc correlating with extraplanar H\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline197.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"9\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline197.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E emission. ATCA H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E images (Dahlem et al. \u003Ca class=\"xref bibr\" href=\"#r30\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Dahlem, Ehle, Ryder, Vlajić and Haynes\u003C\u002Fspan\u003E2005\u003C\u002Fa\u003E) reveal an asymmetric, slightly disturbed disc matching the stellar extent. Another galaxy of interest is the nearly face-on spiral NGC 7125 (see \u003Ca class=\"xref fig\" href=\"#f27\"\u003EFigure 27\u003C\u002Fa\u003E), which forms an interacting pair with its northern companion NGC 7126, separated by six arcmin (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline198.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline198.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E80 kpc). ATCA H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E maps (Nordgren et al. \u003Ca class=\"xref bibr\" href=\"#r90\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Nordgren, Chengalur, Salpeter and Terzian\u003C\u002Fspan\u003E1997\u003C\u002Fa\u003E) show a large gas envelope encompassing both galaxies. Once detailed H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E spectral line and radio continuum maps are available for large numbers of nearby resolved galaxies, the local and global SFRs and efficiencies can be analysed as a function of H \u003Cspan class=\"sc\"\u003Ei\u003C\u002Fspan\u003E column density and environment (e.g. Koribalski & López-Sánchez \u003Ca class=\"xref bibr\" href=\"#r65\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Koribalski and López-Sánchez\u003C\u002Fspan\u003E2009\u003C\u002Fa\u003E; Wong et al. \u003Ca class=\"xref bibr\" href=\"#r128\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Wong, Meurer, Zheng, Heckman, Thilker and Zwaan\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-4\" id=\"s6-4\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.4.\u003C\u002Fspan\u003E Giant Radio Galaxies\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E Giant Radio Galaxies (GRGs) were originally defined as Radio Galaxies (RGs) whose projected linear size was greater than 1 Mpc for a Hubble constant of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline199.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"144\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline199.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mathrm{H}_0=50\\,\\mathrm{km\\,s}^{-1}\\,\\mathrm{Mpc}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (e.g. Ishwara-Chandra & Saikia \u003Ca class=\"xref bibr\" href=\"#r57\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Ishwara-Chandra and Saikia\u003C\u002Fspan\u003E1999\u003C\u002Fa\u003E). However, based on the currently accepted value of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline200.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"143\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline200.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mathrm{H}_0 \\sim 70\\,\\mathrm{km\\,s}^{-1}\\,\\mathrm{Mpc}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, RGs larger than 0.7 Mpc are now also considered GRGs. In the compilation of GRGs by Kużmicz et al. (\u003Ca class=\"xref bibr\" href=\"#r69\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Kużmicz, Jamrozy, Bronarska, Janda-Boczar and Saikia\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E), the EMU-PS area contains only a single GRG, namely PKS 2014\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline201.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline201.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E558, first mentioned as a GRG by Jones & McAdam (\u003Ca class=\"xref bibr\" href=\"#r62\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jones and McAdam\u003C\u002Fspan\u003E1992\u003C\u002Fa\u003E) and recently studied in detail by Cotton et al. (\u003Ca class=\"xref bibr\" href=\"#r28\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Cotton\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E In a recent ASKAP observation covering \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline202.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline202.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$30 \\,\\mathrm{deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E centred on the Abell 3391\u002F3395 galaxy cluster pair, and of comparable depth and angular resolution as the EMU-PS, Brüggen et al. (\u003Ca class=\"xref bibr\" href=\"#r18\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Brüggen\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E) found the surface density of GRGs \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline203.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"11\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline203.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\gtrsim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E1 Mpc to be \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline204.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"69\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline204.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}0.8\\,\\mathrm{deg}^{-2}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, and that of GRGs \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline205.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"35\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline205.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\gtrsim0.7$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E Mpc to be at least \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline206.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"69\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline206.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}1.7\\,\\mathrm{deg}^{-2}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, suggesting that the EMU-PS should contain \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline207.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline207.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E200 and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline208.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline208.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E460 such GRGs, respectively.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E From a preliminary visual inspection of the EMU-PS area, biased towards sources of larger angular size and featuring a radio nucleus, we found \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline209.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline209.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E120 GRGs larger than 1 Mpc and a similar number with sizes between 0.7 and 1 Mpc. We visually cross-identified these with the DES images and catalogues (Abbott et al. \u003Ca class=\"xref bibr\" href=\"#r1\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Abbott\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E) and estimated linear sizes based on photometric redshifts (Bilicki et al. \u003Ca class=\"xref bibr\" href=\"#r8\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bilicki\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E; Drlica-Wagner et al. \u003Ca class=\"xref bibr\" href=\"#r32\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Drlica-Wagner\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E; Zou et al. \u003Ca class=\"xref bibr\" href=\"#r131\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Zou, Gao, Zhou and Kong\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E). The number of GRGs in EMU-PS is likely to increase with a more thorough visual inspection, the results of which will be reported by Andernach et al. (in prep.).\u003C\u002Fp\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-4-1\" id=\"s6-4-1\"\u003E\n \u003Ch4 class=\"C\"\u003E\u003Cspan class=\"label\"\u003E6.4.1.\u003C\u002Fspan\u003E The Giant Radio Galaxy EMU PS J205139.8–570434\u003C\u002Fh4\u003E\n\u003Cp class=\"p\"\u003E The GRG EMU PS J205139.8–570434 (hereafter GRG J2051–5704), shown in \u003Ca class=\"xref fig\" href=\"#f28\"\u003EFigure 28\u003C\u002Fa\u003E, is hosted by 2MASX J20513976–5704334 at \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline210.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"76\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline210.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z_{sp}=0.0602$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (Jones et al. \u003Ca class=\"xref bibr\" href=\"#r64\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jones\u003C\u002Fspan\u003E2009\u003C\u002Fa\u003E) and its radio emission can be traced over a largest angular size \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline211.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"39\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline211.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}22.1$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E arcmin and thus a linear projected size of 1.53 Mpc. It has an FR I radio morphology whose jets are oriented roughly north-south, feature several wiggles, and terminate in diffuse lobes at both extremes of the source. The strong (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline212.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"84\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline212.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mathrm{S}_{944}=2.12\\,\\mathrm{Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) source 3.1 arcmin due E, surrounded by diffraction rings, is the well-studied galaxy IC 5063 at \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline213.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"84\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline213.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z_{sp} =0.01135$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The central region of the new GRG can be recognised in the SUMSS (Bock et al. \u003Ca class=\"xref bibr\" href=\"#r10\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bock, Large and Sadler\u003C\u002Fspan\u003E1999\u003C\u002Fa\u003E) images and was even detected at mm wavelengths by the South Pole Telescope (Mocanu et al. \u003Ca class=\"xref bibr\" href=\"#r83\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mocanu\u003C\u002Fspan\u003E2013\u003C\u002Fa\u003E). However, the full extended structure shown here has not been previously detected, despite extensive imaging of the neighbouring source IC 5063 (Murphy et al. \u003Ca class=\"xref bibr\" href=\"#r87\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Murphy\u003C\u002Fspan\u003E2010\u003C\u002Fa\u003E and references therein), probably because of the brightness sensitivity and dynamic range limitations.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The host galaxy of GRG J2051–5704 is the brightest galaxy of cluster 400d J2051–5704 (aka MCXC J2051.6–5704, Burenin et al. \u003Ca class=\"xref bibr\" href=\"#r21\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Burenin, Vikhlinin, Hornstrup, Ebeling, Quintana and Mescheryakov\u003C\u002Fspan\u003E2007\u003C\u002Fa\u003E; Piffaretti et al. \u003Ca class=\"xref bibr\" href=\"#r98\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Piffaretti, Arnaud, Pratt, Pointecouteau and Melin\u003C\u002Fspan\u003E2011\u003C\u002Fa\u003E) at a redshift of 0.0599. The radio morphology is reminiscent of archetypal FR I sources such as 3C 31 and Hydra A, with wiggles consistent with either the presence of jet instabilities due to interaction with the surrounding gas, or jet precession (e.g. Nawaz et al. \u003Ca class=\"xref bibr\" href=\"#r89\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Nawaz, Bicknell, Wagner, Sutherland and McNamara\u003C\u002Fspan\u003E2016\u003C\u002Fa\u003E). While FR I type sources are rare among GRGs larger than 1 Mpc, a recent LOFAR image showed that the GRG 3C 31 also had an extent \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline214.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"57\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline214.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>\\ 1\\,\\mathrm{Mpc}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (Heesen et al. \u003Ca class=\"xref bibr\" href=\"#r51\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Heesen\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E It is likely that more of these very large GRGs will be detected with next-generation radio telescopes such as ASKAP thanks to the combination of good angular resolution necessary to reveal the inner jet structure and identify the host, as well as high sensitivity to the low surface brightness features such as the outer tails or lobes. We note that Turner et al. (\u003Ca class=\"xref bibr\" href=\"#r117\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Turner, Rogers, Shabala and Krause\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E) showed from simulations that more sensitive, or lower frequency, observations will reveal FR I galaxies to be much larger than previously thought.\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f27\" id=\"f27\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig27.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1499\" height=\"1370\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig27.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 27.\u003C\u002Fspan\u003E DES-DR1 optical composite image of the nearby face-on spiral galaxy NGC 7125 overlaid with contours from the EMU-PS. The contour levels are: 0.1, 0.25, 0.5, 1.0, 1.3, 1.6, 2.0, and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline215.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"99\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline215.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$2.4\\ \\mathrm{mJy\\,beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. NGC 7125 and its neighbour NGC 7216 form an interacting galaxy pair (HIPASS J2149–60) with a large pool of hydrogen gas for star formation.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-6\" id=\"s6-6\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.5.\u003C\u002Fspan\u003E Radio counterparts to 6dF galaxies\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E EMU and the EMU-PS overlap the 6dF Galaxy Survey (6dFGS; Jones et al. \u003Ca class=\"xref bibr\" href=\"#r63\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jones\u003C\u002Fspan\u003E2004\u003C\u002Fa\u003E; \u003Ca class=\"xref bibr\" href=\"#r64\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jones\u003C\u002Fspan\u003E2009\u003C\u002Fa\u003E), a spectroscopic survey of most of the southern sky containing 125 071 galaxy redshifts with a median redshift of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline216.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"34\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline216.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$0.053$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. While a variety of selection criteria were used for 6dFGS, most 6dFGS galaxies are brighter than \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline217.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"64\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline217.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$K=12.65$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and have redshifts of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline218.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"52\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline218.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z<0.15$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. In the EMU-PS region, there are 2506 6dFGS galaxies and, as we discuss below, a large fraction of these galaxies are detected by the EMU-PS.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E We measured the flux density of each 6dFGS galaxy using the pixel in the radio continuum maps corresponding to each galaxy’s position. This will underestimate the total flux density of spatially resolved galaxies, and aperture bias is relevant as the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline219.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"62\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline219.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$13^{\\prime\\prime}\\times 11^{\\prime\\prime}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E EMU-PS beam and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline220.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"25\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline220.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$6.7^{\\prime\\prime}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E 6dFGS spectroscopic fibre correspond to less than \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline221.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline221.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$3.4\\,{\\rm kpc}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline222.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"47\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline222.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$2.0\\,{\\rm kpc,}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E respectively, for galaxies within \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline223.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"47\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline223.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$60\\,{\\rm Mpc}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E of Earth. Despite these limitations, our preliminary measurements allow us to quantify the fraction of 6dFGS galaxies that are radio sources and allows us to push fainter than blind radio source catalogues. Of the 2506 6dFGS galaxies in the EMU-PS region, 1887 (75%) have a flux density greater than 75 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline224.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline224.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, corresponding to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline225.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"32\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline225.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\gtrsim 3\\sigma$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. As SFGs and passive galaxies have different distributions of radio continuum luminosities, we roughly split these two populations using the presence and absence of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline226.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"21\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline226.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\rm H\\alpha}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, measured from the 6dFGS spectra (Jones et al. \u003Ca class=\"xref bibr\" href=\"#r63\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jones\u003C\u002Fspan\u003E2004\u003C\u002Fa\u003E; \u003Ca class=\"xref bibr\" href=\"#r64\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jones\u003C\u002Fspan\u003E2009\u003C\u002Fa\u003E). To quantify noise and source confusion, we also measure flux density at positions offset by 100 pixels (200 arcsec, so well outside the relevant galaxy).\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E In \u003Ca class=\"xref fig\" href=\"#f29\"\u003EFigure 29\u003C\u002Fa\u003E, we present the histogram of EMU-PS flux densities of 6dFGS galaxies with \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline227.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"21\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline227.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\rm H\\alpha}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and with \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline228.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"64\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline228.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$K<12.65$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, along with the histogram of flux densities measured at offset positions. Roughly half of the SFGs are fainter than \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline229.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"36\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline229.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$1\\,{\\rm mJy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and would not have been detected by previous generations of wide-field radio continuum surveys. Almost all 6dFGS galaxies with detectable \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline230.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"21\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline230.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\rm H\\alpha}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E emission and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline231.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"64\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline231.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$K<12.65$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E in the EMU-PS area are detected, with just 17 of the 623 galaxies having flux densities below \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline232.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"42\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline232.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$75\\,{\\rm \\mu Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. For comparison, at the 623 offset positions there are just 22 flux density measurements brighter than 75 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline233.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"75\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline233.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (corresponding to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline234.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"31\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline234.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\gtrsim 3\\sigma$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) and only 8 flux density measurements brighter than 125 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline235.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"75\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline235.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E (corresponding to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline236.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"31\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline236.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\gtrsim 5 \\sigma$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E).\n\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The radio continuum flux densities of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline237.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline237.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$K<12$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E galaxies with and without \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline238.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"21\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline238.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\rm H\\alpha}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E emission is presented in \u003Ca class=\"xref fig\" href=\"#f30\"\u003EFigure 30\u003C\u002Fa\u003E. Most \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline239.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline239.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$K<12$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E SFGs are detected by EMU-PS, and a significant fraction of passive galaxies are also detected. While the lowest mass passive galaxies are often undetected by EMU-PS, all but one of the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline240.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"69\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline240.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$M_K<-26$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E passive galaxies has a positive radio continuum flux density, presumably resulting from AGNs. This is consistent with Brown et al. (\u003Ca class=\"xref bibr\" href=\"#r17\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Brown, Jannuzi, Floyd and Mould\u003C\u002Fspan\u003E2011\u003C\u002Fa\u003E) and Sabater et al. (\u003Ca class=\"xref bibr\" href=\"#r110\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Sabater\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E), who have concluded that all massive elliptical galaxies are radio continuum sources, using NVSS and LOFAR, respectively. When complete, EMU will detect thousands of nearby \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline241.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"70\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline241.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$M_K<-26$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E elliptical galaxies, enabling characterisation of the radio luminosities of these objects and the AGNs they host.\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f28\" id=\"f28\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig28.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"3208\" height=\"1851\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig28.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 28.\u003C\u002Fspan\u003E (Left) The Giant Radio Galaxy (GRG) EMU PS J205139.8–570434, with radio (at native resolution) shown in greyscale, overlaid on the DES DR1 colour image. The GRG consists of the roughly north-south jet and the two diffuse plumes above and below it. The strong source to the east, surrounded by diffraction rings, is the well-studied galaxy IC 5063. (Right) A contour diagram of the central part of the GRG at 18 arcsec resolution, overlaid on the DES DR1 colour image. Contour levels are 3, 7, 12, and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline242.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"94\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline242.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$18\\ \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-7\" id=\"s6-7\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.6.\u003C\u002Fspan\u003E Comparison with Gaia\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E The Gaia project (Gaia Collaboration et al. 2016) has measured the parallax and proper motion of over a billion stars, and as a byproduct has also identified a number of quasars and compact galaxies (Bailer-Jones et al. \u003Ca class=\"xref bibr\" href=\"#r4\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bailer-Jones, Fouesneau and Andrae\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E). To produce a catalogue of candidate radio-loud quasars, we therefore cross-match the DES counterparts to EMU radio sources against the Gaia EDR3 catalogue (Gaia Collaboration et al. 2021). We use the same technique as in earlier cross-matches in this paper, resulting in a plot of cross-matches as a function of search radius for shifted and unshifted data, shown in \u003Ca class=\"xref fig\" href=\"#f31\"\u003EFigure 31\u003C\u002Fa\u003E. As a result of this test, we choose a cross-match radius of 0.2 arcsec, resulting in 14 174 cross-matches in the unshifted data, and 14 cross-matches in the shifted data, indicating a false-ID rate of 0.1%.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E To explore the infrared properties of this sample of Gaia-selected sources, we need to use the WISE W3 band, which is absent from the CWISE catalogue, and so we must match our sources against the AllWISE catalogue (Cutri et al. \u003Ca class=\"xref bibr\" href=\"#r29\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Cutri\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E). We therefore cross-match the list of 14 174 sources, using a search radius of 1 arcsec, against the AllWISE catalogue, resulting in a catalogue of 11 142 sources with WISE W1, W2, and W3 flux densities. These sources are shown in \u003Ca class=\"xref fig\" href=\"#f32\"\u003EFigure 32\u003C\u002Fa\u003E, colour-coded by their proper motion.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The sources with the lowest proper motions lie in the region identified by Jarrett et al. (\u003Ca class=\"xref bibr\" href=\"#r59\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jarrett\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E) as being dominated by quasars, while a higher level of proper motion is seen in the region dominated by galaxies. This effect was also noted by Bailer-Jones et al. (\u003Ca class=\"xref bibr\" href=\"#r4\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bailer-Jones, Fouesneau and Andrae\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E) who explained it as extended galaxies not having well-defined centroids, causing the measured Gaia position to vary, resulting in an apparent proper motion. The group with the highest proper motion (coded as yellow) lie in the region designated as stars, confirming that these DES sources are indeed stars. However, most, if not all, of these ‘stars’ are probably false IDs and do not correspond to radio sources.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Of the 11 142 galaxies with W1, W2, and W3 flux densities, 2604 have W1-W2 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline243.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline243.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.8, and we refer to these as quasar candidates. To estimate the false-ID rate, we repeated the above selection process after shifting the declination by 1 arcmin, and this resulted in 2312 sources with W1, W2, and W3 flux densities, of which 503 have W1-W2 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline244.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"8\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline244.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$>$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.8. We therefore expect that 81% of our quasar candidates are radio-loud quasars, assuming that no other types of source fall in that part of the WISE colour diagram.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The combination of the Gaia selection and the WISE colour selection has, therefore, yielded a catalogue of 2312 radio-loud quasar candidates, of which about 81% are true radio-loud quasars. Using the same technique on the entire EMU survey will yield a catalogue of about 230 000 radio-loud quasar candidates, representing a significant increase in the number of known radio-loud quasars.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-8\" id=\"s6-8\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.7.\u003C\u002Fspan\u003E Clusters of galaxies\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E Galaxy clusters represent some of the largest gravitationally bound structures in the universe, and radio emission provides an insight into their formation and evolution. They evolve and grow through a variety of processes including passive accretion of gas, consumption of small galaxy groups, and violent merger events which can deposit vast amounts of energy (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline245.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"39\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline245.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}10^{64}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E erg, e.g. Ferrari et al. \u003Ca class=\"xref bibr\" href=\"#r39\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Ferrari, Govoni, Schindler, Bykov and Rephaeli\u003C\u002Fspan\u003E2008\u003C\u002Fa\u003E) into the ICM.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Many merging galaxy clusters host vast and enigmatic radio continuum sources. These diffuse radio sources are broadly classified into two categories: radio relics (or cluster radio shocks) and radio halos (see van Weeren et al. \u003Ca class=\"xref bibr\" href=\"#r133\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference van Weeren, de Gasperin, Akamatsu, Brüggen, Feretti, Kang, Stroe and Zandanel\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E, for a recent review). To date, some \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline246.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"27\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline246.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}70$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E clusters are known to host radio relics, and some \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline247.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"28\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline247.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}65$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E clusters are known to host radio halos\u003Ca class=\"xref fn\" href=\"#fn10\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Ej\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Radio relics are highly extended (typically \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline248.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"19\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline248.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}1$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E Mpc), highly polarised, diffuse synchrotron sources that lie towards the periphery of galaxy clusters. They often exhibit curved morphologies and filamentary sub-structures and are thought to be powered by shocks which generate relativistic electrons through a form of diffusive shock acceleration.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Radio halos, on the other hand, are largely amorphous, unpolarised diffuse synchrotron sources that are centrally located in merging galaxy clusters, and roughly follow the distribution of the thermal plasma in the ICM (as traced by X-ray emission).The most commonly accepted scenario is that radio halos are powered by turbulence injected in the ICM during cluster merger events, although there are alternatives based on collisions between cosmic ray protons (CRp) and thermal protons from the ICM (for a review, see Brunetti & Jones \u003Ca class=\"xref bibr\" href=\"#r19\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Brunetti and Jones\u003C\u002Fspan\u003E2014\u003C\u002Fa\u003E). On smaller scales (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline249.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"34\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline249.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\lesssim0.5$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E Mpc), ‘mini-halos’ are relatively small diffuse radio sources that are generally co-located with powerful, radio-loud, brightest cluster galaxies (BCGs) in relaxed clusters. One theoretical explanation for mini-halos is that ‘core-sloshing’ in the ICM from minor or off-axis mergers produces small-scale turbulence which can then provide sufficient energy for re-acceleration of the relativistic electrons.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E For relics, halos, and mini-halos, the shape of the synchrotron emitting spectrum provides a diagnostic for these relativistic particle (re-)acceleration processes. Historically, our understanding of the relevant physics has been limited by (i) the generally relatively poor quality of low-frequency radio data, (ii) missing short spacings, leading to loss of highly-extended radio emission, and (iii) narrow bandwidths, limiting the spectral shape measurements. By circumventing these limitations with the EMU survey, the sample of clusters suitable for study can be increased by at least two orders of magnitude.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E There are already \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline250.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline250.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E20 known X-ray detected galaxy clusters in the EMU-PS area. All show compact or moderately extended radio sources that are likely associated with AGN. The eROSITA survey (Predehl et al. \u003Ca class=\"xref bibr\" href=\"#r104\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Predehl\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E) will provide many more X-ray clusters for radio investigation. The first eROSITA all-sky survey (eRASS1) will find as many as \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline251.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"107\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline251.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$1.5\\ \\mathrm{clusters\u002F\\,deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E; more than \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline252.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"97\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline252.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$3\\ \\mathrm{clusters\u002F\\,deg}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E are expected after all eight all-sky surveys are completed (e.g., Pillepich et al. \u003Ca class=\"xref bibr\" href=\"#r99\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Pillepich, Reiprich, Porciani, Borm and Merloni\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E). Hence, we expect as many as 400 X-ray-detected clusters will soon be available in the EMU-PS area alone, and more than 10 000 AGN.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Early EMU\u002FeROSITA results on the Abell 3391\u002F95 galaxy cluster system (Reiprich et al. \u003Ca class=\"xref bibr\" href=\"#r108\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Reiprich\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E; Brüggen et al. \u003Ca class=\"xref bibr\" href=\"#r18\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Brüggen\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E) have already helped constrain physical processes in the merger. We show two additional examples of diffuse radio sources detected in the EMU-PS area in \u003Ca class=\"xref fig\" href=\"#f33\"\u003EFigures 33\u003C\u002Fa\u003E and \u003Ca class=\"xref fig\" href=\"#f34\"\u003E34\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f29\" id=\"f29\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig29.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1499\" height=\"970\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig29.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 29.\u003C\u002Fspan\u003E The histogram of EMU-PS flux densities for 6dFGS galaxies with \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline253.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"21\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline253.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\rm H\\alpha}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E emission and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline254.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"64\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline254.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$K<12.65$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, along with the corresponding histogram of flux densities measured at offset positions. Just 17 of the 623 6dFGS galaxies with detectable \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline255.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"21\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline255.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\rm H\\alpha}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E emission have radio flux densities below 75 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline256.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline256.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f30\" id=\"f30\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig30.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"983\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig30.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 30.\u003C\u002Fspan\u003E The EMU-PS flux densities of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline257.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline257.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$K<12$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E galaxies with and without \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline258.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"21\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline258.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\rm H\\alpha}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E emission as a function of absolute magnitude. The dashed line shows \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline259.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"42\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline259.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$75\\,{\\rm \\mu Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, roughly corresponding to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline260.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"17\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline260.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$3\\sigma$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Almost all star-forming galaxies are detected by the EMU-PS. While low mass passive galaxies can have no detectable radio continuum emission, all but one \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline261.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"70\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline261.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$M_K<-26$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E passive galaxy has a positive radio continuum flux density.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f31\" id=\"f31\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig31.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1039\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig31.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 31.\u003C\u002Fspan\u003E The number of cross-matches between DES counterparts to EMU-PS sources, and Gaia sources, for unshifted data (blue), and data shifted by one arcmin (orange).\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f32\" id=\"f32\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig32.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1090\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig32.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 32.\u003C\u002Fspan\u003E The AllWISE colour-colour plot for EMU-PS sources cross-matched with Gaia, colour-coded according to their measured proper motion. The dashed lines divide the graph into the regions identified by Jarrett et al. (\u003Ca class=\"xref bibr\" href=\"#r59\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Jarrett\u003C\u002Fspan\u003E2017\u003C\u002Fa\u003E).\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f33\" id=\"f33\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig33.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1276\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig33.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 33.\u003C\u002Fspan\u003E Multi-wavelength composite image of SPT-CL J2023\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline262.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline262.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E5535. Contours denote the EMU-PS surface brightness at 944 MHz at 18 arcsec resolution, at \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline263.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"66\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline263.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$3\\sigma_{\\rm{rms}} \\times 2^{n}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E where \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline264.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"91\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline264.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$n=0, 1, 2, 3, 4$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline265.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"71\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline265.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sigma_{rms}=\\sim25$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline266.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline266.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Background colourmap shows a composite \u003Cem class=\"italic\"\u003Eg\u003C\u002Fem\u003E, \u003Cem class=\"italic\"\u003Er\u003C\u002Fem\u003E, and \u003Cem class=\"italic\"\u003Ei\u003C\u002Fem\u003E image from DECam. X-ray emission from \u003Cem class=\"italic\"\u003EChandra\u003C\u002Fem\u003E is also overlaid in red. New diffuse radio sources identified by HyeongHan et al. (\u003Ca class=\"xref bibr\" href=\"#r56\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference HyeongHan\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E) are also indicated.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f34\" id=\"f34\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig34.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1301\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig34.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 34.\u003C\u002Fspan\u003E Multi-wavelength composite image of the cluster SPT-CL J2032\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline267.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline267.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E5627. Colour map and contours are the same as \u003Ca class=\"xref fig\" href=\"#f33\"\u003EFigure 33\u003C\u002Fa\u003E, but with \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline268.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"32\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline268.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$25\\,\\mathrm{ks}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E XMM- \u003Cem class=\"italic\"\u003ENewton\u003C\u002Fem\u003E surface brightness shown in red. It appears that the cluster hosts one of the rare class of double-radio relics with the northern (A and B) and southern (C) relics as indicated.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E Other cluster catalogues will similarly provide important targets for EMU-PS and the full EMU Survey. For example, Aguena et al. (\u003Ca class=\"xref bibr\" href=\"#r3\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Aguena\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E) provide the WaZP catalogue of 60542 clusters from the DES\u003Ca class=\"xref fn\" href=\"#fn11\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003Ek\u003C\u002Fa\u003E. About 30 of their BCGs are coincident with extended RGs in the EMU-PS and will be discussed by Andernach et al. (in preparation).\u003C\u002Fp\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-8-1\" id=\"s6-8-1\"\u003E\n \u003Ch4 class=\"C\"\u003E\u003Cspan class=\"label\"\u003E6.7.1.\u003C\u002Fspan\u003E SPT-CL J2023-5535\u003C\u002Fh4\u003E\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref fig\" href=\"#f33\"\u003EFigure 33\u003C\u002Fa\u003E presents the radio halo and relic in the massive merging galaxy cluster, SPT-CL J2023\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline269.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline269.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E5535 (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline270.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"52\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline270.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z=0.23$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E), reported by HyeongHan et al. (\u003Ca class=\"xref bibr\" href=\"#r56\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference HyeongHan\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E). Their weak-lensing analysis has revealed significant substructure in this massive (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline271.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"191\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline271.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$M_{200}=1.04\\pm0.36\\times 10^{15}\\,M_{\\odot}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) cluster, which comprises three subclusters.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The merger event between the eastern and central subclusters appears to have generated a \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline272.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"31\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline272.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}0.5$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E Mpc radio relic on the western edge of the central subcluster. The results presented by HyeongHan et al. (\u003Ca class=\"xref bibr\" href=\"#r56\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference HyeongHan\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E) show an unusually flat spectral index \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline273.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"125\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline273.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha_{\\rm{int}}=-0.76 \\pm 0.06$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, which may indicate that this relic is powered by the re-acceleration of fossil electrons, perhaps originally seeded by a nearby (photometric) cluster member AGN. Follow-up observations at other radio frequencies will be required to confirm this flat spectrum.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-8-2\" id=\"s6-8-2\"\u003E\n \u003Ch4 class=\"C\"\u003E\u003Cspan class=\"label\"\u003E6.7.2.\u003C\u002Fspan\u003E SPT-CL J2032-5627\u003C\u002Fh4\u003E\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref fig\" href=\"#f34\"\u003EFigure 34\u003C\u002Fa\u003E shows a rare class of a possible double-radio relic with an elongation of X-ray emission in the massive (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline274.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"173\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline274.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$M_{500}=4.77^{+0.71}_{-0.63}\\times 10^{14}\\,M_{\\odot}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E; Bulbul et al. \u003Ca class=\"xref bibr\" href=\"#r20\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bulbul\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E) cluster SPT-CL J2032\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline275.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline275.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E5627 (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline276.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"52\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline276.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$z=0.28$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E). The north-western (sources A & B) and south-eastern (source C) all exhibit steep radio spectra (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline277.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"80\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline277.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha_{\\rm{int}} = -1.75$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline278.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"79\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline278.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha_{\\rm{int}} = -1.69$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline279.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"81\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline279.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha_{\\rm{int}} =-1.46$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, respectively).\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f35\" id=\"f35\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig35.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1425\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig35.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 35.\u003C\u002Fspan\u003E Radio contours overlaid on a multi-wavelength (irg) composite image of 6dFGS g2212485-614658 from DES. The radio image was made from the EMU-PS native resolution data by subtracting four unresolved sources and then convolving to a resolution of 18 arcsec. Contours are at 75, 150, 300, and 600 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline280.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline280.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The subtracted sources were at 22:12:48.64 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline281.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline281.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E61:46:58.5 (14.9 mJy), 22:12:43.04 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline282.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline282.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E61:46:50.1 (0.3 mJy), 22:12:51.19 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline283.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline283.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E61:46:15.5 (0.2 mJy), 22:12:37.17 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline284.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline284.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E61:47:24.5 (0.1 mJy)\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E The highly asymmetric X-ray surface brightness profile and large projected separation between the radio relics in this cluster suggest that the merger event is occurring close to the plane of the sky. Curiously, no evidence of a shock has been found in the X-ray surface brightness. However, the presence of a cold front towards the leading edge to the south-east of the cluster may suggest that the lack of a shock detection is due to the relatively shallow depth (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline285.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"32\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline285.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$25\\,\\mathrm{ks}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) of the existing XMM- \u003Cem class=\"italic\"\u003ENewton\u003C\u002Fem\u003E observations. See also Duchesne et al. (\u003Ca class=\"xref bibr\" href=\"#r33\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Duchesne, Johnston-Hollitt, Bartalucci, Hodgson and Pratt\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E) for further discussion of SPT-CL J2032\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline286.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"10\" height=\"2\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline286.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$-$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E5627.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-8-3\" id=\"s6-8-3\"\u003E\n \u003Ch4 class=\"C\"\u003E\u003Cspan class=\"label\"\u003E6.7.3.\u003C\u002Fspan\u003E A Mini-Halo in a poor cluster\u003C\u002Fh4\u003E\n\u003Cp class=\"p\"\u003E \n\u003Ca class=\"xref fig\" href=\"#f35\"\u003EFigure 35\u003C\u002Fa\u003E shows a very low surface brightness structure, much fainter (50\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline287.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"75\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline287.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E) than the embedded compact 14.8\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline288.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"67\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline288.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\pm0.07\\,\\textrm{mJy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E source associated with 6dFGS g2212485-614658 at a redshift of z=0.054. The low surface brightness emission was found using the multi-resolution filtering technique of Rudnick (\u003Ca class=\"xref bibr\" href=\"#r109\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Rudnick\u003C\u002Fspan\u003E2002\u003C\u002Fa\u003E), using a filter box size of 34 arcsec which removes the emission from compact components. It has a total extent of 150 arcsec (160 kpc) and a total flux density of 5\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline289.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline289.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\pm$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E0.5 mJy, corresponding to a luminosity of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline290.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"67\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline290.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\approx 3\\times10^{22}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E W\u002FHz. No substructure is apparent.\n\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The diffuse structure could be the dying remains of a radio galaxy, faded to a luminosity comparable to the faintest AGN or to typical SFGs (Mauch & Sadler \u003Ca class=\"xref bibr\" href=\"#r77\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Mauch and Sadler\u003C\u002Fspan\u003E2007\u003C\u002Fa\u003E). The lack of radio structure, however, suggests that it could also be an underluminous mini-halo, an option we briefly explore here.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E There is no catalogued cluster associated with 6dFGS g2212485-614658, although there are five galaxies with a similar redshift listed in Vizier, out to a separation of 17 arcmin (1 Mpc). This, and the presence of many smaller galaxies embedded in the 6dFGS g2212485-614658 envelope (\u003Ca class=\"xref fig\" href=\"#f35\"\u003EFigure 35\u003C\u002Fa\u003E) suggest that this could be a poor cluster or group.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The radio and extended (as opposed to AGN) X-ray luminosities of mini-halo systems are well correlated (Giacintucci et al. \u003Ca class=\"xref bibr\" href=\"#r42\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Giacintucci, Markevitch, Cassano, Venturi, Clarke, Kale and Cuciti\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E). For this system, we determined upper limits to the bolometric (0.2–2 keV) X-ray emission using both RASS and XMM Slew archives, yielding limits in the range 1.4–2.4\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline291.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"114\" height=\"17\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline291.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\times10^{-13}\\ \\mathrm{erg\u002Fs\u002Fcm}^2$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. At mid-range, the inferred luminosity upper limit of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline292.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"25\" height=\"13\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline292.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$10^{42}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E erg\u002Fs is two orders of magnitude lower than that of the mini-halo clusters summarised in Giacintucci et al. (\u003Ca class=\"xref bibr\" href=\"#r42\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Giacintucci, Markevitch, Cassano, Venturi, Clarke, Kale and Cuciti\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E) and than the value expected from the radio-X-ray correlation.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Probing mini-halo-like structures in these poor-cluster, low X-ray luminosity type systems is important for understanding the physical mechanisms which form and continue to power the radio emission. We do not know whether the current observed radio-X-ray correlation is influenced by X-ray selection effects, or whether the correlation breaks down at very low cluster masses.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The sensitivity of EMU to very low surface brightness emission such as presented here will provide a powerful tool for exploring the connection between compact and extended AGN emissions and pure cluster\u002Fgroup particle acceleration processes in mini-halos.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-12\" id=\"s6-12\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.8.\u003C\u002Fspan\u003E Cosmology\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E The spatial distribution of radio sources is a tracer of the underlying matter distribution and can be used to probe the formation conditions of radio galaxies, as well as the underlying fundamental ingredients and physics of the universe. As these continuum sources are not easy to localise in redshift, we use measurements of angular clustering for the EMU-PS.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E Here, we use the Landy & Szalay (\u003Ca class=\"xref bibr\" href=\"#r71\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Landy and Szalay\u003C\u002Fspan\u003E1993\u003C\u002Fa\u003E) estimator, which is defined as: \n\u003C\u002Fp\u003E\u003Cdiv data-mathjax-status=\"alt-graphic\" class=\"disp-formula\" data-magellan-destination=\"disp1\" id=\"disp1\"\u003E\n\u003Cspan class=\"label\"\u003E(1)\u003C\u002Fspan\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_eqn1.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"232\" height=\"37\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_eqn1.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n\\begin{equation} w_{\\mathrm{LS}}(\\theta) = \\frac{DD(\\theta) + RR(\\theta) - 2DR(\\theta)}{RR(\\theta)},\\end{equation}\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fdiv\u003E\u003Cp class=\"p continuation\"\u003Ewhere \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline293.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"42\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline293.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$DD(\\theta)$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E is the number of observed galaxy pairs at distance between \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline294.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"8\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline294.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\theta$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline295.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"43\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline295.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\theta+d\\theta$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline296.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"37\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline296.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$RR(\\theta)$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E is the number of random galaxies pairs at this separation, and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline297.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"40\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline297.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$DR(\\theta)$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E is the number of observed random pairs. We apply this statistic to the pilot survey catalogue, using the island data catalogue as the data vector (\u003Cem class=\"italic\"\u003ED\u003C\u002Fem\u003E), and generated random catalogues (\u003Cem class=\"italic\"\u003ER\u003C\u002Fem\u003E), normalising the number over all angles such the angular correlation function \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline298.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"29\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline298.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$w(\\theta)$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E functions as a probability excess or decrement relative to an entirely random distribution of galaxies on the sky.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The random catalogue (\u003Cem class=\"italic\"\u003ER\u003C\u002Fem\u003E) is generated using the method used in Hale et al. (\u003Ca class=\"xref bibr\" href=\"#r46\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Hale, Jarvis, Delvecchio, Hatfield, Novak, Smolčić and Zamorani\u003C\u002Fspan\u003E2018\u003C\u002Fa\u003E) and Siewert et al. (\u003Ca class=\"xref bibr\" href=\"#r114\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Siewert\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E) where random positions for simulated sources are generated across the EMU-PS field of view and for each simulated source a flux density is randomly assigned to the source using flux densities from the SKADS simulation (Wilman et al. \u003Ca class=\"xref bibr\" href=\"#r127\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Wilman\u003C\u002Fspan\u003E2008\u003C\u002Fa\u003E)\u003Ca class=\"xref fn\" href=\"#fn12\"\u003E\u003Cspan class=\"show-for-sr\"\u003EFootnote \u003C\u002Fspan\u003El\u003C\u002Fa\u003E. We assign noise to the flux density of the simulated source by sampling from a Gaussian distribution with spread given by the RMS at the random source location. A source remains within the random catalogue provided the simulated source peak flux density (where we assume the random sources are unresolved) added to the noise would be detectable at \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline300.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline300.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\geq 5 \\times$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E the RMS at the simulated source position.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f36\" id=\"f36\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig36.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1499\" height=\"1097\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig36.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 36.\u003C\u002Fspan\u003E The number of sources in the EMU-PS with a flux density greater than some limit (\u003Cem class=\"italic\"\u003ES\u003C\u002Fem\u003E), as a function of that limit, compared to scaled predictions from the SKADS and T-RECS simulated catalogues. The dashed black vertical line gives the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline301.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"48\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline301.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$500\\mu\\mathrm{Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E limit we assume for the clustering analysis presented in this paper. There is some discretisation of the prediction for the larger flux density limits, due to a scaling of some small integer value for the original prediction that was made for a much smaller value.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E The robustness of this approach to generate the randoms is checked by comparing the fluxes of the simulated catalogues to the island catalogue of the EMU-PS. We selected both AGN and SFG galaxies from SKADS and T-RECS (Bonaldi et al. \u003Ca class=\"xref bibr\" href=\"#r12\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Bonaldi, Bonato, Galluzzi, Harrison, Massardi, Kay, De Zotti and Brown\u003C\u002Fspan\u003E2019\u003C\u002Fa\u003E) simulations. In \u003Ca class=\"xref fig\" href=\"#f36\"\u003EFigure 36\u003C\u002Fa\u003E, we compare the number counts for different flux density cuts \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline302.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"48\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline302.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$N(>S)$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E between the EMU-PS island catalogue and the number counts from both simulated radio catalogues at 1 GHz.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E In order to calculate the expected \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline303.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"42\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline303.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$w_{\\mathrm LS}(\\theta)$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E distribution, we must know the redshift distribution \u003Cem class=\"italic\"\u003EN\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003Ez\u003C\u002Fem\u003E) of the sources. For the analysis here, the SKADS and T-RECS simulations are used for \u003Cem class=\"italic\"\u003EN\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003Ez\u003C\u002Fem\u003E) and are shown in \u003Ca class=\"xref fig\" href=\"#f37\"\u003EFigure 37\u003C\u002Fa\u003E. There is good agreement in the redshift distribution between these two catalogues, and this consistency indicates that we are accurately modelling \u003Cem class=\"italic\"\u003EN\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003Ez\u003C\u002Fem\u003E) and choosing the SKADS catalogue should not introduce a significant error. Using the \u003Cem class=\"italic\"\u003EN\u003C\u002Fem\u003E(\u003Cem class=\"italic\"\u003Ez\u003C\u002Fem\u003E) distribution estimated from SKADS, we compute the theoretical expectation for the clustering statistics at the flux density cut of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline304.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"47\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline304.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$500 \\mu\\mathrm{Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f37\" id=\"f37\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig37.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1096\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig37.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 37.\u003C\u002Fspan\u003E The predicted number of sources in the EMU Pilot Survey as a function of redshift, generated by scaling the predictions from the SKADS and T-RECS simulated catalogues. This assumes a flux density limit of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline305.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"48\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline305.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$500\\mu\\mathrm{Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003Cp class=\"p\"\u003E The measured angular correlation function \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline306.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"29\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline306.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$w(\\theta)$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E is shown in \u003Ca class=\"xref fig\" href=\"#f38\"\u003EFigure 38\u003C\u002Fa\u003E, estimating the errors from boostrap resampling the data and random simulated data 100 times. We also show the predicted angular correlation function, assuming a cosmological model with values fixed at the values listed in \u003Ca class=\"xref table\" href=\"#tbl2\"\u003ETable 2\u003C\u002Fa\u003E, with a number distribution and bias model from SKADS. We show that the theoretical prediction, with no tuning of free parameters, is a reasonable fit to the data in the angular range \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline307.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"92\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline307.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$0.1^{\\circ} < \\theta < 10^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. There is somewhat of a discrepancy at small scales (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline308.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"51\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline308.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\theta < 0.1^{\\circ}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E), which is probably generated by the multiple components that can be generated by the same radio galaxy, but which here are being treated as independent tracers of the cosmological density field. A more complete analysis, including calibration of the effect of multi-component sources on the angular correlation function on small scales, is planned for future work.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f38\" id=\"f38\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig38.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"1500\" height=\"1112\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig38.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 38.\u003C\u002Fspan\u003E The measured angular correlation function (ACF) \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline309.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"30\" height=\"15\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline309.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$w(\\theta)$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E as a function of angular separation with one-sigma error bar computed from bootstrap re-sampling from 100 bootstraps. The correlation function is measured from the integrated flux-corrected EMU-PS island catalogue, using all sources above a flux density limit of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline310.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"47\" height=\"14\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline310.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$500\\mu\\mathrm{Jy}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. The blue curve is the theoretical prediction for the correlation function, assuming the Planck 2018 best fit cosmology and a SKADS model for the number distribution with redshift and the bias. No fitting of the cosmological or bias parameters was performed to change the prediction curve. As negative values cannot be shown on a log scale, in bins where the ACF becomes negative, we show (in red) the value of (-ACF) instead.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec\" data-magellan-destination=\"s6-13\" id=\"s6-13\"\u003E\n\n\u003Ch3 class=\"B\"\u003E\u003Cspan class=\"label\"\u003E6.9.\u003C\u002Fspan\u003E The excess of flat spectral index sources\u003C\u002Fh3\u003E\n\u003Cp class=\"p\"\u003E To investigate the skew towards flatter and inverted spectral indices shown in \u003Ca class=\"xref fig\" href=\"#f10\"\u003EFigures 10\u003C\u002Fa\u003E and \u003Ca class=\"xref fig\" href=\"#f11\"\u003E11\u003C\u002Fa\u003E, we compare the spectral index distributions for a sample of clearly resolved and unresolved components from the EMU-PS. The unresolved population contains radio cores and therefore includes flat-spectrum radio quasars (Urry & Padovani \u003Ca class=\"xref bibr\" href=\"#r118\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Urry and Padovani\u003C\u002Fspan\u003E1995\u003C\u002Fa\u003E) and peaked-spectrum sources (O’Dea & Saikia \u003Ca class=\"xref bibr\" href=\"#r97\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference O’Dea and Saikia\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E). At the observing frequency of EMU-PS (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline311.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"50\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline311.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\nu \\sim 900\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003EMHz), the radio spectra of Gigahertz Peaked-Spectrum sources tend to have shallow spectral index values as EMU-PS is observing close to their turnover frequency (O’Dea \u003Ca class=\"xref bibr\" href=\"#r96\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference O’Dea\u003C\u002Fspan\u003E1998\u003C\u002Fa\u003E). For this comparison, we define each source to be resolved or unresolved using the component size after deconvolution from the beam, \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline312.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"11\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline312.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\Psi$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, considering components with \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline313.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"80\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline313.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\Psi < 2\\,\\mathrm{arcsec}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E to be unresolved and components with \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline314.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"87\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline314.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\Psi > 20\\,\\mathrm{arcsec}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E to be resolved.\n\u003C\u002Fp\u003E\u003Csection\u003E\u003Cdiv class=\"fig\" data-magellan-destination=\"f39\" id=\"f39\"\u003E\n\n\n\u003Cdiv class=\"figure-thumb\"\u003E\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig39.png?pub-status=live\" class=\"aop-lazy-load-image\" width=\"667\" height=\"732\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_fig39.png\" data-zoomable=\"true\"\u003E\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"caption\"\u003E\u003Cp class=\"p\"\u003E \n\u003C\u002Fp\u003E\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003EFigure 39.\u003C\u002Fspan\u003E The spectral index distributions for unresolved (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline315.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline315.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\Psi < 2''$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, blue) and resolved (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline316.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"52\" height=\"12\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline316.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\Psi > 20''$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, red) EMU components. The three panels show different minimum brightness levels, corresponding to \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline317.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"135\" height=\"19\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline317.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\text{peak}} > 1\\,\\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline318.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"134\" height=\"19\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline318.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\text{peak}} > 3\\,\\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline319.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"142\" height=\"19\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline319.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\text{peak}} > 10\\,\\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E from top to bottom. The legend in each panel denotes the number of components contributing to each distribution shown. Each plot is normalised to the area under the curve.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\u003C\u002Fdiv\u003E\u003C\u002Fsection\u003E\n\u003Cp class=\"p\"\u003E In \u003Ca class=\"xref fig\" href=\"#f39\"\u003EFigure 39\u003C\u002Fa\u003E, we show the spectral index distributions for the resolved and unresolved EMU components at three levels of minimum peak brightness: \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline320.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"134\" height=\"19\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline320.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\text{peak}} > 1\\, \\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline321.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"135\" height=\"19\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline321.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\text{peak}} > 3\\,\\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, and \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline322.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"141\" height=\"19\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline322.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\text{peak}} > 10\\,\\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Resolved components have symmetric distributions around a peak of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline323.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"60\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline323.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha \\sim -0.7$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. However, while the spectral index distribution for the unresolved population is comparable to the resolved population at steep negative spectral indices (\u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline324.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"60\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline324.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha < -0.7$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E), the distributions differ at flatter spectral indices. At \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline325.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"60\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline325.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\alpha > -0.7$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E, the unresolved population dominates over the resolved population at all three brightness levels. Due to the large scatter in the spectral index distribution at sub-mJy levels (\u003Ca class=\"xref fig\" href=\"#f10\"\u003EFigure 10\u003C\u002Fa\u003E), we have only performed this analysis on EMU components with \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline326.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"134\" height=\"19\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline326.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S_{\\text{peak}}>1\\,\\mathrm{mJy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E. Future EMU data, where potential issues in the spectral index calibration at lower signal to noise are better understood, will present the opportunity to study the spectral index distributions of fainter resolved and unresolved components. Such an analysis, particularly for the full EMU survey, will enable tests of the potential flattening of the spectral index distribution for radio sources with \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline327.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"45\" height=\"16\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline327.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$S \\lesssim 0.5\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E mJy (Prandoni et al. \u003Ca class=\"xref bibr\" href=\"#r102\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Prandoni, Parma, Wieringa, de Ruiter, Gregorini, Mignano, Vettolani and Ekers\u003C\u002Fspan\u003E2006\u003C\u002Fa\u003E; Whittam et al. \u003Ca class=\"xref bibr\" href=\"#r126\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Whittam\u003C\u002Fspan\u003E2013\u003C\u002Fa\u003E).\n\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The different spectral index distributions of resolved and unresolved components we observe with the EMU-PS are consistent with what is seen with higher angular resolution and higher frequency observations. Recently, Gordon et al. (\u003Ca class=\"xref bibr\" href=\"#r43\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Gordon\u003C\u002Fspan\u003E2021\u003C\u002Fa\u003E) demonstrated the \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline328.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"43\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline328.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$1.4 - 3\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003EGHz spectral index distributions for point-like radio components are skewed to flatter values than well-resolved components using observations from the Faint Images of the Radio Sky at Twenty cm survey (FIRST; \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline329.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"47\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline329.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\nu \\sim 1.4\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003EGHz, Becker et al. \u003Ca class=\"xref bibr\" href=\"#r6\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Becker, White and Helfand\u003C\u002Fspan\u003E1995\u003C\u002Fa\u003E) and the Very Large Array Sky Survey (VLASS, \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline330.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"33\" height=\"11\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline330.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\nu \\sim 3\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003EGHz, Lacy et al. \u003Ca class=\"xref bibr\" href=\"#r70\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Lacy\u003C\u002Fspan\u003E2020\u003C\u002Fa\u003E). Further comparisons between EMU and radio observations in other bands, such as those from VLASS and the Australia Telescope Large Area Survey (ATLAS, \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline331.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"55\" height=\"10\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline331.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$1.4 - 2.3\\,$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003EGHz, Zinn et al. \u003Ca class=\"xref bibr\" href=\"#r130\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Zinn, Middelberg, Norris, Hales, Mao and Randall\u003C\u002Fspan\u003E2012\u003C\u002Fa\u003E), may help quantify the fractions of peaked-spectrum sources with different turnover frequencies, and this will be the focus of a follow-up work.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"sec conclusions\" data-magellan-destination=\"s7\" id=\"s7\"\u003E\n\n\u003Ch2 class=\"A\"\u003E\u003Cspan class=\"label\"\u003E7.\u003C\u002Fspan\u003E Conclusion\u003C\u002Fh2\u003E\n\u003Cp class=\"p\"\u003E We have presented the first pilot survey of EMU, using the ASKAP telescope.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The resulting images reach an rms sensitivity of about 25–30 \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline332.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"74\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline332.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E rms at a spatial resolution of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline333.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline333.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E11–18 arcsec and result in a catalogue of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline334.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline334.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E220 000 sources, of which \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg src=\"data:image\u002Fgif;base64,R0lGODlhAQABAIAAAMLCwgAAACH5BAAAAAAALAAAAAABAAEAAAICRAEAOw==\" data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline335.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"12\" height=\"4\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline335.png\" data-zoomable=\"false\"\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n$\\sim$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E180 000 are compact. We have presented the catalogue of compact sources, together with optical and infrared cross-identifications and redshifts. We have also shown some preliminary science results, on both these compact sources and on diffuse sources, which will be discussed in more detail in subsequent papers.\u003C\u002Fp\u003E\n\u003Cp class=\"p\"\u003E The results presented here testify to the outstanding observational characteristics of ASKAP, including its high survey speed and unprecedented sensitivity to low surface brightness emission. Nevertheless, at the time of the pilot survey, several aspects of ASKAP correlator operation, calibration, and data processing were incomplete. We therefore expect future results from ASKAP, including the main EMU survey, to have even better sensitivity and dynamic range than the results presented in this paper.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E\n\u003Cdiv class=\"back\"\u003E\n\u003Cdiv class=\"ack\"\u003E\n\u003Ch2 class=\"A\"\u003E Acknowledgements\u003C\u002Fh2\u003E\n\u003Cp class=\"p\"\u003E We thank an anonymous referee for valuable feedback on an earlier iteration of this paper. The Australian SKA Pathfinder is part of the Australia Telescope National Facility which is managed by CSIRO. Operation of ASKAP is funded by the Australian Government with support from the National Collaborative Research Infrastructure Strategy. Establishment of the Murchison Radio-astronomy Observatory was funded by the Australian Government and the Government of Western Australia. ASKAP uses advanced supercomputing resources at the Pawsey Supercomputing Centre. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. This work makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory\u002FCalifornia Institute of Technology, funded by the National Aeronautics and Space Administration. It also makes use of data from the European Space Agency (ESA) mission Gaia, and we acknowledge the institutions listed on \u003Ca class=\"uri\" href=\"https:\u002F\u002Fgea.esac.esa.int\u002Farchive\u002Fdocumentation\u002FGEDR3\u002FMiscellaneous\u002Fsec_acknowl\u002F\"\u003Ehttps:\u002F\u002Fgea.esac.esa.int\u002Farchive\u002Fdocumentation\u002FGEDR3\u002FMiscellaneous\u002Fsec\u002F_acknowl\u002F\u003C\u002Fa\u003E It also uses public archival data from the DES and we acknowledge the institutions listed on \u003Ca class=\"uri\" href=\"https:\u002F\u002Fwww.darkenergysurvey.org\u002Fthe-des-project\u002Fdata-access\u002F\"\u003Ehttps:\u002F\u002Fwww.darkenergysurvey.org\u002Fthe-des-project\u002F\u003C\u002Fa\u003E \u003Ca class=\"uri\" href=\"https:\u002F\u002Fwww.darkenergysurvey.org\u002Fthe-des-project\u002Fdata-access\u002F\"\u003Edata-access\u002F.\u003C\u002Fa\u003E This research has made use of the ‘Aladin sky atlas’ developed at CDS, Strasbourg Observatory, France (Boch & Fernique \u003Ca class=\"xref bibr\" href=\"#r9\"\u003E\u003Cspan class=\"show-for-sr\"\u003EReference Boch, Fernique, Manset and Forshay\u003C\u002Fspan\u003E2014\u003C\u002Fa\u003E). This research uses services or data provided by the Astro Data Lab at NSF’s National Optical-Infrared Astronomy Research Laboratory. NOIRLab is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. Partial support for LR comes from US National Science Foundation Grant AST 17-14205 to the University of Minnesota. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. CLH acknowledges support from the Leverhulme Trust through an Early Career Research Fellowship. IP acknowledges support from CSIRO under its Distinguished Research Visitor Programme, and from INAF through the SKA\u002FCTA PRIN “FORECaST” and the PRIN MAIN STREAM “SAuROS” projects. MJJ acknowledges support from the National Research Foundation of Korea under the program nos. 2017R1A2B2004644 and 2017R1A4A1015178. CJR acknowledges financial support from the ERC Starting Grant ‘DRANOEL’, number 714245. HA benefited from grant CIIC 174\u002F2021 of Universidad de Guanajuato.\u003C\u002Fp\u003E\n\u003C\u002Fdiv\u003E\n\n\n\u003C\u002Fdiv\u003E\n\u003C\u002Fdiv\u003E",tableOfContent:[{level:q,current:b,title:"\u003Cdiv class=\"toc-title\"\u003EIntroduction\u003C\u002Fdiv\u003E",url:"s1"},{level:q,current:b,title:"\u003Cdiv class=\"toc-title\"\u003EObservations\u003C\u002Fdiv\u003E",url:"s2"},{level:q,current:b,title:"\u003Cdiv class=\"toc-title\"\u003EPipeline data reduction\u003C\u002Fdiv\u003E",url:"s3"},{level:q,current:b,title:"\u003Cdiv class=\"toc-title\"\u003EValue-added processing\u003C\u002Fdiv\u003E",url:"s4"},{level:q,current:b,title:"\u003Cdiv class=\"toc-title\"\u003EResults\u003C\u002Fdiv\u003E",url:"s5"},{level:q,current:b,title:"\u003Cdiv class=\"toc-title\"\u003EPreliminary science results\u003C\u002Fdiv\u003E",url:"s6"},{level:q,current:b,title:"\u003Cdiv class=\"toc-title\"\u003EConclusion\u003C\u002Fdiv\u003E",url:"s7"}],footnotes:[],fulltextNotes:[{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Ea\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E \n\u003Ca class=\"uri\" href=\"https:\u002F\u002Fconfluence.csiro.au\u002Fdisplay\u002Faskapsst\u002FContinuum+Validation\"\u003Ehttps:\u002F\u002Fconfluence.csiro.au\u002Fdisplay\u002Faskapsst\u002FContinuum+Validation\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn1",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Eb\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E \n\u003Ca class=\"uri\" href=\"https:\u002F\u002Fconfluence.csiro.au\u002Fdisplay\u002Faskapsst\u002FContinuum+validation+metrics\"\u003Ehttps:\u002F\u002Fconfluence.csiro.au\u002Fdisplay\u002Faskapsst\u002FContinuum+validation+metrics\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn2",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Ec\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E Reports are available from \u003Ca class=\"uri\" href=\"https:\u002F\u002Fwww.atnf.csiro.au\u002Fresearch\u002FASKAP\u002FASKAP-validation\u002Fcommissioning\u002FAS101\u002FSB9325\u002Fvalidation_image.i.SB9325.cont.taylor.0.restored__askapops_2019-09-03-101300\u002F\"\u003Ehttps:\u002F\u002Fwww.atnf.csiro.au\u002Fresearch\u002FASKAP\u002FASKAP-\u003C\u002Fa\u003E \u003Ca class=\"uri\" href=\"https:\u002F\u002Fwww.atnf.csiro.au\u002Fresearch\u002FASKAP\u002FASKAP-validation\u002Fcommissioning\u002FAS101\u002FSB9325\u002Fvalidation_image.i.SB9325.cont.taylor.0.restored__askapops_2019-09-03-101300\u002F\"\u003Evalidation\u002Fcommissioning\u002FAS101\u002FSB9325\u002Fvalidation_image.i.SB9325.cont.taylor.0.restored_\u003C\u002Fa\u003E \u003Ca class=\"uri\" href=\"https:\u002F\u002Fwww.atnf.csiro.au\u002Fresearch\u002FASKAP\u002FASKAP-validation\u002Fcommissioning\u002FAS101\u002FSB9325\u002Fvalidation_image.i.SB9325.cont.taylor.0.restored__askapops_2019-09-03-101300\u002F\"\u003Easkapops_2019-09-03-101300\u002F\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn3",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Ed\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E The metrics are described in detail in \u003Ca class=\"uri\" href=\"https:\u002F\u002Fconfluence.csiro.au\u002Fdisplay\u002Faskapsst\u002FContinuum+validation+metrics\"\u003Ehttps:\u002F\u002Fconfluence.csiro.au\u002Fdisplay\u002F\u003C\u002Fa\u003E \u003Ca class=\"uri\" href=\"https:\u002F\u002Fconfluence.csiro.au\u002Fdisplay\u002Faskapsst\u002FContinuum+validation+metrics\"\u003Easkapsst\u002FContinuum+validation+metrics\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn4",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Ee\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E \n\u003Ca class=\"uri\" href=\"https:\u002F\u002Fwww.atnf.csiro.au\u002Fresearch\u002FASKAP\u002FASKAP-validation\u002Fcommissioning\u002FAS101\u002F\"\u003Ehttps:\u002F\u002Fwww.atnf.csiro.au\u002Fresearch\u002FASKAP\u002FASKAP-validation\u002Fcommissioning\u002FAS101\u002F\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn5",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Ef\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E \n\u003Ca class=\"uri\" href=\"https:\u002F\u002Fopal.atnf.csiro.au\u002F\"\u003Ehttps:\u002F\u002Fopal.atnf.csiro.au\u002F\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn6",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Eg\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E \n\u003Ca class=\"uri\" href=\"https:\u002F\u002Fcasda.csiro.au\"\u003Ehttps:\u002F\u002Fcasda.csiro.au\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn7",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Eh\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E \n\u003Ca class=\"uri\" href=\"https:\u002F\u002Fastroquery.readthedocs.io\"\u003Ehttps:\u002F\u002Fastroquery.readthedocs.io\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn8",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Ei\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E \n\u003Ca class=\"uri\" href=\"https:\u002F\u002Fapps.atnf.csiro.au\u002FOMP\u002Findex.jsp\"\u003Ehttps:\u002F\u002Fapps.atnf.csiro.au\u002FOMP\u002Findex.jsp\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn9",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Ej\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E An up-to-date database of these sources is maintained at \u003Ca class=\"uri\" href=\"https:\u002F\u002FGalaxyClusters.com\"\u003EGalaxyClusters.com\u003C\u002Fa\u003E.\u003C\u002Fp\u003E\n",targetId:"fn10",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003Ek\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E \n\u003Ca class=\"uri\" href=\"https:\u002F\u002Fwww.linea.gov.br\u002Fcatalogs\u002Fwazp\u002F\"\u003Ehttps:\u002F\u002Fwww.linea.gov.br\u002Fcatalogs\u002Fwazp\u002F\u003C\u002Fa\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn11",displayNumber:a},{content:"\n\n\u003Cp class=\"p\"\u003E\u003Cspan class=\"label\"\u003E\n\u003Csup class=\"sup\"\u003El\u003C\u002Fsup\u003E\n\u003C\u002Fspan\u003E We use the SKADS 1.4 GHz flux scaled to 944 MHz assuming a spectral index of -0.8. We also apply a minimum flux density cut on the 944 MHz converted SKADS flux of \u003Cspan data-mathjax-status=\"alt-graphic\" class=\"inline-formula\"\u003E\n\u003Cspan class=\"alternatives\"\u003E\n\u003Cimg data-src=\"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline299.png?pub-status=live\" class=\"aop-lazy-load-image mathjax-alternative mathjax-alt-graphic mathjax-off\" width=\"102\" height=\"18\" data-original-image=\"\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary:20210906095204165-0100:S1323358021000424:S1323358021000424_inline299.png\" data-zoomable=\"false\" \u002F\u003E\n\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E\n${\\sim}30 \\mu\\mathrm{Jy\\ beam}^{-1}$\n\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fspan\u003E\n\u003C\u002Fp\u003E\n",targetId:"fn12",displayNumber:a}],references:[{id:"ref1",displayNumber:a,existInContent:b,content:"\u003Cspan class=\"string-name\"\u003E\u003Cspan class=\"surname\"\u003EAbbott\u003C\u002Fspan\u003E, \u003Cspan class=\"given-names\"\u003ET. 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J.\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, \u003Cspan class=\"string-name\"\u003E\u003Cspan class=\"surname\"\u003Ede Gasperin\u003C\u002Fspan\u003E, \u003Cspan class=\"given-names\"\u003EF.\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, \u003Cspan class=\"string-name\"\u003E\u003Cspan class=\"surname\"\u003EAkamatsu\u003C\u002Fspan\u003E, \u003Cspan class=\"given-names\"\u003EH.\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, \u003Cspan class=\"string-name\"\u003E\u003Cspan class=\"surname\"\u003EBrüggen\u003C\u002Fspan\u003E, \u003Cspan class=\"given-names\"\u003EM.\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, \u003Cspan class=\"string-name\"\u003E\u003Cspan class=\"surname\"\u003EFeretti\u003C\u002Fspan\u003E, \u003Cspan class=\"given-names\"\u003EL.\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, \u003Cspan class=\"string-name\"\u003E\u003Cspan class=\"surname\"\u003EKang\u003C\u002Fspan\u003E, \u003Cspan class=\"given-names\"\u003EH.\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, \u003Cspan class=\"string-name\"\u003E\u003Cspan class=\"surname\"\u003EStroe\u003C\u002Fspan\u003E, \u003Cspan class=\"given-names\"\u003EA.\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, & \u003Cspan class=\"string-name\"\u003E\u003Cspan class=\"surname\"\u003EZandanel\u003C\u002Fspan\u003E, \u003Cspan class=\"given-names\"\u003EF.\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E \u003Cspan class=\"year\"\u003E2019\u003C\u002Fspan\u003E, \u003Cspan class=\"source\"\u003ESSRv\u003C\u002Fspan\u003E, 215, 16\n\u003Ca class='ref-link' target='_blank' aria-label='CrossRef link for van Weeren, R. 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J., de Gasperin, F., Akamatsu, H., Brüggen, M., Feretti, L., Kang, H., Stroe, A., & Zandanel, F. 2019, SSRv, 215, 16",doi:"10.1007\u002Fs11214-019-0584-z",crossRefLink:"https:\u002F\u002Fdx.doi.org\u002F10.1007\u002Fs11214-019-0584-z",pubMedLink:a}]}],figures:[{contentId:"f1",label:"Figure 1.",description:"\u003Cspan class=\"p\"\u003EThe number of known extragalactic radio sources discovered by surveys as a function of time, adapted from Norris (2017a). The symbols indicate the type of telescope used to make the survey, and are fully described in Norris (2017a). The dates and survey size are based on estimates made in 2017, and some later surveys (e.g. RACS McConnell et al. 2020, with 2.8 million sources) are missing from this plot. Survey abbreviations and references are given in Norris (2017a). The shading under the curve is merely to improve readability.\u003C\u002Fspan\u003E",thumbnailSrc:d_,enlargedSrc:d_,attrib:[]},{contentId:"f2",label:"Figure 2.",description:"\u003Cspan class=\"p\"\u003ESome of the ASKAP antennas equipped with phased array feeds, located in the Murchison Region of Western Australia. Photo credit: CSIRO\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-17464-mediumThumb-S1323358021000424_fig2.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-55270-optimisedImage-S1323358021000424_fig2.jpg",attrib:[]},{contentId:"f3",label:"Figure 3.",description:"\u003Cspan class=\"p\"\u003EOne of the phased array feeds. Each square on the chequerboard is an antenna element connected to two receivers. Photo credit: CSIRO\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-80652-mediumThumb-S1323358021000424_fig3.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-72019-optimisedImage-S1323358021000424_fig3.jpg",attrib:[]},{contentId:"tbl1",label:"Table 1.",description:"\u003Cspan class=\"p\"\u003EEMU Pilot Survey specifications.\u003C\u002Fspan\u003E",thumbnailSrc:d$,enlargedSrc:d$,attrib:[]},{contentId:"tbl2",label:"Table 2.",description:"\u003Cspan class=\"p\"\u003ECosmological parameters used in this paper and adopted for EMU-PS.\u003C\u002Fspan\u003E",thumbnailSrc:ea,enlargedSrc:ea,attrib:[]},{contentId:"tbl3",label:"Table 3.",description:"\u003Cspan class=\"p\"\u003EEMU pilot observation details.\u003C\u002Fspan\u003E",thumbnailSrc:eb,enlargedSrc:eb,attrib:[]},{contentId:"f4",label:"Figure 4.",description:"\u003Cspan class=\"p\"\u003EThe arrangement of the 36 ASKAP beams in the ‘closepack36’ configuration. The beams are numbered from 0 to 35 (diagram adapted from McConnell et al. 2019). The circles shown are for illustration only. For EMU-PS, the actual full width half maximum of each beam is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline45.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E${\\sim}1.5^{\\circ}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E at the band centre, and the pitch spacing is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline46.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$0.9^{\\circ}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, giving an approximately uniform sensitivity over the field of view.\u003C\u002Fspan\u003E",thumbnailSrc:ec,enlargedSrc:ec,attrib:[]},{contentId:"f5",label:"Figure 5.",description:"\u003Cspan class=\"p\"\u003EThe sky tiling scheme adopted for the EMU-PS. The red rectangles covering the celestial sphere show the tiles planned for the EMU survey, and the orange area indicates the 10 tiles of the EMU-PS. The white strip shows the Galactic plane, and the south celestial pole is at the bottom of the figure.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-18841-mediumThumb-S1323358021000424_fig5.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-77890-optimisedImage-S1323358021000424_fig5.jpg",attrib:[]},{contentId:"f6",label:"Figure 6.",description:"\u003Cspan class=\"p\"\u003EThe location of the EMU Pilot Survey area on the sky within DES DR1, adapted from Abbott et al. (2018). The diagram is in equatorial coordinates, and the solid line marks the Galactic plane, flanked by two dashed lines showing Galactic latitude \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline49.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\pm 10 ^{\\circ}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:ed,enlargedSrc:ed,attrib:[]},{contentId:"tbl4",label:"Table 4.",description:"\u003Cspan class=\"p\"\u003EEMU pilot processing parameters. The first column shows the parameter name used by ASKAPsoft.\u003C\u002Fspan\u003E",thumbnailSrc:ee,enlargedSrc:ee,attrib:[]},{contentId:"tbl5",label:"Table 5.",description:"\u003Cspan class=\"p\"\u003EResults of tests to measure the optimum robustness.\u003C\u002Fspan\u003E",thumbnailSrc:ef,enlargedSrc:ef,attrib:[]},{contentId:"f7",label:"Figure 7.",description:"\u003Cspan class=\"p\"\u003EThe arrangement of the ten individual ASKAP tiles on the sky for EMU-PS with their SBID numbers as listed in Table 3. The rectangles are separated in this diagram for clarity, but there is actually overlapping coverage as illustrated by the greyscale background.\u003C\u002Fspan\u003E",thumbnailSrc:eg,enlargedSrc:eg,attrib:[]},{contentId:"f8",label:"Figure 8.",description:"\u003Cspan class=\"p\"\u003EAn example validation report for one of the processing runs for SB9325, including the metrics and their flags. A higher-resolution version is available online2.\u003C\u002Fspan\u003E",thumbnailSrc:eh,enlargedSrc:eh,attrib:[]},{contentId:"f9",label:"Figure 9.",description:"\u003Cspan class=\"p\"\u003EThe resulting native resolution (\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline86.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$13'' \\times 11''$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E) image of the \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline87.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$270 \\,\\mathrm{deg}^2$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E EMU Pilot Survey, containing about 220 000 radio sources. The rms noise level is 25–30 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline88.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, and the peak flux density is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline89.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$3.14 \\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:ei,enlargedSrc:ei,attrib:[]},{contentId:"tbl6",label:"Table 6.",description:"\u003Cspan class=\"p\"\u003ENumbers of sources remaining after each stage of the value-added processing.\u003C\u002Fspan\u003E",thumbnailSrc:ej,enlargedSrc:ej,attrib:[]},{contentId:"f10",label:"Figure 10.",description:"\u003Cspan class=\"p\"\u003EThe measured spectral index as a function of flux density. The two solid lines show the 3\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline94.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\sigma$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E uncertainty for a source of spectral index -0.8. Note the excess of sources with a positive spectral index, discussed in Section 6.9.\u003C\u002Fspan\u003E",thumbnailSrc:ek,enlargedSrc:ek,attrib:[]},{contentId:"f11",label:"Figure 11.",description:"\u003Cspan class=\"p\"\u003EA histogram of measured spectral index as a function of flux density, for the 10458 sources with flux density \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline97.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$>$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E 2.5 mJy.\u003C\u002Fspan\u003E",thumbnailSrc:el,enlargedSrc:el,attrib:[]},{contentId:"f12",label:"Figure 12.",description:"\u003Cspan class=\"p\"\u003EThe fraction of simple radio sources (as listed in Table 6) matched with a CWISE source as a function of separation, both for unshifted data and for data shifted by one arcmin.\u003C\u002Fspan\u003E",thumbnailSrc:em,enlargedSrc:em,attrib:[]},{contentId:"f13",label:"Figure 13.",description:"\u003Cspan class=\"p\"\u003EThe fraction of radio sources with a CWISE position matched with a DES DR1 source as a function of separation, both for unshifted data and for data shifted by one arcmin.\u003C\u002Fspan\u003E",thumbnailSrc:en,enlargedSrc:en,attrib:[]},{contentId:"f14",label:"Figure 14.",description:"\u003Cspan class=\"p\"\u003EA plot showing the difference in position of radio sources compared to the matching CWISE source in the W1 band, showing a mean offset of \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline101.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\sim$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E0.3 arcsec, which is small compared to the 18 arcsec resolution of the convolved data. The horizontal axis is Right Ascension and the vertical axis is Declination.\u003C\u002Fspan\u003E",thumbnailSrc:eo,enlargedSrc:eo,attrib:[]},{contentId:"f15",label:"Figure 15.",description:"\u003Cspan class=\"p\"\u003EThe ratio of peak flux densities between EMU-PS and SUMSS for simple sources with EMU-PS flux densities \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline102.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$>$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E 6 mJy, and with catalogued positions within 3 arcsec.\u003C\u002Fspan\u003E",thumbnailSrc:ep,enlargedSrc:ep,attrib:[]},{contentId:"f16",label:"Figure 16.",description:"\u003Cspan class=\"p\"\u003EA typical section of the survey field, covering about \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline103.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$0.3 \\,\\mathrm{deg}^2$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E (or about one thousandth of the area of the EMU Pilot Survey) which contains about 250 radio sources). On the left is the SUMSS image (Mauch et al. 2003) and on the right is the EMU-PS image. Prominent in this image is the Giant Radio Galaxy ESO 234-68. The maximum flux density of ESO 234-68 in the EMU-PS image is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline104.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$58.8 \\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, and that of the strong source at the bottom of the image (PMN J2045-5135) is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline105.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$1.06 \\mathrm{Jy beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. The rms of the EMU-PS image is 25–30 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline106.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, and that of the SUMSS image is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline107.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E${\\sim}1.25\\ \\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-27981-mediumThumb-S1323358021000424_fig16.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-87086-optimisedImage-S1323358021000424_fig16.jpg",attrib:[]},{contentId:"f17",label:"Figure 17.",description:"\u003Cspan class=\"p\"\u003EA sample of the final image, showing the three data products on a region, covered by three tiles, containing two of the ‘Odd Radio Circles’(Norris et al. 2021): (a) the initial public data release from a single tile (SB9351) (resolution 11 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline116.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\times$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E 13 arcsec, rms = \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline117.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$40 \\,\\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, (b) the added-value ‘native’ data release with 11\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline118.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\times$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E13 arcsec resolution, from the merged tiles, rms = 25 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline119.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, and (c) the added-value ‘convolved’ data release with 18 arcsec resolution, rms = 25 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline120.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. The peak flux density in this image is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline121.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$4.6\\ \\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-25420-mediumThumb-S1323358021000424_fig17.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-70959-optimisedImage-S1323358021000424_fig17.jpg",attrib:[]},{contentId:"tbl7",label:"Table 7.",description:"\u003Cspan class=\"p\"\u003EAvailable data products, including Digital Object Identifiers (DOIs) that can be used to access the data described in this paper.\u003C\u002Fspan\u003E",thumbnailSrc:eq,enlargedSrc:eq,attrib:[]},{contentId:"f18",label:"Figure 18.",description:"\u003Cspan class=\"p\"\u003EThe sensitivity of EMU-PS as a function of spatial scale. The plot was made using visibility data from a single beam and pointing of an interleaved observation (2-h observation, 288-MHz bandwidth, scaled to the EMU-PS observing frequency of 944 MHz) which was filled with Gaussian noise and various uv tapers were applied to shape the beam size. We then measured the image noise (effectively the sensitivity at the scale associated with the uv taper). The two plots show the same result over different ranges of spatial scale.\u003C\u002Fspan\u003E",thumbnailSrc:er,enlargedSrc:er,attrib:[]},{contentId:"f19",label:"Figure 19.",description:"\u003Cspan class=\"p\"\u003ENormalised differential source counts derived from the \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline133.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$270\\ \\mathrm{deg}^2$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E EMU-PS survey for the \u003Cspan class=\"italic\"\u003Eisland\u003C\u002Fspan\u003E catalogue (black filled diamonds) and for simple sources only (black empty diamonds). The counts have been rescaled from 943.5 MHz to 1.4 GHz by assuming \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline134.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\alpha=-0.7$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. Also shown for comparison are the counts derived from 1.4 GHz \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline135.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$>$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E degree-scale surveys (symbols and colours as indicated in the figure). Vertical bars represent Poissonian errors on the normalised counts. Systematic errors due to incompleteness corrections and spectral index assumptions are approximately included in the size of the plotted symbols. The result of the \u003Cspan class=\"italic\"\u003EP\u003C\u002Fspan\u003E(\u003Cspan class=\"italic\"\u003ED\u003C\u002Fspan\u003E) analysis performed by (Vernstrom et al. 2014, rescaled from 3 to 1.4 GHz by assuming \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline136.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\alpha $\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E = \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline137.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$-$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E0.7) is indicated in dark green. The black solid line represents the predicted counts from 200 sq. degr. of the S3-SEX simulations (Wilman et al. 2008). The light blue and yellow shaded areas illustrate the predicted cosmic variance effects for survey coverages of 5 and \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline138.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$10\\ \\mathrm{deg}^2$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, respectively (obtained by splitting the S3-SEX simulation in 40 5-\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline139.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mathrm{deg}^2$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E and 20 10-\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline140.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mathrm{deg}^2$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E fields, respectively). The \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline141.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$25\\ \\mathrm{deg}^2$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E medium tier of the more recent T-RECS simulations (Bonaldi et al. 2019) is represented by the purple shaded area. Finally, the Mancuso et al. (2017) radio source evolutionary model is shown by the light green line.\u003C\u002Fspan\u003E",thumbnailSrc:es,enlargedSrc:es,attrib:[]},{contentId:"f20",label:"Figure 20.",description:"\u003Cspan class=\"p\"\u003EThe EMU-PS preliminary \u003Cspan class=\"italic\"\u003EP\u003C\u002Fspan\u003E(\u003Cspan class=\"italic\"\u003ED\u003C\u002Fspan\u003E) distributions. The solid black line is the probability distribution made from sections of the pilot away from bright sources. The upper right inset shows bright flux density tail of the \u003Cspan class=\"italic\"\u003EP\u003C\u002Fspan\u003E(\u003Cspan class=\"italic\"\u003ED\u003C\u002Fspan\u003E) distributions. The blue dot-dashed line shows a Gaussian noise distribution of \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline160.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\sigma= 23 \\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. The red dashed line shows the predicted or model \u003Cspan class=\"italic\"\u003EP\u003C\u002Fspan\u003E(\u003Cspan class=\"italic\"\u003ED\u003C\u002Fspan\u003E) generated from the source count shown in the lower right inset.\u003C\u002Fspan\u003E",thumbnailSrc:et,enlargedSrc:et,attrib:[]},{contentId:"f21",label:"Figure 21.",description:"\u003Cspan class=\"p\"\u003EA peculiar radio source found in the EMU Pilot Survey, consisting of a group of distorted radio components, collectively known as PKS 2130–538, and nicknamed ‘the dancing ghosts’. The two host galaxies (\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline163.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$z \\sim 0.077$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E) are seen at the centre of the narrow jets (shown with numbers in the figure to indicate their putative host) which expand into diffuse lobes, probably bent by interactions. On the left is the total intensity greyscale image (shown in turquoise), superimposed on a background of the DES optical image, assembled from the r, g, and i images. On the right is the total intensity image of PKS 2130-538, colour-coded by spectral index. The unconventional colour scheme was constructed using sequential colours on the ‘colour wheel’ (e.g. Itten 1970). The colours were fixed in luminosity, that is, fixed to be constant in luminosity-chroma-hue colour space (Ferrand 2019). In this way, the brightness level on the image represents only the total intensity values. The colour bar indicates the spectral index at a single fixed intensity. Since the spectral index map in this colour scheme was multiplied by the total intensity map, darker versions of colours are associated with fainter regions in the data. The peak flux density in this image is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline164.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$103\\ \\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-80985-mediumThumb-S1323358021000424_fig21.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-15185-optimisedImage-S1323358021000424_fig21.jpg",attrib:[]},{contentId:"f22",label:"Figure 22.",description:"\u003Cspan class=\"p\"\u003EAnother peculiar radio source found in the EMU Pilot Survey: a double-lobed radio AGN, known as PMN J2041–5256, with a curious ‘double’ bent tail. The radio data from EMU-PS has been ‘stretched’ to show the faint emission, and then coloured turquoise, and adjusted to emphasise the double tail. DES g-, r-, and i-band data are combined to form the background, which is combined with the radio data using a layer mask in GIMP. Embedded in the tails are several radio sources that may be unrelated to the tailed galaxy. The peak flux density in this image is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline175.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$58.3\\ \\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-88490-mediumThumb-S1323358021000424_fig22.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-13700-optimisedImage-S1323358021000424_fig22.jpg",attrib:[]},{contentId:"f23",label:"Figure 23.",description:"\u003Cspan class=\"p\"\u003EThe ‘Smoking Gun’ Galaxy EMU PS J204835.0–491137 consists of the two diffuse radio clouds seen in this image. These are presumably the remnants of a classical double-lobed radio galaxy in which the central engine has switched off. The labels A and B indicate two possible host galaxies, discussed in the text. The peak flux density in this image is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline176.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$0.87\\ \\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:eu,enlargedSrc:eu,attrib:[]},{contentId:"f24",label:"Figure 24.",description:"\u003Cspan class=\"p\"\u003EEMU PS J210700.0–501128.8 is an ambiguous case, appearing at first to be a double-lobed source with material blown to the east. But with no host between the bright patches, and the southern bright component coincident with a quasar, marked with an ‘X’, these may be two independent sources with serendipitously similar appearances The peak flux density in this image is \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline180.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$11.6\\ \\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:ev,enlargedSrc:ev,attrib:[]},{contentId:"f25",label:"Figure 25.",description:"\u003Cspan class=\"p\"\u003EAn image of the first ‘Odd Radio Circle’, or ORC, found in EMU-PS (Norris et al. 2021). It has no optical counterpart to the diffuse ring, or to other diffuse structure, but has a galaxy at its centre which may be the origin of the ring. The image is based on EMU-PS data at native resolution but enhanced to show faint features as described in Norris et al. (2021), particularly the internal structure or “spokes” of the ORC. Radio data are shown in green, and DES optical data are shown in turquoise, magenta, yellow and red, and mainly appear in this image as white.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-62673-mediumThumb-S1323358021000424_fig25.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-49417-optimisedImage-S1323358021000424_fig25.jpg",attrib:[]},{contentId:"f26",label:"Figure 26.",description:"\u003Cspan class=\"p\"\u003EA selection of ASKAP-detected nearby galaxies in the EMU-PS. Optical DSS2 \u003Cspan class=\"italic\"\u003ER\u003C\u002Fspan\u003E-band images are overlaid with ASKAP radio continuum contours. The contour levels are –0.09, 0.09 (\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline195.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E${\\sim}3 \\sigma$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E), 0.18, 0.36, 0.75, 1.5, 3.0, 7.5, 15.0, and \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline196.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$30\\ \\mathrm{mJy\\,beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. The convolved 18 arcsec beam is shown in the bottom left corner of each panel. The galaxy name and heliocentric velocity (all but one, ESO233-IG004, from HIPASS) are also displayed. The velocity of ESO233-IG004 is taken from Jones et al. (2009).\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-77883-mediumThumb-S1323358021000424_fig26.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-91916-optimisedImage-S1323358021000424_fig26.jpg",attrib:[]},{contentId:"f27",label:"Figure 27.",description:"\u003Cspan class=\"p\"\u003EDES-DR1 optical composite image of the nearby face-on spiral galaxy NGC 7125 overlaid with contours from the EMU-PS. The contour levels are: 0.1, 0.25, 0.5, 1.0, 1.3, 1.6, 2.0, and \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline215.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$2.4\\ \\mathrm{mJy\\,beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. NGC 7125 and its neighbour NGC 7216 form an interacting galaxy pair (HIPASS J2149–60) with a large pool of hydrogen gas for star formation.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-80083-mediumThumb-S1323358021000424_fig27.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-72933-optimisedImage-S1323358021000424_fig27.jpg",attrib:[]},{contentId:"f28",label:"Figure 28.",description:"\u003Cspan class=\"p\"\u003E(Left) The Giant Radio Galaxy (GRG) EMU PS J205139.8–570434, with radio (at native resolution) shown in greyscale, overlaid on the DES DR1 colour image. The GRG consists of the roughly north-south jet and the two diffuse plumes above and below it. The strong source to the east, surrounded by diffraction rings, is the well-studied galaxy IC 5063. (Right) A contour diagram of the central part of the GRG at 18 arcsec resolution, overlaid on the DES DR1 colour image. Contour levels are 3, 7, 12, and \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline242.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$18\\ \\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-45019-mediumThumb-S1323358021000424_fig28.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-06142-optimisedImage-S1323358021000424_fig28.jpg",attrib:[]},{contentId:"f29",label:"Figure 29.",description:"\u003Cspan class=\"p\"\u003EThe histogram of EMU-PS flux densities for 6dFGS galaxies with \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline253.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E${\\rm H\\alpha}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E emission and \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline254.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$K<12.65$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, along with the corresponding histogram of flux densities measured at offset positions. Just 17 of the 623 6dFGS galaxies with detectable \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline255.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E${\\rm H\\alpha}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E emission have radio flux densities below 75 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline256.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E.\u003C\u002Fspan\u003E",thumbnailSrc:ew,enlargedSrc:ew,attrib:[]},{contentId:"f30",label:"Figure 30.",description:"\u003Cspan class=\"p\"\u003EThe EMU-PS flux densities of \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline257.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$K<12$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E galaxies with and without \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline258.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E${\\rm H\\alpha}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E emission as a function of absolute magnitude. The dashed line shows \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline259.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$75\\,{\\rm \\mu Jy}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, roughly corresponding to \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline260.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$3\\sigma$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. Almost all star-forming galaxies are detected by the EMU-PS. While low mass passive galaxies can have no detectable radio continuum emission, all but one \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline261.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$M_K<-26$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E passive galaxy has a positive radio continuum flux density.\u003C\u002Fspan\u003E",thumbnailSrc:ex,enlargedSrc:ex,attrib:[]},{contentId:"f31",label:"Figure 31.",description:"\u003Cspan class=\"p\"\u003EThe number of cross-matches between DES counterparts to EMU-PS sources, and Gaia sources, for unshifted data (blue), and data shifted by one arcmin (orange).\u003C\u002Fspan\u003E",thumbnailSrc:ey,enlargedSrc:ey,attrib:[]},{contentId:"f32",label:"Figure 32.",description:"\u003Cspan class=\"p\"\u003EThe AllWISE colour-colour plot for EMU-PS sources cross-matched with Gaia, colour-coded according to their measured proper motion. The dashed lines divide the graph into the regions identified by Jarrett et al. (2017).\u003C\u002Fspan\u003E",thumbnailSrc:ez,enlargedSrc:ez,attrib:[]},{contentId:"f33",label:"Figure 33.",description:"\u003Cspan class=\"p\"\u003EMulti-wavelength composite image of SPT-CL J2023\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline262.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$-$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E5535. Contours denote the EMU-PS surface brightness at 944 MHz at 18 arcsec resolution, at \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline263.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$3\\sigma_{\\rm{rms}} \\times 2^{n}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E where \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline264.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$n=0, 1, 2, 3, 4$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E and \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline265.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\sigma_{rms}=\\sim25$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline266.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. Background colourmap shows a composite \u003Cspan class=\"italic\"\u003Eg\u003C\u002Fspan\u003E, \u003Cspan class=\"italic\"\u003Er\u003C\u002Fspan\u003E, and \u003Cspan class=\"italic\"\u003Ei\u003C\u002Fspan\u003E image from DECam. X-ray emission from \u003Cspan class=\"italic\"\u003EChandra\u003C\u002Fspan\u003E is also overlaid in red. New diffuse radio sources identified by HyeongHan et al. (2020) are also indicated.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-85763-mediumThumb-S1323358021000424_fig33.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-63763-optimisedImage-S1323358021000424_fig33.jpg",attrib:[]},{contentId:"f34",label:"Figure 34.",description:"\u003Cspan class=\"p\"\u003EMulti-wavelength composite image of the cluster SPT-CL J2032\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline267.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$-$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E5627. Colour map and contours are the same as Figure 33, but with \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline268.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$25\\,\\mathrm{ks}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E XMM- \u003Cspan class=\"italic\"\u003ENewton\u003C\u002Fspan\u003E surface brightness shown in red. It appears that the cluster hosts one of the rare class of double-radio relics with the northern (A and B) and southern (C) relics as indicated.\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-42254-mediumThumb-S1323358021000424_fig34.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-40250-optimisedImage-S1323358021000424_fig34.jpg",attrib:[]},{contentId:"f35",label:"Figure 35.",description:"\u003Cspan class=\"p\"\u003ERadio contours overlaid on a multi-wavelength (irg) composite image of 6dFGS g2212485-614658 from DES. The radio image was made from the EMU-PS native resolution data by subtracting four unresolved sources and then convolving to a resolution of 18 arcsec. Contours are at 75, 150, 300, and 600 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline280.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\mu\\mathrm{Jy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. The subtracted sources were at 22:12:48.64 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline281.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$-$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E61:46:58.5 (14.9 mJy), 22:12:43.04 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline282.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$-$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E61:46:50.1 (0.3 mJy), 22:12:51.19 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline283.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$-$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E61:46:15.5 (0.2 mJy), 22:12:37.17 \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline284.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$-$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E61:47:24.5 (0.1 mJy)\u003C\u002Fspan\u003E",thumbnailSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-60188-mediumThumb-S1323358021000424_fig35.jpg",enlargedSrc:"https:\u002F\u002Fstatic.cambridge.org\u002Fbinary\u002Fversion\u002Fid\u002Furn:cambridge.org:id:binary-alt:20210906095333-28830-optimisedImage-S1323358021000424_fig35.jpg",attrib:[]},{contentId:"f36",label:"Figure 36.",description:"\u003Cspan class=\"p\"\u003EThe number of sources in the EMU-PS with a flux density greater than some limit (\u003Cspan class=\"italic\"\u003ES\u003C\u002Fspan\u003E), as a function of that limit, compared to scaled predictions from the SKADS and T-RECS simulated catalogues. The dashed black vertical line gives the \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline301.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$500\\mu\\mathrm{Jy}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E limit we assume for the clustering analysis presented in this paper. There is some discretisation of the prediction for the larger flux density limits, due to a scaling of some small integer value for the original prediction that was made for a much smaller value.\u003C\u002Fspan\u003E",thumbnailSrc:eA,enlargedSrc:eA,attrib:[]},{contentId:"f37",label:"Figure 37.",description:"\u003Cspan class=\"p\"\u003EThe predicted number of sources in the EMU Pilot Survey as a function of redshift, generated by scaling the predictions from the SKADS and T-RECS simulated catalogues. This assumes a flux density limit of \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline305.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$500\\mu\\mathrm{Jy}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E",thumbnailSrc:eB,enlargedSrc:eB,attrib:[]},{contentId:"f38",label:"Figure 38.",description:"\u003Cspan class=\"p\"\u003EThe measured angular correlation function (ACF) \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline309.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$w(\\theta)$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E as a function of angular separation with one-sigma error bar computed from bootstrap re-sampling from 100 bootstraps. The correlation function is measured from the integrated flux-corrected EMU-PS island catalogue, using all sources above a flux density limit of \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline310.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$500\\mu\\mathrm{Jy}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E. The blue curve is the theoretical prediction for the correlation function, assuming the Planck 2018 best fit cosmology and a SKADS model for the number distribution with redshift and the bias. No fitting of the cosmological or bias parameters was performed to change the prediction curve. As negative values cannot be shown on a log scale, in bins where the ACF becomes negative, we show (in red) the value of (-ACF) instead.\u003C\u002Fspan\u003E",thumbnailSrc:eC,enlargedSrc:eC,attrib:[]},{contentId:"f39",label:"Figure 39.",description:"\u003Cspan class=\"p\"\u003EThe spectral index distributions for unresolved (\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline315.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\Psi < 2''$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, blue) and resolved (\u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline316.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$\\Psi > 20''$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, red) EMU components. The three panels show different minimum brightness levels, corresponding to \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline317.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$S_{\\text{peak}} > 1\\,\\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline318.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$S_{\\text{peak}} > 3\\,\\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E, and \u003Cspan class=\"alternatives\"\u003E\u003Cimg class=\"inline-graphic mathjax-alternative mathjax-alt-graphic mathjax-off\" data-mimesubtype=\"png\" data-type src=\"${staticDomain}\u002Fcontent\u002Fid\u002Furn:cambridge.org:id:article:S1323358021000424\u002Fresource\u002Fname\u002FS1323358021000424_inline319.png?pub-status=live\" \u002F\u003E\u003Cspan class=\"mathjax-tex-wrapper\" data-mathjax-type=\"texmath\"\u003E\u003Cspan class=\"tex-math mathjax-tex-math mathjax-on\"\u003E$S_{\\text{peak}} > 10\\,\\mathrm{mJy\\ beam}^{-1}$\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E\u003C\u002Fspan\u003E from top to bottom. The legend in each panel denotes the number of components contributing to each distribution shown. Each plot is normalised to the area under the curve.\u003C\u002Fspan\u003E",thumbnailSrc:eD,enlargedSrc:eD,attrib:[]}]},pdf:{standardResolution:{fileUrl:"\u002Fcore\u002Fservices\u002Faop-cambridge-core\u002Fcontent\u002Fview\u002F6FD673731F193C01A133A89602B75F86\u002FS1323358021000424a.pdf\u002Fthe-evolutionary-map-of-the-universe-pilot-survey.pdf",fileSizeInMb:5,articleTitle:x,slugTitle:"the-evolutionary-map-of-the-universe-pilot-survey"},highResolution:c,media:c},classification:[],supplementaryMaterials:[],relations:{corrections:[],correctionsOriginals:[],retractions:[],retractionsOriginals:[],addendums:[{title:eE,type:"addendum",authors:[{givenNames:M,surname:N,nameStyle:c,affiliations:[{text:i},{text:h}],isCorresponding:b,notes:a,isAnonymous:b,fullName:O,searchUrl:P,orcidUrl:c},{givenNames:Q,surname:R,nameStyle:c,affiliations:[{text:h},{text:r}],isCorresponding:b,notes:a,isAnonymous:b,fullName:S,searchUrl:T,orcidUrl:c},{givenNames:U,surname:V,nameStyle:c,affiliations:[{text:i},{text:h},{text:W}],isCorresponding:b,notes:a,isAnonymous:b,fullName:X,searchUrl:Y,orcidUrl:c},{givenNames:Z,surname:_,nameStyle:c,affiliations:[{text:r}],isCorresponding:b,notes:a,isAnonymous:b,fullName:$,searchUrl:aa,orcidUrl:c},{givenNames:ab,surname:ac,nameStyle:c,affiliations:[{text:i},{text:h},{text:ad}],isCorresponding:b,notes:a,isAnonymous:b,fullName:ae,searchUrl:af,orcidUrl:c},{givenNames:ag,surname:ah,nameStyle:c,affiliations:[{text:ai}],isCorresponding:b,notes:a,isAnonymous:b,fullName:aj,searchUrl:ak,orcidUrl:c},{givenNames:al,surname:am,nameStyle:c,affiliations:[{text:an}],isCorresponding:b,notes:a,isAnonymous:b,fullName:ao,searchUrl:ap,orcidUrl:c},{givenNames:aq,surname:ar,nameStyle:c,affiliations:[{text:as}],isCorresponding:b,notes:a,isAnonymous:b,fullName:at,searchUrl:au,orcidUrl:c},{givenNames:av,surname:aw,nameStyle:c,affiliations:[{text:y}],isCorresponding:b,notes:a,isAnonymous:b,fullName:ax,searchUrl:ay,orcidUrl:c},{givenNames:az,surname:aA,nameStyle:c,affiliations:[{text:aB}],isCorresponding:b,notes:a,isAnonymous:b,fullName:aC,searchUrl:aD,orcidUrl:c},{givenNames:aE,surname:aF,nameStyle:c,affiliations:[{text:i}],isCorresponding:b,notes:a,isAnonymous:b,fullName:aG,searchUrl:aH,orcidUrl:c},{givenNames:aI,surname:aJ,nameStyle:c,affiliations:[{text:z}],isCorresponding:b,notes:a,isAnonymous:b,fullName:aK,searchUrl:aL,orcidUrl:c},{givenNames:aM,surname:aN,nameStyle:c,affiliations:[{text:aO}],isCorresponding:b,notes:a,isAnonymous:b,fullName:aP,searchUrl:aQ,orcidUrl:c},{givenNames:aR,surname:aS,nameStyle:c,affiliations:[{text:i}],isCorresponding:b,notes:a,isAnonymous:b,fullName:aT,searchUrl:aU,orcidUrl:c},{givenNames:aV,surname:aW,nameStyle:c,affiliations:[{text:z}],isCorresponding:b,notes:a,isAnonymous:b,fullName:aX,searchUrl:aY,orcidUrl:c},{givenNames:aZ,surname:a_,nameStyle:c,affiliations:[{text:k},{text:a$}],isCorresponding:b,notes:a,isAnonymous:b,fullName:ba,searchUrl:bb,orcidUrl:c},{givenNames:bc,surname:bd,nameStyle:c,affiliations:[{text:k},{text:"School of Physics and Astronomy, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, EH9 3HJ Edinburgh, UK"}],isCorresponding:b,notes:a,isAnonymous:b,fullName:be,searchUrl:bf,orcidUrl:c},{givenNames:bg,surname:bh,nameStyle:c,affiliations:[{text:i},{text:bi}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bj,searchUrl:bk,orcidUrl:c},{givenNames:bl,surname:bm,nameStyle:c,affiliations:[{text:k}],isCorresponding:b,notes:a,isAnonymous:b,fullName:bn,searchUrl:bo,orcidUrl:c},{givenNames:bp,surname:bq,nameStyle:c,affiliations:[{text:A}],isCorresponding:b,notes:a,isAnonymous:b,fullName:br,searchUrl:bs,orcidUrl:c},{givenNames:"M. 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Evolutionary Map of the Universe Pilot Survey – ADDENDUM"));</script><script src="/core/page-component/06cd607.js" defer></script><script src="/core/page-component/20147ec.js" defer></script><script src="/core/page-component/66884fb.js" defer></script><script src="/core/page-component/6f4302c.js" defer></script> </div> </div> <div id="article-new-home-productCitations" class="product-citations-modal reveal-modal medium" data-reveal role="dialog" aria-labelledby="article-new-home-citedByModalHeader"> <div class="header"> <div class="heading_07 margin-bottom" id="article-new-home-citedByModalHeader">Cited by</div> </div> <div class="citation-content"> <div class="row collapse header margin-top productCitations-content"> <ul class="small-12 small-centered columns citations"> <li class="fade-in section-container active"> <a href="#" class="section-button" data-id="article-new-home-crossref-citations"> <div class="circular medium citation"> <img 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If this is the first time you used this feature, you will be asked to authorise Cambridge Core to connect with your Dropbox account. <a href="/core/help">Find out more about saving content to Dropbox</a>. </p> </div> </div> <div class="row book-title"> <div class="small-12 columns"> <div class="heading_08"><div class="title">The Evolutionary Map of the Universe pilot survey</div></div> </div> </div> <div class="row book-details book-overview"> <div class="small-12 columns"> <ul> <li class="volume-issue">Volume 38</li> <li class="author"> <a href="/core/search?filters%5BauthorTerms%5D=Ray P. Norris&eventCode=SE-AU" class="more-by-this-author ">Ray P. Norris</a><a target="_blank" class="orcid-logo " href="https://orcid.org/0000-0002-4597-1906" aria-label="Open the ORCID record for Ray P. 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