Search | arXiv e-print repository

<!DOCTYPE html> <html lang="en"> <head> <meta charset="utf-8"/> <meta name="viewport" content="width=device-width, initial-scale=1"/>  <link rel="apple-touch-icon" sizes="180x180" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/apple-touch-icon.png"> <link rel="icon" type="image/png" sizes="32x32" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-32x32.png"> <link rel="icon" type="image/png" sizes="16x16" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-16x16.png"> <link rel="manifest" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/site.webmanifest"> <link rel="mask-icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/safari-pinned-tab.svg" color="#b31b1b"> <link rel="shortcut icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon.ico"> <meta name="msapplication-TileColor" content="#b31b1b"> <meta name="msapplication-config" content="images/icons/browserconfig.xml"> <meta name="theme-color" content="#b31b1b">  <title>Search | arXiv e-print repository</title> <script defer src="https://static.arxiv.org/static/base/1.0.0a5/fontawesome-free-5.11.2-web/js/all.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/base/1.0.0a5/css/arxivstyle.css" /> <script type="text/x-mathjax-config"> MathJax.Hub.Config({ messageStyle: "none", extensions: ["tex2jax.js"], jax: ["input/TeX", "output/HTML-CSS"], tex2jax: { inlineMath: [ ['$','$'], ["\$","\$"] ], displayMath: [ ['$$','$$'], ["\\[","\\]"] ], processEscapes: true, ignoreClass: '.*', processClass: 'mathjax.*' }, TeX: { extensions: ["AMSmath.js", "AMSsymbols.js", "noErrors.js"], noErrors: { inlineDelimiters: ["$","$"], multiLine: false, style: { "font-size": "normal", "border": "" } } }, "HTML-CSS": { availableFonts: ["TeX"] } }); </script> <script src='//static.arxiv.org/MathJax-2.7.3/MathJax.js'></script> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/notification.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/bulma-tooltip.min.css" /> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/search.css" /> <script src="https://code.jquery.com/jquery-3.2.1.slim.min.js" integrity="sha256-k2WSCIexGzOj3Euiig+TlR8gA0EmPjuc79OEeY5L45g=" crossorigin="anonymous"></script> <script src="https://static.arxiv.org/static/search/0.5.6/js/fieldset.js"></script> <style> radio#cf-customfield_11400 { display: none; } </style> </head> <body> <header><a href="#main-container" class="is-sr-only">Skip to main content</a>  <div class="attribution level is-marginless" role="banner"> <div class="level-left"> <a class="level-item" href="https://cornell.edu/"><img src="https://static.arxiv.org/static/base/1.0.0a5/images/cornell-reduced-white-SMALL.svg" alt="Cornell University" width="200" aria-label="logo" /></a> </div> <div class="level-right is-marginless"><p class="sponsors level-item is-marginless"><span id="support-ack-url">We gratefully acknowledge support from<br /> the Simons Foundation, <a href="https://info.arxiv.org/about/ourmembers.html">member institutions</a>, and all contributors. <a href="https://info.arxiv.org/about/donate.html">Donate</a></span></p></div> </div>  <div class="identity level is-marginless"> <div class="level-left"> <div class="level-item"> <a class="arxiv" href="https://arxiv.org/" aria-label="arxiv-logo"> <img src="https://static.arxiv.org/static/base/1.0.0a5/images/arxiv-logo-one-color-white.svg" aria-label="logo" alt="arxiv logo" width="85" style="width:85px;"/> </a> </div> </div> <div class="search-block level-right"> <form class="level-item mini-search" method="GET" action="https://arxiv.org/search"> <div class="field has-addons"> <div class="control"> <input class="input is-small" type="text" name="query" placeholder="Search..." aria-label="Search term or terms" /> <p class="help"><a href="https://info.arxiv.org/help">Help</a> | <a href="https://arxiv.org/search/advanced">Advanced Search</a></p> </div> <div class="control"> <div class="select is-small"> <select name="searchtype" aria-label="Field to search"> <option value="all" selected="selected">All fields</option> <option value="title">Title</option> <option value="author">Author</option> <option value="abstract">Abstract</option> <option value="comments">Comments</option> <option value="journal_ref">Journal reference</option> <option value="acm_class">ACM classification</option> <option value="msc_class">MSC classification</option> <option value="report_num">Report number</option> <option value="paper_id">arXiv identifier</option> <option value="doi">DOI</option> <option value="orcid">ORCID</option> <option value="author_id">arXiv author ID</option> <option value="help">Help pages</option> <option value="full_text">Full text</option> </select> </div> </div> <input type="hidden" name="source" value="header"> <button class="button is-small is-cul-darker">Search</button> </div> </form> </div> </div>  <div class="container"> <div class="user-tools is-size-7 has-text-right has-text-weight-bold" role="navigation" aria-label="User menu"> <a href="https://arxiv.org/login">Login</a> </div> </div> </header> <main class="container" id="main-container"> <div class="level is-marginless"> <div class="level-left"> <h1 class="title is-clearfix"> Showing 1–50 of 117 results for author: <span class="mathjax">Kraan-Korteweg, R C</span> </h1> </div> <div class="level-right is-hidden-mobile">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> <div class="content"> <form method="GET" action="/search/" aria-role="search"> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Kraan-Korteweg, R C"> </div> <div class="select control is-medium"> <label class="is-hidden" for="searchtype">Field</label> <select class="is-medium" id="searchtype" name="searchtype"><option value="all">All fields</option><option value="title">Title</option><option selected value="author">Author(s)</option><option value="abstract">Abstract</option><option value="comments">Comments</option><option value="journal_ref">Journal reference</option><option value="acm_class">ACM classification</option><option value="msc_class">MSC classification</option><option value="report_num">Report number</option><option value="paper_id">arXiv identifier</option><option value="doi">DOI</option><option value="orcid">ORCID</option><option value="license">License (URI)</option><option value="author_id">arXiv author ID</option><option value="help">Help pages</option><option value="full_text">Full text</option></select> </div> <div class="control"> <button class="button is-link is-medium">Search</button> </div> </div> <div class="field"> <div class="control is-size-7"> <label class="radio"> <input checked id="abstracts-0" name="abstracts" type="radio" value="show"> Show abstracts </label> <label class="radio"> <input id="abstracts-1" name="abstracts" type="radio" value="hide"> Hide abstracts </label> </div> </div> <div class="is-clearfix" style="height: 2.5em"> <div class="is-pulled-right"> <a href="/search/advanced?terms-0-term=Kraan-Korteweg%2C+R+C&terms-0-field=author&size=50&order=-announced_date_first">Advanced Search</a> </div> </div> <input type="hidden" name="order" value="-announced_date_first"> <input type="hidden" name="size" value="50"> </form> <div class="level breathe-horizontal"> <div class="level-left"> <form method="GET" action="/search/"> <div style="display: none;"> <select id="searchtype" name="searchtype"><option value="all">All fields</option><option value="title">Title</option><option selected value="author">Author(s)</option><option value="abstract">Abstract</option><option value="comments">Comments</option><option value="journal_ref">Journal reference</option><option value="acm_class">ACM classification</option><option value="msc_class">MSC classification</option><option value="report_num">Report number</option><option value="paper_id">arXiv identifier</option><option value="doi">DOI</option><option value="orcid">ORCID</option><option value="license">License (URI)</option><option value="author_id">arXiv author ID</option><option value="help">Help pages</option><option value="full_text">Full text</option></select> <input id="query" name="query" type="text" value="Kraan-Korteweg, R C"> <ul id="abstracts"><li><input checked id="abstracts-0" name="abstracts" type="radio" value="show"> <label for="abstracts-0">Show abstracts</label></li><li><input id="abstracts-1" name="abstracts" type="radio" value="hide"> <label for="abstracts-1">Hide abstracts</label></li></ul> </div> <div class="box field is-grouped is-grouped-multiline level-item"> <div class="control"> <span class="select is-small"> <select id="size" name="size"><option value="25">25</option><option selected value="50">50</option><option value="100">100</option><option value="200">200</option></select> </span> <label for="size">results per page</label>. </div> <div class="control"> <label for="order">Sort results by</label> <span class="select is-small"> <select id="order" name="order"><option selected value="-announced_date_first">Announcement date (newest first)</option><option value="announced_date_first">Announcement date (oldest first)</option><option value="-submitted_date">Submission date (newest first)</option><option value="submitted_date">Submission date (oldest first)</option><option value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.07084">arXiv:2411.07084</a> <span> [<a href="https://arxiv.org/pdf/2411.07084">pdf</a>, <a href="https://arxiv.org/format/2411.07084">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Revealing hidden structures in the Zone of Avoidance -- a blind MeerKAT HI Survey of the Vela Supercluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">Bradley S. Frank</a>, <a href="/search/?searchtype=author&query=Chen%2C+H">Hao Chen</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/?searchtype=author&query=Steyn%2C+N">Nadia Steyn</a>, <a href="/search/?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/?searchtype=author&query=Goedhart%2C+S">Sharmila Goedhart</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.07084v1-abstract-short" style="display: inline;"> We conducted the MeerKAT Vela Supercluster survey, named Vela$-$HI, to bridge the gap between the Vela SARAO MeerKAT Galactic Plane Survey (Vela$-$SMGPS, $-2^{\circ} \leq b \leq 1^{\circ}$), and optical and near-infrared spectroscopic observations of the Vela Supercluster (hereafter Vela$-$OPT/NIR) at $|b| \gtrsim 7^{\circ}$. Covering coordinates from $263^{\circ} \leq \ell \leq 284^{\circ}$ and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07084v1-abstract-full').style.display = 'inline'; document.getElementById('2411.07084v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.07084v1-abstract-full" style="display: none;"> We conducted the MeerKAT Vela Supercluster survey, named Vela$-$HI, to bridge the gap between the Vela SARAO MeerKAT Galactic Plane Survey (Vela$-$SMGPS, $-2^{\circ} \leq b \leq 1^{\circ}$), and optical and near-infrared spectroscopic observations of the Vela Supercluster (hereafter Vela$-$OPT/NIR) at $|b| \gtrsim 7^{\circ}$. Covering coordinates from $263^{\circ} \leq \ell \leq 284^{\circ}$ and $1^{\circ} \leq b \leq 6.2^{\circ}$ above, and $-6.7^{\circ} \leq b \leq -2^{\circ}$ below the Galactic Plane (GP), we sampled 667 fields spread across an area of ${\sim} \rm 242 ~deg^2$. With a beam size of ${\sim} 38'' \times 31''$, Vela$-$HI achieved a sensitivity of $\langle \rm rms \rangle = 0.74$ mJy beam$^{-1}$ at 44.3 km s$^{-1}$ velocity resolution over ${\sim}$67 hours of observations. We cataloged 719 galaxies, with only 211 (29%) previously documented in the literature, primarily through the HIZOA, 2MASX, and WISE databases. Among these known galaxies, only 66 had optical spectroscopic redshift information. We found marginal differences of less than one channel resolution for all galaxies in common between HIZOA and Vela$-$SMGPS, and a mean difference of $70 \pm 15$ km s$^{-1}$ between optical and HI velocities. Combining data from Vela$-$SMGPS, Vela$-$HI, and Vela$-$OPT/NIR confirmed the connection of the Hydra/Antlia filament across the GP and revealed a previously unknown diagonal wall at a heliocentric velocity range of $6500-8000$ km s$^{-1}$. Vela$-$HI reinforces the connection between the first wall at $18500-20000$ km s$^{-1}$ and the inner ZOA. The second wall seems to traverse the GP at $270^{\circ} \leq \ell \leq 279^{\circ}$, where it appears that both walls intersect, jointly covering the velocity range $18500-21500$ km s$^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07084v1-abstract-full').style.display = 'none'; document.getElementById('2411.07084v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, this version contains the full catalogue of detections</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.13130">arXiv:2409.13130</a> <span> [<a href="https://arxiv.org/pdf/2409.13130">pdf</a>, <a href="https://arxiv.org/format/2409.13130">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> WALLABY Pilot Survey: Public data release of ~1800 HI sources and high-resolution cut-outs from Pilot Survey Phase 2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Murugeshan%2C+C">C. Murugeshan</a>, <a href="/search/?searchtype=author&query=Deg%2C+N">N. Deg</a>, <a href="/search/?searchtype=author&query=Westmeier%2C+T">T. Westmeier</a>, <a href="/search/?searchtype=author&query=Shen%2C+A+X">A. X. Shen</a>, <a href="/search/?searchtype=author&query=For%2C+B+-">B. -Q. For</a>, <a href="/search/?searchtype=author&query=Spekkens%2C+K">K. Spekkens</a>, <a href="/search/?searchtype=author&query=Wong%2C+O+I">O. I. Wong</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">L. Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Catinella%2C+B">B. Catinella</a>, <a href="/search/?searchtype=author&query=Lee-Waddell%2C+K">K. Lee-Waddell</a>, <a href="/search/?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/?searchtype=author&query=Rhee%2C+J">J. Rhee</a>, <a href="/search/?searchtype=author&query=Cortese%2C+L">L. Cortese</a>, <a href="/search/?searchtype=author&query=Goliath%2C+S">S. Goliath</a>, <a href="/search/?searchtype=author&query=Halloran%2C+R">R. Halloran</a>, <a href="/search/?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Lelli%2C+F">F. Lelli</a>, <a href="/search/?searchtype=author&query=Venkataraman%2C+P">P. Venkataraman</a>, <a href="/search/?searchtype=author&query=Verdes-Montenegro%2C+L">L. Verdes-Montenegro</a>, <a href="/search/?searchtype=author&query=Yu%2C+N">N. Yu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.13130v1-abstract-short" style="display: inline;"> We present the Pilot Survey Phase 2 data release for the Wide-field ASKAP L-band Legacy All-sky Blind surveY (WALLABY), carried-out using the Australian SKA Pathfinder (ASKAP). We present 1760 HI detections (with a default spatial resolution of 30") from three pilot fields including the NGC 5044 and NGC 4808 groups as well as the Vela field, covering a total of ~180 deg$^2$ of the sky and spanning… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13130v1-abstract-full').style.display = 'inline'; document.getElementById('2409.13130v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.13130v1-abstract-full" style="display: none;"> We present the Pilot Survey Phase 2 data release for the Wide-field ASKAP L-band Legacy All-sky Blind surveY (WALLABY), carried-out using the Australian SKA Pathfinder (ASKAP). We present 1760 HI detections (with a default spatial resolution of 30") from three pilot fields including the NGC 5044 and NGC 4808 groups as well as the Vela field, covering a total of ~180 deg$^2$ of the sky and spanning a redshift up to $z \simeq 0.09$. This release also includes kinematic models for over 126 spatially resolved galaxies. The observed median rms noise in the image cubes is 1.7 mJy per 30" beam and 18.5 kHz channel. This corresponds to a 5$蟽$ HI column density sensitivity of $\sim 9.1\times10^{19}(1 + z)^4$ cm$^{-2}$ per 30" beam and $\sim 20$ km/s channel, and a 5$蟽$ HI mass sensitivity of $\sim 5.5\times10^8 (D/100$ Mpc)$^{2}$ M$_{\odot}$ for point sources. Furthermore, we also present for the first time 12" high-resolution images ("cut-outs") and catalogues for a sub-sample of 80 sources from the Pilot Survey Phase 2 fields. While we are able to recover sources with lower signal-to-noise ratio compared to sources in the Public Data Release 1, we do note that some data quality issues still persist, notably, flux discrepancies that are linked to the impact of side lobes associated with the dirty beams due to inadequate deconvolution. However, in spite of these limitations, the WALLABY Pilot Survey Phase 2 has already produced roughly a third of the number of HIPASS sources, making this the largest spatially resolved HI sample from a single survey to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13130v1-abstract-full').style.display = 'none'; document.getElementById('2409.13130v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 16 figures, 6 tables, accepted for publication in Publications of the Astronomical Society of Australia (PASA)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.14425">arXiv:2407.14425</a> <span> [<a href="https://arxiv.org/pdf/2407.14425">pdf</a>, <a href="https://arxiv.org/format/2407.14425">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad5a90">10.3847/1538-4357/ad5a90 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The $K_s$-band luminosity function of the rich cluster VC04 in the Vela supercluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hatamkhani%2C+N">N. Hatamkhani</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Blyth%2C+S+L">S. L. Blyth</a>, <a href="/search/?searchtype=author&query=Skelton%2C+R+E">R. E. Skelton</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.14425v1-abstract-short" style="display: inline;"> To learn more about the properties of the Vela Supercluster (VSCL) located behind the Milky Way at $cz\sim 18000$~km~s$^{-1}$, we determined the $K_s$-band Luminosity Function (LF) of VC04, the richest known galaxy cluster in the VSCL, and two other VSCL clusters (VC02 and VC08). The galaxy sample is based on NIR observations which are complete to an extinction-corrected absolute magnitude of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14425v1-abstract-full').style.display = 'inline'; document.getElementById('2407.14425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.14425v1-abstract-full" style="display: none;"> To learn more about the properties of the Vela Supercluster (VSCL) located behind the Milky Way at $cz\sim 18000$~km~s$^{-1}$, we determined the $K_s$-band Luminosity Function (LF) of VC04, the richest known galaxy cluster in the VSCL, and two other VSCL clusters (VC02 and VC08). The galaxy sample is based on NIR observations which are complete to an extinction-corrected absolute magnitude of $M_{Ks}^o<-21.5$ mag ($\sim 2.5$ mag below $M_K^*$), within the clustercentric radius of $r_c<1.5~$Mpc ($\sim 70 \%$ of the Abell radius). For VC04 we obtained 90 new spectroscopic redshifts of galaxies observed with the 11-m Southern African Large Telescope. We found the Schechter parameters of the VC04 LF to be $M^*=-24.41\pm 0.44$ mag, $伪=-1.10\pm 0.20$ and $蠁^*=8.84\pm 0.20$. Both the redshift data and the LF confirm VC04 to be a rich, not yet fully relaxed cluster. We independently determined the LF of VC04 on membership defined by the Red-Sequence method and demonstrated that this method can be used in the absence of high spectroscopic coverage over a cluster. This allowed us to determine the LFs of VC02 and VC08. We also derived the LFs of the Coma, Norma and Virgo clusters to similar depth and extent as the VSCL clusters. We found that the Schechter parameters of VC04 are within $1蟽$ uncertainties of these local clusters, as well as VC02 and VC08. We do not find significant differences between the LFs in the different cluster environments probed in this work down to $M_K^*+2.5$ mag. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14425v1-abstract-full').style.display = 'none'; document.getElementById('2407.14425v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 12 figures and 9 tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.15629">arXiv:2405.15629</a> <span> [<a href="https://arxiv.org/pdf/2405.15629">pdf</a>, <a href="https://arxiv.org/format/2405.15629">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey -- III. Unveiling the obscured part of the Vela Supercluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Chen%2C+H">Hao Chen</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">Bradley S. Frank</a>, <a href="/search/?searchtype=author&query=Steyn%2C+N">Nadia Steyn</a>, <a href="/search/?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/?searchtype=author&query=Goedhart%2C+S">Sharmila Goedhart</a>, <a href="/search/?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.15629v1-abstract-short" style="display: inline;"> We conducted a search for HI emission of the gas-rich galaxies in the Vela region ($260^{\circ} \leq \ell \leq 290^{\circ}, -2^{\circ} \leq b \leq 1^{\circ}$) to explore the Vela Supercluster (VSCL) at $V_\mathrm{hel} \sim 18000$ km s$^{-1}$, largely obscured by Galactic dust. Within the mostly RFI-free band ($250 < V_\mathrm{hel} < 25000$ km s$^{-1}$) of MeerKAT, the analysis focuses on $157$ hex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15629v1-abstract-full').style.display = 'inline'; document.getElementById('2405.15629v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.15629v1-abstract-full" style="display: none;"> We conducted a search for HI emission of the gas-rich galaxies in the Vela region ($260^{\circ} \leq \ell \leq 290^{\circ}, -2^{\circ} \leq b \leq 1^{\circ}$) to explore the Vela Supercluster (VSCL) at $V_\mathrm{hel} \sim 18000$ km s$^{-1}$, largely obscured by Galactic dust. Within the mostly RFI-free band ($250 < V_\mathrm{hel} < 25000$ km s$^{-1}$) of MeerKAT, the analysis focuses on $157$ hexagonally distributed pointings extracted from the SARAO MeerKAT Galactic Plane Survey located in the Vela region (Vela$-$SMGPS). These were combined into 10 contiguous mosaics, covering a ${\sim}90$ deg$^2$ area. Among the $843$ HI detected sources, 39 were previously discovered in the Parkes HIZOA survey ($V_\mathrm{hel} < 12000$ km s$^{-1}$; rms $\sim 6$ mJy beam$^{-1}$). With the improved rms level of the Vela$-$SMGPS, i.e., $0.29 - 0.56$ mJy beam$^{-1}$, our study unveils nearly 12 times more detections (471 candidates) in that same velocity range. We furthermore could identify $187$ galaxy candidates with an HI mass limit reaching $\log (M_{\rm HI}/\rm M_{\odot}) = 9.44$ in the VSCL velocity range $V_\mathrm{hel} \sim 19500 \pm 3500$ km s$^{-1}$. We find indications of two wall-like overdensities that confirm the original suspicion that these walls intersect at low latitudes around longitudes of $\ell \sim 272^{\circ} - 278^{\circ}$. We also find a strong signature most likely associated with the Hydra/Antlia extension and evidence of a previously unknown narrow filament at $V_\mathrm{hel} \sim 12000$ km s$^{-1}$. This paper demonstrates the efficiency of systematic HI surveys with the SKA precursor MeerKAT, even in the most obscured part of the Zone of Avoidance (ZOA). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15629v1-abstract-full').style.display = 'none'; document.getElementById('2405.15629v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, this version contains the full catalogue of detections</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.07275">arXiv:2312.07275</a> <span> [<a href="https://arxiv.org/pdf/2312.07275">pdf</a>, <a href="https://arxiv.org/format/2312.07275">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The SARAO MeerKAT 1.3 GHz Galactic Plane Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Goedhart%2C+S">S. Goedhart</a>, <a href="/search/?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</a>, <a href="/search/?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/?searchtype=author&query=Bietenholz%2C+M">M. Bietenholz</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a>, <a href="/search/?searchtype=author&query=Anderson%2C+L+D">L. D. Anderson</a>, <a href="/search/?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/?searchtype=author&query=Chen%2C+H">H. Chen</a>, <a href="/search/?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/?searchtype=author&query=Egbo%2C+D">D. Egbo</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/?searchtype=author&query=Hoare%2C+M+G">M. G. Hoare</a>, <a href="/search/?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/?searchtype=author&query=Irabor%2C+T">T. Irabor</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Kurapati%2C+S">S. Kurapati</a>, <a href="/search/?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/?searchtype=author&query=Mutale%2C+M">M. Mutale</a> , et al. (105 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.07275v2-abstract-short" style="display: inline;"> We present the SARAO MeerKAT Galactic Plane Survey (SMGPS), a 1.3 GHz continuum survey of almost half of the Galactic Plane (251掳$\le l \le$ 358掳and 2掳$\le l \le$ 61掳at $|b| \le 1.5掳$). SMGPS is the largest, most sensitive and highest angular resolution 1 GHz survey of the Plane yet carried out, with an angular resolution of 8" and a broadband RMS sensitivity of $\sim$10--20 $渭$ Jy/beam. Here we d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07275v2-abstract-full').style.display = 'inline'; document.getElementById('2312.07275v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.07275v2-abstract-full" style="display: none;"> We present the SARAO MeerKAT Galactic Plane Survey (SMGPS), a 1.3 GHz continuum survey of almost half of the Galactic Plane (251掳$\le l \le$ 358掳and 2掳$\le l \le$ 61掳at $|b| \le 1.5掳$). SMGPS is the largest, most sensitive and highest angular resolution 1 GHz survey of the Plane yet carried out, with an angular resolution of 8" and a broadband RMS sensitivity of $\sim$10--20 $渭$ Jy/beam. Here we describe the first publicly available data release from SMGPS which comprises data cubes of frequency-resolved images over 908--1656 MHz, power law fits to the images, and broadband zeroth moment integrated intensity images. A thorough assessment of the data quality and guidance for future usage of the data products are given. Finally, we discuss the tremendous potential of SMGPS by showcasing highlights of the Galactic and extragalactic science that it permits. These highlights include the discovery of a new population of non-thermal radio filaments; identification of new candidate supernova remnants, pulsar wind nebulae and planetary nebulae; improved radio/mid-IR classification of rare Luminous Blue Variables and discovery of associated extended radio nebulae; new radio stars identified by Bayesian cross-matching techniques; the realisation that many of the largest radio-quiet WISE HII region candidates are not true HII regions; and a large sample of previously undiscovered background HI galaxies in the Zone of Avoidance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07275v2-abstract-full').style.display = 'none'; document.getElementById('2312.07275v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. The data release is live and links can be found in the Data Availability Statement in the paper</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.05237">arXiv:2312.05237</a> <span> [<a href="https://arxiv.org/pdf/2312.05237">pdf</a>, <a href="https://arxiv.org/format/2312.05237">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad3823">10.1093/mnras/stad3823 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey -- II. The Local Void and its substructure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/?searchtype=author&query=Chen%2C+H">Hao Chen</a>, <a href="/search/?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/?searchtype=author&query=Steyn%2C+N">Nadia Steyn</a>, <a href="/search/?searchtype=author&query=Frank%2C+B">Bradley Frank</a>, <a href="/search/?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/?searchtype=author&query=Goedhart%2C+S">Sharmila Goedhart</a>, <a href="/search/?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.05237v1-abstract-short" style="display: inline;"> The Local Void is one of the nearest large voids, located at a distance of 23 Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21 cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its surroundings over the Galactic longitude range 329$^{\circ}< \ell <$ 55$^{\circ}$, Galactic latitude… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05237v1-abstract-full').style.display = 'inline'; document.getElementById('2312.05237v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.05237v1-abstract-full" style="display: none;"> The Local Void is one of the nearest large voids, located at a distance of 23 Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21 cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its surroundings over the Galactic longitude range 329$^{\circ}< \ell <$ 55$^{\circ}$, Galactic latitude $|b| <$ 1.5$^{\circ}$, and redshift $cz <$ 7500 km/s. We have detected 291 galaxies to median rms sensitivity of 0.44 mJy per beam per 44 km/s channel. We find 17 galaxies deep inside the Void, 96 at the border of the Void, while the remaining 178 galaxies are in average density environments. The extent of the Void is ~ 58 Mpc. It is severely under-dense for the longitude range 350$^{\circ}< \ell <$ 35$^{\circ}$ up to redshift $z <$ 4500 km/s. The galaxies in the Void tend to have \HI masses that are lower (by approximately 0.25 dex) than their average density counterparts. We find several potential candidates for small groups of galaxies, of which two groups (with 3 members and 5 members) in the Void show signs of filamentary substructure within the Void. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05237v1-abstract-full').style.display = 'none'; document.getElementById('2312.05237v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS; 16 pages, 14 figures, Supplementary data are available online at MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.03545">arXiv:2312.03545</a> <span> [<a href="https://arxiv.org/pdf/2312.03545">pdf</a>, <a href="https://arxiv.org/format/2312.03545">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey $-$ I. Probing the richness of the Great Attractor Wall across the inner Zone of Avoidance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Steyn%2C+N">Nadia Steyn</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/?searchtype=author&query=Chen%2C+H">Hao Chen</a>, <a href="/search/?searchtype=author&query=Frank%2C+B">Bradley Frank</a>, <a href="/search/?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/?searchtype=author&query=Goedhart%2C+S">Sharmila Goedhart</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.03545v1-abstract-short" style="display: inline;"> This paper presents the first HI results extracted from the SARAO MeerKAT Galactic Plane Survey (SMGPS) $-$ a narrow strip ($b \sim 3^\circ$) along the southern Milky Way. The primary goal consisted in tracing the Great Attractor (GA) Wall across the innermost Zone of Avoidance. We reduced a segment spanning the longitude range $302^\circ \leq \ell \leq 332^\circ$ for the redshift range… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03545v1-abstract-full').style.display = 'inline'; document.getElementById('2312.03545v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.03545v1-abstract-full" style="display: none;"> This paper presents the first HI results extracted from the SARAO MeerKAT Galactic Plane Survey (SMGPS) $-$ a narrow strip ($b \sim 3^\circ$) along the southern Milky Way. The primary goal consisted in tracing the Great Attractor (GA) Wall across the innermost Zone of Avoidance. We reduced a segment spanning the longitude range $302^\circ \leq \ell \leq 332^\circ$ for the redshift range $z \leq 0.08$. The superb SMGPS sensitivity (rms = 0.3-0.5 mJy beam$^{-1}$ per 44 kms$^{-1}$ channel) and angular resolution ($\sim$ 31" $\times$ 26") lead to a detection limit of log$(M_{\rm HI}/$M$_\odot) \geq$ 8.5 at the GA distance ($V_{\rm hel} \sim 3500 - 6500$ kms$^{-1}$). A total of 477 galaxy candidates were identified over the full redshift range. A comparison of the few HI detections with counterparts in the literature (mostly HIZOA) found the HI fluxes and other HI parameters to be highly consistent. The continuation of the GA Wall is confirmed through a prominent overdensity of $N = 214$ detections in the GA distance range. At higher latitudes, the wall moves to higher redshifts, supportive of a possible link with the Ophiuchus cluster located behind the Galactic Bulge. This deep interferometric HI survey demonstrates the power of the SMGPS in improving our insight of large-scale structures at these extremely low latitudes, despite the high obscuration and continuum background. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03545v1-abstract-full').style.display = 'none'; document.getElementById('2312.03545v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 7 figures, 2 appendices of 12 pages. Journal reference: MNRAS Letters, accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.15624">arXiv:2311.15624</a> <span> [<a href="https://arxiv.org/pdf/2311.15624">pdf</a>, <a href="https://arxiv.org/format/2311.15624">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The star formation histories of galaxies in different stages of pre-processing in the Fornax A group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Loubser%2C+S+I">S. I. Loubser</a>, <a href="/search/?searchtype=author&query=Mosia%2C+K">K. Mosia</a>, <a href="/search/?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/?searchtype=author&query=Peletier%2C+R+F">R. F. Peletier</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/?searchtype=author&query=Loni%2C+A">A. Loni</a>, <a href="/search/?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/?searchtype=author&query=Zabel%2C+N">N. Zabel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.15624v1-abstract-short" style="display: inline;"> We study the recent star formation histories of ten galaxies in the Fornax A galaxy group, on the outskirts of the Fornax cluster. The group galaxies are gas-rich, and their neutral atomic hydrogen (HI) was studied in detail with observations from the MeerKAT telescope. This allowed them to be classified into different stages of pre-processing (early, ongoing, advanced). We use long-slit spectra o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.15624v1-abstract-full').style.display = 'inline'; document.getElementById('2311.15624v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.15624v1-abstract-full" style="display: none;"> We study the recent star formation histories of ten galaxies in the Fornax A galaxy group, on the outskirts of the Fornax cluster. The group galaxies are gas-rich, and their neutral atomic hydrogen (HI) was studied in detail with observations from the MeerKAT telescope. This allowed them to be classified into different stages of pre-processing (early, ongoing, advanced). We use long-slit spectra obtained with the South African Large Telescope (SALT) to analyse stellar population indicators to constrain quenching timescales and to compare these to the HI gas content of the galaxies. The H$伪$ equivalent width, EW(H$伪$), suggest that the pre-processing stage is closely related to the recent (< 10 Myr) specific Star Formation Rate (sSFR). The early-stage galaxy (NGC 1326B) is not yet quenched in its outer parts, while the ongoing-stage galaxies mostly have a distributed population of very young stars, though less so in their outer parts. The galaxies in the advanced stage of pre-processing show very low recent sSFR in the outer parts. Our results suggest that NGC 1326B, FCC 35 and FCC 46 underwent significantly different histories from secular evolution during the last Gyr. The fact that most galaxies are on the secular evolution sequence implies that pre-processing has a negligible effect on these galaxies compared to secular evolution. We find EW(H$伪$) to be a useful tool for classifying the stage of pre-processing in group galaxies. The recent sSFR and HI morphology show that galaxies in the Fornax A vicinity are pre-processing from the outside in. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.15624v1-abstract-full').style.display = 'none'; document.getElementById('2311.15624v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.07208">arXiv:2304.07208</a> <span> [<a href="https://arxiv.org/pdf/2304.07208">pdf</a>, <a href="https://arxiv.org/format/2304.07208">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1134">10.1093/mnras/stad1134 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy clusters in the Vela supercluster. -- I. Deep NIR catalogues </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hatamkhani%2C+N">N. Hatamkhani</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Blyth%2C+S+L">S. L. Blyth</a>, <a href="/search/?searchtype=author&query=Said%2C+K">K. Said</a>, <a href="/search/?searchtype=author&query=Elagali%2C+A">A. Elagali</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.07208v1-abstract-short" style="display: inline;"> We present six deep Near-InfraRed (JHK_s) photometric catalogues of galaxies identified in six cluster candidates (VC02, VC04, VC05, VC08, VC10, VC11) within the Vela Supercluster (VSCL) as part of our efforts to learn more about this large supercluster which extends across the zone of avoidance (l=272.5 \pm 20 deg, b= \pm 10 deg, at cz~ 18000 km/s). The observations were conducted with the InfraR… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.07208v1-abstract-full').style.display = 'inline'; document.getElementById('2304.07208v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.07208v1-abstract-full" style="display: none;"> We present six deep Near-InfraRed (JHK_s) photometric catalogues of galaxies identified in six cluster candidates (VC02, VC04, VC05, VC08, VC10, VC11) within the Vela Supercluster (VSCL) as part of our efforts to learn more about this large supercluster which extends across the zone of avoidance (l=272.5 \pm 20 deg, b= \pm 10 deg, at cz~ 18000 km/s). The observations were conducted with the InfraRed Survey Facility (IRSF), a 1.4m telescope situated at the South African Astronomical Observatory (SAAO) in Sutherland. The images in each cluster cover ~ 80% of their respective Abell radii. We identified a total number of 1715 galaxies distributed over the six cluster candidates, of which only ~ 15% were previously known. We study the structures and richnesses of the six clusters out to the cluster-centric completeness radius of r_c<1.5 Mpc and magnitude completeness limit of K_s^0<15.5 mag, using their iso-density contour maps and radial density profiles. The analysis shows VC04 to be the richest of the six. It is a massive cluster comparable to the Coma and Norma clusters, although its velocity dispersion, sigma=455 km/s, seems rather low for a rich cluster. VC02 and VC05 are found to be relatively rich clusters while VC08 is rather poor. Also, VC05 has the highest central number density among the six. VC11 is an intermediate cluster that contains two major subclusters while VC10 has a filament-like structure and is likely not to be a cluster after all. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.07208v1-abstract-full').style.display = 'none'; document.getElementById('2304.07208v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 10 Figures, 13 Tables. Accepted for publication in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS 2023 522 (2): 2223-2240 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.12789">arXiv:2301.12789</a> <span> [<a href="https://arxiv.org/pdf/2301.12789">pdf</a>, <a href="https://arxiv.org/format/2301.12789">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acb048">10.3847/1538-4357/acb048 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A nearby isolated dwarf: star formation and structure of ESO 006-001 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Makarova%2C+L+N">Lidia N. Makarova</a>, <a href="/search/?searchtype=author&query=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/?searchtype=author&query=Lambert%2C+T+S">Trystan S. Lambert</a>, <a href="/search/?searchtype=author&query=Sharina%2C+M+E">Margarita E. Sharina</a>, <a href="/search/?searchtype=author&query=Koribalski%2C+B+S">B盲rbel S. Koribalski</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.12789v1-abstract-short" style="display: inline;"> Observations with the Hubble Space Telescope unexpectedly revealed that the dwarf galaxy ESO 006-001 is a near neighbor to the Local Group at a distance of 2.70 +- 0.11 Mpc. The stellar population in the galaxy is well resolved into individual stars to a limit of M I ~ -0.5 mag. The dominant population is older than 12 Gyr yet displays a significant range in metallicity of -2 < [Fe/H] < -1, as evi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.12789v1-abstract-full').style.display = 'inline'; document.getElementById('2301.12789v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.12789v1-abstract-full" style="display: none;"> Observations with the Hubble Space Telescope unexpectedly revealed that the dwarf galaxy ESO 006-001 is a near neighbor to the Local Group at a distance of 2.70 +- 0.11 Mpc. The stellar population in the galaxy is well resolved into individual stars to a limit of M I ~ -0.5 mag. The dominant population is older than 12 Gyr yet displays a significant range in metallicity of -2 < [Fe/H] < -1, as evidenced by a Red Giant Branch with substantial width. Superimposed on the dominant population are stars on the Main Sequence with ages less than 100 Myr and Helium burning Blue Loop stars with ages of several hundred Myr. ESO 006-001 is an example of a transition dwarf; a galaxy dominated by old stars but one that has experienced limited recent star formation in a swath near the center. No H i gas is detected at the location of the optical galaxy in spite of the evidence for young stars. Intriguingly, an H i cloud with a similar redshift is detected 9 kpc away in projection. Otherwise, ESO 006-001 is a galaxy in isolation with its nearest known neighbor IC 3104, itself a dwarf, at a distance of ~ 500 kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.12789v1-abstract-full').style.display = 'none'; document.getElementById('2301.12789v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 9 figures, accepted at ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.12498">arXiv:2210.12498</a> <span> [<a href="https://arxiv.org/pdf/2210.12498">pdf</a>, <a href="https://arxiv.org/format/2210.12498">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac3246">10.1093/mnras/stac3246 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WALLABY Pre-Pilot and Pilot Survey: the Tully Fisher Relation in Eridanus, Hydra, Norma and NGC4636 fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Courtois%2C+H+M">H茅l猫ne M. Courtois</a>, <a href="/search/?searchtype=author&query=Said%2C+K">Khaled Said</a>, <a href="/search/?searchtype=author&query=Mould%2C+J">Jeremy Mould</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Pomar%C3%A8de%2C+D">Daniel Pomar猫de</a>, <a href="/search/?searchtype=author&query=Westmeier%2C+T">Tobias Westmeier</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Dupuy%2C+A">Alexandra Dupuy</a>, <a href="/search/?searchtype=author&query=Hong%2C+T">Tao Hong</a>, <a href="/search/?searchtype=author&query=Guinet%2C+D">Daniel Guinet</a>, <a href="/search/?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/?searchtype=author&query=Deg%2C+N">Nathan Deg</a>, <a href="/search/?searchtype=author&query=For%2C+B">Bi-Qing For</a>, <a href="/search/?searchtype=author&query=Kleiner%2C+D">Dane Kleiner</a>, <a href="/search/?searchtype=author&query=Koribalski%2C+B">B盲rbel Koribalski</a>, <a href="/search/?searchtype=author&query=Lee-Waddell%2C+K">Karen Lee-Waddell</a>, <a href="/search/?searchtype=author&query=Rhee%2C+J">Jonghwan Rhee</a>, <a href="/search/?searchtype=author&query=Spekkens%2C+K">Kristine Spekkens</a>, <a href="/search/?searchtype=author&query=Wang%2C+J">Jing Wang</a>, <a href="/search/?searchtype=author&query=Wong%2C+O+I">O. I. Wong</a>, <a href="/search/?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/?searchtype=author&query=Bosma%2C+A">Albert Bosma</a>, <a href="/search/?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/?searchtype=author&query=Davis%2C+T">Tamara Davis</a>, <a href="/search/?searchtype=author&query=Holwerda%2C+B">Benne Holwerda</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.12498v1-abstract-short" style="display: inline;"> The WALLABY pilot survey has been conducted using the Australian SKA Pathfinder (ASKAP). The integrated 21-cm HI line spectra are formed in a very different manner compared to usual single-dish spectra Tully-Fisher measurements. It is thus extremely important to ensure that slight differences (e.g. biases due to missing flux) are quantified and understood in order to maximise the use of the large… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12498v1-abstract-full').style.display = 'inline'; document.getElementById('2210.12498v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.12498v1-abstract-full" style="display: none;"> The WALLABY pilot survey has been conducted using the Australian SKA Pathfinder (ASKAP). The integrated 21-cm HI line spectra are formed in a very different manner compared to usual single-dish spectra Tully-Fisher measurements. It is thus extremely important to ensure that slight differences (e.g. biases due to missing flux) are quantified and understood in order to maximise the use of the large amount of data becoming available soon. This article is based on four fields for which the data are scientifically interesting by themselves. The pilot data discussed here consist of 614 galaxy spectra at a rest wavelength of 21cm. Of these spectra, 472 are of high enough quality to be used to potentially derive distances using the Tully-Fisher relation. We further restrict the sample to the 251 galaxies whose inclination is sufficiently close to edge-on. For these, we derive Tully-Fisher distances using the deprojected WALLABY velocity widths combined with infrared (WISE W1) magnitudes. The resulting Tully-Fisher distances for the Eridanus, Hydra, Norma and NGC 4636 clusters are 21.5, 53.5, 69.4 and 23.0 Mpc respectively, with uncertainties of 5--10\%, which are better or equivalent to the ones obtained in studies using data obtained with giant single dish telescopes. The pilot survey data show the benefits of WALLABY over previous giant single-dish telescope surveys. WALLABY is expected to detect around half a million galaxies with a mean redshift of $z = 0.05 (200 Mpc)$. This study suggests that about 200,000 Tully-Fisher distances might result from the survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12498v1-abstract-full').style.display = 'none'; document.getElementById('2210.12498v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 12 Figures, 6 Tables, accepted for publication in the MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.05605">arXiv:2209.05605</a> <span> [<a href="https://arxiv.org/pdf/2209.05605">pdf</a>, <a href="https://arxiv.org/format/2209.05605">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243412">10.1051/0004-6361/202243412 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGC 3314a/b and NGC 3312: Ram pressure stripping in Hydra I Cluster substructure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hess%2C+K+M">Kelley M. Hess</a>, <a href="/search/?searchtype=author&query=Kotulla%2C+R">Ralf Kotulla</a>, <a href="/search/?searchtype=author&query=Chen%2C+H">Hao Chen</a>, <a href="/search/?searchtype=author&query=Carignan%2C+C">Claude Carignan</a>, <a href="/search/?searchtype=author&query=Gallagher%2C+J+S">John S. Gallagher</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.05605v1-abstract-short" style="display: inline;"> Cluster substructure and ram pressure stripping in individual galaxies are among the primary evidence for the ongoing growth of galaxy clusters as they accrete galaxies and groups from their surroundings. We present a multi-wavelength study of the center of the Hydra I galaxy cluster, including exquisite new MeerKAT HI and DECam Halpha imaging which reveal conclusive evidence for ram pressure stri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05605v1-abstract-full').style.display = 'inline'; document.getElementById('2209.05605v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.05605v1-abstract-full" style="display: none;"> Cluster substructure and ram pressure stripping in individual galaxies are among the primary evidence for the ongoing growth of galaxy clusters as they accrete galaxies and groups from their surroundings. We present a multi-wavelength study of the center of the Hydra I galaxy cluster, including exquisite new MeerKAT HI and DECam Halpha imaging which reveal conclusive evidence for ram pressure stripping in NGC 3312, NGC 3314a and NGC 3314b through compressed HI contours, well-defined HI tails, and ongoing star formation in the stripped gas. In particular, we quantify the stripped material in NGC 3312 and NGC 3314a, which makes up between 8% and 35% of the gas still in the disk, is forming stars at ~0.5 M_Sun yr^-1, and extends ~30-60 kpc from the main disk. The estimated stellar mass in the tails is an order of magnitude less than the HI mass. A fourth "ring" galaxy at the same velocity does not show signs of ram pressure in HI. In addition, we use the HI and stellar morphologies, combined with a Beta model of the hot intracluster medium, to constrain the real distances of the galaxies to the cluster center, and we use the chance alignment of NGC 3314b behind NGC 3314a to break the degeneracy between whether the galaxies are in front or in back of the cluster. The drag seen in the HI tails supports our preferred scenario that NGC 3312 and NGC 3314a are moving towards us as part of a foreground substructure which has already passed its pericenter and is on "out fall" from the cluster. The high surviving HI content of the galaxies may suggest that the substructure/intragroup medium can protect them from the harshest effects of ram pressure, or that in fact the galaxies are on more tangential orbits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05605v1-abstract-full').style.display = 'none'; document.getElementById('2209.05605v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 9 figures, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.02523">arXiv:2204.02523</a> <span> [<a href="https://arxiv.org/pdf/2204.02523">pdf</a>, <a href="https://arxiv.org/format/2204.02523">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac63b0">10.3847/2041-8213/ac63b0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LADUMA: Discovery of a luminous OH megamaser at $z > 0.5$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Glowacki%2C+M">Marcin Glowacki</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">Jordan D. Collier</a>, <a href="/search/?searchtype=author&query=Kazemi-Moridani%2C+A">Amir Kazemi-Moridani</a>, <a href="/search/?searchtype=author&query=Frank%2C+B">Bradley Frank</a>, <a href="/search/?searchtype=author&query=Roberts%2C+H">Hayley Roberts</a>, <a href="/search/?searchtype=author&query=Darling%2C+J">Jeremy Darling</a>, <a href="/search/?searchtype=author&query=Kl%C3%B6ckner%2C+H">Hans-Rainer Kl枚ckner</a>, <a href="/search/?searchtype=author&query=Adams%2C+N">Nathan Adams</a>, <a href="/search/?searchtype=author&query=Baker%2C+A+J">Andrew J. Baker</a>, <a href="/search/?searchtype=author&query=Bershady%2C+M">Matthew Bershady</a>, <a href="/search/?searchtype=author&query=Blecher%2C+T">Tariq Blecher</a>, <a href="/search/?searchtype=author&query=Blyth%2C+S">Sarah-Louise Blyth</a>, <a href="/search/?searchtype=author&query=Bowler%2C+R">Rebecca Bowler</a>, <a href="/search/?searchtype=author&query=Catinella%2C+B">Barbara Catinella</a>, <a href="/search/?searchtype=author&query=Chemin%2C+L">Laurent Chemin</a>, <a href="/search/?searchtype=author&query=Crawford%2C+S+M">Steven M. Crawford</a>, <a href="/search/?searchtype=author&query=Cress%2C+C">Catherine Cress</a>, <a href="/search/?searchtype=author&query=Dav%C3%A9%2C+R">Romeel Dav茅</a>, <a href="/search/?searchtype=author&query=Deane%2C+R">Roger Deane</a>, <a href="/search/?searchtype=author&query=de+Blok%2C+E">Erwin de Blok</a>, <a href="/search/?searchtype=author&query=Delhaize%2C+J">Jacinta Delhaize</a>, <a href="/search/?searchtype=author&query=Duncan%2C+K">Kenneth Duncan</a>, <a href="/search/?searchtype=author&query=Elson%2C+E">Ed Elson</a>, <a href="/search/?searchtype=author&query=February%2C+S">Sean February</a>, <a href="/search/?searchtype=author&query=Gawiser%2C+E">Eric Gawiser</a> , et al. (43 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.02523v1-abstract-short" style="display: inline;"> In the local Universe, OH megamasers (OHMs) are detected almost exclusively in infrared-luminous galaxies, with a prevalence that increases with IR luminosity, suggesting that they trace gas-rich galaxy mergers. Given the proximity of the rest frequencies of OH and the hyperfine transition of neutral atomic hydrogen (HI), radio surveys to probe the cosmic evolution of HI in galaxies also offer exc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.02523v1-abstract-full').style.display = 'inline'; document.getElementById('2204.02523v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.02523v1-abstract-full" style="display: none;"> In the local Universe, OH megamasers (OHMs) are detected almost exclusively in infrared-luminous galaxies, with a prevalence that increases with IR luminosity, suggesting that they trace gas-rich galaxy mergers. Given the proximity of the rest frequencies of OH and the hyperfine transition of neutral atomic hydrogen (HI), radio surveys to probe the cosmic evolution of HI in galaxies also offer exciting prospects for exploiting OHMs to probe the cosmic history of gas-rich mergers. Using observations for the Looking At the Distant Universe with the MeerKAT Array (LADUMA) deep HI survey, we report the first untargeted detection of an OHM at $z > 0.5$, LADUMA J033046.20$-$275518.1 (nicknamed "Nkalakatha"). The host system, WISEA J033046.26$-$275518.3, is an infrared-luminous radio galaxy whose optical redshift $z \approx 0.52$ confirms the MeerKAT emission line detection as OH at a redshift $z_{\rm OH} = 0.5225 \pm 0.0001$ rather than HI at lower redshift. The detected spectral line has 18.4$蟽$ peak significance, a width of $459 \pm 59\,{\rm km\,s^{-1}}$, and an integrated luminosity of $(6.31 \pm 0.18\,{\rm [statistical]}\,\pm 0.31\,{\rm [systematic]}) \times 10^3\,L_\odot$, placing it among the most luminous OHMs known. The galaxy's far-infrared luminosity $L_{\rm FIR} = (1.576 \pm 0.013) \times 10^{12}\,L_\odot$ marks it as an ultra-luminous infrared galaxy; its ratio of OH and infrared luminosities is similar to those for lower-redshift OHMs. A comparison between optical and OH redshifts offers a slight indication of an OH outflow. This detection represents the first step towards a systematic exploitation of OHMs as a tracer of galaxy growth at high redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.02523v1-abstract-full').style.display = 'none'; document.getElementById('2204.02523v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures. Accepted to ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.06149">arXiv:2203.06149</a> <span> [<a href="https://arxiv.org/pdf/2203.06149">pdf</a>, <a href="https://arxiv.org/format/2203.06149">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac693">10.1093/mnras/stac693 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MIGHTEE-HI: the HI Size-Mass relation over the last billion years </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">Bradley S. Frank</a>, <a href="/search/?searchtype=author&query=Ponomareva%2C+A+A">Anastasia A. Ponomareva</a>, <a href="/search/?searchtype=author&query=Maddox%2C+N">Natasha Maddox</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Jarvis%2C+M+J">Matt J. Jarvis</a>, <a href="/search/?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/?searchtype=author&query=Oosterloo%2C+T">Tom Oosterloo</a>, <a href="/search/?searchtype=author&query=Baes%2C+M">Maarten Baes</a>, <a href="/search/?searchtype=author&query=Spekkens%2C+K">Kristine Spekkens</a>, <a href="/search/?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/?searchtype=author&query=Glowacki%2C+M">Marcin Glowacki</a>, <a href="/search/?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/?searchtype=author&query=Prandoni%2C+I">Isabella Prandoni</a>, <a href="/search/?searchtype=author&query=Heywood%2C+I">Ian Heywood</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">Jordan D. Collier</a>, <a href="/search/?searchtype=author&query=Sekhar%2C+S">Srikrishna Sekhar</a>, <a href="/search/?searchtype=author&query=Taylor%2C+R">Russ Taylor</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.06149v1-abstract-short" style="display: inline;"> We present the observed HI size-mass relation of $204$ galaxies from the MIGHTEE Survey Early Science data. The high sensitivity of MeerKAT allows us to detect galaxies spanning more than 4 orders of magnitude in HI mass, ranging from dwarf galaxies to massive spirals, and including all morphological types. This is the first time the relation has been explored on a blind homogeneous data set which… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06149v1-abstract-full').style.display = 'inline'; document.getElementById('2203.06149v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.06149v1-abstract-full" style="display: none;"> We present the observed HI size-mass relation of $204$ galaxies from the MIGHTEE Survey Early Science data. The high sensitivity of MeerKAT allows us to detect galaxies spanning more than 4 orders of magnitude in HI mass, ranging from dwarf galaxies to massive spirals, and including all morphological types. This is the first time the relation has been explored on a blind homogeneous data set which extends over a previously unexplored redshift range of $0 < z < 0.084$, i.e. a period of around one billion years in cosmic time. The sample follows the same tight logarithmic relation derived from previous work, between the diameter ($D_{\rm HI}$) and the mass ($M_{\rm HI}$) of HI discs. We measure a slope of $0.501\pm 0.008$, an intercept of $-3.252^{+0.073}_{-0.074}$, and an observed scatter of $0.057$ dex. For the first time, we quantify the intrinsic scatter of $0.054 \pm 0.003$ dex (${\sim} 10 \%$), which provides a constraint for cosmological simulations of galaxy formation and evolution. We derive the relation as a function of galaxy type and find that their intrinsic scatters and slopes are consistent within the errors. We also calculate the $D_{\rm HI} - M_{\rm HI}$ relation for two redshift bins and do not find any evidence for evolution with redshift. These results suggest that over a period of one billion years in lookback time, galaxy discs have not undergone significant evolution in their gas distribution and mean surface mass density, indicating a lack of dependence on both morphological type and redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06149v1-abstract-full').style.display = 'none'; document.getElementById('2203.06149v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 5 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.05673">arXiv:2111.05673</a> <span> [<a href="https://arxiv.org/pdf/2111.05673">pdf</a>, <a href="https://arxiv.org/format/2111.05673">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141488">10.1051/0004-6361/202141488 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Galaxy Cluster Legacy Survey I. Survey Overview and Highlights </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Knowles%2C+K">K. Knowles</a>, <a href="/search/?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/?searchtype=author&query=Goedhart%2C+S">S. Goedhart</a>, <a href="/search/?searchtype=author&query=Deane%2C+R">R. Deane</a>, <a href="/search/?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/?searchtype=author&query=Bietenholz%2C+M+F">M. F. Bietenholz</a>, <a href="/search/?searchtype=author&query=Br%C3%BCggen%2C+M">M. Br眉ggen</a>, <a href="/search/?searchtype=author&query=Button%2C+C">C. Button</a>, <a href="/search/?searchtype=author&query=Chen%2C+H">H. Chen</a>, <a href="/search/?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/?searchtype=author&query=Clarke%2C+T+E">T. E. Clarke</a>, <a href="/search/?searchtype=author&query=de+Gasperin%2C+F">F. de Gasperin</a>, <a href="/search/?searchtype=author&query=Ianjamasimanana%2C+R">R. Ianjamasimanana</a>, <a href="/search/?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/?searchtype=author&query=Hilton%2C+M">M. Hilton</a>, <a href="/search/?searchtype=author&query=Kesebonye%2C+K+C">K. C. Kesebonye</a>, <a href="/search/?searchtype=author&query=Kolokythas%2C+K">K. Kolokythas</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Lawrie%2C+G">G. Lawrie</a>, <a href="/search/?searchtype=author&query=Lochner%2C+M">M. Lochner</a>, <a href="/search/?searchtype=author&query=Loubser%2C+S+I">S. I. Loubser</a>, <a href="/search/?searchtype=author&query=Marchegiani%2C+P">P. Marchegiani</a>, <a href="/search/?searchtype=author&query=Mhlahlo%2C+N">N. Mhlahlo</a> , et al. (126 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.05673v1-abstract-short" style="display: inline;"> MeerKAT's large number of antennas, spanning 8 km with a densely packed 1 km core, create a powerful instrument for wide-area surveys, with high sensitivity over a wide range of angular scales. The MeerKAT Galaxy Cluster Legacy Survey (MGCLS) is a programme of long-track MeerKAT L-band (900-1670 MHz) observations of 115 galaxy clusters, observed for $\sim$6-10 hours each in full polarisation. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05673v1-abstract-full').style.display = 'inline'; document.getElementById('2111.05673v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05673v1-abstract-full" style="display: none;"> MeerKAT's large number of antennas, spanning 8 km with a densely packed 1 km core, create a powerful instrument for wide-area surveys, with high sensitivity over a wide range of angular scales. The MeerKAT Galaxy Cluster Legacy Survey (MGCLS) is a programme of long-track MeerKAT L-band (900-1670 MHz) observations of 115 galaxy clusters, observed for $\sim$6-10 hours each in full polarisation. The first legacy product data release (DR1), made available with this paper, includes the MeerKAT visibilities, basic image cubes at $\sim$8" resolution, and enhanced spectral and polarisation image cubes at $\sim$8" and 15" resolutions. Typical sensitivities for the full-resolution MGCLS image products are $\sim$3-5 渭Jy/beam. The basic cubes are full-field and span 4 deg^2. The enhanced products consist of the inner 1.44 deg^2 field of view, corrected for the primary beam. The survey is fully sensitive to structures up to $\sim$10' scales and the wide bandwidth allows spectral and Faraday rotation mapping. HI mapping at 209 kHz resolution can be done at $0<z<0.09$ and $0.19<z<0.48$. In this paper, we provide an overview of the survey and DR1 products, including caveats for usage. We present some initial results from the survey, both for their intrinsic scientific value and to highlight the capabilities for further exploration with these data. These include a primary beam-corrected compact source catalogue of $\sim$626,000 sources for the full survey, and an optical/infrared cross-matched catalogue for compact sources in Abell 209 and Abell S295. We examine dust unbiased star-formation rates as a function of clustercentric radius in Abell 209 and present a catalogue of 99 diffuse cluster sources (56 are new), some of which have no suitable characterisation. We also highlight some of the radio galaxies which challenge current paradigms and present first results from HI studies of four targets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05673v1-abstract-full').style.display = 'none'; document.getElementById('2111.05673v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">43 pages, 33 figures, 6 tables. Accepted for publication in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.04992">arXiv:2109.04992</a> <span> [<a href="https://arxiv.org/pdf/2109.04992">pdf</a>, <a href="https://arxiv.org/format/2109.04992">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab2654">10.1093/mnras/stab2654 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MIGHTEE-HI: The baryonic Tully-Fisher relation over the last billion years </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ponomareva%2C+A+A">Anastasia A. Ponomareva</a>, <a href="/search/?searchtype=author&query=Mulaudzi%2C+W">Wanga Mulaudzi</a>, <a href="/search/?searchtype=author&query=Maddox%2C+N">Natasha Maddox</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">Bradley S. Frank</a>, <a href="/search/?searchtype=author&query=Jarvis%2C+M+J">Matt J. Jarvis</a>, <a href="/search/?searchtype=author&query=Di+Teodoro%2C+E+M">Enrico M. Di Teodoro</a>, <a href="/search/?searchtype=author&query=Glowacki%2C+M">Marcin Glowacki</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Oosterloo%2C+T+A">Tom A. Oosterloo</a>, <a href="/search/?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/?searchtype=author&query=Pan%2C+H">Hengxing Pan</a>, <a href="/search/?searchtype=author&query=Prandoni%2C+I">Isabella Prandoni</a>, <a href="/search/?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/?searchtype=author&query=Sinigaglia%2C+F">Francesco Sinigaglia</a>, <a href="/search/?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/?searchtype=author&query=Heywood%2C+I">Ian Heywood</a>, <a href="/search/?searchtype=author&query=Bowler%2C+R+A+A">Rebecca A. A. Bowler</a>, <a href="/search/?searchtype=author&query=Hatfield%2C+P+W">Peter W. Hatfield</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">Jordan D. Collier</a>, <a href="/search/?searchtype=author&query=Sekhar%2C+S">Srikrishna Sekhar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.04992v1-abstract-short" style="display: inline;"> Using a sample of 67 galaxies from the MIGHTEE Survey Early Science data we study the HI-based baryonic Tully-Fisher relation (bTFr), covering a period of $\sim$one billion years ($0 \leq z \leq 0.081 $). We consider the bTFr based on two different rotational velocity measures: the width of the global HI profile and $\rm V_{out}$, measured as the outermost rotational velocity from the resolved HI… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.04992v1-abstract-full').style.display = 'inline'; document.getElementById('2109.04992v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.04992v1-abstract-full" style="display: none;"> Using a sample of 67 galaxies from the MIGHTEE Survey Early Science data we study the HI-based baryonic Tully-Fisher relation (bTFr), covering a period of $\sim$one billion years ($0 \leq z \leq 0.081 $). We consider the bTFr based on two different rotational velocity measures: the width of the global HI profile and $\rm V_{out}$, measured as the outermost rotational velocity from the resolved HI rotation curves. Both relations exhibit very low intrinsic scatter orthogonal to the best-fit relation ($蟽_{\perp}=0.07\pm0.01$), comparable to the SPARC sample at $z \simeq 0$. The slopes of the relations are similar and consistent with the $ z \simeq 0$ studies ($3.66^{+0.35}_{-0.29}$ for $\rm W_{50}$ and $3.47^{+0.37}_{-0.30}$ for $\rm V_{out}$). We find no evidence that the bTFr has evolved over the last billion years, and all galaxies in our sample are consistent with the same relation independent of redshift and the rotational velocity measure. Our results set up a reference for all future studies of the HI-based bTFr as a function of redshift that will be conducted with the ongoing deep SKA pathfinders surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.04992v1-abstract-full').style.display = 'none'; document.getElementById('2109.04992v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.12244">arXiv:2102.12244</a> <span> [<a href="https://arxiv.org/pdf/2102.12244">pdf</a>, <a href="https://arxiv.org/ps/2102.12244">ps</a>, <a href="https://arxiv.org/format/2102.12244">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab569">10.1093/mnras/stab569 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A comparative analysis of Galactic extinction at low Galactic latitudes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schr%C3%B6der%2C+A+C">A. C. Schr枚der</a>, <a href="/search/?searchtype=author&query=van+Driel%2C+W">W. van Driel</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.12244v1-abstract-short" style="display: inline;"> We use near-infrared (J-K)-colours of bright 2MASS galaxies, measured within a 7"-radius aperture, to calibrate the Schlegel et al. (1998) DIRBE/IRAS Galactic extinction map at low Galactic latitudes ($|b| < 10^{\rm o}$). Using 3460 galaxies covering a large range in extinction (up to $A_K$ = 1.15 or E(B-V) ~ 3.19), we derive a correction factor $f = 0.83 \pm 0.01$ by fitting a linear regression t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.12244v1-abstract-full').style.display = 'inline'; document.getElementById('2102.12244v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.12244v1-abstract-full" style="display: none;"> We use near-infrared (J-K)-colours of bright 2MASS galaxies, measured within a 7"-radius aperture, to calibrate the Schlegel et al. (1998) DIRBE/IRAS Galactic extinction map at low Galactic latitudes ($|b| < 10^{\rm o}$). Using 3460 galaxies covering a large range in extinction (up to $A_K$ = 1.15 or E(B-V) ~ 3.19), we derive a correction factor $f = 0.83 \pm 0.01$ by fitting a linear regression to the colour-extinction relation, confirming that the Schlegel et al. maps overestimate the extinction. We argue that the use of only a small range in extinction (e.g., $A_K$ < 0.4) increases the uncertainty in the correction factor and may overestimate it. Our data confirms the Fitzpatrick (1999) extinction law for the J- and K-band. We also tested four all-sky extinction maps based on Planck satellite data. All maps require a correction factor as well. In three cases the application of the respective extinction correction to the galaxy colours results in a reduced scatter in the colour-extinction relation, indicating a more reliable extinction correction. Finally, the large galaxy sample allows an analysis of the calibration of the extinction maps as a function of Galactic longitude and latitude. For all but one extinction map we find a marked offset between the Galactic Centre and Anticentre region, but not with the dipole of the Cosmic Microwave Background. Based on our analysis, we recommend the use of the GNILC extinction map by Planck Collaboration (2016b) with a correction factor $f = 0.86 \pm 0.01$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.12244v1-abstract-full').style.display = 'none'; document.getElementById('2102.12244v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 14 figures, accepted by MNRAS; online material available through MNRAS, CDS or by request from the main author</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.09470">arXiv:2011.09470</a> <span> [<a href="https://arxiv.org/pdf/2011.09470">pdf</a>, <a href="https://arxiv.org/ps/2011.09470">ps</a>, <a href="https://arxiv.org/format/2011.09470">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039655">10.1051/0004-6361/202039655 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MIGHTEE-HI: The HI emission project of the MeerKAT MIGHTEE survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Maddox%2C+N">Natasha Maddox</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">Bradley S. Frank</a>, <a href="/search/?searchtype=author&query=Ponomareva%2C+A+A">A. A. Ponomareva</a>, <a href="/search/?searchtype=author&query=Jarvis%2C+M+J">M. J. Jarvis</a>, <a href="/search/?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/?searchtype=author&query=Dav%C3%A9%2C+R">R. Dav茅</a>, <a href="/search/?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/?searchtype=author&query=Santos%2C+M+G">M. G. Santos</a>, <a href="/search/?searchtype=author&query=Blyth%2C+S+L">S. L. Blyth</a>, <a href="/search/?searchtype=author&query=Glowacki%2C+M">M. Glowacki</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Mulaudzi%2C+W">W. Mulaudzi</a>, <a href="/search/?searchtype=author&query=Namumba%2C+B">B. Namumba</a>, <a href="/search/?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/?searchtype=author&query=Rajohnson%2C+S+H+A">S. H. A. Rajohnson</a>, <a href="/search/?searchtype=author&query=Spekkens%2C+K">K. Spekkens</a>, <a href="/search/?searchtype=author&query=Adams%2C+N+J">N. J. Adams</a>, <a href="/search/?searchtype=author&query=Bowler%2C+R+A+A">R. A. A. Bowler</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/?searchtype=author&query=Sekhar%2C+S">S. Sekhar</a>, <a href="/search/?searchtype=author&query=Taylor%2C+A+R">A. R. Taylor</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.09470v1-abstract-short" style="display: inline;"> We present the HI emission project within the MIGHTEE survey, currently being carried out with the newly commissioned MeerKAT radio telescope. This is one of the first deep, blind, medium-wide interferometric surveys for neutral hydrogen (HI) ever undertaken, extending our knowledge of HI emission to z=0.6. The science goals of this medium-deep, medium-wide survey are extensive, including the evol… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.09470v1-abstract-full').style.display = 'inline'; document.getElementById('2011.09470v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.09470v1-abstract-full" style="display: none;"> We present the HI emission project within the MIGHTEE survey, currently being carried out with the newly commissioned MeerKAT radio telescope. This is one of the first deep, blind, medium-wide interferometric surveys for neutral hydrogen (HI) ever undertaken, extending our knowledge of HI emission to z=0.6. The science goals of this medium-deep, medium-wide survey are extensive, including the evolution of the neutral gas content of galaxies over the past 5 billion years. Simulations predict nearly 3000 galaxies over 0<z<0.4 will be detected directly in HI, with statistical detections extending to z=0.6. The survey allows us to explore HI as a function of galaxy environment, with massive groups and galaxy clusters within the survey volume. Additionally, the area is large enough to contain as many as 50 local galaxies with HI mass $<10^8$ Msun, which allows us to study the low-mass galaxy population. The 20 deg$^2$ main survey area is centred on fields with exceptional multi-wavelength ancillary data, with photometry ranging from optical through far-infrared wavelengths, supplemented with multiple spectroscopic campaigns. We describe here the survey design and the key science goals. We also show first results from the Early Science observations, including kinematic modelling of individual sources, along with the redshift, HI, and stellar mass ranges of the sample to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.09470v1-abstract-full').style.display = 'none'; document.getElementById('2011.09470v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 9 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 646, A35 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.03749">arXiv:2009.03749</a> <span> [<a href="https://arxiv.org/pdf/2009.03749">pdf</a>, <a href="https://arxiv.org/format/2009.03749">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038342">10.1051/0004-6361/202038342 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A near-infrared study of the obscured 3C129 galaxy cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/?searchtype=author&query=Verheijen%2C+M+A+W">M. A. W Verheijen</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Said%2C+K">K. Said</a>, <a href="/search/?searchtype=author&query=Schr%C3%B6der%2C+A+C">A. C. Schr枚der</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.03749v1-abstract-short" style="display: inline;"> We present a catalogue of 261 new infrared selected members of the 3C129 galaxy cluster. The cluster, located at $z \approx$ 0.02, forms part of the Perseus-Pisces filament and is obscured at optical wavelengths due to its location in the zone of avoidance. We identified these galaxies using the $J-$ and $K-$band imaging data provided by the UKIDSS Galactic Plane Survey within an area with a radiu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.03749v1-abstract-full').style.display = 'inline'; document.getElementById('2009.03749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.03749v1-abstract-full" style="display: none;"> We present a catalogue of 261 new infrared selected members of the 3C129 galaxy cluster. The cluster, located at $z \approx$ 0.02, forms part of the Perseus-Pisces filament and is obscured at optical wavelengths due to its location in the zone of avoidance. We identified these galaxies using the $J-$ and $K-$band imaging data provided by the UKIDSS Galactic Plane Survey within an area with a radius of $1.1^{\circ}$ centred on the X-ray emission of the cluster at $\ell, b \approx 160.52^{\circ}, 0.27^{\circ}$. A total of 26 of the identified galaxy members have known redshifts 24 of which are from our 2016 Westerbork HI survey and two are from optical spectroscopy. An analysis of the galaxy density at the core of the 3C129 cluster shows it to be less dense than the Coma and Norma clusters, but comparable to the galaxy density in the core of the Perseus cluster. From an assessment of the spatial and velocity distributions of the 3C129 cluster galaxies that have redshifts, we derived a velocity of $cz = 5227 \pm 171$ km/s and $蟽= 1097 \pm 252$ km/s for the main cluster, with a substructure in the cluster outskirts at $cz = 6923 \pm 71$ km/s with $蟽= 422 \pm 100$ km/s. The presence of this substructure is consistent with previous claims based on the X-ray analysis that the cluster is not yet virialised and may have undergone a recent merger. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.03749v1-abstract-full').style.display = 'none'; document.getElementById('2009.03749v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 16 figures, includes an appendix, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.00581">arXiv:2007.00581</a> <span> [<a href="https://arxiv.org/pdf/2007.00581">pdf</a>, <a href="https://arxiv.org/format/2007.00581">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa1946">10.1093/mnras/staa1946 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 2MASS redshift survey galaxy group catalogue derived from a graph-theory based friends-of-friends algorithm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lambert%2C+T+S">T. S. Lambert</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Macri%2C+L+M">L. M. Macri</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.00581v1-abstract-short" style="display: inline;"> We present the galaxy group catalogue for the recently-completed 2MASS Redshift Survey (2MRS, Macri2019) which consists of 44572 redshifts, including 1041 new measurements for galaxies mostly located within the Zone of Avoidance. The galaxy group catalogue is generated by using a novel, graph-theory based, modified version of the Friends-of-Friends algorithm. Several graph-theory examples are pres… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.00581v1-abstract-full').style.display = 'inline'; document.getElementById('2007.00581v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.00581v1-abstract-full" style="display: none;"> We present the galaxy group catalogue for the recently-completed 2MASS Redshift Survey (2MRS, Macri2019) which consists of 44572 redshifts, including 1041 new measurements for galaxies mostly located within the Zone of Avoidance. The galaxy group catalogue is generated by using a novel, graph-theory based, modified version of the Friends-of-Friends algorithm. Several graph-theory examples are presented throughout this paper, including a new method for identifying substructures within groups. The results and graph-theory methods have been thoroughly interrogated against previous 2MRS group catalogues and a Theoretical Astrophysical Observatory (TAO) mock by making use of cutting-edge visualization techniques including immersive facilities, a digital planetarium, and virtual reality. This has resulted in a stable and robust catalogue with on-sky positions and line-of-sight distances within 0.5 Mpc and 2 Mpc, respectively, and has recovered all major groups and clusters. The final catalogue consists of 3022 groups, resulting in the most complete "whole-sky" galaxy group catalogue to date. We determine the 3D positions of these groups, as well as their luminosity and comoving distances, observed and corrected number of members, richness metric, velocity dispersion, and estimates of $R_{200}$ and $M_{200}$. We present three additional data products, i.e. the 2MRS galaxies found in groups, a catalogue of subgroups, and a catalogue of 687 new group candidates with no counterparts in previous 2MRS-based analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.00581v1-abstract-full').style.display = 'none'; document.getElementById('2007.00581v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 15 figures; accepted for publication in MNRAS; high quality PDF and python code available at https://github.com/BrutishGuy/pyfriends</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.06178">arXiv:2005.06178</a> <span> [<a href="https://arxiv.org/pdf/2005.06178">pdf</a>, <a href="https://arxiv.org/format/2005.06178">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa1333">10.1093/mnras/staa1333 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The optical polarization of the blazar PKS 2155$-$304 during an optical flare in 2010 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Peceur%2C+N+W">N. W. Peceur</a>, <a href="/search/?searchtype=author&query=Taylor%2C+A+R">A. R. Taylor</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.06178v3-abstract-short" style="display: inline;"> An analysis is presented of the optical polarimetric and multicolour photometric ($BVRJ$) behaviour of the blazar PKS 2155$-$304 during an outburst in 2010. This flare develops over roughly 117 days, with a flux doubling time $蟿\sim 11$ days that increases from blue to red wavelengths. The polarization angle is initially aligned with the jet axis but rotates by roughly $90^\circ$ as the flare grow… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.06178v3-abstract-full').style.display = 'inline'; document.getElementById('2005.06178v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.06178v3-abstract-full" style="display: none;"> An analysis is presented of the optical polarimetric and multicolour photometric ($BVRJ$) behaviour of the blazar PKS 2155$-$304 during an outburst in 2010. This flare develops over roughly 117 days, with a flux doubling time $蟿\sim 11$ days that increases from blue to red wavelengths. The polarization angle is initially aligned with the jet axis but rotates by roughly $90^\circ$ as the flare grows. Two distinct states are evident at low and high fluxes. Below 18 mJy, the polarization angle takes on a wide range of values, without any clear relation to the flux. In contrast, there is a positive correlation between the polarization angle and flux above 18 mJy. The polarization degree does not display a clear correlation with the flux. We find that the photopolarimetric behaviour for the high flux state can be attributed to a variable component with a steady power-law spectral energy distribution and high optical polarization degree (13.3%). These properties are interpreted within the shock-in-jet model, which shows that the observed variability can be explained by a shock that is seen nearly edge-on. Some parameters derived for the relativistic jet within the shock-in-jet model are: $B=0.06$ G for the magnetic field, $未=22.3$ for the Doppler factor and $桅=2.6^\circ$ for the viewing angle. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.06178v3-abstract-full').style.display = 'none'; document.getElementById('2005.06178v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.07311">arXiv:2002.07311</a> <span> [<a href="https://arxiv.org/pdf/2002.07311">pdf</a>, <a href="https://arxiv.org/format/2002.07311">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10509-020-03831-4">10.1007/s10509-020-03831-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WALLABY -- An SKA Pathfinder HI Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">L. Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Westmeier%2C+T">T. Westmeier</a>, <a href="/search/?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/?searchtype=author&query=Spekkens%2C+K">K. Spekkens</a>, <a href="/search/?searchtype=author&query=Wong%2C+O+I">O. I. Wong</a>, <a href="/search/?searchtype=author&query=Lagos%2C+C+D+P">C. D. P. Lagos</a>, <a href="/search/?searchtype=author&query=Obreschkow%2C+D">D. Obreschkow</a>, <a href="/search/?searchtype=author&query=Ryan-Weber%2C+E+V">E. V. Ryan-Weber</a>, <a href="/search/?searchtype=author&query=Zwaan%2C+M">M. Zwaan</a>, <a href="/search/?searchtype=author&query=Kilborn%2C+V">V. Kilborn</a>, <a href="/search/?searchtype=author&query=Bekiaris%2C+G">G. Bekiaris</a>, <a href="/search/?searchtype=author&query=Bekki%2C+K">K. Bekki</a>, <a href="/search/?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/?searchtype=author&query=Boselli%2C+A">A. Boselli</a>, <a href="/search/?searchtype=author&query=Bosma%2C+A">A. Bosma</a>, <a href="/search/?searchtype=author&query=Catinella%2C+B">B. Catinella</a>, <a href="/search/?searchtype=author&query=Chauhan%2C+G">G. Chauhan</a>, <a href="/search/?searchtype=author&query=Cluver%2C+M+E">M. E. Cluver</a>, <a href="/search/?searchtype=author&query=Colless%2C+M">M. Colless</a>, <a href="/search/?searchtype=author&query=Courtois%2C+H+M">H. M. Courtois</a>, <a href="/search/?searchtype=author&query=Crain%2C+R+A">R. A. Crain</a>, <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/?searchtype=author&query=Duffy%2C+A+R">A. R. Duffy</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.07311v2-abstract-short" style="display: inline;"> The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (HI) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 x 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radio-quiet zone in Western A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.07311v2-abstract-full').style.display = 'inline'; document.getElementById('2002.07311v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.07311v2-abstract-full" style="display: none;"> The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (HI) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 x 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radio-quiet zone in Western Australia. WALLABY aims to survey three-quarters of the sky (-90 degr < Dec < +30 degr) to a redshift of z < 0.26, and generate spectral line image cubes at ~30 arcsec resolution and ~1.6 mJy/beam per 4 km/s channel sensitivity. ASKAP's instantaneous field of view at 1.4 GHz, delivered by the PAF's 36 beams, is about 30 sq deg. At an integrated signal-to-noise ratio of five, WALLABY is expected to detect over half a million galaxies with a mean redshift of z ~ 0.05 (~200 Mpc). The scientific goals of WALLABY include: (a) a census of gas-rich galaxies in the vicinity of the Local Group; (b) a study of the HI properties of galaxies, groups and clusters, in particular the influence of the environment on galaxy evolution; and (c) the refinement of cosmological parameters using the spatial and redshift distribution of low-bias gas-rich galaxies. For context we provide an overview of previous large-scale HI surveys. Combined with existing and new multi-wavelength sky surveys, WALLABY will enable an exciting new generation of panchromatic studies of the Local Universe. - First results from the WALLABY pilot survey are revealed, with initial data products publicly available in the CSIRO ASKAP Science Data Archive (CASDA). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.07311v2-abstract-full').style.display = 'none'; document.getElementById('2002.07311v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApSS (38 pages, 14 figures), see also https://www.atnf.csiro.au/research/WALLABY/ - Contact email: Baerbel.Koribalski@csiro.au</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Ap&SS 365, 118 (2020) - https://rdcu.be/b5Bfg </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.08875">arXiv:1909.08875</a> <span> [<a href="https://arxiv.org/pdf/1909.08875">pdf</a>, <a href="https://arxiv.org/format/1909.08875">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnrasl/slz146">10.1093/mnrasl/slz146 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A kinematic confirmation of the hidden Vela supercluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Courtois%2C+H+M">Helene M. Courtois</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Renee. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Dupuy%2C+A">Alexandra Dupuy</a>, <a href="/search/?searchtype=author&query=Graziani%2C+R">Romain Graziani</a>, <a href="/search/?searchtype=author&query=Libeskind%2C+N+I">Noam I Libeskind</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.08875v1-abstract-short" style="display: inline;"> The universe region obscured by the Milky Way is very large and only future blind large HI redshift, and targeted peculiar surveys on the outer borders will determine how much mass is hidden there. Meanwhile, we apply for the first time two independent techniques to the galaxy peculiar velocity catalog $CosmicFlows-3$ in order to explore for the kinematic signature of a specific large-scale struct… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.08875v1-abstract-full').style.display = 'inline'; document.getElementById('1909.08875v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.08875v1-abstract-full" style="display: none;"> The universe region obscured by the Milky Way is very large and only future blind large HI redshift, and targeted peculiar surveys on the outer borders will determine how much mass is hidden there. Meanwhile, we apply for the first time two independent techniques to the galaxy peculiar velocity catalog $CosmicFlows-3$ in order to explore for the kinematic signature of a specific large-scale structure hidden behind this zone : the Vela supercluster at cz $\sim 18,000$,km s$^{-1}$ . Using the gravitational velocity and density contrast fields, we find excellent agreement when comparing our results to the Vela object as traced in redshift space. The article provides the first kinematic evidence of a major mass concentration (knot of the Cosmic Web) located in the direction behind Vela constellation, pin-pointing that the Zone of Avoidance should be surveyed in detail in the future . <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.08875v1-abstract-full').style.display = 'none'; document.getElementById('1909.08875v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 3 figures, accepted in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.01581">arXiv:1904.01581</a> <span> [<a href="https://arxiv.org/pdf/1904.01581">pdf</a>, <a href="https://arxiv.org/ps/1904.01581">ps</a>, <a href="https://arxiv.org/format/1904.01581">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz956">10.1093/mnras/stz956 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The HI mass function in the Parkes HI Zone of Avoidance survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Said%2C+K">Khaled Said</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.01581v1-abstract-short" style="display: inline;"> An HI mass function (HIMF) was derived for 751 galaxies selected from the deep Parkes HI survey across the Zone of Avoidance (HIZOA). HIZOA contains both the Great Attractor Wall and the Local Void, two of the most extreme environments in the local Universe, making the sample eminently suitable to explore the overall HIMF as well as its dependence on local environment. To avoid any selection bias… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01581v1-abstract-full').style.display = 'inline'; document.getElementById('1904.01581v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.01581v1-abstract-full" style="display: none;"> An HI mass function (HIMF) was derived for 751 galaxies selected from the deep Parkes HI survey across the Zone of Avoidance (HIZOA). HIZOA contains both the Great Attractor Wall and the Local Void, two of the most extreme environments in the local Universe, making the sample eminently suitable to explore the overall HIMF as well as its dependence on local environment. To avoid any selection bias because of the different distances of these large-scale structures, we first used the two-dimensional stepwise maximum-likelihood method for the definition of an average HIMF. The resulting parameters of a Schechter-type HIMF for the whole sample are $伪= -1.33\pm0.05$, $\log(M_{\rm HI}^*/M_{\odot})=9.93\pm0.04$, and $蠁^* = (3.9\pm0.6)\times 10^{-3}$ Mpc$^{-3}$. We then used the $k$-th nearest-neighbour method to subdivide the sample into four environments of decreasing local density and derived the Schechter parameters for each subsample. A strong trend is observed, for the slope $伪$ of the low-mass end of the HIMF. The slope changes from being nearly flat, i.e. $伪= -0.99\pm0.19$ for galaxies residing in the densest bin, to the steep value of $伪= -1.31\pm0.10$ in the lowest density bin. The characteristic mass, however, does not show a clear trend between the highest and lowest density bins. We find similar trends in the low-mass slope when we compare the results for a region dominated by the Great Attractor, and the Local Void, which are found to be over-, respectively underdense by 1.35 and 0.59 compared to the whole sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01581v1-abstract-full').style.display = 'none'; document.getElementById('1904.01581v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 13 figures, 4 tables, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.02773">arXiv:1811.02773</a> <span> [<a href="https://arxiv.org/pdf/1811.02773">pdf</a>, <a href="https://arxiv.org/ps/1811.02773">ps</a>, <a href="https://arxiv.org/format/1811.02773">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/sty3022">10.1093/mnras/sty3022 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Zone of Avoidance catalogue of 2MASS bright galaxies. I. Sample description and analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schr%C3%B6der%2C+A+C">Anja C. Schr枚der</a>, <a href="/search/?searchtype=author&query=van+Driel%2C+W">Wim van Driel</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Renee C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1811.02773v1-abstract-short" style="display: inline;"> We present a homogeneous 2MASS bright galaxy catalogue at low Galactic latitudes ($|b| \le 10.0^{\rm o}$, called Zone of Avoidance) which is complete to a Galactic extinction-corrected magnitude of $K^o_s \le 11.25^{\rm m}$. It also includes galaxies in regions of high foreground extinctions ($E(B-V) > 0.95^{\rm m}$) situated at higher latitudes. This catalogue forms the basis of studies of large-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.02773v1-abstract-full').style.display = 'inline'; document.getElementById('1811.02773v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.02773v1-abstract-full" style="display: none;"> We present a homogeneous 2MASS bright galaxy catalogue at low Galactic latitudes ($|b| \le 10.0^{\rm o}$, called Zone of Avoidance) which is complete to a Galactic extinction-corrected magnitude of $K^o_s \le 11.25^{\rm m}$. It also includes galaxies in regions of high foreground extinctions ($E(B-V) > 0.95^{\rm m}$) situated at higher latitudes. This catalogue forms the basis of studies of large-scale structures, flow fields and extinction across the ZoA and complements the ongoing 2MASS Redshift and Tully-Fisher surveys. It comprises 3763 galaxies, 70% of which have at least one radial velocity measurement in the literature. The catalogue is complete up to star density levels of $\log N_*/{\rm deg}^2 <4.5$ and at least for $A_K < 0.6^{\rm m}$ and likely as high as $A_K = 20^{\rm m}$. Thus the ZoA in terms of bright NIR galaxies covers only $2.5-4$% of the whole sky. We use a diameter-dependent extinction correction to compare our sample with an unobscured, high-latitude sample. While the correction to the $K_s$ -band magnitude is sufficient, the corrected diameters are too small by about $4''$ on average. The omission of applying such a diameter-dependent extinction correction may lead to a biased flow field even at intermediate extinction values as found in the 2MRS survey. A slight dependence of galaxy colour with stellar density indicates that unsubtracted foreground stars make galaxies appear bluer. Furthermore, far-infrared sources in the DIRBE/IRAS extinction maps that were not removed at low latitudes affect the foreground extinction corrections of three galaxies and may weakly affect a further estimated $\approx 20$% of our galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.02773v1-abstract-full').style.display = 'none'; document.getElementById('1811.02773v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 16 figures; accepted for publication in MNRAS; full catalogue available as ancillary file in sourcefile package</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.05985">arXiv:1808.05985</a> <span> [<a href="https://arxiv.org/pdf/1808.05985">pdf</a>, <a href="https://arxiv.org/ps/1808.05985">ps</a>, <a href="https://arxiv.org/format/1808.05985">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/sty2285">10.1093/mnras/sty2285 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Nancay HI Zone of Avoidance survey of 2MASS bright galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=van+Driel%2C+W">Wim van Driel</a>, <a href="/search/?searchtype=author&query=Schr%C3%B6der%2C+A+C">Anja C. Schr枚der</a>, <a href="/search/?searchtype=author&query=Ramatsoku%2C+M">Mpati Ramatsoku</a>, <a href="/search/?searchtype=author&query=Henning%2C+P+A">Patricia A. Henning</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1808.05985v1-abstract-short" style="display: inline;"> To complement the 2MASS Redshift Survey (2MRS) and the 2MASS Tully-Fisher survey (2MTF) a search for 21cm HI line emission of 2MASS bright galaxy candidates has been pursued along the dust-obscured plane of the Milky Way with the 100m Nancay Radio Telescope. For our sample selection we adopted an isophotal extinction-corrected K-band magnitude limit of $K_s^o = 11.25$mag, corresponding to the firs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05985v1-abstract-full').style.display = 'inline'; document.getElementById('1808.05985v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.05985v1-abstract-full" style="display: none;"> To complement the 2MASS Redshift Survey (2MRS) and the 2MASS Tully-Fisher survey (2MTF) a search for 21cm HI line emission of 2MASS bright galaxy candidates has been pursued along the dust-obscured plane of the Milky Way with the 100m Nancay Radio Telescope. For our sample selection we adopted an isophotal extinction-corrected K-band magnitude limit of $K_s^o = 11.25$mag, corresponding to the first 2MRS data release and 2MTF, for which the 2MASX completeness level remains fairly constant deep into the Zone of Avoidance (ZoA). About one thousand galaxies without prior redshift measurement accessible from Nancay (Dec > -40掳) were observed to an rms noise level of ~3 mJy for the velocity range -250 to 10'600 km/s. This resulted in 220 clear and 12 marginal detections of the target sample. Only few detections have redshifts above 8000 km/s due to recurring radio frequency interference (RFI). A further 29 detections and 6 marginals have their origin in non-target galaxies in the telescope beam. The newly detected galaxies are on average considerably more \HI-rich (mostly $10^9 - 10^{10}$M$_\odot$) compared to systematic (blind) HI surveys. The HI detections reveal various new filaments crossing the mostly uncharted northern ZoA (e.g. at $\ell \sim 90掳, 130掳, 160掳$), whilst consolidating galaxy agglomerations in Monoceros and Puppis ($\ell \sim 220掳, 240掳$). Considerably new insight has been gained about the extent of the Perseus-Pisces Supercluster through the confirmation of a ridge ($\ell \sim 160掳$) encompassing the 3C129 cluster that links Perseus-Pisces to Lynx, and the continuation of the second Perseus-Pisces arm ($\ell \sim 90掳$) across the ZoA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05985v1-abstract-full').style.display = 'none'; document.getElementById('1808.05985v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 11 figures, 7 tables; accepted for publication in MNRAS; supplementary material available at http://www.acgc.uct.ac.za/~kraan/NRT_ZOA/Supplement.pdf</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.08458">arXiv:1709.08458</a> <span> [<a href="https://arxiv.org/pdf/1709.08458">pdf</a>, <a href="https://arxiv.org/format/1709.08458">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> An Overview of the MHONGOOSE Survey: Observing Nearby Galaxies with MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/?searchtype=author&query=Amram%2C+P">P. Amram</a>, <a href="/search/?searchtype=author&query=Athanassoula%2C+E">E. Athanassoula</a>, <a href="/search/?searchtype=author&query=Bagetakos%2C+I">I. Bagetakos</a>, <a href="/search/?searchtype=author&query=Balkowski%2C+C">C. Balkowski</a>, <a href="/search/?searchtype=author&query=Bershady%2C+M+A">M. A. Bershady</a>, <a href="/search/?searchtype=author&query=Beswick%2C+R">R. Beswick</a>, <a href="/search/?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/?searchtype=author&query=Blyth%2C+S+-">S. -L. Blyth</a>, <a href="/search/?searchtype=author&query=Bosma%2C+A">A. Bosma</a>, <a href="/search/?searchtype=author&query=Booth%2C+R+S">R. S. Booth</a>, <a href="/search/?searchtype=author&query=Bouchard%2C+A">A. Bouchard</a>, <a href="/search/?searchtype=author&query=Brinks%2C+E">E. Brinks</a>, <a href="/search/?searchtype=author&query=Carignan%2C+C">C. Carignan</a>, <a href="/search/?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/?searchtype=author&query=Conway%2C+J">J. Conway</a>, <a href="/search/?searchtype=author&query=Elson%2C+E+C">E. C. Elson</a>, <a href="/search/?searchtype=author&query=English%2C+J">J. English</a>, <a href="/search/?searchtype=author&query=Epinat%2C+B">B. Epinat</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/?searchtype=author&query=Fiege%2C+J">J. Fiege</a>, <a href="/search/?searchtype=author&query=Fraternali%2C+F">F. Fraternali</a>, <a href="/search/?searchtype=author&query=Gallagher%2C+J+S">J. S. Gallagher</a> , et al. (43 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1709.08458v1-abstract-short" style="display: inline;"> MHONGOOSE is a deep survey of the neutral hydrogen distribution in a representative sample of 30 nearby disk and dwarf galaxies with HI masses from 10^6 to ~10^{11} M_sun, and luminosities from M_R ~ -12 to M_R ~ -22. The sample is selected to uniformly cover the available range in log(M_HI). Our extremely deep observations, down to HI column density limits of well below 10^{18} cm^{-2} - or a few… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.08458v1-abstract-full').style.display = 'inline'; document.getElementById('1709.08458v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.08458v1-abstract-full" style="display: none;"> MHONGOOSE is a deep survey of the neutral hydrogen distribution in a representative sample of 30 nearby disk and dwarf galaxies with HI masses from 10^6 to ~10^{11} M_sun, and luminosities from M_R ~ -12 to M_R ~ -22. The sample is selected to uniformly cover the available range in log(M_HI). Our extremely deep observations, down to HI column density limits of well below 10^{18} cm^{-2} - or a few hundred times fainter than the typical HI disks in galaxies - will directly detect the effects of cold accretion from the intergalactic medium and the links with the cosmic web. These observations will be the first ever to probe the very low-column density neutral gas in galaxies at these high resolutions. Combination with data at other wavelengths, most of it already available, will enable accurate modelling of the properties and evolution of the mass components in these galaxies and link these with the effects of environment, dark matter distribution, and other fundamental properties such as halo mass and angular momentum. MHONGOOSE can already start addressing some of the SKA-1 science goals and will provide a comprehensive inventory of the processes driving the transformation and evolution of galaxies in the nearby universe at high resolution and over 5 orders of magnitude in column density. It will be a Nearby Galaxies Legacy Survey that will be unsurpassed until the advent of the SKA, and can serve as a highly visible, lasting statement of MeerKAT's capabilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.08458v1-abstract-full').style.display = 'none'; document.getElementById('1709.08458v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To be published in "MeerKAT Science: On the Pathway to the SKA". Proceedings of Science. Workshop held 25-27 May, 2016 Stellenbosch, South Africa</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.01289">arXiv:1709.01289</a> <span> [<a href="https://arxiv.org/pdf/1709.01289">pdf</a>, <a href="https://arxiv.org/format/1709.01289">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Fornax Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/?searchtype=author&query=Bryan%2C+G+L">G. L. Bryan</a>, <a href="/search/?searchtype=author&query=Colafrancesco%2C+S">S. Colafrancesco</a>, <a href="/search/?searchtype=author&query=Dettmar%2C+R+-">R. -J. Dettmar</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/?searchtype=author&query=Govoni%2C+F">F. Govoni</a>, <a href="/search/?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Loubser%2C+S+I">S. I. Loubser</a>, <a href="/search/?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/?searchtype=author&query=Murgia%2C+M">M. Murgia</a>, <a href="/search/?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/?searchtype=author&query=Peletier%2C+R+F">R. F. Peletier</a>, <a href="/search/?searchtype=author&query=Pizzo%2C+R">R. Pizzo</a>, <a href="/search/?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/?searchtype=author&query=Richter%2C+L">L. Richter</a>, <a href="/search/?searchtype=author&query=Smith%2C+M+W+L">M. W. L. Smith</a>, <a href="/search/?searchtype=author&query=Trager%2C+S+C">S. C. Trager</a>, <a href="/search/?searchtype=author&query=van+Gorkom%2C+J+H">J. H. van Gorkom</a>, <a href="/search/?searchtype=author&query=Verheijen%2C+M+A+W">M. A. W. Verheijen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1709.01289v1-abstract-short" style="display: inline;"> We present the science case and observations plan of the MeerKAT Fornax Survey, an HI and radio continuum survey of the Fornax galaxy cluster to be carried out with the SKA precursor MeerKAT. Fornax is the second most massive cluster within 20 Mpc and the largest nearby cluster in the southern hemisphere. Its low X-ray luminosity makes it representative of the environment where most galaxies live… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.01289v1-abstract-full').style.display = 'inline'; document.getElementById('1709.01289v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.01289v1-abstract-full" style="display: none;"> We present the science case and observations plan of the MeerKAT Fornax Survey, an HI and radio continuum survey of the Fornax galaxy cluster to be carried out with the SKA precursor MeerKAT. Fornax is the second most massive cluster within 20 Mpc and the largest nearby cluster in the southern hemisphere. Its low X-ray luminosity makes it representative of the environment where most galaxies live and where substantial galaxy evolution takes place. Fornax's ongoing growth makes it an excellent laboratory for studying the assembly of clusters, the physics of gas accretion and stripping in galaxies falling in the cluster, and the connection between these processes and the neutral medium in the cosmic web. We will observe a region of 12 deg$^2$ reaching a projected distance of 1.5 Mpc from the cluster centre. This will cover a wide range of environment density out to the outskirts of the cluster, where gas-rich in-falling groups are found. We will: study the HI morphology of resolved galaxies down to a column density of a few times 1e+19 cm$^{-2}$ at a resolution of 1 kpc; measure the slope of the HI mass function down to M(HI) 5e+5 M(sun); and attempt to detect HI in the cosmic web reaching a column density of 1e+18 cm$^{-2}$ at a resolution of 10 kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.01289v1-abstract-full').style.display = 'none'; document.getElementById('1709.01289v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings of Science, "MeerKAT Science: On the Pathway to the SKA", Stellenbosch, 25-27 May 2016</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.03587">arXiv:1708.03587</a> <span> [<a href="https://arxiv.org/pdf/1708.03587">pdf</a>, <a href="https://arxiv.org/format/1708.03587">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Towards a Full Census of the Obscure(d) Vela Supercluster using MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Elson%2C+E+C">E. C. Elson</a>, <a href="/search/?searchtype=author&query=Blyth%2C+S+L">S. L. Blyth</a>, <a href="/search/?searchtype=author&query=Carignan%2C+C">C. Carignan</a>, <a href="/search/?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Cluver%2C+M+E">M. E. Cluver</a>, <a href="/search/?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1708.03587v1-abstract-short" style="display: inline;"> Recent spectroscopic observations of a few thousand partially obscured galaxies in the Vela constellation revealed a massive overdensity on supercluster scales straddling the Galactic Equator (l $\sim$ 272.5deg) at $cz \sim 18000$km/s. It remained unrecognised because it is located just beyond the boundaries and volumes of systematic whole-sky redshift and peculiar velocity surveys - and is obscur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.03587v1-abstract-full').style.display = 'inline'; document.getElementById('1708.03587v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.03587v1-abstract-full" style="display: none;"> Recent spectroscopic observations of a few thousand partially obscured galaxies in the Vela constellation revealed a massive overdensity on supercluster scales straddling the Galactic Equator (l $\sim$ 272.5deg) at $cz \sim 18000$km/s. It remained unrecognised because it is located just beyond the boundaries and volumes of systematic whole-sky redshift and peculiar velocity surveys - and is obscured by the Milky Way. The structure lies close to the apex where residual bulkflows suggest considerable mass excess. The uncovered Vela Supercluster (VSCL) conforms of a confluence of merging walls, but its core remains uncharted. At the thickest foreground dust column densities (|b| < 6 deg) galaxies are not visible and optical spectroscopy is not effective. This precludes a reliable estimate of the mass of VSCL, hence its effect on the cosmic flow field and the peculiar velocity of the Local Group. Only systematic HI-surveys can bridge that gap. We have run simulations and will present early-science observing scenarios with MeerKAT 32 (M32) to complete the census of this dynamically and cosmologically relevant supercluster. M32 has been put forward because this pilot project will also serve as precursor project for HI MeerKAT Large Survey Projects, like Fornax and Laduma. Our calculations have shown that a survey area of the fully obscured part of the supercluster, where the two walls cross and the potential core of the supercluster resides, can be achieved on reasonable time-scales (200 hrs) with M32. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.03587v1-abstract-full').style.display = 'none'; document.getElementById('1708.03587v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 3 figures, accepted for publication, Proceedings of Science, workshop on "MeerKAT Science: On the Pathway to the SKA", held in Stellenbosch 25-27 May 2016</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.04267">arXiv:1707.04267</a> <span> [<a href="https://arxiv.org/pdf/1707.04267">pdf</a>, <a href="https://arxiv.org/ps/1707.04267">ps</a>, <a href="https://arxiv.org/format/1707.04267">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx1800">10.1093/mnras/stx1800 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Predicting Structures in the Zone of Avoidance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sorce%2C+J+G">Jenny G. Sorce</a>, <a href="/search/?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Renee C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Gottloeber%2C+S">Stefan Gottloeber</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.04267v1-abstract-short" style="display: inline;"> The Zone of Avoidance (ZOA), whose emptiness is an artifact of our Galaxy dust, has been challenging observers as well as theorists for many years. Multiple attempts have been made on the observational side to map this region in order to better understand the local flows. On the theoretical side, however, this region is often simply statistically populated with structures but no real attempt has b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.04267v1-abstract-full').style.display = 'inline'; document.getElementById('1707.04267v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.04267v1-abstract-full" style="display: none;"> The Zone of Avoidance (ZOA), whose emptiness is an artifact of our Galaxy dust, has been challenging observers as well as theorists for many years. Multiple attempts have been made on the observational side to map this region in order to better understand the local flows. On the theoretical side, however, this region is often simply statistically populated with structures but no real attempt has been made to confront theoretical and observed matter distributions. This paper takes a step forward using constrained realizations of the local Universe shown to be perfect substitutes of local Universe-like simulations for smoothed high density peak studies. Far from generating completely `random' structures in the ZOA, the reconstruction technique arranges matter according to the surrounding environment of this region. More precisely, the mean distributions of structures in a series of constrained and random realizations differ: while densities annihilate each other when averaging over 200 random realizations, structures persist when summing 200 constrained realizations. The probability distribution function of ZOA grid cells to be highly overdense is a Gaussian with a 15% mean in the random case, while that of the constrained case exhibits large tails. This implies that areas with the largest probabilities host most likely a structure. Comparisons between these predictions and observations, like those of the Puppis 3 cluster, show a remarkable agreement and allow us to assert the presence of the, recently highlighted by observations, Vela supercluster at about 180 Mpc/h, right behind the thickest dust layers of our Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.04267v1-abstract-full').style.display = 'none'; document.getElementById('1707.04267v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, 11 pages, 6 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.04615">arXiv:1611.04615</a> <span> [<a href="https://arxiv.org/pdf/1611.04615">pdf</a>, <a href="https://arxiv.org/format/1611.04615">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnrasl/slw229">10.1093/mnrasl/slw229 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a supercluster in the ZOA in Vela </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Cluver%2C+M+E">Michelle E. Cluver</a>, <a href="/search/?searchtype=author&query=Bilicki%2C+M">Maciej Bilicki</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">Thomas H. Jarrett</a>, <a href="/search/?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/?searchtype=author&query=Elagali%2C+A">Ahmed Elagali</a>, <a href="/search/?searchtype=author&query=B%C3%B6hringer%2C+H">Hans B枚hringer</a>, <a href="/search/?searchtype=author&query=Chon%2C+G">Gayoung Chon</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1611.04615v3-abstract-short" style="display: inline;"> We report the discovery of a potentially major supercluster that extends across the Galactic Plane in the constellation of Vela, at a mean recessional velocity of ~18,000 km/s. Recent multi-object spectroscopic observations of this Vela Supercluster (VSCL), using AAOmega+2dF and the Southern African Large Telescope, confirm an extended galaxy overdensity in the Zone of Avoidance (ZOA) located wher… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.04615v3-abstract-full').style.display = 'inline'; document.getElementById('1611.04615v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.04615v3-abstract-full" style="display: none;"> We report the discovery of a potentially major supercluster that extends across the Galactic Plane in the constellation of Vela, at a mean recessional velocity of ~18,000 km/s. Recent multi-object spectroscopic observations of this Vela Supercluster (VSCL), using AAOmega+2dF and the Southern African Large Telescope, confirm an extended galaxy overdensity in the Zone of Avoidance (ZOA) located where residual bulk flows predict a considerable mass excess. We present a preliminary analysis of ~4,500 new spectroscopic galaxy redshifts obtained in the ZOA centred on the Vela region (l=272.5+-20 deg, b=0+-10 deg). The presently sparsely-sampled dataset traces an overdensity that covers 25 deg in Galactic longitude on either side of the Plane, suggesting an extent of 25 deg x 20 deg, corresponding to ~115 x 90 $h_{70}$ Mpc at the supercluster redshift. In redshift space, the overdensity appears to consist of two merging wall-like structures, interspersed with clusters and groups. Both the velocity histogram and the morphology of the multi-branching wall structure are consistent with a supercluster classification. $K_s^o$ galaxy counts show an enhancement of ~1.2 over the survey area for galaxies brighter than $M_K^*$ at the VSCL distance, and a galaxy overdensity of $未=0.50\rm{-}0.77$ within a photometric redshift shell around the VSCL, when compared to various Two-Micron All-Sky Survey samples. Taking account of selection effects, the VSCL is estimated to contribute $v_\rm{LG} \gtrsim 50$ km/s to the motion of the Local Group. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.04615v3-abstract-full').style.display = 'none'; document.getElementById('1611.04615v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Matches the final version published in MNRAS Letters. Updated author list, spelling, references</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS Letters, 466 (1): L29-L33 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.08596">arXiv:1607.08596</a> <span> [<a href="https://arxiv.org/pdf/1607.08596">pdf</a>, <a href="https://arxiv.org/ps/1607.08596">ps</a>, <a href="https://arxiv.org/format/1607.08596">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw1887">10.1093/mnras/stw1887 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NIR Tully-Fisher in the Zone of Avoidance. -- III. Deep NIR catalogue of the HIZOA galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Said%2C+K">Khaled Said</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Williams%2C+W+L">Wendy L. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1607.08596v1-abstract-short" style="display: inline;"> We present a deep near-infrared (NIR) photometric catalogue of sources from the Parkes HI Zone of Avoidance (HIZOA) survey, which forms the basis for an investigation of the matter distribution in the Zone of Avoidance. Observations were conducted between 2006 and 2013 using the Infrared Survey Facility (IRSF), a 1.4-m telescope situated at the South African Astronomical Observatory site in Suther… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.08596v1-abstract-full').style.display = 'inline'; document.getElementById('1607.08596v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.08596v1-abstract-full" style="display: none;"> We present a deep near-infrared (NIR) photometric catalogue of sources from the Parkes HI Zone of Avoidance (HIZOA) survey, which forms the basis for an investigation of the matter distribution in the Zone of Avoidance. Observations were conducted between 2006 and 2013 using the Infrared Survey Facility (IRSF), a 1.4-m telescope situated at the South African Astronomical Observatory site in Sutherland. The images cover all 1108 HIZOA detections and yield 915 galaxies. An additional 105 bright 2MASS galaxies in the southern ZOA were imaged with the IRSF, resulting in 129 galaxies. The average $K_s$-band seeing and sky background for the survey are 1.38 arcsec and 20.1 mag, respectively. The detection rate as a function of stellar density and dust extinction is found to depend mainly on the HI mass of the HI detected galaxies, which in principal correlates with the NIR brightness of the spiral galaxies. The measured isophotal magnitudes are of sufficient accuracy (errors $\sim$ 0.02 mag) to be used in a Tully-Fisher analysis. In the final NIR catalogue, 285 galaxies have both IRSF and 2MASS photometry (180 HIZOA plus 105 bright 2MASX galaxies). The $K_s$-band isophotal magnitudes presented in this paper agree, within the uncertainties, with those reported in the 2MASX catalogue. Another 30 galaxies, from the HIZOA northern extension, are also covered by UKIDSS Galactic Plane Survey (GPS) images, which are one magnitude deeper than our IRSF images. A modified version of our photometry pipeline was used to derive the photometric parameters of these UKIDSS galaxies. Good agreement was found between the respective $K_s$-band isophotal magnitudes. These comparisons confirm the robustness of the isophotal parameters and demonstrate that the IRSF images do not suffer from foreground contamination, after star removal, nor under-estimate the isophotal fluxes of ZoA galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.08596v1-abstract-full').style.display = 'none'; document.getElementById('1607.08596v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures, 3 tables, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.03771">arXiv:1607.03771</a> <span> [<a href="https://arxiv.org/pdf/1607.03771">pdf</a>, <a href="https://arxiv.org/format/1607.03771">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnrasl/slw129">10.1093/mnrasl/slw129 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for quasi-periodic oscillations in the optical polarization of the blazar PKS 2155-304 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pekeur%2C+N+W">N. W. Pekeur</a>, <a href="/search/?searchtype=author&query=Taylor%2C+A+R">A. R. Taylor</a>, <a href="/search/?searchtype=author&query=Potter%2C+S+B">S. B. Potter</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1607.03771v1-abstract-short" style="display: inline;"> Evidence for the presence of quasi-periodic oscillations (QPOs) in the optical polarization of the blazar PKS 2155-304, during a period of enhanced gamma-ray brightness, is presented. The periodogram of the polarized flux revealed the existence of a prominent peak at $T\sim 13$ min, detected at >99.7% significance, and $T\sim 30$ min, which was nominally significant at >99%. This is the first evid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.03771v1-abstract-full').style.display = 'inline'; document.getElementById('1607.03771v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.03771v1-abstract-full" style="display: none;"> Evidence for the presence of quasi-periodic oscillations (QPOs) in the optical polarization of the blazar PKS 2155-304, during a period of enhanced gamma-ray brightness, is presented. The periodogram of the polarized flux revealed the existence of a prominent peak at $T\sim 13$ min, detected at >99.7% significance, and $T\sim 30$ min, which was nominally significant at >99%. This is the first evidence of QPOs in the polarization of an active galactic nucleus, potentially opening up a new avenue of studying this phenomenon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.03771v1-abstract-full').style.display = 'none'; document.getElementById('1607.03771v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 5 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.02787">arXiv:1607.02787</a> <span> [<a href="https://arxiv.org/pdf/1607.02787">pdf</a>, <a href="https://arxiv.org/format/1607.02787">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201528048">10.1051/0004-6361/201528048 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NIBLES - an HI census of stellar mass selected SDSS galaxies: I. The Nan莽ay HI survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=van+Driel%2C+W">W. van Driel</a>, <a href="/search/?searchtype=author&query=Butcher%2C+Z">Z. Butcher</a>, <a href="/search/?searchtype=author&query=Schneider%2C+S">S. Schneider</a>, <a href="/search/?searchtype=author&query=Lehnert%2C+M+D">M. D. Lehnert</a>, <a href="/search/?searchtype=author&query=Minchin%2C+R">R. Minchin</a>, <a href="/search/?searchtype=author&query=Blyth%2C+S">S-L. Blyth</a>, <a href="/search/?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/?searchtype=author&query=Hallet%2C+N">N. Hallet</a>, <a href="/search/?searchtype=author&query=Joseph%2C+T">T. Joseph</a>, <a href="/search/?searchtype=author&query=Kotze%2C+P">P. Kotze</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+A+O+H">A. O. H. Olofsson</a>, <a href="/search/?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1607.02787v1-abstract-short" style="display: inline;"> To investigate galaxy properties as a function of their total stellar mass, we obtained 21cm HI line observations at the 100-m class Nan莽ay Radio Telescope of 2839 galaxies from the Sloan Digital Sky Survey (SDSS) in the Local Volume (900<cz<12,000 km/s), dubbed the Nan莽ay Interstellar Baryons Legacy Extragalactic Survey (NIBLES) sample. They were selected evenly over their entire range of absolut… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.02787v1-abstract-full').style.display = 'inline'; document.getElementById('1607.02787v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.02787v1-abstract-full" style="display: none;"> To investigate galaxy properties as a function of their total stellar mass, we obtained 21cm HI line observations at the 100-m class Nan莽ay Radio Telescope of 2839 galaxies from the Sloan Digital Sky Survey (SDSS) in the Local Volume (900<cz<12,000 km/s), dubbed the Nan莽ay Interstellar Baryons Legacy Extragalactic Survey (NIBLES) sample. They were selected evenly over their entire range of absolute SDSS z-band magnitudes (-13.5 to -24 mag), which were used as a proxy for their stellar masses. Here, a first, global presentation of the observations and basic results is given, their further analysis will be presented in other papers in this series. The galaxies were selected based on their properties, as listed in SDSS DR5. Comparing this photometry to their total HI masses, we noted that, for a few percent, the SDSS magnitudes appeared severely misunderestimated, as confirmed by our re-measurements for selected objects. Although using the later DR9 results eliminated this problem in most cases, 384 still required manual photometric source selection. Usable HI spectra were obtained for 2600 galaxies, of which 1733 (67%) were clearly detected and 174 (7%) marginally. The spectra for 241 other observed galaxies could not be used for further analysis owing to problems with either the HI or the SDSS data. We reached the target number of about 150 sources per half-magnitude bin over the Mz range -16.5 to -23 mag. Down to -21 mag the overall detection rate is rather constant at the ~75% level but it starts to decline steadily towards the 30% level at -23 mag. Making regression fits by comparing total HI and stellar masses for our sample, including our conservatively estimated HI upper limits for non-detections, we find the relationship log(M_HI/M*) = -0.59 log(M*) + 5.05, which lies significantly below the relationship found in the M_HI/M* - M* plane when only using HI detections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.02787v1-abstract-full').style.display = 'none'; document.getElementById('1607.02787v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">71 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 595, A118 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.02603">arXiv:1605.02603</a> <span> [<a href="https://arxiv.org/pdf/1605.02603">pdf</a>, <a href="https://arxiv.org/format/1605.02603">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw968">10.1093/mnras/stw968 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The WSRT ZoA Perseus-Pisces Filament wide-field HI imaging survey I. HI catalogue and atlas </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/?searchtype=author&query=Verheijen%2C+M+A+W">M. A. W Verheijen</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/?searchtype=author&query=Schr%C3%B6der%2C+A+C">A. C. Schr枚der</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Elson%2C+E+C">E. C Elson</a>, <a href="/search/?searchtype=author&query=van+Driel%2C+W">W. van Driel</a>, <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/?searchtype=author&query=Henning%2C+P+A">P. A. Henning</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1605.02603v1-abstract-short" style="display: inline;"> We present results of a blind 21cm HI-line imaging survey of a galaxy overdensity located behind the Milky Way at $\ell,b$ $\approx$ 160 deg, 0.5 deg. The overdensity corresponds to a Zone-of-Avoidance crossing of the Perseus-Pisces Supercluster filament. Although it is known that this filament contains an X-ray galaxy cluster (3C129) hosting two strong radio galaxies, little is known about galaxi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.02603v1-abstract-full').style.display = 'inline'; document.getElementById('1605.02603v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.02603v1-abstract-full" style="display: none;"> We present results of a blind 21cm HI-line imaging survey of a galaxy overdensity located behind the Milky Way at $\ell,b$ $\approx$ 160 deg, 0.5 deg. The overdensity corresponds to a Zone-of-Avoidance crossing of the Perseus-Pisces Supercluster filament. Although it is known that this filament contains an X-ray galaxy cluster (3C129) hosting two strong radio galaxies, little is known about galaxies associated with this potentially rich cluster because of the high Galactic dust extinction. We mapped a sky area of $\sim$9.6 sq.deg using the Westerbork Synthesis Radio Telescope in a hexagonal mosaic of 35 pointings observed for 12 hours each, in the radial velocity range $cz = 2400 - 16600$ km/s. The survey has a sensitivity of 0.36 mJy/beam rms at a velocity resolution of 16.5 km/s. We detected 211 galaxies, 62% of which have a near-infrared counterpart in the UKIDSS Galactic Plane Survey. We present a catalogue of the HI properties and an HI atlas containing total intensity maps, position-velocity diagrams, global HI profiles and UKIDSS counterpart images. For the resolved galaxies we also present HI velocity fields and radial HI surface density profiles. A brief analysis of the structures outlined by these galaxies finds that 87 of them lie at the distance of the Perseus-Pisces Supercluster ($cz \sim 4000 - 8000$ km/s) and seem to form part of the 3C129 cluster. Further 72 detections trace an overdensity at a velocity of $cz \approx$ 10000 km/s and seem to coincide with a structure predicted from mass density reconstructions in the first 2MASS Redshift Survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.02603v1-abstract-full').style.display = 'none'; document.getElementById('1605.02603v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 18 figures, 6 Tables, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.02922">arXiv:1602.02922</a> <span> [<a href="https://arxiv.org/pdf/1602.02922">pdf</a>, <a href="https://arxiv.org/ps/1602.02922">ps</a>, <a href="https://arxiv.org/format/1602.02922">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0004-6256/151/3/52">10.3847/0004-6256/151/3/52 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Parkes HI Zone of Avoidance Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">L. Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Schr%C3%B6der%2C+A+C">A. C. Schr枚der</a>, <a href="/search/?searchtype=author&query=Henning%2C+P+A">P. A. Henning</a>, <a href="/search/?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/?searchtype=author&query=Stewart%2C+I+M">I. M. Stewart</a>, <a href="/search/?searchtype=author&query=Heald%2C+G">G. Heald</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1602.02922v2-abstract-short" style="display: inline;"> A blind HI survey of the extragalactic sky behind the southern Milky Way has been conducted with the multibeam receiver on the 64-m Parkes radio telescope. The survey covers the Galactic longitude range 212 < l < 36 and Galactic latitudes |b| < 5, and yields 883 galaxies to a recessional velocity of 12,000 km/s. The survey covers the sky within the HIPASS area to greater sensitivity, finding lower… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.02922v2-abstract-full').style.display = 'inline'; document.getElementById('1602.02922v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.02922v2-abstract-full" style="display: none;"> A blind HI survey of the extragalactic sky behind the southern Milky Way has been conducted with the multibeam receiver on the 64-m Parkes radio telescope. The survey covers the Galactic longitude range 212 < l < 36 and Galactic latitudes |b| < 5, and yields 883 galaxies to a recessional velocity of 12,000 km/s. The survey covers the sky within the HIPASS area to greater sensitivity, finding lower HI-mass galaxies at all distances, and probing more completely the large-scale structures at and beyond the distance of the Great Attractor. Fifty-one percent of the HI detections have an optical/NIR counterpart in the literature. A further 27% have new counterparts found in existing, or newly obtained, optical/NIR images. The counterpart rate drops in regions of high foreground stellar crowding and extinction, and for low-HI mass objects. Only 8% of all counterparts have a previous optical redshift measurement. A notable new galaxy is HIZOA J1353-58, a possible companion to the Circinus galaxy. Merging this catalog with the similarly-conducted northern extension (Donley et al. 2005), large-scale structures are delineated, including those within the Puppis and Great Attractor regions, and the Local Void. Several newly-identified structures are revealed here for the first time. Three new galaxy concentrations (NW1, NW2 and NW3) are key in confirming the diagonal crossing of the Great Attractor Wall between the Norma cluster and the CIZA J1324.7-5736 cluster. Further contributors to the general mass overdensity in that area are two new clusters (CW1 and CW2) in the nearer Centaurus Wall, one of which forms part of the striking 180 deg (100/h Mpc) long filament that dominates the southern sky at velocities of ~3000 km/s, and the suggestion of a further Wall at the Great Attractor distance at slightly higher longitudes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.02922v2-abstract-full').style.display = 'none'; document.getElementById('1602.02922v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Astronomical Journal 9 February 2016 (accepted 26 September 2015); 42 pages, 7 tables, 18 figures, main figures data tables only available in the on-line version of journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomical Journal, 151, 52 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.07162">arXiv:1601.07162</a> <span> [<a href="https://arxiv.org/pdf/1601.07162">pdf</a>, <a href="https://arxiv.org/ps/1601.07162">ps</a>, <a href="https://arxiv.org/format/1601.07162">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw105">10.1093/mnras/stw105 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NIR Tully-Fisher in the Zone of Avoidance. - II. 21 cm HI-line spectra of southern ZOA galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Said%2C+K">Khaled Said</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Williams%2C+W+L">Wendy L. Williams</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Springob%2C+C+M">Christopher M. Springob</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1601.07162v1-abstract-short" style="display: inline;"> High-accuracy HI profiles and linewidths are presented for inclined ($(b/a)^o < 0.5$) spiral galaxies in the southern Zone of Avoidance (ZOA). These galaxies define a sample for use in the determinations of peculiar velocities using the near-infrared Tully-Fisher (TF) relation. The sample is based on the 394 HI-selected galaxies from the Parkes HI Zone of Avoidance survey (HIZOA). Follow-up narrow… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.07162v1-abstract-full').style.display = 'inline'; document.getElementById('1601.07162v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.07162v1-abstract-full" style="display: none;"> High-accuracy HI profiles and linewidths are presented for inclined ($(b/a)^o < 0.5$) spiral galaxies in the southern Zone of Avoidance (ZOA). These galaxies define a sample for use in the determinations of peculiar velocities using the near-infrared Tully-Fisher (TF) relation. The sample is based on the 394 HI-selected galaxies from the Parkes HI Zone of Avoidance survey (HIZOA). Follow-up narrow-band Parkes HI observations were obtained in 2010 and 2015 for 290 galaxies, while for the further 104 galaxies, sufficiently high signal-to-noise spectra were available from the original HIZOA data. All 394 spectra are reduced and parameterized in the same systematic way. Five different types of linewidth measurements were derived, and a Bayesian mixture model was used to derive conversion equations between these five widths. Of the selected and measure galaxies, 342 have adequate signal-to-noise (S/N $\geq$ 5) for use in TF distance estimation. The average value of the signal-to-noise ratio of the sample is 14.7. We present the HI parameters for these galaxies. The sample will allow a more accurate determination of the flow field in the southern ZOA which bisects dynamically important large-scale structures such as Puppis, the Great Attractor, and the Local Void. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.07162v1-abstract-full').style.display = 'none'; document.getElementById('1601.07162v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, 4 tables, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.5324">arXiv:1412.5324</a> <span> [<a href="https://arxiv.org/pdf/1412.5324">pdf</a>, <a href="https://arxiv.org/format/1412.5324">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Extragalactic large-scale structures in the northern Zone of Avoidance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ramatsoku%2C+M">M Ramatsoku</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R C Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Schr%C3%B6der%2C+A+C">A C Schr枚der</a>, <a href="/search/?searchtype=author&query=van+Driel%2C+W">W van Driel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1412.5324v1-abstract-short" style="display: inline;"> We used the Nan莽ay Radio Telescope (NRT) to measure the 21 cm line emission of near-infrared bright galaxies in the northern Zone of Avoidance (ZoA) without previous redshift determinations. We selected galaxies with extinction-corrected magnitudes $K_s^o \leq 11\hbox{$.\!\!^{\rm m}$}25$ from the 2MASS Extended Source Catalog. These data will complement the existing 2MASS Redshift Survey (2MRS; fi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.5324v1-abstract-full').style.display = 'inline'; document.getElementById('1412.5324v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.5324v1-abstract-full" style="display: none;"> We used the Nan莽ay Radio Telescope (NRT) to measure the 21 cm line emission of near-infrared bright galaxies in the northern Zone of Avoidance (ZoA) without previous redshift determinations. We selected galaxies with extinction-corrected magnitudes $K_s^o \leq 11\hbox{$.\!\!^{\rm m}$}25$ from the 2MASS Extended Source Catalog. These data will complement the existing 2MASS Redshift Survey (2MRS; first data release) as well as the ongoing 2MASS Tully-Fisher survey, both of which exclude the inner ZoA ($|b|< 5^{\circ}$), where the identification of galaxy candidates is the hardest. Of the $\sim$1000 identified 2MASX galaxy candidates we have so far detected 252 to our 3.0 mJy rms sensitivity limit and the velocity limit of 10500 km/s. The resulting redshift distribution reveals various new structures that were hitherto uncharted. They seem to form part of the larger Perseus-Pisces Supercluster (PPS). The most conspicuous is a ridge at about $\ell\approx 160^{\circ}$,$v \approx 6500$ km/s. Within this wall-like structure, two strong radio galaxies (3C 129 and 3C 129.1) are embedded which lie at the same distance as the ridge. They seem to form part of an X-ray cluster. Another prominent filament has been identified crossing the ZoA at $\ell \approx 90^\circ$, hence suggesting the second Perseus-Pisces arm is more extended than previously thought. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.5324v1-abstract-full').style.display = 'none'; document.getElementById('1412.5324v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 1 figure, in Proceedings of SAIP2012: the 57th Annual Conference of the South African Institute of Physics, edited by Johan Janse van Rensburg (2014), pp. 368 - 372. ISBN: 978-1-77592-070-0</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.7361">arXiv:1411.7361</a> <span> [<a href="https://arxiv.org/pdf/1411.7361">pdf</a>, <a href="https://arxiv.org/ps/1411.7361">ps</a>, <a href="https://arxiv.org/format/1411.7361">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stu2496">10.1093/mnras/stu2496 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On How to Extend the NIR Tully-Fisher Relation to be Truly All-Sky </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Said%2C+K">K. Said</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1411.7361v1-abstract-short" style="display: inline;"> Dust extinction and stellar confusion by the Milky Way reduce the efficiency of detecting galaxies at low Galactic latitudes, creating the so-called Zone of Avoidance. This stands as a stumbling block in charting the distribution of galaxies and cosmic flow fields, and therewith our understanding of the local dynamics in the Universe (CMB dipole, convergence radius of bulk flows). For instance, Zo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.7361v1-abstract-full').style.display = 'inline'; document.getElementById('1411.7361v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.7361v1-abstract-full" style="display: none;"> Dust extinction and stellar confusion by the Milky Way reduce the efficiency of detecting galaxies at low Galactic latitudes, creating the so-called Zone of Avoidance. This stands as a stumbling block in charting the distribution of galaxies and cosmic flow fields, and therewith our understanding of the local dynamics in the Universe (CMB dipole, convergence radius of bulk flows). For instance, ZoA galaxies are generally excluded from the whole-sky Tully-Fisher Surveys ($|b| \leq 5^\circ$) even if catalogued. We show here that by fine-tuning the near-infrared TF relation, there is no reason not to extend peculiar velocity surveys deeper into the ZoA. Accurate axial ratios ($b/a$) are crucial to both the TF sample selection and the resulting TF distances. We simulate the effect of dust extinction on the geometrical properties of galaxies. As expected, galaxies appear rounder with increasing obscuration level, even affecting existing TF samples. We derive correction models and demonstrate that we can reliably reproduce the intrinsic axial ratio from the observed value up to extinction level of about $A_J\simeq3$ mag ($A_V\sim11$ mag), we also recover a fair fraction of galaxies that otherwise would fall out of an uncorrected inclination limited galaxy sample. We present a re-calibration of the 2MTF relation in the NIR $J$, $H$, and $K_s$-bands for isophotal rather than total magnitudes, using their same calibration sample. Both TF relations exhibit similar scatter at high Galactic latitudes. However, the isophotal TF relation results in a significant improvement in the scatter for galaxies in the ZoA, and low surface brightness galaxies in general, because isophotal apertures are more robust in the face of significant stellar confusion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.7361v1-abstract-full').style.display = 'none'; document.getElementById('1411.7361v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures, 4 tables, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.0596">arXiv:1411.0596</a> <span> [<a href="https://arxiv.org/pdf/1411.0596">pdf</a>, <a href="https://arxiv.org/format/1411.0596">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stu2345">10.1093/mnras/stu2345 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SNIa Host Galaxy Properties and the Dust Extinction Distribution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/?searchtype=author&query=Reynolds%2C+A">A. Reynolds</a>, <a href="/search/?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1411.0596v1-abstract-short" style="display: inline;"> Supernovae Type Ia display a complex relation with their host galaxies. An important prior to the fit of the supernovae's lightcurve is the distribution of host galaxy extinction values that can be encountered. The SDSS-SN project has published light curve fits using both MLCS2k2 and SALT2. We use the former fits extinction parameter ($A_V$) to map this distribution of extinction values. We expl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.0596v1-abstract-full').style.display = 'inline'; document.getElementById('1411.0596v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.0596v1-abstract-full" style="display: none;"> Supernovae Type Ia display a complex relation with their host galaxies. An important prior to the fit of the supernovae's lightcurve is the distribution of host galaxy extinction values that can be encountered. The SDSS-SN project has published light curve fits using both MLCS2k2 and SALT2. We use the former fits extinction parameter ($A_V$) to map this distribution of extinction values. We explore the dependence of this distribution on four observables; the inclination of the host galaxy disk, radial position of the supernova, redshift of the supernova and host, and the level of star-formation in the host galaxy. The distribution of $A_V$ values encountered by supernovae is typically characterised by: $\rm N_0 ~ e^{-A_V/蟿}$, with $蟿$= 0.4 or 0.33. We find that the inclination correction using an infinitely thin disk for the SNIa is sufficient, resulting in similar exponential $A_V$ distributions for high- and low-inclination disks. The $A_V$ distribution also depends on the radial position in the disk, consistent with previous results on the transparency of spiral disks. The distribution of $A_V$ values narrows with increased star-formation, possibly due to the destruction or dispersion of the dusty ISM by stellar winds prior to the ignition of the supernova. In future supernova searches, certainly the inclination of the host galaxy disk, should be considered in the construction of the \av \ prior with $蟿=0.4/cos(i)$ as the most likely prior in each individual host galaxy's case. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.0596v1-abstract-full').style.display = 'none'; document.getElementById('1411.0596v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 14 figures, accepted for publication by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1410.2992">arXiv:1410.2992</a> <span> [<a href="https://arxiv.org/pdf/1410.2992">pdf</a>, <a href="https://arxiv.org/ps/1410.2992">ps</a>, <a href="https://arxiv.org/format/1410.2992">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Galaxy peculiar velocities in the Zone of Avoidance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Said%2C+K">K. Said</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1410.2992v1-abstract-short" style="display: inline;"> Dust extinction and stellar confusion of the Milky Way hinder the detection of galaxies at low Galactic latitude, creating the so-called Zone of Avoidance (ZoA). This has hampered our understanding of the local dynamics, cosmic flow fields and the origin of the Cosmic Microwave Background dipole. The ZoA ($|b| \le 5^\circ$) is also excluded from the "whole-sky" Two Micron All-Sky Survey (2MASS) Re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.2992v1-abstract-full').style.display = 'inline'; document.getElementById('1410.2992v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.2992v1-abstract-full" style="display: none;"> Dust extinction and stellar confusion of the Milky Way hinder the detection of galaxies at low Galactic latitude, creating the so-called Zone of Avoidance (ZoA). This has hampered our understanding of the local dynamics, cosmic flow fields and the origin of the Cosmic Microwave Background dipole. The ZoA ($|b| \le 5^\circ$) is also excluded from the "whole-sky" Two Micron All-Sky Survey (2MASS) Redshift Survey (2MRS) and 2MASS Tully-Fisher Survey (2MTF). The latter aims to provide distances and peculiar velocities for all bright inclined 2MASS galaxies with $K_s^o$ $\leq 11\hbox{$.\!\!^{\rm m}$}25$. Correspondingly, knowledge about the density distribution in the ZoA remains limited to statistical interpolations. To improve on this bias we pursued two different surveys to fill in the southern and northern ZoA. These data will allow a direct measurement of galaxy peculiar velocities. In this paper we will present a newly derived optimized Tully-Fisher (TF) relation that allow accurate measures of galaxy distances and peculiar velocities for dust-obscured galaxies. We discuss further corrections for magnitudes and biases and present some preliminary results on flow fields in the southern ZoA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.2992v1-abstract-full').style.display = 'none'; document.getElementById('1410.2992v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 3 figures, to appear in Proceedings of SAIP2013, the 58th Annual Conference of the South African Institute of Physics, edited by Roelf Botha and Thulani Jili (SAIP and University of Zululand, 2014). ISBN: 978-0-620-62819-8</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.5918">arXiv:1406.5918</a> <span> [<a href="https://arxiv.org/pdf/1406.5918">pdf</a>, <a href="https://arxiv.org/ps/1406.5918">ps</a>, <a href="https://arxiv.org/format/1406.5918">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stu1155">10.1093/mnras/stu1155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep NIR photometry of HI galaxies in the Zone of Avoidance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Williams%2C+W+L">Wendy L. Williams</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P+A">Patrick A. Woudt</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1406.5918v1-abstract-short" style="display: inline;"> Current studies of the peculiar velocity flow field in the Local Universe are limited by either the lack of detection or accurate photometry for galaxies at low Galactic latitudes. The contribution to the dynamics of the Local Group of the largely unknown mass distribution in this 'Zone of Avoidance' remains controversial. We present here the results of a pilot project to obtain deep near infrared… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.5918v1-abstract-full').style.display = 'inline'; document.getElementById('1406.5918v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.5918v1-abstract-full" style="display: none;"> Current studies of the peculiar velocity flow field in the Local Universe are limited by either the lack of detection or accurate photometry for galaxies at low Galactic latitudes. The contribution to the dynamics of the Local Group of the largely unknown mass distribution in this 'Zone of Avoidance' remains controversial. We present here the results of a pilot project to obtain deep near infrared (NIR) observations of galaxies detected in the systematic Parkes deep HI survey of the ZoA - 578 galaxies with recession velocities out to 6000 km/s were observed with the 1.4m InfraRed Survey Facility SIRIUS camera providing J, H and K_s imaging ~2 mag deeper than 2MASS. After star-subtraction, the resulting isophotal magnitudes and inclinations of ZoA galaxies are of sufficient accuracy (magnitude errors under 0.1 mag even at high extinction) to ultimately be used to determine cosmic flow fields "in" the ZoA via the NIR Tully-Fisher relation. We further used the observed NIR colours to assess the ratio of the true extinction to the DIRBE/IRAS extinction deep into the dust layers of the Milky Way. The derived ratio was found to be 0.87 across the HIZOA survey region with no significant variation with Galactic latitude or longitude. This value is in excellent agreement with the completely independently derived factor of 0.86 by Schlafly & Finkbeiner based on Sloan data far away from the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.5918v1-abstract-full').style.display = 'none'; document.getElementById('1406.5918v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 15 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1301.2889">arXiv:1301.2889</a> <span> [<a href="https://arxiv.org/pdf/1301.2889">pdf</a>, <a href="https://arxiv.org/format/1301.2889">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/sts526">10.1093/mnras/sts526 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HI synthesis observations of the blue compact dwarf NGC 1705 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Elson%2C+E+C">E. C. Elson</a>, <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1301.2889v1-abstract-short" style="display: inline;"> Australia Telescope Compact Array HI-line observations of the nearby dwarf galaxy NGC 1705 are presented. The data are used to trace the gravitational potential of the galaxy out to several stellar disc scale lengths. A rotation curve is derived for the system and used to generate mass models. Dark matter dominates the gravitational potential at nearly all galactocentric radii. NFW and pseudo-isot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.2889v1-abstract-full').style.display = 'inline'; document.getElementById('1301.2889v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.2889v1-abstract-full" style="display: none;"> Australia Telescope Compact Array HI-line observations of the nearby dwarf galaxy NGC 1705 are presented. The data are used to trace the gravitational potential of the galaxy out to several stellar disc scale lengths. A rotation curve is derived for the system and used to generate mass models. Dark matter dominates the gravitational potential at nearly all galactocentric radii. NFW and pseudo-isothermal sphere halo parameterisations allowing for good reproductions of the observations. The models suggest NGC 1705 to have a dark matter halo that it much denser and more compact than previously thought. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.2889v1-abstract-full').style.display = 'none'; document.getElementById('1301.2889v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 January, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in MNRAS. 13 pages, 14 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1112.0379">arXiv:1112.0379</a> <span> [<a href="https://arxiv.org/pdf/1112.0379">pdf</a>, <a href="https://arxiv.org/format/1112.0379">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1017/S1743921312009088">10.1017/S1743921312009088 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SED of the nearby HI-massive LIRG HIZOA J0836-43: from the NIR to the radio domain </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Renee C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Cluver%2C+M+E">Michelle E. Cluver</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1112.0379v1-abstract-short" style="display: inline;"> HIZOA J0836-43is one of the most HI-massive galaxies in the local (z<0.1) Universe. Not only are such galaxies extremely rare, but this "coelacanth" galaxy exhibits characteristics -- in particular its active, inside-out stellar disk-building -- that appear more typical of past (z ~ 1) star formation, when large gas fractions were more common. Unlike most local giant HI galaxies, it is actively st… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1112.0379v1-abstract-full').style.display = 'inline'; document.getElementById('1112.0379v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1112.0379v1-abstract-full" style="display: none;"> HIZOA J0836-43is one of the most HI-massive galaxies in the local (z<0.1) Universe. Not only are such galaxies extremely rare, but this "coelacanth" galaxy exhibits characteristics -- in particular its active, inside-out stellar disk-building -- that appear more typical of past (z ~ 1) star formation, when large gas fractions were more common. Unlike most local giant HI galaxies, it is actively star forming. Moreover, the strong infrared emission is not induced by a merger event or AGN, as is commonly found in other local LIRGs. The galaxy is suggestive of a scaled-up version of local spiral galaxies; its extended star formation activity likely being fueled by its large gas reservoir and, as such, can aid our understanding of star formation in systems expected to dominate at higher redshifts. The multi-wavelength imaging and spectroscopic observations that have led to these deductions will be presented. These include NIR (J H K) and MIR (Spitzer; 3-24micron) imaging and photometry, MIR spectroscopy, ATCA HI-interferometry and Mopra CO line emission observations. But no optical data, as the galaxy is heavily obscured due to its location in Vela behind the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1112.0379v1-abstract-full').style.display = 'none'; document.getElementById('1112.0379v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 3 figures, to appear in the proceedings of IAU Symposium 284, "The Spectral Energy Distribution of Galaxies" (SED2011), 5-9 September 2011, Preston, UK, editors R.J. Tuffs & C.C.Popescu</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1110.1148">arXiv:1110.1148</a> <span> [<a href="https://arxiv.org/pdf/1110.1148">pdf</a>, <a href="https://arxiv.org/ps/1110.1148">ps</a>, <a href="https://arxiv.org/format/1110.1148">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/143/1/1">10.1088/0004-6256/143/1/1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Star Formation Models for the Dwarf Galaxies NGC 2915 and NGC 1705 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Elson%2C+E+C">E C Elson</a>, <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G">W J G de Blok</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R C Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1110.1148v1-abstract-short" style="display: inline;"> Crucial to a quantitative understanding of galaxy evolution are the properties of the inter-stellar medium that regulate galactic-scale star formation activity. We present here the results of a suite of star formation models applied to the nearby blue compact dwarf galaxies NGC 2915 and NGC 1705. Each of these galaxies has a stellar disk embedded in a much larger, essentially star-less HI disk. Th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1110.1148v1-abstract-full').style.display = 'inline'; document.getElementById('1110.1148v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1110.1148v1-abstract-full" style="display: none;"> Crucial to a quantitative understanding of galaxy evolution are the properties of the inter-stellar medium that regulate galactic-scale star formation activity. We present here the results of a suite of star formation models applied to the nearby blue compact dwarf galaxies NGC 2915 and NGC 1705. Each of these galaxies has a stellar disk embedded in a much larger, essentially star-less HI disk. These atypical stellar morphologies allow for rigorous tests of star formation models that examine the effects on star formation of the HI, stellar and dark matter mass components, as well as the kinematics of the gaseous and stellar disks. We use far ultra-violet and 24 micron imaging from the Galaxy Evolution Explorer and the Spitzer Infrared Nearby Galaxies Survey respectively to map the spatial distribution of the total star formation rate surface density within each galaxy. New high-resolution HI line observations obtained with the Australia Telescope Compact Array are used to study the distribution and dynamics of each galaxy's neutral inter-stellar medium. The standard Toomre Q parameter is unable to distinguish between active and non-active star forming regions, predicting the HI disks of the dwarfs to be sub-critical. Two-fluid instability models incorporating the stellar and dark matter components of each galaxy, in addition to the gaseous component, yield portions of the inner disk unstable. Finally, a formalisation in which the HI kinematics are characterised by the rotational shear of the gas produces models that very accurately match the observations. This suggests the time available for perturbations to collapse in the presence of rotational shear to be an important factor governing galactic-scale star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1110.1148v1-abstract-full').style.display = 'none'; document.getElementById('1110.1148v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 October, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 20 figures, accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1107.1096">arXiv:1107.1096</a> <span> [<a href="https://arxiv.org/pdf/1107.1096">pdf</a>, <a href="https://arxiv.org/format/1107.1096">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Deep NIR Photometry of HI Galaxies Behind the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Williams%2C+W+L">Wendy L. Williams</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P+A">Patrick A. Woudt</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">Renee C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1107.1096v1-abstract-short" style="display: inline;"> Current studies of the peculiar velocity flow field in the Local Universe are limited by the lack of detection of galaxies behind the Milky Way. The contribution of the largely unknown mass distribution in this "Zone of Avoidance" (ZoA) to the dynamics of the Local group remains contraversial. We have undertaken a near infrared (NIR) survey of HI detected galaxies in the ZoA. The photomety derived… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.1096v1-abstract-full').style.display = 'inline'; document.getElementById('1107.1096v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.1096v1-abstract-full" style="display: none;"> Current studies of the peculiar velocity flow field in the Local Universe are limited by the lack of detection of galaxies behind the Milky Way. The contribution of the largely unknown mass distribution in this "Zone of Avoidance" (ZoA) to the dynamics of the Local group remains contraversial. We have undertaken a near infrared (NIR) survey of HI detected galaxies in the ZoA. The photomety derived here will be used in the NIR Tully-Fisher (TF) relation to derive the peculiar velocities of this sample of galaxies in the ZoA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.1096v1-abstract-full').style.display = 'none'; document.getElementById('1107.1096v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in "Ten years of Infrared Survey Facility and the Future", eds. T. Nagayama, S. Sato, and K. Wakamatsu</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1107.1069">arXiv:1107.1069</a> <span> [<a href="https://arxiv.org/pdf/1107.1069">pdf</a>, <a href="https://arxiv.org/format/1107.1069">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Mass Distribution of the Great Attractor as Revealed by a Deep NIR Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Riad%2C+I+F">I. F. Riad</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a>, <a href="/search/?searchtype=author&query=Nagayama%2C+T">T. Nagayama</a>, <a href="/search/?searchtype=author&query=Wakamatsu%2C+K">K. Wakamatsu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1107.1069v1-abstract-short" style="display: inline;"> This paper presents the analysis of a deep near-infrared J,H,Ks-imaging survey (37.5 sq deg) aimed at tracing the galaxy distribution of the Great Attractor (GA) in the Zone of Avoidance along the so-called Norma Wall. The resulting galaxy catalog is complete to extinction-corrected magnitudes Ks^o = 14.8 mag for extinctions less than A_K = 1.0 mag and star densities below log N(Ks<14.0) < 4.72. O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.1069v1-abstract-full').style.display = 'inline'; document.getElementById('1107.1069v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.1069v1-abstract-full" style="display: none;"> This paper presents the analysis of a deep near-infrared J,H,Ks-imaging survey (37.5 sq deg) aimed at tracing the galaxy distribution of the Great Attractor (GA) in the Zone of Avoidance along the so-called Norma Wall. The resulting galaxy catalog is complete to extinction-corrected magnitudes Ks^o = 14.8 mag for extinctions less than A_K = 1.0 mag and star densities below log N(Ks<14.0) < 4.72. Of the 4360 cataloged galaxies, 99.2% lie in the hereby constrained 89.5% of the survey area. Although the analyzed galaxy distribution reveals no new major galaxy clusters at the GA distance (albeit some more distant ones), the overall number counts and luminosity density indicate a clear and surprisingly smooth overdensity at the GA distance that extends over the whole surveyed region. A mass estimate of the Norma Wall overdensity derived from (a) galaxy number counts and (b) photometric redshift distribution gives a lower value compared to the original prediction by Lynden-Bell et al. 1988 (~14%), but is consistent with more recent independent assessments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.1069v1-abstract-full').style.display = 'none'; document.getElementById('1107.1069v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in "Ten years of Infrared Survey Facility and the Future", eds. T. Nagayama, S. Sato, and K. Wakamatsu</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1103.4427">arXiv:1103.4427</a> <span> [<a href="https://arxiv.org/pdf/1103.4427">pdf</a>, <a href="https://arxiv.org/ps/1103.4427">ps</a>, <a href="https://arxiv.org/format/1103.4427">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/j.1365-2966.2011.18701.x">10.1111/j.1365-2966.2011.18701.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Three-dimensional modeling of the HI kinematics of NGC 2915 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Elson%2C+E+C">E. C. Elson</a>, <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1103.4427v1-abstract-short" style="display: inline;"> The nearby blue compact dwarf, NGC 2915, has its stellar disc embedded in a large, extended (~ 22 B-band scale-lengths) HI disc. New high-resolution HI synthesis observations of NGC 2915 have been obtained with the Australia Telescope Compact Array. These observations provide evidence of extremely complex HI kinematics within the immediate vicinity of the galaxy's star-forming core. We identify an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.4427v1-abstract-full').style.display = 'inline'; document.getElementById('1103.4427v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1103.4427v1-abstract-full" style="display: none;"> The nearby blue compact dwarf, NGC 2915, has its stellar disc embedded in a large, extended (~ 22 B-band scale-lengths) HI disc. New high-resolution HI synthesis observations of NGC 2915 have been obtained with the Australia Telescope Compact Array. These observations provide evidence of extremely complex HI kinematics within the immediate vicinity of the galaxy's star-forming core. We identify and quantify double-peaked HI line profiles near the centre of the galaxy and show that the HI energetics can be accounted for by the mechanical energy output of the central high-mass stellar population within time-scales of 10^6-10^7 yr. Full three-dimensional models of the HI data cube are generated and compared to the observations to test various physical scenarios associated with the high-mass star-forming core of NGC 2915. Purely circular HI kinematics are ruled out together with the possibility of a high-velocity-dispersion inter-stellar medium at inner radii. Radial velocities of ~ 30 km/s are required to describe the central-most HI kinematics of the system. Our results lend themselves to the simple physical scenario in which the young stellar core of the galaxy expels the gas outwards from the centre of the disc, thereby creating a central HI under-density. These kinematics should be thought of as being linked to a central HI outflow rather than a large-scale galactic blow-out or wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.4427v1-abstract-full').style.display = 'none'; document.getElementById('1103.4427v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 March, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1010.3550">arXiv:1010.3550</a> <span> [<a href="https://arxiv.org/pdf/1010.3550">pdf</a>, <a href="https://arxiv.org/ps/1010.3550">ps</a>, <a href="https://arxiv.org/format/1010.3550">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/725/2/1550">10.1088/0004-637X/725/2/1550 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Active Disk Building in a local HI-Massive LIRG: The Synergy between Gas, Dust, and Star Formation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cluver%2C+M+E">M. E. Cluver</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/?searchtype=author&query=Appleton%2C+P+N">P. N. Appleton</a>, <a href="/search/?searchtype=author&query=Melbourne%2C+J">J. Melbourne</a>, <a href="/search/?searchtype=author&query=Emonts%2C+B">B. Emonts</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1010.3550v1-abstract-short" style="display: inline;"> HIZOA J0836-43 is the most HI-massive (M_HI = 7.5x10^10 Msun) galaxy detected in the HIPASS volume and lies optically hidden behind the Milky Way. Markedly different from other extreme HI disks in the local universe, it is a luminous infrared galaxy (LIRG) with an actively star forming disk (>50 kpc), central to its ~ 130 kpc gas disk, with a total star formation rate (SFR) of ~20.5 Msun yr^{-1}.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1010.3550v1-abstract-full').style.display = 'inline'; document.getElementById('1010.3550v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1010.3550v1-abstract-full" style="display: none;"> HIZOA J0836-43 is the most HI-massive (M_HI = 7.5x10^10 Msun) galaxy detected in the HIPASS volume and lies optically hidden behind the Milky Way. Markedly different from other extreme HI disks in the local universe, it is a luminous infrared galaxy (LIRG) with an actively star forming disk (>50 kpc), central to its ~ 130 kpc gas disk, with a total star formation rate (SFR) of ~20.5 Msun yr^{-1}. Spitzer spectroscopy reveals an unusual combination of powerful polycyclic aromatic hydrocarbon (PAH) emission coupled to a relatively weak warm dust continuum, suggesting photodissociation region (PDR)-dominated emission. Compared to a typical LIRG with similar total infrared luminosity (L_TIR=10^11 Lsun), the PAHs in HIZOA J0836-43 are more than twice as strong, whereas the warm dust continuum (lambda > 20micron) is best fit by a star forming galaxy with L_TIR=10^10 Lsun. Mopra CO observations suggest an extended molecular gas component (H_2 + He > 3.7x10^9 Msun) and a lower limit of ~ 64% for the gas mass fraction; this is above average compared to local disk systems, but similar to that of z~1.5 BzK galaxies (~57%). However, the star formation efficiency (SFE = L_IR/L'_CO) for HIZOA J0836-43 of 140 Lsun (K km s^{-1} pc^2)^{-1} is similar to that of local spirals and other disk galaxies at high redshift, in strong contrast to the increased SFE seen in merging and strongly interacting systems. HIZOA J0836-43 is actively forming stars and building a massive stellar disk. Its evolutionary phase of star formation (M_stellar, SFR, gas fraction) compared to more distant systems suggests that it would be considered typical at redshift z~1. This galaxy provides a rare opportunity in the nearby universe for studying (at z~0.036) how disks were building and galaxies evolving at z~1, when similarly large gas fractions were likely more common. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1010.3550v1-abstract-full').style.display = 'none'; document.getElementById('1010.3550v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 October, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal. 16 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1009.1753">arXiv:1009.1753</a> <span> [<a href="https://arxiv.org/pdf/1009.1753">pdf</a>, <a href="https://arxiv.org/ps/1009.1753">ps</a>, <a href="https://arxiv.org/format/1009.1753">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/j.1365-2966.2010.17672.x">10.1111/j.1365-2966.2010.17672.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for non-circular flows in the extended HI disc of NGC 2915 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Elson%2C+E+C">E. C. Elson</a>, <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1009.1753v1-abstract-short" style="display: inline;"> NGC 2915 is a nearby blue compact dwarf with a differentially rotating HI disc extending out to ~ 5 R-band R_{25} radii. This disc serves as an ideal tracer of the system's gravitational potential in regions of the galaxy that are dominated by dark matter. We use new HI synthesis observations of NGC 2915, obtained with the Australia Telescope Compact Array, to search for non-circular flows within… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.1753v1-abstract-full').style.display = 'inline'; document.getElementById('1009.1753v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1009.1753v1-abstract-full" style="display: none;"> NGC 2915 is a nearby blue compact dwarf with a differentially rotating HI disc extending out to ~ 5 R-band R_{25} radii. This disc serves as an ideal tracer of the system's gravitational potential in regions of the galaxy that are dominated by dark matter. We use new HI synthesis observations of NGC 2915, obtained with the Australia Telescope Compact Array, to search for non-circular flows within the outer HI disc. Two independent methods are used, and the results of each interpreted in the context of relevant axisymmetric and non-axisymmetric perturbations of the potential. We find evidence for: (1) elliptical streaming associated with the spiral structure of the HI disc and the central bar-like feature in the mass distribution, (2) a spherical dark matter halo, and (3) an axisymmetric radial outflow of ~ 5-17 km/s (~ 6-20 percent of the circular speed). A possible bar-like perturbation of the potential hinders attempts to unambiguously detect kinematic signatures of radial flows in the HI velocity field. The radial outflows are inconsistent with the plausible disc formation scenario in which gas from the surrounding inter-galactic medium is deposited on the outer HI disc and then transported towards the centre of the galaxy. They are, however, consistent with the possibility of some material being re-distributed towards the outer disc in order to conserve angular momentum as material flows inwards along a bar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.1753v1-abstract-full').style.display = 'none'; document.getElementById('1009.1753v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 September, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. 12 pages, 7 figures</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Kraan-Korteweg%2C+R+C&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

CINXE.COM

Search | arXiv e-print repository