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 196 results for author: <span class="mathjax">Umana, G</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/astro-ph" aria-role="search"> Searching in archive <strong>astro-ph</strong>. <a href="/search/?searchtype=author&query=Umana%2C+G">Search in all archives.</a> <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="Umana, G"> </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=Umana%2C+G&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="Umana, G"> <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=Umana%2C+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Umana%2C+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Umana%2C+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Umana%2C+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Umana%2C+G&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </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/2411.13051">arXiv:2411.13051</a> <span> [<a href="https://arxiv.org/pdf/2411.13051">pdf</a>, <a href="https://arxiv.org/ps/2411.13051">ps</a>, <a href="https://arxiv.org/format/2411.13051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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"> EWOCS-III: JWST observations of the supermassive star cluster Westerlund 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guarcello%2C+M+G">M. G. Guarcello</a>, <a href="/search/astro-ph?searchtype=author&query=Almendros-Abad%2C+V">V. Almendros-Abad</a>, <a href="/search/astro-ph?searchtype=author&query=Lovell%2C+J+B">J. B. Lovell</a>, <a href="/search/astro-ph?searchtype=author&query=Monsch%2C+K">K. Monsch</a>, <a href="/search/astro-ph?searchtype=author&query=Muzic%2C+K">K. Muzic</a>, <a href="/search/astro-ph?searchtype=author&query=Martiinez-Galarza%2C+J+R">J. R. Martiinez-Galarza</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">J. J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasopoulou%2C+K">K. Anastasopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M">M. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Argiroffi%2C+C">C. Argiroffi</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito%2C+R">R. Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=Capela%2C+D">D. Capela</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">M. Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ginsburg%2C+A">A. Ginsburg</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">E. K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Hora%2C+J+L">J. L. Hora</a>, <a href="/search/astro-ph?searchtype=author&query=Moraux%2C+E">E. Moraux</a>, <a href="/search/astro-ph?searchtype=author&query=Najarro%2C+F">F. Najarro</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Richardson%2C+N+D">N. D. Richardson</a>, <a href="/search/astro-ph?searchtype=author&query=Ritchie%2C+B">B. Ritchie</a>, <a href="/search/astro-ph?searchtype=author&query=Robberto%2C+M">M. Robberto</a> , et al. (7 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="2411.13051v1-abstract-short" style="display: inline;"> The typically large distances, extinction, and crowding of Galactic supermassive star clusters have so far hampered the identification of their very low mass members, required to extend our understanding of star and planet formation, and early stellar evolution, to starburst. This situation has now evolved thanks to the James Webb Space Telescope (JWST), and its unmatched resolution and sensitivit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13051v1-abstract-full').style.display = 'inline'; document.getElementById('2411.13051v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.13051v1-abstract-full" style="display: none;"> The typically large distances, extinction, and crowding of Galactic supermassive star clusters have so far hampered the identification of their very low mass members, required to extend our understanding of star and planet formation, and early stellar evolution, to starburst. This situation has now evolved thanks to the James Webb Space Telescope (JWST), and its unmatched resolution and sensitivity in the infrared. In this paper, the third of the series of the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS), we present JWST/NIRCam and JWST/MIRI observations of the supermassive star cluster Westerlund 1. These observations are specifically designed to unveil the cluster members down to the BD mass regime, and to allow us to select and study the protoplanetary disks and to study the mutual feedback between the cluster members and the surrounding environment. Westerlund 1 was observed as part of JWST GO-1905 for 23.6 hours. The data have been reduced using the JWST calibration pipeline, together with specific tools necessary to remove artifacts. Source identification and photometry were performed with DOLPHOT. The MIRI images show a plethora of different features. Diffuse nebular emission is observed around the cluster, which is typically composed of myriads of droplet-like features pointing toward the cluster center or the group of massive stars surrounding the WR star W72/A. A long pillar is also observed in the NW. The MIRI images also show resolved shells and outflows surrounding the M-type RSG W20, W26, W75, and W237, the sgB[e] star W9 and the YHG W4. The color-magnitude diagrams built using the NIRCam photometry show a clear cluster sequence, which is marked in its upper part by the 1828 NIRCam stars with X-ray counterparts. NIRCam observations using the F115W filter have reached the 23.8 mag limit with 50\% completeness (roughly corresponding to a 0.06 Msol brown dwarf). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13051v1-abstract-full').style.display = 'none'; document.getElementById('2411.13051v1-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> 20 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 Astronomy & 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/2409.16607">arXiv:2409.16607</a> <span> [<a href="https://arxiv.org/pdf/2409.16607">pdf</a>, <a href="https://arxiv.org/format/2409.16607">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"> Supernova Remnant Candidates Discovered by the SARAO MeerKAT Galactic Plane Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+L+D">L. D. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Faerber%2C+T">Timothy Faerber</a>, <a href="/search/astro-ph?searchtype=author&query=Bietenholz%2C+M">M. Bietenholz</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Rigby%2C+A">A. Rigby</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+G+M">G. M. 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="2409.16607v1-abstract-short" style="display: inline;"> Context. Sensitive radio continuum data could remove the difference between the number of known supernova remnants (SNRs) in the Galaxy compared to that expected, but due to confusion in the Galactic plane, faint SNRs can be challenging to distinguish from brighter HII regions and filamentary radio emission. Aims. We wish to exploit new SARAO MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS) radio con… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16607v1-abstract-full').style.display = 'inline'; document.getElementById('2409.16607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.16607v1-abstract-full" style="display: none;"> Context. Sensitive radio continuum data could remove the difference between the number of known supernova remnants (SNRs) in the Galaxy compared to that expected, but due to confusion in the Galactic plane, faint SNRs can be challenging to distinguish from brighter HII regions and filamentary radio emission. Aims. We wish to exploit new SARAO MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS) radio continuum data, which covers $251掳\le l \le 358掳$ and $2掳\le l \le 61掳$ at $|b|\le 1.5掳$, to search for SNR candidates in the Milky Way disk. Methods. We also use MIR data from the Spitzer GLIMPSE, Spitzer MIPSGAL, and WISE surveys to help identify SNR candidates. The identified SNR candidate are sources of extended radio continuum emission that lack MIR counterparts, are not known as HII regions in the WISE Catalog of Galactic HII Regions, and are not known previously as SNRs Results. We locate 237 new Galactic SNR candidates in the SMGPS data. We also identify and confirm the expected radio morphology for 201 objects listed in the literature as being SNRs and 130 previously-identified SNR candidates. The known and candidate SNRs have similar spatial distributions and angular sizes. Conclusions. The SMGPS data allowed us to identify a large population of SNR candidates that can be confirmed as true SNRs using radio polarization measurements or by deriving radio spectral indices. If the 237 candidates are confirmed as true SNRs, it would approximately double the number of known Galactic SNRs in the survey area, alleviating much of the difference between the known and expected populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16607v1-abstract-full').style.display = 'none'; document.getElementById('2409.16607v1-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, 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">Accepted by A&A. Images and FITS files of each source can be found here: https://doi.org/10.48479/0n8c-5q84</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.06383">arXiv:2409.06383</a> <span> [<a href="https://arxiv.org/pdf/2409.06383">pdf</a>, <a href="https://arxiv.org/format/2409.06383">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="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/10.1051/0004-6361/202451096">10.1051/0004-6361/202451096 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sifting the debris: Patterns in the SNR population with unsupervised ML methods </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Munari%2C+M">M. Munari</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A">A. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Vizzari%2C+G">G. Vizzari</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+A">A. De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</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="2409.06383v1-abstract-short" style="display: inline;"> Supernova remnants (SNRs) carry vast amounts of mechanical and radiative energy that heavily influence the structural, dynamical, and chemical evolution of galaxies. To this day, more than 300 SNRs have been discovered in the Milky Way, exhibiting a wide variety of observational features. However, existing classification schemes are mainly based on their radio morphology. In this work, we introduc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06383v1-abstract-full').style.display = 'inline'; document.getElementById('2409.06383v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.06383v1-abstract-full" style="display: none;"> Supernova remnants (SNRs) carry vast amounts of mechanical and radiative energy that heavily influence the structural, dynamical, and chemical evolution of galaxies. To this day, more than 300 SNRs have been discovered in the Milky Way, exhibiting a wide variety of observational features. However, existing classification schemes are mainly based on their radio morphology. In this work, we introduce a novel unsupervised deep learning pipeline to analyse a representative subsample of the Galactic SNR population ($\sim$ 50% of the total) with the aim of finding a connection between their multi-wavelength features and their physical properties. The pipeline involves two stages: (1) a representation learning stage, consisting of a convolutional autoencoder that feeds on imagery from infrared and radio continuum surveys (WISE 22$渭$m, Hi-GAL 70 $渭$m and SMGPS 30 cm) and produces a compact representation in a lower-dimensionality latent space; and (2) a clustering stage that seeks meaningful clusters in the latent space that can be linked to the physical properties of the SNRs and their surroundings. Our results suggest that this approach, when combined with an intermediate uniform manifold approximation and projection (UMAP) reprojection of the autoencoded embeddings into a more clusterable manifold, enables us to find reliable clusters. Despite a large number of sources being classified as outliers, most clusters relate to the presence of distinctive features, such as the distribution of infrared emission, the presence of radio shells and pulsar wind nebulae, and the existence of dust filaments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06383v1-abstract-full').style.display = 'none'; document.getElementById('2409.06383v1-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, 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">Accepted in A&A. 17 pages, 11 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/2408.07727">arXiv:2408.07727</a> <span> [<a href="https://arxiv.org/pdf/2408.07727">pdf</a>, <a href="https://arxiv.org/ps/2408.07727">ps</a>, <a href="https://arxiv.org/format/2408.07727">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="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1051/0004-6361/202450766">10.1051/0004-6361/202450766 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT reveals a ghostly thermal radio ring towards the Galactic Centre </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B">B. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Lazarevic%2C+S">S. Lazarevic</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Lundqvist%2C+P">P. Lundqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Mackey%2C+J">J. Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Payne%2C+J">J. Payne</a>, <a href="/search/astro-ph?searchtype=author&query=Rowell%2C+G">G. Rowell</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+J+R">J. R. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Ruggeri%2C+A+C">A. C. Ruggeri</a> , et al. (4 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="2408.07727v1-abstract-short" style="display: inline;"> We present the serendipitous discovery of a new radio-continuum ring-like object nicknamed Kyklos (J1802-3353), with MeerKAT UHF and L-band observations. The radio ring, which resembles the recently discovered odd radio circles (ORCs), has a diameter of 80 arcsec and is located just 6 deg from the Galactic plane. However, Kyklos exhibits an atypical thermal radio-continuum spectrum (伪 = -0.1 +/- 0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07727v1-abstract-full').style.display = 'inline'; document.getElementById('2408.07727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.07727v1-abstract-full" style="display: none;"> We present the serendipitous discovery of a new radio-continuum ring-like object nicknamed Kyklos (J1802-3353), with MeerKAT UHF and L-band observations. The radio ring, which resembles the recently discovered odd radio circles (ORCs), has a diameter of 80 arcsec and is located just 6 deg from the Galactic plane. However, Kyklos exhibits an atypical thermal radio-continuum spectrum (伪 = -0.1 +/- 0.3), which led us to explore different possible formation scenarios. We concluded that a circumstellar shell around an evolved massive star, possibly a Wolf-Rayet, is the most convincing explanation with the present data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07727v1-abstract-full').style.display = 'none'; document.getElementById('2408.07727v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">7 pages, 5 figures, accepted 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/2407.14217">arXiv:2407.14217</a> <span> [<a href="https://arxiv.org/pdf/2407.14217">pdf</a>, <a href="https://arxiv.org/format/2407.14217">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey 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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The chemistry of star and planet formation with SKA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Codella%2C+C">C. Codella</a>, <a href="/search/astro-ph?searchtype=author&query=Testi%2C+L">L. Testi</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+S">S. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+E">E. Bianchi</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="2407.14217v1-abstract-short" style="display: inline;"> In this contribution, we aim to summarise the efforts of the Italian SKA scientific community in conducting surveys of star-forming regions within our Galaxy, in the development of astrochemical research on protostellar envelopes and disks, and in studying the planet formation process itself. The objective is dual: Firstly, to investigate the accumulation and development of dust throughout the for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14217v1-abstract-full').style.display = 'inline'; document.getElementById('2407.14217v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.14217v1-abstract-full" style="display: none;"> In this contribution, we aim to summarise the efforts of the Italian SKA scientific community in conducting surveys of star-forming regions within our Galaxy, in the development of astrochemical research on protostellar envelopes and disks, and in studying the planet formation process itself. The objective is dual: Firstly, to investigate the accumulation and development of dust throughout the formation of planets, and secondly, to chemically examine protoplanetary disks and protostellar envelopes by studying heavy molecules, such as chains and rings containing over seven carbon atoms, which exhibit significantly reduced strength at millimeter wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14217v1-abstract-full').style.display = 'none'; document.getElementById('2407.14217v1-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">Mem. S.A.It. in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.18462">arXiv:2404.18462</a> <span> [<a href="https://arxiv.org/pdf/2404.18462">pdf</a>, <a href="https://arxiv.org/format/2404.18462">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1017/pasa.2024.84">10.1017/pasa.2024.84 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Self-supervised contrastive learning of radio data for source detection, classification and peculiar object discovery </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Palazzo%2C+S">S. Palazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+N">N. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Ruggeri%2C+A+C">A. C. Ruggeri</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</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="2404.18462v1-abstract-short" style="display: inline;"> New advancements in radio data post-processing are underway within the SKA precursor community, aiming to facilitate the extraction of scientific results from survey images through a semi-automated approach. Several of these developments leverage deep learning (DL) methodologies for diverse tasks, including source detection, object or morphology classification, and anomaly detection. Despite subst… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18462v1-abstract-full').style.display = 'inline'; document.getElementById('2404.18462v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.18462v1-abstract-full" style="display: none;"> New advancements in radio data post-processing are underway within the SKA precursor community, aiming to facilitate the extraction of scientific results from survey images through a semi-automated approach. Several of these developments leverage deep learning (DL) methodologies for diverse tasks, including source detection, object or morphology classification, and anomaly detection. Despite substantial progress, the full potential of these methods often remains untapped due to challenges associated with training large supervised models, particularly in the presence of small and class-unbalanced labelled datasets. Self-supervised learning has recently established itself as a powerful methodology to deal with some of the aforementioned challenges, by directly learning a lower-dimensional representation from large samples of unlabelled data. The resulting model and data representation can then be used for data inspection and various downstream tasks if a small subset of labelled data is available. In this work, we explored contrastive learning methods to learn suitable radio data representation from unlabelled images taken from the ASKAP EMU and SARAO MeerKAT GPS surveys. We evaluated trained models and the obtained data representation over smaller labelled datasets, also taken from different radio surveys, in selected analysis tasks: source detection and classification, and search for objects with peculiar morphology. For all explored downstream tasks, we reported and discussed the benefits brought by self-supervised foundational models built on radio data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18462v1-abstract-full').style.display = 'none'; document.getElementById('2404.18462v1-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> 29 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">21 pages, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Publ. Astron. Soc. Aust. 41 (2024) e085 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.04647">arXiv:2403.04647</a> <span> [<a href="https://arxiv.org/pdf/2403.04647">pdf</a>, <a href="https://arxiv.org/format/2403.04647">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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"> The distance to CRL 618 through its radio expansion parallax </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Menten%2C+K+M">K. M. Menten</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</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="2403.04647v1-abstract-short" style="display: inline;"> CRL 618 is a post-AGB star that has started to ionize its ejecta. Its central HII region has been observed over the last 40 years and has steadily increased in flux density at radio wavelengths. In this paper, we present data that we obtained with the Very Large Array in its highest frequency band (43 GHz) in 2011 and compare these with archival data in the same frequency band from 1998. By applyi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04647v1-abstract-full').style.display = 'inline'; document.getElementById('2403.04647v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.04647v1-abstract-full" style="display: none;"> CRL 618 is a post-AGB star that has started to ionize its ejecta. Its central HII region has been observed over the last 40 years and has steadily increased in flux density at radio wavelengths. In this paper, we present data that we obtained with the Very Large Array in its highest frequency band (43 GHz) in 2011 and compare these with archival data in the same frequency band from 1998. By applying the so-called expansion-parallax method, we are able to estimate an expansion rate of 4.0$\pm$0.4 mas yr$^{-1}$ along the major axis of the nebula and derive a distance of 1.1$\pm$0.2 kpc. Within errors, this distance estimation is in good agreement with the value of ~900 pc derived from the expansion of the optical lobes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04647v1-abstract-full').style.display = 'none'; document.getElementById('2403.04647v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">6 pages, 6 figures, accepted for publication on 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/2402.15232">arXiv:2402.15232</a> <span> [<a href="https://arxiv.org/pdf/2402.15232">pdf</a>, <a href="https://arxiv.org/format/2402.15232">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">stat.ML</span> </div> </div> <p class="title is-5 mathjax"> Classification of compact radio sources in the Galactic plane with supervised machine learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+Y">Y. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCrkan%2C+G">G. G眉rkan</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</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="2402.15232v1-abstract-short" style="display: inline;"> Generation of science-ready data from processed data products is one of the major challenges in next-generation radio continuum surveys with the Square Kilometre Array (SKA) and its precursors, due to the expected data volume and the need to achieve a high degree of automated processing. Source extraction, characterization, and classification are the major stages involved in this process. In this… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.15232v1-abstract-full').style.display = 'inline'; document.getElementById('2402.15232v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.15232v1-abstract-full" style="display: none;"> Generation of science-ready data from processed data products is one of the major challenges in next-generation radio continuum surveys with the Square Kilometre Array (SKA) and its precursors, due to the expected data volume and the need to achieve a high degree of automated processing. Source extraction, characterization, and classification are the major stages involved in this process. In this work we focus on the classification of compact radio sources in the Galactic plane using both radio and infrared images as inputs. To this aim, we produced a curated dataset of ~20,000 images of compact sources of different astronomical classes, obtained from past radio and infrared surveys, and novel radio data from pilot surveys carried out with the Australian SKA Pathfinder (ASKAP). Radio spectral index information was also obtained for a subset of the data. We then trained two different classifiers on the produced dataset. The first model uses gradient-boosted decision trees and is trained on a set of pre-computed features derived from the data, which include radio-infrared colour indices and the radio spectral index. The second model is trained directly on multi-channel images, employing convolutional neural networks. Using a completely supervised procedure, we obtained a high classification accuracy (F1-score>90%) for separating Galactic objects from the extragalactic background. Individual class discrimination performances, ranging from 60% to 75%, increased by 10% when adding far-infrared and spectral index information, with extragalactic objects, PNe and HII regions identified with higher accuracies. The implemented tools and trained models were publicly released, and made available to the radioastronomical community for future application on new radio data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.15232v1-abstract-full').style.display = 'none'; document.getElementById('2402.15232v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">27 pages, 15 figures, 9 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.08947">arXiv:2312.08947</a> <span> [<a href="https://arxiv.org/pdf/2312.08947">pdf</a>, <a href="https://arxiv.org/ps/2312.08947">ps</a>, <a href="https://arxiv.org/format/2312.08947">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey 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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Westerlund 1 and 2 Open Clusters Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guarcello%2C+M+G">M. G. Guarcello</a>, <a href="/search/astro-ph?searchtype=author&query=Flaccomio%2C+E">E. Flaccomio</a>, <a href="/search/astro-ph?searchtype=author&query=Albacete-Colombo%2C+J+F">J. F. Albacete-Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Almendros-Abad%2C+V">V. Almendros-Abad</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasopoulou%2C+K">K. Anastasopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M">M. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Argiroffi%2C+C">C. Argiroffi</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Bartlett%2C+E+S">E. S. Bartlett</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=De+Becker%2C+M">M. De Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Best%2C+W">W. Best</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito%2C+R">R. Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=Borghese%2C+A">A. Borghese</a>, <a href="/search/astro-ph?searchtype=author&query=Calzetti%2C+D">D. Calzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Castellanos%2C+R">R. Castellanos</a>, <a href="/search/astro-ph?searchtype=author&query=Cecchi-Pestellini%2C+C">C. Cecchi-Pestellini</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+S">S. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Clarke%2C+C+J">C. J. Clarke</a>, <a href="/search/astro-ph?searchtype=author&query=Zelati%2C+F+C">F. Coti Zelati</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">J. J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">M. Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ginsburg%2C+A">A. Ginsburg</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">E. K. Grebel</a> , et al. (26 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="2312.08947v2-abstract-short" style="display: inline;"> Context. With a mass exceeding several 10^4 solar masses and a rich and dense population of massive stars, supermassive young star clusters represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions among stars. Aims. In this paper we present the "Extended Westerlund 1 and 2 Open Clusters Survey" (EWOCS) project, which ai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08947v2-abstract-full').style.display = 'inline'; document.getElementById('2312.08947v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08947v2-abstract-full" style="display: none;"> Context. With a mass exceeding several 10^4 solar masses and a rich and dense population of massive stars, supermassive young star clusters represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions among stars. Aims. In this paper we present the "Extended Westerlund 1 and 2 Open Clusters Survey" (EWOCS) project, which aims to investigate the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars. The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun. Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically, the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec. Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation were carried out using the ACIS-Extract software. Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a photon flux threshold of approximately 2x10^-8 photons/cm^2/s. The X-ray sources exhibit a highly concentrated spatial distribution, with 1075 sources located within the central 1 arcminute. We have successfully detected X-ray emissions from 126 out of the 166 known massive stars of the cluster, and we have collected over 71000 photons from the magnetar CXO J164710.20-455217 <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08947v2-abstract-full').style.display = 'none'; document.getElementById('2312.08947v2-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> 15 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">The paper has been accepted for publication by 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/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/astro-ph?searchtype=author&query=Goedhart%2C+S">S. Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Bietenholz%2C+M">M. Bietenholz</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+L+D">L. D. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Egbo%2C+D">D. Egbo</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/astro-ph?searchtype=author&query=Hoare%2C+M+G">M. G. Hoare</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Irabor%2C+T">T. Irabor</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">S. Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?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/2312.06961">arXiv:2312.06961</a> <span> [<a href="https://arxiv.org/pdf/2312.06961">pdf</a>, <a href="https://arxiv.org/format/2312.06961">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/pasa.2024.13">10.1017/pasa.2024.13 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fast as Potoroo: Radio Continuum Detection of a Bow-Shock Pulsar Wind Nebula Powered by Pulsar J1638-4713 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lazarevi%C4%87%2C+S">Sanja Lazarevi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">Shi Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">Roland Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmad%2C+A">Adeel Ahmad</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">Rami Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Balzan%2C+J+C+F">Joel C. F. Balzan</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+L+A">Luke A. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">William D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Edwards%2C+P+G">Philip G. Edwards</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+Y+A">Yjan A. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B盲rbel S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">Denis Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">Chandreyee Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Mi%C4%87i%C4%87%2C+M">Marko Mi膰i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Rowell%2C+G">Gavin Rowell</a>, <a href="/search/astro-ph?searchtype=author&query=Sasaki%2C+M">Manami Sasaki</a>, <a href="/search/astro-ph?searchtype=author&query=Tothill%2C+N+F+H">Nicholas F. H. Tothill</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">Grazia Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Velovi%C4%87%2C+V">Velibor Velovi膰</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="2312.06961v2-abstract-short" style="display: inline;"> We report the discovery of a bow-shock pulsar wind nebula (PWN), named Potoroo, and the detection of a young pulsar J1638-4713 that powers the nebula. We present a radio continuum study of the PWN based on 20-cm observations obtained from the Australian Square Kilometre Array Pathfinder (ASKAP) and MeerKAT. PSR J1638-4713 was identified using Parkes radio telescope observations at frequencies abov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06961v2-abstract-full').style.display = 'inline'; document.getElementById('2312.06961v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.06961v2-abstract-full" style="display: none;"> We report the discovery of a bow-shock pulsar wind nebula (PWN), named Potoroo, and the detection of a young pulsar J1638-4713 that powers the nebula. We present a radio continuum study of the PWN based on 20-cm observations obtained from the Australian Square Kilometre Array Pathfinder (ASKAP) and MeerKAT. PSR J1638-4713 was identified using Parkes radio telescope observations at frequencies above 3 GHz. The pulsar has the second-highest dispersion measure of all known radio pulsars (1553 pc/cm^3), a spin period of 65.74 ms and a spin-down luminosity of 6.1x10^36 erg/s. The PWN has a cometary morphology and one of the greatest projected lengths among all the observed pulsar radio tails, measuring over 21 pc for an assumed distance of 10 kpc. The remarkably long tail and atypically steep radio spectral index are attributed to the interplay of a supernova reverse shock and the PWN. The originating supernova remnant is not known so far. We estimated the pulsar kick velocity to be in the range of 1000-2000 km/s for ages between 23 and 10 kyr. The X-ray counterpart found in Chandra data, CXOU J163802.6-471358, shows the same tail morphology as the radio source but is shorter by a factor of 10. The peak of the X-ray emission is offset from the peak of the radio total intensity (Stokes I) emission by approximately 4.7", but coincides well with circularly polarised (Stokes V) emission. No infrared counterpart was found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06961v2-abstract-full').style.display = 'none'; document.getElementById('2312.06961v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">16 pages, 8 figures, 4 tables; Accepted for publication in PASA on 18 Jan 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.08716">arXiv:2308.08716</a> <span> [<a href="https://arxiv.org/pdf/2308.08716">pdf</a>, <a href="https://arxiv.org/format/2308.08716">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> <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"> EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8-6.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">Shi Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Arbutina%2C+B">Bojan Arbutina</a>, <a href="/search/astro-ph?searchtype=author&query=Hurley-Walker%2C+N">Natasha Hurley-Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">Robert Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+W">Werner Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Sano%2C+H">Hidetoshi Sano</a>, <a href="/search/astro-ph?searchtype=author&query=Uro%C5%A1evi%C4%87%2C+D">Dejan Uro拧evi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">Rami Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Alsulami%2C+R">R. Alsulami</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">Cristobal Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Ball%2C+B">Brianna Ball</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">Christopher Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E">Evan Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=English%2C+J">Jayanne English</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">Adriano Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Kapinska%2C+A+D">Anna D. Kapinska</a>, <a href="/search/astro-ph?searchtype=author&query=Kavanagh%2C+P+J">Patrick J. Kavanagh</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B盲rbel S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">Roland Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Lazarevi%C4%87%2C+S">Sanja Lazarevi膰</a> , et al. (14 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="2308.08716v1-abstract-short" style="display: inline;"> We present the serendipitous detection of a new Galactic Supernova Remnant (SNR), G288.8-6.3 using data from the Australian Square Kilometre Array Pathfinder (ASKAP)-Evolutionary Map of the Universe (EMU) survey. Using multi-frequency analysis, we confirm this object as an evolved Galactic SNR at high Galactic latitude with low radio surface brightness and typical SNR spectral index of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.08716v1-abstract-full').style.display = 'inline'; document.getElementById('2308.08716v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.08716v1-abstract-full" style="display: none;"> We present the serendipitous detection of a new Galactic Supernova Remnant (SNR), G288.8-6.3 using data from the Australian Square Kilometre Array Pathfinder (ASKAP)-Evolutionary Map of the Universe (EMU) survey. Using multi-frequency analysis, we confirm this object as an evolved Galactic SNR at high Galactic latitude with low radio surface brightness and typical SNR spectral index of $伪= -0.41\pm0.12$. To determine the magnetic field strength in SNR G288.8-6.3, we present the first derivation of the equipartition formulae for SNRs with spectral indices $伪>-0.5$. The angular size is $1.\!^\circ 8\times 1.\!^\circ 6$ $(107.\!^\prime 6 \times 98.\!^\prime 4)$ and we estimate that its intrinsic size is $\sim40$pc which implies a distance of $\sim1.3$kpc and a position of $\sim140$pc above the Galactic plane. This is one of the largest angular size and closest Galactic SNRs. Given its low radio surface brightness, we suggest that it is about 13000 years old. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.08716v1-abstract-full').style.display = 'none'; document.getElementById('2308.08716v1-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> 16 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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 The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.11851">arXiv:2307.11851</a> <span> [<a href="https://arxiv.org/pdf/2307.11851">pdf</a>, <a href="https://arxiv.org/format/2307.11851">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1051/0004-6361/202346980">10.1051/0004-6361/202346980 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The rich molecular environment of the luminous blue variable star AFGL 2298 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+J+R">J. R. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</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="2307.11851v1-abstract-short" style="display: inline;"> We investigated the molecular environment of AFGL 2298, an obscured Galactic Luminous blue variable (LBV) star which hosts a highly structured circumstellar environment with hints of multiple mass-loss events in the last few $10^4$ a. We present spectral line observations of AFGL 2298 at 1 and 3 mm performed with the IRAM 30m radio telescope. Furthermore, we report the detection of several carbon-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.11851v1-abstract-full').style.display = 'inline'; document.getElementById('2307.11851v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.11851v1-abstract-full" style="display: none;"> We investigated the molecular environment of AFGL 2298, an obscured Galactic Luminous blue variable (LBV) star which hosts a highly structured circumstellar environment with hints of multiple mass-loss events in the last few $10^4$ a. We present spectral line observations of AFGL 2298 at 1 and 3 mm performed with the IRAM 30m radio telescope. Furthermore, we report the detection of several carbon- and nitrogen- bearing species (CO, $^{13}$CO, C$^{18}$O, C$^{17}$O, HCO$^+$, HCN, HNC, H$^{13}$CO$^+$, CN, N$_2$H$^+$, and C$_2$H) in the surroundings of AFGL 2298. In addition, we identified three velocity components that clearly stand out from the Galactic background. The morphology, kinematics, masses and isotopic ratios, together with a comparative study of the fractional abundances, lead us to suggest that two of these components (36 and 70 km/s) have a stellar origin. The other component (46 km/s) most likely traces swept-up interstellar material, probably harbouring also a photon-dominated region. The first inventory of the circumstellar molecular gas around AFGL 2298 is provided. The results are compatible with the hypothesis of former mass-loss events, produced before the one that created the infrared nebula. There are chemical hints of the presence of ejected stellar material, and also swept up gas. These findings will help to better understand the mass-loss history of this class of evolved massive stars, which heavily influence the overall chemical evolution of the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.11851v1-abstract-full').style.display = 'none'; document.getElementById('2307.11851v1-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> 21 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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 to Astronomy and Astrophysics. 15 pages, 4 tables, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A55 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.00809">arXiv:2305.00809</a> <span> [<a href="https://arxiv.org/pdf/2305.00809">pdf</a>, <a href="https://arxiv.org/format/2305.00809">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Star-Planet Interaction at radio wavelengths in YZ Ceti: Inferring planetary magnetic field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">Corrado Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Biswas%2C+A">Ayan Biswas</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">Paolo Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">Grazia Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Busa%2C+I">Innocenza Busa</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">Francesco Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+B">Barnali Das</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+P">Poonam Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Torres%2C+M">Miguel Perez-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Wade%2C+G+A">Gregg A. Wade</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">Cristobal Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">Carla S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">Adriano Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">Sara Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</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="2305.00809v1-abstract-short" style="display: inline;"> In exoplanetary systems, the interaction between the central star and the planet can trigger Auroral Radio Emission (ARE), due to the Electron Cyclotron Maser mechanism. The high brightness temperature of this emission makes it visible at large distances, opening new opportunities to study exoplanets and to search for favourable conditions for the development of extra-terrestrial life, as magnetic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.00809v1-abstract-full').style.display = 'inline'; document.getElementById('2305.00809v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.00809v1-abstract-full" style="display: none;"> In exoplanetary systems, the interaction between the central star and the planet can trigger Auroral Radio Emission (ARE), due to the Electron Cyclotron Maser mechanism. The high brightness temperature of this emission makes it visible at large distances, opening new opportunities to study exoplanets and to search for favourable conditions for the development of extra-terrestrial life, as magnetic fields act as a shield that protects life against external particles and influences the evolution of the planetary atmospheres. In the last few years, we started an observational campaign to observe a sample of nearby M-type stars known to host exoplanets with the aim to detect ARE. We observed YZ Ceti with the upgraded Giant Metrewave Radio Telescope (uGMRT) in band 4 (550-900 MHz) nine times over a period of five months. We detected radio emission four times, two of which with high degree of circular polarization. With statistical considerations we exclude the possibility of flares due to stellar magnetic activity. Instead, when folding the detections to the orbital phase of the closest planet YZ Cet b, they are at positions where we would expect ARE due to star-planet interaction (SPI) in sub-Alfvenic regime. With a degree of confidence higher than 4.37 sigma, YZ Cet is the first extrasolar systems with confirmed SPI at radio wavelengths. Modelling the ARE, we estimate a magnetic field for the star of about 2.4 kG and we find that the planet must have a magnetosphere. The lower limit for the polar magnetic field of the planet is 0.4 G. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.00809v1-abstract-full').style.display = 'none'; document.getElementById('2305.00809v1-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">11 pages, 7 figures, submitted to ApJ Letters in March 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.01988">arXiv:2301.01988</a> <span> [<a href="https://arxiv.org/pdf/2301.01988">pdf</a>, <a href="https://arxiv.org/format/2301.01988">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="Solar and Stellar Astrophysics">astro-ph.SR</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/stad005">10.1093/mnras/stad005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Co-Ordinated Radio and Infrared Survey for High-Mass Star Formation. V. The CORNISH-South Survey and Catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Irabor%2C+T">T. Irabor</a>, <a href="/search/astro-ph?searchtype=author&query=Hoare%2C+M+G">M. G. Hoare</a>, <a href="/search/astro-ph?searchtype=author&query=Burton%2C+M">M. Burton</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Diamond%2C+P">P. Diamond</a>, <a href="/search/astro-ph?searchtype=author&query=Dougherty%2C+S">S. Dougherty</a>, <a href="/search/astro-ph?searchtype=author&query=Ellingsen%2C+S+P">S. P. Ellingsen</a>, <a href="/search/astro-ph?searchtype=author&query=Fender%2C+R">R. Fender</a>, <a href="/search/astro-ph?searchtype=author&query=Fuller%2C+G+A">G. A. Fuller</a>, <a href="/search/astro-ph?searchtype=author&query=Garrington%2C+S">S. Garrington</a>, <a href="/search/astro-ph?searchtype=author&query=Goldsmith%2C+P+F">P. F. Goldsmith</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+J">J. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Gunn%2C+A+G">A. G. Gunn</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+J">J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtz%2C+S">S. Kurtz</a>, <a href="/search/astro-ph?searchtype=author&query=Lumsden%2C+S+L">S. L. Lumsden</a>, <a href="/search/astro-ph?searchtype=author&query=Marti%2C+J">J. Marti</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+I">I. McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+S">S. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Moore%2C+T+J">T. J. Moore</a>, <a href="/search/astro-ph?searchtype=author&query=Mutale%2C+M">M. Mutale</a>, <a href="/search/astro-ph?searchtype=author&query=Muxlow%2C+T">T. Muxlow</a>, <a href="/search/astro-ph?searchtype=author&query=OBrien%2C+T">T. OBrien</a>, <a href="/search/astro-ph?searchtype=author&query=Oudmaijer%2C+R+D">R. D. Oudmaijer</a>, <a href="/search/astro-ph?searchtype=author&query=Paladini%2C+R">R. Paladini</a> , et al. (10 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="2301.01988v1-abstract-short" style="display: inline;"> We present the first high spatial resolution radio continuum survey of the southern Galactic plane. The CORNISH project has mapped the region defined by $295^{\circ} < l < 350^{\circ}$; $|b| < 1^{\circ}$ at 5.5-GHz, with a resolution of 2.5$^{''}$ (FWHM). As with the CORNISH-North survey, this is designed to primarily provide matching radio data to the Spitzer GLIMPSE survey region. The CORNISH-So… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.01988v1-abstract-full').style.display = 'inline'; document.getElementById('2301.01988v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.01988v1-abstract-full" style="display: none;"> We present the first high spatial resolution radio continuum survey of the southern Galactic plane. The CORNISH project has mapped the region defined by $295^{\circ} < l < 350^{\circ}$; $|b| < 1^{\circ}$ at 5.5-GHz, with a resolution of 2.5$^{''}$ (FWHM). As with the CORNISH-North survey, this is designed to primarily provide matching radio data to the Spitzer GLIMPSE survey region. The CORNISH-South survey achieved a root mean square noise level of $\sim$ 0.11 mJy beam$^{-1}$, using the 6A configuration of the Australia Telescope Compact Array (ATCA). In this paper, we discuss the observations, data processing and measurements of the source properties. Above a 7$蟽$ detection limit, 4701 sources were detected, and their ensemble properties show similar distributions with their northern counterparts. The catalogue is highly reliable and is complete to 90 per cent at a flux density level of 1.1 mJy. We developed a new way of measuring the integrated flux densities and angular sizes of non-Gaussian sources. The catalogue primarily provides positions, flux density measurements and angular sizes. All sources with IR counterparts at 8$渭m$ have been visually classified, utilizing additional imaging data from optical, near-IR, mid-IR, far-IR and sub-millimetre galactic plane surveys. This has resulted in the detection of 524 H II regions of which 255 are ultra-compact H II regions, 287 planetary nebulae, 79 radio stars and 6 massive young stellar objects. The rest of the sources are likely to be extra-galactic. These data are particularly important in the characterization and population studies of compact ionized sources such as UCHII regions and PNe towards the Galactic mid-plane. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.01988v1-abstract-full').style.display = 'none'; document.getElementById('2301.01988v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.02538">arXiv:2212.02538</a> <span> [<a href="https://arxiv.org/pdf/2212.02538">pdf</a>, <a href="https://arxiv.org/format/2212.02538">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Astronomical source detection in radio continuum maps with deep neural networks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Magro%2C+D">D. Magro</a>, <a href="/search/astro-ph?searchtype=author&query=Sortino%2C+R">R. Sortino</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+A">A. De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Marvil%2C+J">J. Marvil</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Fiameni%2C+G">G. Fiameni</a>, <a href="/search/astro-ph?searchtype=author&query=Spampinato%2C+C">C. Spampinato</a>, <a href="/search/astro-ph?searchtype=author&query=Adami%2C+K+Z">K. Zarb Adami</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="2212.02538v1-abstract-short" style="display: inline;"> Source finding is one of the most challenging tasks in upcoming radio continuum surveys with SKA precursors, such as the Evolutionary Map of the Universe (EMU) survey of the Australian SKA Pathfinder (ASKAP) telescope. The resolution, sensitivity, and sky coverage of such surveys is unprecedented, requiring new features and improvements to be made in existing source finders. Among them, reducing t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02538v1-abstract-full').style.display = 'inline'; document.getElementById('2212.02538v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.02538v1-abstract-full" style="display: none;"> Source finding is one of the most challenging tasks in upcoming radio continuum surveys with SKA precursors, such as the Evolutionary Map of the Universe (EMU) survey of the Australian SKA Pathfinder (ASKAP) telescope. The resolution, sensitivity, and sky coverage of such surveys is unprecedented, requiring new features and improvements to be made in existing source finders. Among them, reducing the false detection rate, particularly in the Galactic plane, and the ability to associate multiple disjoint islands into physical objects. To bridge this gap, we developed a new source finder, based on the Mask R-CNN object detection framework, capable of both detecting and classifying compact, extended, spurious, and poorly imaged sources in radio continuum images. The model was trained using ASKAP EMU data, observed during the Early Science and pilot survey phase, and previous radio survey data, taken with the VLA and ATCA telescopes. On the test sample, the final model achieves an overall detection completeness above 85\%, a reliability of $\sim$65\%, and a classification precision/recall above 90\%. Results obtained for all source classes are reported and discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02538v1-abstract-full').style.display = 'none'; document.getElementById('2212.02538v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">18 pages, 11 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/2210.09774">arXiv:2210.09774</a> <span> [<a href="https://arxiv.org/pdf/2210.09774">pdf</a>, <a href="https://arxiv.org/format/2210.09774">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="Solar and Stellar Astrophysics">astro-ph.SR</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/ac9b10">10.3847/2041-8213/ac9b10 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First detection of silicon-bearing molecules in $畏$ Car </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+J+R">J. R. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana-Lacaci%2C+G">G. Quintana-Lacaci</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</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="2210.09774v1-abstract-short" style="display: inline;"> We present ALMA band 6 observations of the luminous blue variable Eta Car, obtained within the ALMAGAL program. We report SiO J=5-4, SiS J=12-11 and SiN N=5-4 emission in the equatorial region of the Homunculus nebula, constituting the first detection of silicon- and sulphur-bearing molecules in the outskirts of a highly evolved, early-type massive star. SiO, SiS and SiN trace a clumpy equatorial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.09774v1-abstract-full').style.display = 'inline'; document.getElementById('2210.09774v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.09774v1-abstract-full" style="display: none;"> We present ALMA band 6 observations of the luminous blue variable Eta Car, obtained within the ALMAGAL program. We report SiO J=5-4, SiS J=12-11 and SiN N=5-4 emission in the equatorial region of the Homunculus nebula, constituting the first detection of silicon- and sulphur-bearing molecules in the outskirts of a highly evolved, early-type massive star. SiO, SiS and SiN trace a clumpy equatorial ring that surrounds the central binary at a projected distance of 2 arcsec, delineating the inner rims of the butterfly-shaped dusty region. The formation of silicon-bearing compounds is presumably related to the continuous recycling of dust due to the variable wind regime of Eta Car, that destroys grains and releases silicon back to gas phase. We discuss possible formation routes for the observed species, contextualizing them within the current molecular inventory of Eta Car. We find that the SiO and SiS fractional abundances in localised clumps of the ring, $6.7\times10^{-9}$ and $1.2\times10^{-8}$ respectively, are exceptionally lower than those measured in C- and O-rich AGB stars and cool supergiants; while the higher SiN abundance, $3.6\times10^{-8}$, evidences the nitrogen-rich chemistry of the ejecta. These abundances must be regarded as strict upper limits, since the distribution of H2 in the Homunculus is unknown. In any case, these findings shed new light onto the peculiar molecular ecosystem of Eta Car, and establish its surroundings as a new laboratory to investigate the lifecycle of silicate dust in extreme astrophysical conditions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.09774v1-abstract-full').style.display = 'none'; document.getElementById('2210.09774v1-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, 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">17 pages, 7 figures. Accepted in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.03181">arXiv:2208.03181</a> <span> [<a href="https://arxiv.org/pdf/2208.03181">pdf</a>, <a href="https://arxiv.org/format/2208.03181">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> <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/10.1016/j.jheap.2022.06.006">10.1016/j.jheap.2022.06.006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galactic Observatory Science with the ASTRI Mini-Array at the Observatorio del Teide </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27A%C3%AC%2C+A">A. D'A矛</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Burtovoi%2C+A">A. Burtovoi</a>, <a href="/search/astro-ph?searchtype=author&query=Compagnino%2C+A+A">A. A. Compagnino</a>, <a href="/search/astro-ph?searchtype=author&query=Fiori%2C+M">M. Fiori</a>, <a href="/search/astro-ph?searchtype=author&query=Giuliani%2C+A">A. Giuliani</a>, <a href="/search/astro-ph?searchtype=author&query=La+Palombara%2C+N">N. La Palombara</a>, <a href="/search/astro-ph?searchtype=author&query=Paizis%2C+A">A. Paizis</a>, <a href="/search/astro-ph?searchtype=author&query=Piano%2C+G">G. Piano</a>, <a href="/search/astro-ph?searchtype=author&query=Saturni%2C+F+G">F. G. Saturni</a>, <a href="/search/astro-ph?searchtype=author&query=Tutone%2C+A">A. Tutone</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+A">A. Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Cardillo%2C+M">M. Cardillo</a>, <a href="/search/astro-ph?searchtype=author&query=Crestan%2C+S">S. Crestan</a>, <a href="/search/astro-ph?searchtype=author&query=Cusumano%2C+G">G. Cusumano</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Valle%2C+M">M. Della Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Santo%2C+M">M. Del Santo</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+A">A. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=La+Parola%2C+V">V. La Parola</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+S">S. Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Mereghetti%2C+S">S. Mereghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Morlino%2C+G">G. Morlino</a>, <a href="/search/astro-ph?searchtype=author&query=Pintore%2C+F">F. Pintore</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+P">P. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a> , et al. (30 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="2208.03181v1-abstract-short" style="display: inline;"> The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Mini-Array will be composed of nine imaging atmospheric Cherenkov telescopes at the Observatorio del Teide site. The array will be best suited for astrophysical observations in the 0.3-200 TeV range with an angular resolution of few arc-minutes and an energy resolution of 10-15\%. A core-science programme in the first four years… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.03181v1-abstract-full').style.display = 'inline'; document.getElementById('2208.03181v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.03181v1-abstract-full" style="display: none;"> The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Mini-Array will be composed of nine imaging atmospheric Cherenkov telescopes at the Observatorio del Teide site. The array will be best suited for astrophysical observations in the 0.3-200 TeV range with an angular resolution of few arc-minutes and an energy resolution of 10-15\%. A core-science programme in the first four years will be devoted to a limited number of key targets, addressing the most important open scientific questions in the very-high energy domain. At the same time, thanks to a wide field of view of about 10 degrees, ASTRI Mini-Array will observe many additional field sources, which will constitute the basis for the long-term observatory programme that will eventually cover all the accessible sky. In this paper, we review different astrophysical Galactic environments, e.g. pulsar wind nebulae, supernova remnants, and gamma-ray binaries, and show the results from a set of ASTRI Mini-Array simulations of some of these field sources made to highlight the expected performance of the array (even at large offset angles) and the important additional observatory science that will complement the core-science program. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.03181v1-abstract-full').style.display = 'none'; document.getElementById('2208.03181v1-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Accepted for publication in Journal of High-Energy Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEAP, Volume 35, August 2022, Pages 139-175 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.03177">arXiv:2208.03177</a> <span> [<a href="https://arxiv.org/pdf/2208.03177">pdf</a>, <a href="https://arxiv.org/format/2208.03177">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> <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/10.1016/j.jheap.2022.05.005">10.1016/j.jheap.2022.05.005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ASTRI Mini-Array Core Science at the Observatorio del Teide </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/astro-ph?searchtype=author&query=Burtovoi%2C+A">A. Burtovoi</a>, <a href="/search/astro-ph?searchtype=author&query=Cardillo%2C+M">M. Cardillo</a>, <a href="/search/astro-ph?searchtype=author&query=Catalano%2C+O">O. Catalano</a>, <a href="/search/astro-ph?searchtype=author&query=Franceschini%2C+A">A. Franceschini</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+S">S. Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Nava%2C+L">L. Nava</a>, <a href="/search/astro-ph?searchtype=author&query=Pintore%2C+F">F. Pintore</a>, <a href="/search/astro-ph?searchtype=author&query=Stamerra%2C+A">A. Stamerra</a>, <a href="/search/astro-ph?searchtype=author&query=Tavecchio%2C+F">F. Tavecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Zampieri%2C+L">L. Zampieri</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+J+B">J. Becerra Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Bottcher%2C+M">M. Bottcher</a>, <a href="/search/astro-ph?searchtype=author&query=Brunetti%2C+G">G. Brunetti</a>, <a href="/search/astro-ph?searchtype=author&query=Compagnino%2C+A+A">A. A. Compagnino</a>, <a href="/search/astro-ph?searchtype=author&query=Crestan%2C+S">S. Crestan</a>, <a href="/search/astro-ph?searchtype=author&query=Ai%2C+A+D">A. D Ai</a>, <a href="/search/astro-ph?searchtype=author&query=Fiori%2C+M">M. Fiori</a>, <a href="/search/astro-ph?searchtype=author&query=Galanti%2C+G">G. Galanti</a> , et al. (62 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="2208.03177v1-abstract-short" style="display: inline;"> The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Project led by the Italian National Institute for Astrophysics (INAF) is developing and will deploy at the Observatorio del Teide a mini-array (ASTRI Mini-Array) composed of nine telescopes similar to the small-size dual-mirror Schwarzschild-Couder telescope (ASTRI-Horn) currently operating on the slopes of Mt. Etna in Sicily.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.03177v1-abstract-full').style.display = 'inline'; document.getElementById('2208.03177v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.03177v1-abstract-full" style="display: none;"> The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Project led by the Italian National Institute for Astrophysics (INAF) is developing and will deploy at the Observatorio del Teide a mini-array (ASTRI Mini-Array) composed of nine telescopes similar to the small-size dual-mirror Schwarzschild-Couder telescope (ASTRI-Horn) currently operating on the slopes of Mt. Etna in Sicily. The ASTRI Mini-Array will surpass the current Cherenkov telescope array differential sensitivity above a few tera-electronvolt (TeV), extending the energy band well above hundreds of TeV. This will allow us to explore a new window of the electromagnetic spectrum, by convolving the sensitivity performance with excellent angular and energy resolution figures. In this paper we describe the Core Science that we will address during the first four years of operation, providing examples of the breakthrough results that we will obtain when dealing with current open questions, such as the acceleration of cosmic rays, cosmology and fundamental physics and the new window, for the TeV energy band, of the time-domain astrophysics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.03177v1-abstract-full').style.display = 'none'; document.getElementById('2208.03177v1-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Published in Journal of High Energy Astrophysics. 46 Figures, 7 Tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of High Energy Astrophysics, Volume 35, August 2022, Pages 1-42 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.14075">arXiv:2207.14075</a> <span> [<a href="https://arxiv.org/pdf/2207.14075">pdf</a>, <a href="https://arxiv.org/ps/2207.14075">ps</a>, <a href="https://arxiv.org/format/2207.14075">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/stac2163">10.1093/mnras/stac2163 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery and origin of the radio emission from the multiple stellar system KQVel </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Shultz%2C+M+E">M. E. Shultz</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Krticka%2C+J">J. Krticka</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzaro%2C+G">G. Catanzaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Giarrusso%2C+M">M. Giarrusso</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Owocki%2C+S+P">S. P. Owocki</a>, <a href="/search/astro-ph?searchtype=author&query=Postnov%2C+K+A">K. A. Postnov</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</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="2207.14075v1-abstract-short" style="display: inline;"> KQVel is a binary system composed of a slowly rotating magnetic Ap star with a companion of unknown nature. In this paper, we report the detection of its radio emission. We conducted a multi-frequency radio campaign using the ATCA interferometer (band-names: 16cm, 4cm, and 15mm). The target was detected in all bands. The most obvious explanation for the radio emission is that it originates in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.14075v1-abstract-full').style.display = 'inline'; document.getElementById('2207.14075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.14075v1-abstract-full" style="display: none;"> KQVel is a binary system composed of a slowly rotating magnetic Ap star with a companion of unknown nature. In this paper, we report the detection of its radio emission. We conducted a multi-frequency radio campaign using the ATCA interferometer (band-names: 16cm, 4cm, and 15mm). The target was detected in all bands. The most obvious explanation for the radio emission is that it originates in the magnetosphere of the Ap star, but this is shown unfeasible. The known stellar parameters of the Ap star enable us to exploit the scaling relationship for non-thermal gyro-synchrotron emission from early-type magnetic stars. This is a general relation demonstrating how radio emission from stars with centrifugal magnetospheres is supported by rotation. Using KQVel's parameters the predicted radio luminosity is more than five orders of magnitudes lower than the measured one. The extremely long rotation period rules out the Ap star as the source of the observed radio emission. Other possible explanations for the radio emission from KQVel, involving its unknown companion, have been explored. A scenario that matches the observed features (i.e. radio luminosity and spectrum, correlation to X-rays) is a hierarchical stellar system, where the possible companion of the magnetic star is a close binary (possibly of RSCVn type) with at least one magnetically active late-type star. To be compatible with the total mass of the system, the last scenario places strong constraints on the orbital inclination of the KQVel stellar system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.14075v1-abstract-full').style.display = 'none'; document.getElementById('2207.14075v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Accepted to MNRAS; 16 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/2201.10026">arXiv:2201.10026</a> <span> [<a href="https://arxiv.org/pdf/2201.10026">pdf</a>, <a href="https://arxiv.org/format/2201.10026">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> <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/stac210">10.1093/mnras/stac210 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mysterious Odd Radio Circle near the Large Magellanic Cloud -- An Intergalactic Supernova Remnant? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Macgregor%2C+P+J">P. J. Macgregor</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Ducci%2C+L">L. Ducci</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+L">L. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I+S">I. S. Boji膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Crocker%2C+R+M">R. M. Crocker</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Galvin%2C+T+J">T. J. Galvin</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Heber%2C+U">U. Heber</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+T">T. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Hurley-Walker%2C+N">N. Hurley-Walker</a> , et al. (26 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="2201.10026v1-abstract-short" style="display: inline;"> We report the discovery of J0624-6948, a low-surface brightness radio ring, lying between the Galactic Plane and the Large Magellanic Cloud (LMC). It was first detected at 888 MHz with the Australian Square Kilometre Array Pathfinder (ASKAP), and with a diameter of ~196 arcsec. This source has phenomenological similarities to Odd Radio Circles (ORCs). Significant differences to the known ORCs - a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10026v1-abstract-full').style.display = 'inline'; document.getElementById('2201.10026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.10026v1-abstract-full" style="display: none;"> We report the discovery of J0624-6948, a low-surface brightness radio ring, lying between the Galactic Plane and the Large Magellanic Cloud (LMC). It was first detected at 888 MHz with the Australian Square Kilometre Array Pathfinder (ASKAP), and with a diameter of ~196 arcsec. This source has phenomenological similarities to Odd Radio Circles (ORCs). Significant differences to the known ORCs - a flatter radio spectral index, the lack of a prominent central galaxy as a possible host, and larger apparent size - suggest that J0624-6948 may be a different type of object. We argue that the most plausible explanation for J0624-6948 is an intergalactic supernova remnant due to a star that resided in the LMC outskirts that had undergone a single-degenerate type Ia supernova, and we are seeing its remnant expand into a rarefied, intergalactic environment. We also examine if a massive star or a white dwarf binary ejected from either galaxy could be the supernova progenitor. Finally, we consider several other hypotheses for the nature of the object, including the jets of an active galactic nucleus (AGN) or the remnant of a nearby stellar super-flare. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10026v1-abstract-full').style.display = 'none'; document.getElementById('2201.10026v1-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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 accepted to 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/2108.01951">arXiv:2108.01951</a> <span> [<a href="https://arxiv.org/pdf/2108.01951">pdf</a>, <a href="https://arxiv.org/format/2108.01951">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey 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/10.1051/0004-6361/202141569">10.1051/0004-6361/202141569 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modeling the Remnants of Core-collapse Supernovae from Luminous Blue Variable stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ustamujic%2C+S">S. Ustamujic</a>, <a href="/search/astro-ph?searchtype=author&query=Orlando%2C+S">S. Orlando</a>, <a href="/search/astro-ph?searchtype=author&query=Miceli%2C+M">M. Miceli</a>, <a href="/search/astro-ph?searchtype=author&query=Bocchino%2C+F">F. Bocchino</a>, <a href="/search/astro-ph?searchtype=author&query=Limongi%2C+M">M. Limongi</a>, <a href="/search/astro-ph?searchtype=author&query=Chieffi%2C+A">A. Chieffi</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Peres%2C+G">G. Peres</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="2108.01951v1-abstract-short" style="display: inline;"> LBVs are massive evolved stars that suffer sporadic and violent mass-loss events. They have been proposed as the progenitors of some core-collapse SNe, but this idea is still debated due to the lack of direct evidence. Since SNRs can carry in their morphology the fingerprints of the progenitor stars as well as of the inhomogeneous CSM sculpted by the progenitors, the study of SNRs from LBVs could… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01951v1-abstract-full').style.display = 'inline'; document.getElementById('2108.01951v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.01951v1-abstract-full" style="display: none;"> LBVs are massive evolved stars that suffer sporadic and violent mass-loss events. They have been proposed as the progenitors of some core-collapse SNe, but this idea is still debated due to the lack of direct evidence. Since SNRs can carry in their morphology the fingerprints of the progenitor stars as well as of the inhomogeneous CSM sculpted by the progenitors, the study of SNRs from LBVs could help to place core-collapse SNe in context with the evolution of massive stars. We investigate the physical, chemical and morphological properties of the remnants of SNe originating from LBVs, in order to search for signatures, revealing the nature of the progenitors, in the ejecta distribution and morphology of the remnants. As a template of LBVs, we considered the actual LBV candidate Gal 026.47+0.02. We selected a grid of models, which describe the evolution of a massive star with properties consistent with those of Gal 026.47+0.02 and its final fate as core-collapse SN. We developed a 3D HD model that follows the post-explosion evolution of the ejecta from the breakout of the shock wave at the stellar surface to the interaction of the SNR with a CSM characterized by two dense nested toroidal shells, parametrized in agreement with multi-wavelength observations of Gal 026.47+0.02. Our models show a strong interaction of the blast wave with the CSM which determines an important slowdown of the expansion of the ejecta in the equatorial plane where the two shells lay, determining a high degree of asymmetry in the remnant. After 10000 years of evolution the ejecta show an elongated shape forming a broad jet-like structure caused by the interaction with the shells and oriented along the axis of the toroidal shells. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01951v1-abstract-full').style.display = 'none'; document.getElementById('2108.01951v1-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> 4 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">18 pages, 12 figures; accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, A167 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.11995">arXiv:2107.11995</a> <span> [<a href="https://arxiv.org/pdf/2107.11995">pdf</a>, <a href="https://arxiv.org/ps/2107.11995">ps</a>, <a href="https://arxiv.org/format/2107.11995">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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/stab2168">10.1093/mnras/stab2168 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A scaling relationship for non-thermal radio emission from ordered magnetospheres: from the top of the Main Sequence to planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Krticka%2C+J">J. Krticka</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Shultz%2C+M+E">M. E. Shultz</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Todt%2C+H">H. Todt</a>, <a href="/search/astro-ph?searchtype=author&query=Giarrusso%2C+M">M. Giarrusso</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</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="2107.11995v1-abstract-short" style="display: inline;"> In this paper, we present the analysis of incoherent non-thermal radio emission from a sample of hot magnetic stars, ranging from early-B to early-A spectral type. Spanning a wide range of stellar parameters and wind properties, these stars display a commonality in their radio emission which presents new challenges to the wind scenario as originally conceived. It was thought that relativistic elec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.11995v1-abstract-full').style.display = 'inline'; document.getElementById('2107.11995v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.11995v1-abstract-full" style="display: none;"> In this paper, we present the analysis of incoherent non-thermal radio emission from a sample of hot magnetic stars, ranging from early-B to early-A spectral type. Spanning a wide range of stellar parameters and wind properties, these stars display a commonality in their radio emission which presents new challenges to the wind scenario as originally conceived. It was thought that relativistic electrons, responsible for the radio emission, originate in current sheets formed where the wind opens the magnetic field lines. However, the true mass-loss rates from the cooler stars are too small to explain the observed non-thermal broadband radio spectra. Instead, we suggest the existence of a radiation belt located inside the inner-magnetosphere, similar to that of Jupiter. Such a structure explains the overall indifference of the broadband radio emissions on wind mass-loss rates. Further, correlating the radio luminosities from a larger sample of magnetic stars with their stellar parameters, the combined roles of rotation and magnetic properties have been empirically determined. Finally, our sample of early-type magnetic stars suggests a scaling relationship between the non-thermal radio luminosity and the electric voltage induced by the magnetosphere's co-rotation, which appears to hold for a broader range of stellar types with dipole-dominated magnetospheres (like the cases of the planet Jupiter and the ultra-cool dwarf stars and brown dwarfs). We conclude that well-ordered and stable rotating magnetospheres share a common physical mechanism for supporting the generation of non-thermal electrons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.11995v1-abstract-full').style.display = 'none'; document.getElementById('2107.11995v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Accepted to MNRAS; 26 pages, 13 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/2107.10967">arXiv:2107.10967</a> <span> [<a href="https://arxiv.org/pdf/2107.10967">pdf</a>, <a href="https://arxiv.org/format/2107.10967">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/stab2249">10.1093/mnras/stab2249 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio Continuum Sources behind the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I+S">I. S. Boji膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Grieve%2C+K+R">K. R. Grieve</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Tothill%2C+N+F+H">N. F. H. Tothill</a>, <a href="/search/astro-ph?searchtype=author&query=Shobhana%2C+D">D. Shobhana</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Hurley-Walker%2C+N">N. Hurley-Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+C+S">C. S. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=For%2C+B+-">B. -Q. For</a>, <a href="/search/astro-ph?searchtype=author&query=Galvin%2C+T+J">T. J. Galvin</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Leverenz%2C+H">H. Leverenz</a>, <a href="/search/astro-ph?searchtype=author&query=Maggi%2C+P">P. Maggi</a> , et al. (16 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="2107.10967v1-abstract-short" style="display: inline;"> We present a comprehensive multi-frequency catalogue of radio sources behind the Large Magellanic Cloud between 0.2 and 20 GHz, gathered from a combination of new and legacy radio continuum surveys. This catalogue covers an area of $\sim$144~deg$^2$ at angular resolutions from 45 arcsec to $\sim$3 arcmin. We find 6434 discrete radio sources in total, of which 3789 are detected at two or more radio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10967v1-abstract-full').style.display = 'inline'; document.getElementById('2107.10967v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10967v1-abstract-full" style="display: none;"> We present a comprehensive multi-frequency catalogue of radio sources behind the Large Magellanic Cloud between 0.2 and 20 GHz, gathered from a combination of new and legacy radio continuum surveys. This catalogue covers an area of $\sim$144~deg$^2$ at angular resolutions from 45 arcsec to $\sim$3 arcmin. We find 6434 discrete radio sources in total, of which 3789 are detected at two or more radio frequencies. We estimate the median spectral index ($伪$; where $S_{v}\sim谓^伪$) of $伪= -0.89 $ and mean of $-0.88 \pm 0.48$ for 3636 sources detected exclusively at two frequencies (0.843 and 1.384 GHz) with similar resolution (FWHM $\sim$40-45 arcsec). The large frequency range of the surveys makes it an effective tool to investigate Gigahertz Peak Spectrum (GPS), Compact Steep Spectrum (CSS) and Infrared Faint Radio sources populations within our sample. We find 10 GPS candidates with peak frequencies near 5 GHz, from which we estimate their linear size. 1866 sources from our catalogue are (CSS) candidates with $伪<-0.8$. We found six candidates for High Frequency Peaker (HFP) sources, whose radio fluxes peak above 5 GHz and no sources with unconstrained peaks and $伪~>0.5$. We found optical counterparts for 343 of the radio continuum sources, of which 128have a redshift measurement. Finally, we investigate the population of 123 Infrared Faint Radio Sources (IFRSs) found in this study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10967v1-abstract-full').style.display = 'none'; document.getElementById('2107.10967v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">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/2102.08494">arXiv:2102.08494</a> <span> [<a href="https://arxiv.org/pdf/2102.08494">pdf</a>, <a href="https://arxiv.org/format/2102.08494">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/abe711">10.3847/1538-4357/abe711 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Planck submillimeter properties of Galactic high-mass star forming regions: dust temperatures, luminosities, masses and Star Formation Efficiency </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Paladini%2C+R">R. Paladini</a>, <a href="/search/astro-ph?searchtype=author&query=Mottram%2C+J+C">J. C. Mottram</a>, <a href="/search/astro-ph?searchtype=author&query=Veneziani%2C+M">M. Veneziani</a>, <a href="/search/astro-ph?searchtype=author&query=Traficante%2C+A">A. Traficante</a>, <a href="/search/astro-ph?searchtype=author&query=Schisano%2C+E">E. Schisano</a>, <a href="/search/astro-ph?searchtype=author&query=Giardino%2C+G">G. Giardino</a>, <a href="/search/astro-ph?searchtype=author&query=Falgarone%2C+E">E. Falgarone</a>, <a href="/search/astro-ph?searchtype=author&query=Urquhart%2C+J+S">J. S. Urquhart</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+D+L">D. L. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Joncas%2C+G">G. Joncas</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+S">S. Molinari</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="2102.08494v1-abstract-short" style="display: inline;"> Massive star formation occurs in the interior of giant molecular clouds (GMC) and proceeds through many stages. In this work, we focus on massive young stellar objects (MYSOs) and Ultra-Compact HII regions (UCHII), where the former are enshrouded in dense envelopes of dust and gas, which the latter have begun dispersing. By selecting a complete sample of MYSOs and UCHII from the Red MSX Source (RM… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.08494v1-abstract-full').style.display = 'inline'; document.getElementById('2102.08494v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.08494v1-abstract-full" style="display: none;"> Massive star formation occurs in the interior of giant molecular clouds (GMC) and proceeds through many stages. In this work, we focus on massive young stellar objects (MYSOs) and Ultra-Compact HII regions (UCHII), where the former are enshrouded in dense envelopes of dust and gas, which the latter have begun dispersing. By selecting a complete sample of MYSOs and UCHII from the Red MSX Source (RMS) survey data base, we combine Planck and IRAS data and build their Spectral Energy Distributions (SEDs). With these, we estimate the physical properties (dust temperatures, mass, luminosity) of the sample. Because the RMS database provides unique solar distances, it also allows investigating the instantaneous Star Formation Efficiency (SFE) as a function of Galactocentric radius. We find that the SFE increase between 2 and 4.5 kpc, where it reaches a peak, likely in correspondence of the accumulation of molecular material at the end of the Galactic bar. It then stays approximately constant up to 9 kpc, after which it linearly declines, in agreement with predictions from extragalactic studies. This behavior suggests the presence of a significant amount of undetected molecular gas at R$_G$ $>$ 8 kpc. Finally we present diagnostic colors that can be used to identify sites of massive star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.08494v1-abstract-full').style.display = 'none'; document.getElementById('2102.08494v1-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> 16 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">Accepted for publication to 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/2101.03843">arXiv:2101.03843</a> <span> [<a href="https://arxiv.org/pdf/2101.03843">pdf</a>, <a href="https://arxiv.org/format/2101.03843">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">stat.ML</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/stab028">10.1093/mnras/stab028 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evolutionary Map of the Universe (EMU):Compact radio sources in the SCORPIO field towards the Galactic plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=van+Loon%2C+J+T">J. Th. van Loon</a>, <a href="/search/astro-ph?searchtype=author&query=Micha%C5%82owski%2C+M+J">M. J. Micha艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+T">T. An</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Carretti%2C+E">E. Carretti</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=Joseph%2C+T">T. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=McConnell%2C+D">D. McConnell</a>, <a href="/search/astro-ph?searchtype=author&query=Pommier%2C+M">M. Pommier</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a> , et al. (4 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="2101.03843v1-abstract-short" style="display: inline;"> We present observations of a region of the Galactic plane taken during the Early Science Program of the Australian Square Kilometre Array Pathfinder (ASKAP). In this context, we observed the SCORPIO field at 912 MHz with an uncompleted array consisting of 15 commissioned antennas. The resulting map covers a square region of ~40 deg^2, centred on (l, b)=(343.5掳, 0.75掳), with a synthesized beam of 2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03843v1-abstract-full').style.display = 'inline'; document.getElementById('2101.03843v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.03843v1-abstract-full" style="display: none;"> We present observations of a region of the Galactic plane taken during the Early Science Program of the Australian Square Kilometre Array Pathfinder (ASKAP). In this context, we observed the SCORPIO field at 912 MHz with an uncompleted array consisting of 15 commissioned antennas. The resulting map covers a square region of ~40 deg^2, centred on (l, b)=(343.5掳, 0.75掳), with a synthesized beam of 24"x21" and a background rms noise of 150-200 渭Jy/beam, increasing to 500-600 渭Jy/beam close to the Galactic plane. A total of 3963 radio sources were detected and characterized in the field using the CAESAR source finder. We obtained differential source counts in agreement with previously published data after correction for source extraction and characterization uncertainties, estimated from simulated data. The ASKAP positional and flux density scale accuracy were also investigated through comparison with previous surveys (MGPS, NVSS) and additional observations of the SCORPIO field, carried out with ATCA at 2.1 GHz and 10" spatial resolution. These allowed us to obtain a measurement of the spectral index for a subset of the catalogued sources and an estimated fraction of (at least) 8% of resolved sources in the reported catalogue. We cross-matched our catalogued sources with different astronomical databases to search for possible counterparts, finding ~150 associations to known Galactic objects. Finally, we explored a multiparametric approach for classifying previously unreported Galactic sources based on their radio-infrared colors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03843v1-abstract-full').style.display = 'none'; document.getElementById('2101.03843v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">31 pages, 15 figures, 15 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02116">arXiv:2012.02116</a> <span> [<a href="https://arxiv.org/pdf/2012.02116">pdf</a>, <a href="https://arxiv.org/format/2012.02116">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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/10.1051/0004-6361/202039052">10.1051/0004-6361/202039052 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monitoring the radio emission of Proxima Centauri </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Torres%2C+M">Miguel P茅rez-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+J+F">Jos茅 Francisco G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+J+L">Jos茅 Luis Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">Paolo Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada%2C+G">Guillem Anglada</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+J+L">Jos茅 Luis G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+E">Eloy Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">Corrado Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Amado%2C+P+J">Pedro J. Amado</a>, <a href="/search/astro-ph?searchtype=author&query=Alberdi%2C+A">Antonio Alberdi</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada-Escud%C3%A9%2C+G">Guillem Anglada-Escud茅</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M">Mayra Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">Grazia Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Berdi%C3%B1as%2C+Z">Zaira Berdi帽as</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Gonz%C3%A1lez%2C+M+J">Mar铆a Jos茅 L贸pez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Morales%2C+N">Nicol谩s Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez-L%C3%B3pez%2C+C">Cristina Rodr铆guez-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J">James Chibueze</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="2012.02116v2-abstract-short" style="display: inline;"> We present results from the most comprehensive radio monitoring campaign towards the closest star to our Sun, Proxima Centauri. We report 1.1 to 3.1 GHz observations with the Australian Telescope Compact Array over 18 consecutive days in April 2017. We detect radio emission from Proxima Centauri for most of the observing sessions, which spanned $\sim$1.6 orbital periods of the planet Proxima b. Th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02116v2-abstract-full').style.display = 'inline'; document.getElementById('2012.02116v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02116v2-abstract-full" style="display: none;"> We present results from the most comprehensive radio monitoring campaign towards the closest star to our Sun, Proxima Centauri. We report 1.1 to 3.1 GHz observations with the Australian Telescope Compact Array over 18 consecutive days in April 2017. We detect radio emission from Proxima Centauri for most of the observing sessions, which spanned $\sim$1.6 orbital periods of the planet Proxima b. The radio emission is stronger at the low-frequency band, centered around 1.6 GHz, and is consistent with the expected electron-cyclotron frequency for the known star's magnetic field intensity of about 600 Gauss. The 1.6 GHz light curve shows an emission pattern that is consistent with the orbital period of the planet Proxima b around the star Proxima, with its maxima of emission happening near the quadratures. We also observed two short-duration (a few minutes) flares and a long-duration (about three days) burst whose peaks happened close to the quadratures. We find that the frequency, large degree of circular polarization, change of the sign of circular polarization, and intensity of the observed radio emission are all consistent with expectations from electron cyclotron-maser emission arising from sub-Alfv茅nic star-planet interaction. We interpret our radio observations as signatures of interaction between the planet Proxima b and its host star Proxima. We advocate for monitoring other dwarf stars with planets to eventually reveal periodic radio emission due to star-planet interaction, thus opening a new avenue for exoplanet hunting and the study of a new field of exoplanet-star plasma interaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02116v2-abstract-full').style.display = 'none'; document.getElementById('2012.02116v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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, 11 figures. Accepted on December 2, 2020 in A&A (main journal), several typos corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 645, A77 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.08161">arXiv:2011.08161</a> <span> [<a href="https://arxiv.org/pdf/2011.08161">pdf</a>, <a href="https://arxiv.org/format/2011.08161">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="Solar and Stellar Astrophysics">astro-ph.SR</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/staa3606">10.1093/mnras/staa3606 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A warm molecular ring in AG Car: composing the mass-loss puzzle </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+J+R">J. R. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</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="2011.08161v1-abstract-short" style="display: inline;"> We present APEX observations of CO J=3-2 and ALMA observations of CO J=2-1, 13CO J=2-1 and continuum toward the galactic luminous blue variable AG Car. These new observations reveal the presence of a ring-like molecular structure surrounding the star. Morphology and kinematics of the gas are consistent with a slowly expanding torus located near the equatorial plane of AG Car. Using non-LTE line mo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08161v1-abstract-full').style.display = 'inline'; document.getElementById('2011.08161v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.08161v1-abstract-full" style="display: none;"> We present APEX observations of CO J=3-2 and ALMA observations of CO J=2-1, 13CO J=2-1 and continuum toward the galactic luminous blue variable AG Car. These new observations reveal the presence of a ring-like molecular structure surrounding the star. Morphology and kinematics of the gas are consistent with a slowly expanding torus located near the equatorial plane of AG Car. Using non-LTE line modelling, we derived the physical parameters of the gas, which is warm (50 K) and moderately dense (10$^3$ cm$^{-3}$. The total mass of molecular gas in the ring is 2.7$\pm$0.9 solar masses. We analysed the radio continuum map, which depicts a point-like source surrounded by a shallow nebula. From the flux of the point-like source, we derived a current mass-loss date of $1.55\pm0.21\times10^{-5}$ solar masses / yr. Finally, to better understand the complex circumstellar environment of AG Car, we put the newly detected ring in relation to the main nebula of dust and ionised gas. We discuss possible formation scenarios for the ring, namely, the accumulation of interstellar material due to the action of the stellar wind, the remnant of a close binary interaction or merger, and an equatorially enhanced mass-loss episode. If molecular gas formed in situ as a result of a mass eruption, it would account for at least a 30$\%$ of the total mass ejected by AG Car. This detection adds a new piece to the puzzle of the complex mass-loss history of AG Car, providing new clues about the interplay between LBV stars and their surroundings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08161v1-abstract-full').style.display = 'none'; document.getElementById('2011.08161v1-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> 16 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">16 pages, 13 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/2010.01349">arXiv:2010.01349</a> <span> [<a href="https://arxiv.org/pdf/2010.01349">pdf</a>, <a href="https://arxiv.org/format/2010.01349">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> <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/10.1088/1475-7516/2021/02/048">10.1088/1475-7516/2021/02/048 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=B%2C+R+A">R. Alves B</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Araudo%2C+A">A. Araudo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M">M. Ashley</a> , et al. (474 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="2010.01349v2-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for $纬$-ray astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of $纬$-ray cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nucle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.01349v2-abstract-full').style.display = 'inline'; document.getElementById('2010.01349v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.01349v2-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for $纬$-ray astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of $纬$-ray cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nuclei (AGN) and of their relativistic jets. Observations of AGN with CTA will enable a measurement of $纬$-ray absorption on the extragalactic background light with a statistical uncertainty below 15% up to a redshift $z=2$ and to constrain or detect $纬$-ray halos up to intergalactic-magnetic-field strengths of at least 0.3pG. Extragalactic observations with CTA also show promising potential to probe physics beyond the Standard Model. The best limits on Lorentz invariance violation from $纬$-ray astronomy will be improved by a factor of at least two to three. CTA will also probe the parameter space in which axion-like particles could constitute a significant fraction, if not all, of dark matter. We conclude on the synergies between CTA and other upcoming facilities that will foster the growth of $纬$-ray cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.01349v2-abstract-full').style.display = 'none'; document.getElementById('2010.01349v2-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">71 pages (including affiliations and references), 13 figures, 6 tables. Accepted in JCAP; matches published version. Corresponding authors: Jonathan Biteau, Julien Lefaucheur, Humberto Martinez-Huerta, Manuel Meyer, Santiago Pita, Ievgen Vovk</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 02 (2021) 048 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.09948">arXiv:2009.09948</a> <span> [<a href="https://arxiv.org/pdf/2009.09948">pdf</a>, <a href="https://arxiv.org/format/2009.09948">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/staa2868">10.1093/mnras/staa2868 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New high-frequency radio observations of the Cygnus Loop supernova remnant with the Italian radio telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Pellizzoni%2C+A">A. Pellizzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Egron%2C+E">E. Egron</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Morlino%2C+G">G. Morlino</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">S. Celli</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Iacolina%2C+M+N">M. N. Iacolina</a>, <a href="/search/astro-ph?searchtype=author&query=Righini%2C+S">S. Righini</a>, <a href="/search/astro-ph?searchtype=author&query=Reich%2C+P">P. Reich</a>, <a href="/search/astro-ph?searchtype=author&query=Mulas%2C+S">S. Mulas</a>, <a href="/search/astro-ph?searchtype=author&query=Marongiu%2C+M">M. Marongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">M. Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Melis%2C+A">A. Melis</a>, <a href="/search/astro-ph?searchtype=author&query=Concu%2C+R">R. Concu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+M">M. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Schillir%C3%B2%2C+F">F. Schillir貌</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="2009.09948v1-abstract-short" style="display: inline;"> Supernova remnants (SNRs) represent a powerful laboratory to study the Cosmic-Ray acceleration processes at the shocks, and their relation to the properties of the circumstellar medium. With the aim of studying the high-frequency radio emission and investigating the energy distribution of accelerated electrons and the magnetic field conditions, we performed single-dish observations of the large an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09948v1-abstract-full').style.display = 'inline'; document.getElementById('2009.09948v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.09948v1-abstract-full" style="display: none;"> Supernova remnants (SNRs) represent a powerful laboratory to study the Cosmic-Ray acceleration processes at the shocks, and their relation to the properties of the circumstellar medium. With the aim of studying the high-frequency radio emission and investigating the energy distribution of accelerated electrons and the magnetic field conditions, we performed single-dish observations of the large and complex Cygnus Loop SNR from 7.0 to 24.8 GHz with the Medicina and the Sardinia Radio Telescope, focusing on the northern filament (NGC 6992) and the southern shell. Both regions show a spectrum well fitted by a power-law function ($S\propto谓^{-伪}$), with spectral index $伪=0.45\pm0.05$ for NGC 6992 and $伪=0.49\pm0.01$ for the southern shell and without any indication of a spectral break. The spectra are significantly flatter than the whole Cygnus Loop spectrum ($伪=0.54\pm0.01$), suggesting a departure from the plain shock acceleration mechanisms, which for NGC 6992 could be related to the ongoing transition towards a radiative shock. We model the integrated spectrum of the whole SNR considering the evolution of the maximum energy and magnetic field amplification. Through the radio spectral parameters, we infer a magnetic field at the shock of 10 $渭$G. This value is compatible with a pure adiabatic compression of the interstellar magnetic field, suggesting that the amplification process is currently inefficient. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09948v1-abstract-full').style.display = 'none'; document.getElementById('2009.09948v1-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> 21 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">19 pages, 13 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/2009.02363">arXiv:2009.02363</a> <span> [<a href="https://arxiv.org/pdf/2009.02363">pdf</a>, <a href="https://arxiv.org/ps/2009.02363">ps</a>, <a href="https://arxiv.org/format/2009.02363">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey 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/slaa157">10.1093/mnrasl/slaa157 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The auroral radio emission of the magnetic B-type star rho OphC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Krticka%2C+J">J. Krticka</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzaro%2C+G">G. Catanzaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Schilliro%2C+F">F. Schilliro</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Giarrusso%2C+M">M. Giarrusso</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</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="2009.02363v1-abstract-short" style="display: inline;"> The non-thermal radio emission of main-sequence early-type stars is a signature of stellar magnetism. We present multi-wavelength (1.6-16.7 GHz) ATCA measurements of the early-type magnetic star rho OphC, which is a flat-spectrum non-thermal radio source. The rho OphC radio emission is partially circularly polarized with a steep spectral dependence: the fraction of polarized emission is about 60%… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.02363v1-abstract-full').style.display = 'inline'; document.getElementById('2009.02363v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.02363v1-abstract-full" style="display: none;"> The non-thermal radio emission of main-sequence early-type stars is a signature of stellar magnetism. We present multi-wavelength (1.6-16.7 GHz) ATCA measurements of the early-type magnetic star rho OphC, which is a flat-spectrum non-thermal radio source. The rho OphC radio emission is partially circularly polarized with a steep spectral dependence: the fraction of polarized emission is about 60% at the lowest frequency sub-band (1.6 GHz) while is undetected at 16.7 GHz. This is clear evidence of coherent Auroral Radio Emission (ARE) from the rho OphC magnetosphere. Interestingly, the detection of the rho OphC's ARE is not related to a peculiar rotational phase. This is a consequence of the stellar geometry, which makes the strongly anisotropic radiation beam of the amplified radiation always pointed towards Earth. The circular polarization sign evidences mainly amplification of the ordinary mode of the electromagnetic wave, consistent with a maser amplification occurring within dense regions. This is indirect evidence of the plasma evaporation from the polar caps, a phenomenon responsible for the thermal X-ray aurorae. rho OphC is not the first early-type magnetic star showing the O-mode dominated ARE but is the first star with the ARE always on view. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.02363v1-abstract-full').style.display = 'none'; document.getElementById('2009.02363v1-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> 4 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">5 pages, 4 figures; accepted to MNRAS Letter</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.09251">arXiv:2002.09251</a> <span> [<a href="https://arxiv.org/pdf/2002.09251">pdf</a>, <a href="https://arxiv.org/ps/2002.09251">ps</a>, <a href="https://arxiv.org/format/2002.09251">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/staa587">10.1093/mnras/staa587 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for radio and X-ray auroral emissions from the magnetic B-type star rho Oph A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Krticka%2C+J">J. Krticka</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzaro%2C+G">G. Catanzaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Munari%2C+M">M. Munari</a>, <a href="/search/astro-ph?searchtype=author&query=Gangi%2C+M">M. Gangi</a>, <a href="/search/astro-ph?searchtype=author&query=Giarrusso%2C+M">M. Giarrusso</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</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="2002.09251v2-abstract-short" style="display: inline;"> We present new ATCA multi-wavelength radio measurements (range 2.1-21.2 GHz) of the early-type magnetic star rho Oph A, performed in March 2019 during 3 different observing sessions. These new ATCA observations evidence a clear rotational modulation of the stellar radio emission and the detection of coherent auroral radio emission from rho Oph A at 2.1 GHz. We collected high-resolution optical spe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.09251v2-abstract-full').style.display = 'inline'; document.getElementById('2002.09251v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.09251v2-abstract-full" style="display: none;"> We present new ATCA multi-wavelength radio measurements (range 2.1-21.2 GHz) of the early-type magnetic star rho Oph A, performed in March 2019 during 3 different observing sessions. These new ATCA observations evidence a clear rotational modulation of the stellar radio emission and the detection of coherent auroral radio emission from rho Oph A at 2.1 GHz. We collected high-resolution optical spectra of rho Oph A acquired by several instruments over a time span of about ten years. We also report new magnetic field measurements of rho Oph A that, together with the radio light curves and the temporal variation of the equivalent width of the HeI line (lambda=5015 Angstrom), were used to constrain the rotation period and the stellar magnetic field geometry. The above results have been used to model the stellar radio emission, modelling that allowed us to constrain the physical condition of rho Oph A's magnetosphere. Past XMM measurements showed periodic X-ray pulses from rho Oph A. We correlate the X-ray light curve with the magnetic field geometry of rho Oph A. The already published XMM data have been re-analyzed showing that the X-ray spectra of rho Oph A are compatible with the presence of a non-thermal X-ray component. We discuss a scenario where the emission phenomena occurring at the extremes of the electromagnetic spectrum, radio and X-ray, are directly induced by the same plasma process. We interpret the observed X-ray and radio features of rho Oph A as having an auroral origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.09251v2-abstract-full').style.display = 'none'; document.getElementById('2002.09251v2-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 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">20 pages, 13 figures; accepted to 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/2002.01283">arXiv:2002.01283</a> <span> [<a href="https://arxiv.org/pdf/2002.01283">pdf</a>, <a href="https://arxiv.org/ps/2002.01283">ps</a>, <a href="https://arxiv.org/format/2002.01283">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Distributed, Parallel, and Cluster Computing">cs.DC</span> </div> </div> <p class="title is-5 mathjax"> CHIPP: INAF pilot project for HTC, HPC and HPDA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Taffoni%2C+G">Giuliano Taffoni</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">Ugo Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">Bianca Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Maggio%2C+G">Gianmarco Maggio</a>, <a href="/search/astro-ph?searchtype=author&query=Pasian%2C+F">Fabio Pasian</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">Grazia Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Smareglia%2C+R">Riccardo Smareglia</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">Fabio Vitello</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="2002.01283v1-abstract-short" style="display: inline;"> CHIPP (Computing HTC in INAF Pilot Project) is an Italian project funded by the Italian Institute for Astrophysics (INAF) and promoted by the ICT office of INAF. The main purpose of the CHIPP project is to coordinate the use of, and access to, already existing high throughput computing and high-performance computing and data processing resources (for small/medium size programs) for the INAF commun… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.01283v1-abstract-full').style.display = 'inline'; document.getElementById('2002.01283v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.01283v1-abstract-full" style="display: none;"> CHIPP (Computing HTC in INAF Pilot Project) is an Italian project funded by the Italian Institute for Astrophysics (INAF) and promoted by the ICT office of INAF. The main purpose of the CHIPP project is to coordinate the use of, and access to, already existing high throughput computing and high-performance computing and data processing resources (for small/medium size programs) for the INAF community. Today, Tier2/Tier3 systems (1,200 CPU/core) are provided at the INAF institutes at Trieste and Catania, but in the future, the project will evolve including also other computing infrastructures. During the last two years, more than 30 programs have been approved for a total request of 30 Million CPU-h. Most of the programs are HPC, data reduction and analysis, machine learning. In this paper, we describe in details the CHIPP infrastructures and the results of the first two years of activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.01283v1-abstract-full').style.display = 'none'; document.getElementById('2002.01283v1-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> 4 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">4 pages, conference, ADASS 2019</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.04020">arXiv:1912.04020</a> <span> [<a href="https://arxiv.org/pdf/1912.04020">pdf</a>, <a href="https://arxiv.org/format/1912.04020">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="Solar and Stellar Astrophysics">astro-ph.SR</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/stz3466">10.1093/mnras/stz3466 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hi-GAL catalogue of dusty filamentary structures in the Galactic Plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schisano%2C+E">E. Schisano</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+S">S. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Elia%2C+D">D. Elia</a>, <a href="/search/astro-ph?searchtype=author&query=Benedettini%2C+M">M. Benedettini</a>, <a href="/search/astro-ph?searchtype=author&query=Olmi%2C+L">L. Olmi</a>, <a href="/search/astro-ph?searchtype=author&query=Pezzuto%2C+S">S. Pezzuto</a>, <a href="/search/astro-ph?searchtype=author&query=Traficante%2C+A">A. Traficante</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">S. Cavuoti</a>, <a href="/search/astro-ph?searchtype=author&query=di+Giorgio%2C+A+M">A. M. di Giorgio</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+S+J">S. J. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Moore%2C+T+J+T">T. J. T. Moore</a>, <a href="/search/astro-ph?searchtype=author&query=Noriega-Crespo%2C+A">A. Noriega-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Riccio%2C+G">G. Riccio</a>, <a href="/search/astro-ph?searchtype=author&query=Baldeschi%2C+A">A. Baldeschi</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">U. Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Peretto%2C+N">N. Peretto</a>, <a href="/search/astro-ph?searchtype=author&query=Merello%2C+M">M. Merello</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Zavagno%2C+A">A. Zavagno</a>, <a href="/search/astro-ph?searchtype=author&query=Beltr%C3%A1n%2C+M+T">M. T. Beltr谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Cambr%C3%A9sy%2C+L">L. Cambr茅sy</a>, <a href="/search/astro-ph?searchtype=author&query=Eden%2C+D+J">D. J. Eden</a>, <a href="/search/astro-ph?searchtype=author&query=Causi%2C+G+L">G. Li Causi</a>, <a href="/search/astro-ph?searchtype=author&query=Molinaro%2C+M">M. Molinaro</a> , et al. (5 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="1912.04020v1-abstract-short" style="display: inline;"> The recent data collected by {\it Herschel} have confirmed that interstellar structures with filamentary shape are ubiquitously present in the Milky Way. Filaments are thought to be formed by several physical mechanisms acting from the large Galactic scales down to the sub-pc fractions of molecular clouds, and they might represent a possible link between star formation and the large-scale structur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.04020v1-abstract-full').style.display = 'inline'; document.getElementById('1912.04020v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.04020v1-abstract-full" style="display: none;"> The recent data collected by {\it Herschel} have confirmed that interstellar structures with filamentary shape are ubiquitously present in the Milky Way. Filaments are thought to be formed by several physical mechanisms acting from the large Galactic scales down to the sub-pc fractions of molecular clouds, and they might represent a possible link between star formation and the large-scale structure of the Galaxy. In order to study this potential link, a statistically significant sample of filaments spread throughout the Galaxy is required. In this work we present the first catalogue of $32,059$ candidate filaments automatically identified in the Hi-GAL survey of the entire Galactic Plane. For these objects we determined morphological (length, $l^{a}$, and geometrical shape) and physical (average column density, $N_{\rm H_{2}}$, and average temperature, $T$) properties. We identified filaments with a wide range of properties: 2$'$\,$\leq l^{a}\leq$\, 100$'$, $10^{20} \leq N_{\rm H_{2}} \leq 10^{23}$\,cm$^{-2}$ and $10 \leq T\leq$ 35\,K. We discuss their association with the Hi-GAL compact sources, finding that the most tenuous (and stable) structures do not host any major condensation and we also assign a distance to $\sim 18,400$ filaments for which we determine mass, physical size, stability conditions and Galactic distribution. When compared to the spiral arms structure, we find no significant difference between the physical properties of on-arm and inter-arm filaments. We compared our sample with previous studies, finding that our Hi-GAL filament catalogue represents a significant extension in terms of Galactic coverage and sensitivity. This catalogue represents an unique and important tool for future studies devoted to understanding the filament life-cycle. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.04020v1-abstract-full').style.display = 'none'; document.getElementById('1912.04020v1-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">38 pages, 29 figures, 3 appendices</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.11592">arXiv:1910.11592</a> <span> [<a href="https://arxiv.org/pdf/1910.11592">pdf</a>, <a href="https://arxiv.org/format/1910.11592">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/mnras/stz2982">10.1093/mnras/stz2982 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of the Galactic radio sources in the SCORPIO survey resolved by ATCA at 2.1 GHz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Franzen%2C+T+M+O">T. M. O. Franzen</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Schillir%C3%B2%2C+F">F. Schillir貌</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</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="1910.11592v1-abstract-short" style="display: inline;"> We present a catalogue of a large sample of extended radio sources in the SCORPIO field, observed and resolved by the Australia Telescope Compact Array. SCORPIO, a pathfinder project for addressing the early operations of the Australia SKA Pathfinder, is a survey of ~5 square degrees between 1.4 and 3.1 GHz, centered at l=343.5掳, b=0.75掳 and with an angular resolution of about 10 arcsec. It is aim… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.11592v1-abstract-full').style.display = 'inline'; document.getElementById('1910.11592v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.11592v1-abstract-full" style="display: none;"> We present a catalogue of a large sample of extended radio sources in the SCORPIO field, observed and resolved by the Australia Telescope Compact Array. SCORPIO, a pathfinder project for addressing the early operations of the Australia SKA Pathfinder, is a survey of ~5 square degrees between 1.4 and 3.1 GHz, centered at l=343.5掳, b=0.75掳 and with an angular resolution of about 10 arcsec. It is aimed at understanding the scientific and technical challenges to be faced by future Galactic surveys. With a mean sensitivity around 100 $渭$Jy/beam and the possibility to recover angular scales at least up to 4 arcmin, we extracted 99 extended sources, 35 of them detected for the first time. Among the 64 known sources 55 had at least a tentative classification in literature. Studying the radio morphology and comparing the radio emission with infrared we propose as candidates 6 new H II regions, 2 new planetary nebulae, 2 new luminous blue variable or Wolf--Rayet stars and 3 new supernova remnants. This study provides an overview of the potentiality of future radio surveys in terms of Galactic source extraction and characterization and a discussion on the difficulty to reduce and analyze interferometric data on the Galactic plane. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.11592v1-abstract-full').style.display = 'none'; document.getElementById('1910.11592v1-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.12149">arXiv:1909.12149</a> <span> [<a href="https://arxiv.org/pdf/1909.12149">pdf</a>, <a href="https://arxiv.org/ps/1909.12149">ps</a>, <a href="https://arxiv.org/format/1909.12149">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey 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/10.1051/0004-6361/201936791">10.1051/0004-6361/201936791 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First detection of the Crab Nebula at TeV energies with a Cherenkov telescope in a dual-mirror Schwarzschild-Couder configuration: the ASTRI-Horn telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+S">S. Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Catalano%2C+O">O. Catalano</a>, <a href="/search/astro-ph?searchtype=author&query=Scuderi%2C+S">S. Scuderi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Pareschi%2C+G">G. Pareschi</a>, <a href="/search/astro-ph?searchtype=author&query=Antolini%2C+E">E. Antolini</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Bellassai%2C+G">G. Bellassai</a>, <a href="/search/astro-ph?searchtype=author&query=Bernloehr%2C+K">K. Bernloehr</a>, <a href="/search/astro-ph?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/astro-ph?searchtype=author&query=Biondo%2C+B">B. Biondo</a>, <a href="/search/astro-ph?searchtype=author&query=Bonanno%2C+G">G. Bonanno</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Bottcher%2C+G+M">G. M. Bottcher</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+P">P. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Canestrari%2C+R">R. Canestrari</a>, <a href="/search/astro-ph?searchtype=author&query=Capalbi%2C+M">M. Capalbi</a>, <a href="/search/astro-ph?searchtype=author&query=Caraveo%2C+P">P. Caraveo</a>, <a href="/search/astro-ph?searchtype=author&query=Conconi%2C+P">P. Conconi</a>, <a href="/search/astro-ph?searchtype=author&query=Conforti%2C+V">V. Conforti</a>, <a href="/search/astro-ph?searchtype=author&query=Contino%2C+G">G. Contino</a>, <a href="/search/astro-ph?searchtype=author&query=Cusumano%2C+G">G. Cusumano</a>, <a href="/search/astro-ph?searchtype=author&query=Pino%2C+M+d+G+D">M. de Gouveia Dal Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Distefano%2C+A">A. Distefano</a> , et al. (68 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="1909.12149v3-abstract-short" style="display: inline;"> We report on the first detection of very high-energy (VHE) gamma-ray emission from the Crab Nebula by a Cherenkov telescope in dual-mirror Schwarzschild-Couder (SC) configuration. The result has been achieved by means of the 4 m size ASTRI-Horn telescope, operated on Mt. Etna (Italy) and developed in the context of the Cherenkov Telescope Array Observatory preparatory phase. The dual-mirror SC des… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.12149v3-abstract-full').style.display = 'inline'; document.getElementById('1909.12149v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.12149v3-abstract-full" style="display: none;"> We report on the first detection of very high-energy (VHE) gamma-ray emission from the Crab Nebula by a Cherenkov telescope in dual-mirror Schwarzschild-Couder (SC) configuration. The result has been achieved by means of the 4 m size ASTRI-Horn telescope, operated on Mt. Etna (Italy) and developed in the context of the Cherenkov Telescope Array Observatory preparatory phase. The dual-mirror SC design is aplanatic and characterized by a small plate scale, allowing us to implement large field of view cameras with small-size pixel sensors and a high compactness. The curved focal plane of the ASTRI camera is covered by silicon photo-multipliers (SiPMs), managed by an unconventional front-end electronics based on a customized peak-sensing detector mode. The system includes internal and external calibration systems, hardware and software for control and acquisition, and the complete data archiving and processing chain. The observations of the Crab Nebula were carried out in December 2018, during the telescope verification phase, for a total observation time (after data selection) of 24.4 h, equally divided into on- and off-axis source exposure. The camera system was still under commissioning and its functionality was not yet completely exploited. Furthermore, due to recent eruptions of the Etna Volcano, the mirror reflection efficiency was reduced. Nevertheless, the observations led to the detection of the source with a statistical significance of 5.4 sigma above an energy threshold of ~3 TeV. This result provides an important step towards the use of dual-mirror systems in Cherenkov gamma-ray astronomy. A pathfinder mini-array based on nine large field-of-view ASTRI-like telescopes is under implementation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.12149v3-abstract-full').style.display = 'none'; document.getElementById('1909.12149v3-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 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 634, A22 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.10425">arXiv:1909.10425</a> <span> [<a href="https://arxiv.org/pdf/1909.10425">pdf</a>, <a href="https://arxiv.org/format/1909.10425">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/stz2650">10.1093/mnras/stz2650 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ASKAP-EMU Early Science Project:Radio Continuum Survey of the Small Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Joseph%2C+T+D">T. D. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I">I. Boji膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+E+L">E. L. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+G+F">G. F. Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Leverenz%2C+H">H. Leverenz</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+C">C. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+L+A">L. A. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Bunton%2C+J+D">J. D. Bunton</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+Y">Y. Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Galvin%2C+T">T. Galvin</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Kapinska%2C+A+D">A. D. Kapinska</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a> , et al. (31 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="1909.10425v1-abstract-short" style="display: inline;"> We present two new radio continuum images from the Australian Square Kilometre Array Pathfinder (ASKAP) survey in the direction of the Small Magellanic Cloud (SMC). These images are part of the Evolutionary Map of the Universe (EMU) Early Science Project (ESP) survey of the Small and Large Magellanic Clouds. The two new source lists produced from these images contain radio continuum sources observ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.10425v1-abstract-full').style.display = 'inline'; document.getElementById('1909.10425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.10425v1-abstract-full" style="display: none;"> We present two new radio continuum images from the Australian Square Kilometre Array Pathfinder (ASKAP) survey in the direction of the Small Magellanic Cloud (SMC). These images are part of the Evolutionary Map of the Universe (EMU) Early Science Project (ESP) survey of the Small and Large Magellanic Clouds. The two new source lists produced from these images contain radio continuum sources observed at 960 MHz (4489 sources) and 1320 MHz (5954 sources) with a bandwidth of 192 MHz and beam sizes of 30.0"x30.0" and 16.3"x15.1", respectively. The median Root Mean Squared (RMS) noise values are 186$渭$Jy beam$^{-1}$ (960 MHz) and 165$渭$Jy beam$^{-1}$ (1320 MHz). To create point source catalogues, we use these two source lists, together with the previously published Molonglo Observatory Synthesis Telescope (MOST) and the Australia Telescope Compact Array (ATCA) point source catalogues to estimate spectral indices for the whole population of radio point sources found in the survey region. Combining our ASKAP catalogues with these radio continuum surveys, we found 7736 point-like sources in common over an area of 30 deg$^2$. In addition, we report the detection of two new, low surface brightness supernova remnant candidates in the SMC. The high sensitivity of the new ASKAP ESP survey also enabled us to detect the bright end of the SMC planetary nebula sample, with 22 out of 102 optically known planetary nebulae showing point-like radio continuum emission. Lastly, we present several morphologically interesting background radio galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.10425v1-abstract-full').style.display = 'none'; document.getElementById('1909.10425v1-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 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">18 pages, 23 figues, 9 tables, Accepted for publication in the Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.06116">arXiv:1909.06116</a> <span> [<a href="https://arxiv.org/pdf/1909.06116">pdf</a>, <a href="https://arxiv.org/format/1909.06116">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computation">stat.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">stat.ML</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/pasa.2019.29">10.1017/pasa.2019.29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CAESAR source finder: recent developments and testing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">U. Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Calanducci%2C+A">A. Calanducci</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+A">A. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Schillir%C3%B2%2C+F">F. Schillir貌</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</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="1909.06116v1-abstract-short" style="display: inline;"> A new era in radioastronomy will begin with the upcoming large-scale surveys planned at the Australian Square Kilometre Array Pathfinder (ASKAP). ASKAP started its Early Science program in October 2017 and several target fields were observed during the array commissioning phase. The SCORPIO field was the first observed in the Galactic Plane in Band 1 (792-1032 MHz) using 15 commissioned antennas.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.06116v1-abstract-full').style.display = 'inline'; document.getElementById('1909.06116v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.06116v1-abstract-full" style="display: none;"> A new era in radioastronomy will begin with the upcoming large-scale surveys planned at the Australian Square Kilometre Array Pathfinder (ASKAP). ASKAP started its Early Science program in October 2017 and several target fields were observed during the array commissioning phase. The SCORPIO field was the first observed in the Galactic Plane in Band 1 (792-1032 MHz) using 15 commissioned antennas. The achieved sensitivity and large field of view already allow to discover new sources and survey thousands of existing ones with improved precision with respect to previous surveys. Data analysis is currently ongoing to deliver the first source catalogue. Given the increased scale of the data, source extraction and characterization, even in this Early Science phase, have to be carried out in a mostly automated way. This process presents significant challenges due to the presence of extended objects and diffuse emission close to the Galactic Plane. In this context we have extended and optimized a novel source finding tool, named CAESAR , to allow extraction of both compact and extended sources from radio maps. A number of developments have been done driven by the analysis of the SCORPIO map and in view of the future ASKAP Galactic Plane survey. The main goals are the improvement of algorithm performances and scalability as well as of software maintainability and usability within the radio community. In this paper we present the current status of CAESAR and report a first systematic characterization of its performance for both compact and extended sources using simulated maps. Future prospects are discussed in light of the obtained results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.06116v1-abstract-full').style.display = 'none'; document.getElementById('1909.06116v1-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 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">15 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Publications of the Astronomical Society of Australia, 2019, 36, E037 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.08013">arXiv:1904.08013</a> <span> [<a href="https://arxiv.org/pdf/1904.08013">pdf</a>, <a href="https://arxiv.org/ps/1904.08013">ps</a>, <a href="https://arxiv.org/format/1904.08013">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1051/0004-6361/201935239">10.1051/0004-6361/201935239 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A massive nebula around the Luminous Blue Variable star RMC143 revealed by ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">Claudia Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Mehner%2C+A">Andrea Mehner</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">Neil Matthew Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">Paolo Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Groh%2C+J">Jose Groh</a>, <a href="/search/astro-ph?searchtype=author&query=Noriega-Crespo%2C+A">Alberto Noriega-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">Carla Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">Francesco Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">Luciano Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">Adriano Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Paladini%2C+R">Roberta Paladini</a>, <a href="/search/astro-ph?searchtype=author&query=Pignata%2C+G">Giuliano Pignata</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">Corrado Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">Grazia Umana</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="1904.08013v2-abstract-short" style="display: inline;"> The luminous blue variable (LBV) RMC143 is located in the outskirts of the 30~Doradus complex, a region rich with interstellar material and hot luminous stars. We report the $3蟽$ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.08013v2-abstract-full').style.display = 'inline'; document.getElementById('1904.08013v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.08013v2-abstract-full" style="display: none;"> The luminous blue variable (LBV) RMC143 is located in the outskirts of the 30~Doradus complex, a region rich with interstellar material and hot luminous stars. We report the $3蟽$ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The spectral energy distribution (SED) of RMC143 suggests that two emission mechanisms contribute to the sub-mm emission: optically thin bremsstrahlung and dust. Both the extinction map and the SED are consistent with a dusty massive nebula with a dust mass of $0.055\pm0.018~M_{\odot}$ (assuming $魏_{850}=1.7\rm\,cm^{2}\,g^{-1}$). To date, RMC143 has the most dusty LBV nebula observed in the Magellanic Clouds. We have also re-examined the LBV classification of RMC143 based on VLT/X-shooter spectra obtained in 2015/16 and a review of the publication record. The radiative transfer code CMFGEN is used to derive its fundamental stellar parameters. We find an effective temperature of $\sim 8500$~K, luminosity of log$(L/L_{\odot}) = 5.32$, and a relatively high mass-loss rate of $1.0 \times 10^{-5}~M_{\odot}$~yr$^{-1}$. The luminosity is much lower than previously thought, which implies that the current stellar mass of $\sim8~M_{\odot}$ is comparable to its nebular mass of $\sim 5.5~M_{\odot}$ (from an assumed gas-to-dust ratio of 100), suggesting that the star has lost a large fraction of its initial mass in past LBV eruptions or binary interactions. While the star may have been hotter in the past, it is currently not hot enough to ionize its circumstellar nebula. We propose that the nebula is ionized externally by the hot stars in the 30~Doradus star-forming region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.08013v2-abstract-full').style.display = 'none'; document.getElementById('1904.08013v2-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> 21 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 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">Paper accepted by A&A on 09/05/2019 and in proof stage. Second comments by referee are included in this version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 626, A126 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.01426">arXiv:1904.01426</a> <span> [<a href="https://arxiv.org/pdf/1904.01426">pdf</a>, <a href="https://arxiv.org/format/1904.01426">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1016/j.astropartphys.2019.04.001">10.1016/j.astropartphys.2019.04.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Barai%2C+P">P. Barai</a>, <a href="/search/astro-ph?searchtype=author&query=Barbano%2C+A">A. Barbano</a>, <a href="/search/astro-ph?searchtype=author&query=Barkov%2C+M">M. Barkov</a> , et al. (445 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="1904.01426v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is the major next-generation observatory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01426v1-abstract-full').style.display = 'inline'; document.getElementById('1904.01426v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.01426v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is the major next-generation observatory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possible by using tens of imaging Cherenkov telescopes of three successive sizes. They will be arranged into two arrays, one per hemisphere, located on the La Palma island (Spain) and in Paranal (Chile). We present here the optimised and final telescope arrays for both CTA sites, as well as their foreseen performance, resulting from the analysis of three different large-scale Monte Carlo productions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01426v1-abstract-full').style.display = 'none'; document.getElementById('1904.01426v1-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">48 pages, 16 figures, accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.07504">arXiv:1809.07504</a> <span> [<a href="https://arxiv.org/pdf/1809.07504">pdf</a>, <a href="https://arxiv.org/ps/1809.07504">ps</a>, <a href="https://arxiv.org/format/1809.07504">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/sly179">10.1093/mnrasl/sly179 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The polarization mode of the auroral radio emission from the early-type star HD142301 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Todt%2C+H">H. Todt</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</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="1809.07504v1-abstract-short" style="display: inline;"> We report the detection of the auroral radio emission from the early-type magnetic star HD142301. New VLA observations of HD142301 detected highly polarized amplified emission occurring at fixed stellar orientations. The coherent emission mechanism responsible for the stellar auroral radio emission amplifies the radiation within a narrow beam, making the star where this phenomenon occurs similar t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.07504v1-abstract-full').style.display = 'inline'; document.getElementById('1809.07504v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.07504v1-abstract-full" style="display: none;"> We report the detection of the auroral radio emission from the early-type magnetic star HD142301. New VLA observations of HD142301 detected highly polarized amplified emission occurring at fixed stellar orientations. The coherent emission mechanism responsible for the stellar auroral radio emission amplifies the radiation within a narrow beam, making the star where this phenomenon occurs similar to a radio lighthouse. The elementary emission process responsible for the auroral radiation mainly amplifies one of the two magneto-ionic modes of the electromagnetic wave. This explains why the auroral pulses are highly circularly polarized. The auroral radio emission of HD142301 is characterized by a reversal of the sense of polarization as the star rotates. The effective magnetic field curve of HD142301 is also available making it possible to correlate the transition from the left to the right-hand circular polarization sense (and vice-versa) of the auroral pulses with the known orientation of the stellar magnetic field. The results presented in this letter have implications for the estimation of the dominant magneto-ionic mode amplified within the HD142301 magnetosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.07504v1-abstract-full').style.display = 'none'; document.getElementById('1809.07504v1-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> 20 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">5 pages, 4 figures; accepted to MNRAS 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/1807.09336">arXiv:1807.09336</a> <span> [<a href="https://arxiv.org/pdf/1807.09336">pdf</a>, <a href="https://arxiv.org/format/1807.09336">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/sty1929">10.1093/mnras/sty1929 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Coordinated Radio and Infrared Survey for High-mass Star Formation. IV: A new radio selected sample of compact Galactic Planetary Nebulae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Irabor%2C+T">T. Irabor</a>, <a href="/search/astro-ph?searchtype=author&query=Hoare%2C+M+G">M. G. Hoare</a>, <a href="/search/astro-ph?searchtype=author&query=Oudmaijer%2C+R+D">R. D. Oudmaijer</a>, <a href="/search/astro-ph?searchtype=author&query=Urquhart%2C+J+S">J. S. Urquhart</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtz%2C+S">S. Kurtz</a>, <a href="/search/astro-ph?searchtype=author&query=Lumsden%2C+S+L">S. L. Lumsden</a>, <a href="/search/astro-ph?searchtype=author&query=Purcell%2C+C+R">C. R. Purcell</a>, <a href="/search/astro-ph?searchtype=author&query=Zijlstra%2C+A+A">A. A. Zijlstra</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</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="1807.09336v2-abstract-short" style="display: inline;"> We present a new radio-selected sample of PNe from the CORNISH survey. This is a radio continuum survey of the inner Galactic plane covering Galactic longitude, $10^\circ <l< 65^\circ$ and latitude, $|b| < 1^\circ$ with a resolution of 1.5$^{"}$ and sensitivity better than 0.4 mJy/beam. The radio regime, being unbiased by dust extinction, allows for a more complete sample selection, especially tow… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.09336v2-abstract-full').style.display = 'inline'; document.getElementById('1807.09336v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.09336v2-abstract-full" style="display: none;"> We present a new radio-selected sample of PNe from the CORNISH survey. This is a radio continuum survey of the inner Galactic plane covering Galactic longitude, $10^\circ <l< 65^\circ$ and latitude, $|b| < 1^\circ$ with a resolution of 1.5$^{"}$ and sensitivity better than 0.4 mJy/beam. The radio regime, being unbiased by dust extinction, allows for a more complete sample selection, especially towards the Galactic mid-plane. Visual inspection of the CORNISH data, in combination with data from multi-wavelength surveys of the Galactic plane, allowed the CORNISH team to identify 169 candidate PNe. Here, we explore the use of multi-wavelength diagnostic plots and analysis to verify and classify the candidate PNe. We present the multi-wavelength properties of this new PNe sample. We find 90 new PNe, of which 12 are newly discovered and 78 are newly classified as PN. A further 47 previously suspected PNe are confirmed as such from the analysis presented here and 24 known PNe are detected. Eight sources are classified as possible PNe or other source types. Our sample includes a young sub-sample, with physical diameters < 0.12 pc, brightness temperatures (> 1000 K) and located closer than 7 kpc. Within this sample is a water-maser PN with a spectral index of $-0.55\pm 0.08$, which indicates non-thermal radio emission. Such a radio-selected sample, unaffected by extinction, will be particularly useful to compare with population synthesis models and should contribute to the understanding of the formation and evolution of PNe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.09336v2-abstract-full').style.display = 'none'; document.getElementById('1807.09336v2-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 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.08338">arXiv:1803.08338</a> <span> [<a href="https://arxiv.org/pdf/1803.08338">pdf</a>, <a href="https://arxiv.org/format/1803.08338">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/sty2280">10.1093/mnras/sty2280 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of Alpha Centauri at radio wavelengths: chromospheric emission and search for star-planet interaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</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="1803.08338v2-abstract-short" style="display: inline;"> At radio wavelengths, solar-type stars emit thermal free-free and gyroresonance, gyrosynchrotron, and impulsive coherent emission. Thermal free-free emission originates at layers where the optical depth is close to unit, while high brightness temperature, variable emission, can be due to flares via gyrosynchrotron emission. We observed the alpha Cen system with the Australian Telescope Compact Arr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.08338v2-abstract-full').style.display = 'inline'; document.getElementById('1803.08338v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.08338v2-abstract-full" style="display: none;"> At radio wavelengths, solar-type stars emit thermal free-free and gyroresonance, gyrosynchrotron, and impulsive coherent emission. Thermal free-free emission originates at layers where the optical depth is close to unit, while high brightness temperature, variable emission, can be due to flares via gyrosynchrotron emission. We observed the alpha Cen system with the Australian Telescope Compact Array at 2 GHz for three days and 17 GHz for one day. Both stars have been detected at 17 GHz, while only an upper limit has been obtained at low frequency despite the longer integration time. The brightness temperatures are consistent with the temperature of the upper chromosphere of the Sun. Inverting the formulae of the free-free emission, the average electron density of the plasma has been inferred. The same procedure was applied to the data in the millimetre recently acquired with ALMA. A comparison with the atmospheric solar models reveals a higher level of activity in alpha Cen B rather than in alpha Cen A, even if still at quiescent level. The non detection at 2 GHz allows us to put a lower limit in the filling factor of active regions. The claimed detection of an Earth size planet in close orbit to alpha Cen B, although doubtful, opens the opportunity to check the existence of Star-Planet Magnetic Interaction (SPMI). We constructed dynamic spectra in the 1.3 - 2.9 GHz of the 2 stars to search for time-variable coherent emission but obtained a null result. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.08338v2-abstract-full').style.display = 'none'; document.getElementById('1803.08338v2-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> 20 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Submitted to MNRAS, 9 pages, 7 Figures, MNRAS, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.08738">arXiv:1801.08738</a> <span> [<a href="https://arxiv.org/pdf/1801.08738">pdf</a>, <a href="https://arxiv.org/ps/1801.08738">ps</a>, <a href="https://arxiv.org/format/1801.08738">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey 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/sty244">10.1093/mnras/sty244 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A combined multiwavelength VLA/ALMA/Chandra study unveils the complex magnetosphere of the B-type star HR5907 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Todt%2C+H">H. Todt</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</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="1801.08738v1-abstract-short" style="display: inline;"> We present new radio/millimeter measurements of the hot magnetic star HR5907 obtained with the VLA and ALMA interferometers. We find that HR5907 is the most radio luminous early type star in the cm-mm band among those presently known. Its multi-wavelength radio light curves are strongly variable with an amplitude that increases with radio frequency. The radio emission can be explained by the popul… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08738v1-abstract-full').style.display = 'inline'; document.getElementById('1801.08738v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.08738v1-abstract-full" style="display: none;"> We present new radio/millimeter measurements of the hot magnetic star HR5907 obtained with the VLA and ALMA interferometers. We find that HR5907 is the most radio luminous early type star in the cm-mm band among those presently known. Its multi-wavelength radio light curves are strongly variable with an amplitude that increases with radio frequency. The radio emission can be explained by the populations of the non-thermal electrons accelerated in the current sheets on the outer border of the magnetosphere of this fast rotating magnetic star. We classify HR5907 as another member of the growing class of strongly magnetic fast rotating hot stars where the gyro-synchrotron emission mechanism efficiently operates in their magnetospheres. The new radio observations of HR5907 are combined with archival X-ray data to study the physical condition of its magnetosphere. The X-ray spectra of HR5907 show tentative evidence for the presence of non-thermal spectral component. We suggest that non-thermal X-rays originate a stellar X-ray aurora due to streams of non-thermal electrons impacting on the stellar surface. Taking advantage of the relation between the spectral indices of the X-ray power-law spectrum and the non-thermal electron energy distributions, we perform 3-D modeling of the radio emission for HR5907. The wavelength-dependent radio light-curves probe magnetospheric layers at different heights above the stellar surface. A detailed comparison between simulated and observed radio light-curves leads us to conclude that the stellar magnetic field of HR5907 is likely non-dipolar, providing further indirect evidence of the complex magnetic field topology of HR5907. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08738v1-abstract-full').style.display = 'none'; document.getElementById('1801.08738v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">18 pages, 13 figures; accepted to 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/1711.06263">arXiv:1711.06263</a> <span> [<a href="https://arxiv.org/pdf/1711.06263">pdf</a>, <a href="https://arxiv.org/format/1711.06263">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="Solar and Stellar Astrophysics">astro-ph.SR</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/stx2560">10.1093/mnras/stx2560 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Extended Catalogue of Galactic Bubbles InfraRed Fluxes from WISE and Herschel Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Carey%2C+D">D. Carey</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bulpitt%2C+A">A. Bulpitt</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+S">S. Molinari</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="1711.06263v1-abstract-short" style="display: inline;"> In this paper, we present the first extended catalogue of far-infrared fluxes of Galactic bubbles. Fluxes were estimated for 1814 bubbles, defined here as the `golden sample', and were selected from the Milky Way Project First Data Release (Simpson et al.) The golden sample was comprised of bubbles identified within the Wide-field Infrared Survey Explorer (WISE) dataset (using 12- and 22-$渭$m imag… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.06263v1-abstract-full').style.display = 'inline'; document.getElementById('1711.06263v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.06263v1-abstract-full" style="display: none;"> In this paper, we present the first extended catalogue of far-infrared fluxes of Galactic bubbles. Fluxes were estimated for 1814 bubbles, defined here as the `golden sample', and were selected from the Milky Way Project First Data Release (Simpson et al.) The golden sample was comprised of bubbles identified within the Wide-field Infrared Survey Explorer (WISE) dataset (using 12- and 22-$渭$m images) and Herschel data (using 70-, 160-, 250-, 350- and 500-$渭$m wavelength images). Flux estimation was achieved initially via classical aperture photometry and then by an alternative image analysis algorithm that used active contours. The accuracy of the two methods was tested by comparing the estimated fluxes for a sample of bubbles, made up of 126 H II regions and 43 planetary nebulae, which were identified by Anderson et al. The results of this paper demonstrate that a good agreement between the two was found. This is by far the largest and most homogeneous catalogue of infrared fluxes measured for Galactic bubbles and it is a step towards the fully automated analysis of astronomical datasets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.06263v1-abstract-full').style.display = 'none'; document.getElementById('1711.06263v1-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> 16 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">22 pages, 16 figures, 10 tables, published on MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 473, 3671-3692 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.04702">arXiv:1710.04702</a> <span> [<a href="https://arxiv.org/pdf/1710.04702">pdf</a>, <a href="https://arxiv.org/format/1710.04702">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/stx2445">10.1093/mnras/stx2445 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SCORPIO-II: Spectral indices of weak Galactic radio sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Franzen%2C+T+M+O">T. M. O. Franzen</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Marvil%2C+J">J. Marvil</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</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="1710.04702v1-abstract-short" style="display: inline;"> In the next few years the classification of radio sources observed by the large surveys will be a challenging problem, and spectral index is a powerful tool for addressing it. Here we present an algorithm to estimate the spectral index of sources from multiwavelength radio images. We have applied our algorithm to SCORPIO (Umana et al. 2015), a Galactic Plane survey centred around 2.1 GHz carried o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.04702v1-abstract-full').style.display = 'inline'; document.getElementById('1710.04702v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.04702v1-abstract-full" style="display: none;"> In the next few years the classification of radio sources observed by the large surveys will be a challenging problem, and spectral index is a powerful tool for addressing it. Here we present an algorithm to estimate the spectral index of sources from multiwavelength radio images. We have applied our algorithm to SCORPIO (Umana et al. 2015), a Galactic Plane survey centred around 2.1 GHz carried out with ATCA, and found we can measure reliable spectral indices only for sources stronger than 40 times the rms noise. Above a threshold of 1 mJy, the source density in SCORPIO is 20 percent greater than in a typical extra-galactic field, like ATLAS (Norris et al. 2006), because of the presence of Galactic sources. Among this excess population, 16 sources per square degree have a spectral index of about zero, suggesting optically thin thermal emission such as Hii regions and planetary nebulae, while 12 per square degree present a rising spectrum, suggesting optically thick thermal emission such as stars and UCHii regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.04702v1-abstract-full').style.display = 'none'; document.getElementById('1710.04702v1-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 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">12 pages, 11 figures, accepted 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/1709.07997">arXiv:1709.07997</a> <span> [<a href="https://arxiv.org/pdf/1709.07997">pdf</a>, <a href="https://arxiv.org/format/1709.07997">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</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/10.1142/10986">10.1142/10986 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Science with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+B+S">B. S. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Antolini%2C+E">E. Antolini</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Araya%2C+M">M. Araya</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M">M. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a> , et al. (558 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="1709.07997v2-abstract-short" style="display: inline;"> The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black ho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.07997v2-abstract-full').style.display = 'inline'; document.getElementById('1709.07997v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.07997v2-abstract-full" style="display: none;"> The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black holes to cosmic voids on the largest scales. Covering a huge range in photon energy from 20 GeV to 300 TeV, CTA will improve on all aspects of performance with respect to current instruments. The observatory will operate arrays on sites in both hemispheres to provide full sky coverage and will hence maximize the potential for the rarest phenomena such as very nearby supernovae, gamma-ray bursts or gravitational wave transients. With 99 telescopes on the southern site and 19 telescopes on the northern site, flexible operation will be possible, with sub-arrays available for specific tasks. CTA will have important synergies with many of the new generation of major astronomical and astroparticle observatories. Multi-wavelength and multi-messenger approaches combining CTA data with those from other instruments will lead to a deeper understanding of the broad-band non-thermal properties of target sources. The CTA Observatory will be operated as an open, proposal-driven observatory, with all data available on a public archive after a pre-defined proprietary period. Scientists from institutions worldwide have combined together to form the CTA Consortium. This Consortium has prepared a proposal for a Core Programme of highly motivated observations. The programme, encompassing approximately 40% of the available observing time over the first ten years of CTA operation, is made up of individual Key Science Projects (KSPs), which are presented in this document. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.07997v2-abstract-full').style.display = 'none'; document.getElementById('1709.07997v2-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> 21 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">213 pages, including references and glossary. Version 2: credits and references updated, some figures updated, and author list updated</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.03483">arXiv:1709.03483</a> <span>  </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> <p class="title is-5 mathjax"> Cherenkov Telescope Array Contributions to the 35th International Cosmic Ray Conference (ICRC2017) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+B+S">B. S. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Portella%2C+V+A">V. Ac铆n Portella</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/astro-ph?searchtype=author&query=Alcubierre%2C+M">M. Alcubierre</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrogi%2C+L">L. Ambrogi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anduze%2C+M">M. Anduze</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antolini%2C+E">E. Antolini</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Antonuccio%2C+V">V. Antonuccio</a> , et al. (1117 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="1709.03483v5-abstract-short" style="display: inline;"> List of contributions from the Cherenkov Telescope Array Consortium presented at the 35th International Cosmic Ray Conference, July 12-20 2017, Busan, Korea. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.03483v5-abstract-full" style="display: none;"> List of contributions from the Cherenkov Telescope Array Consortium presented at the 35th International Cosmic Ray Conference, July 12-20 2017, Busan, Korea. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.03483v5-abstract-full').style.display = 'none'; document.getElementById('1709.03483v5-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">Index of Cherenkov Telescope Array conference proceedings at the ICRC2017, Busan, Korea</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.01046">arXiv:1706.01046</a> <span> [<a href="https://arxiv.org/pdf/1706.01046">pdf</a>, <a href="https://arxiv.org/format/1706.01046">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/stx1357">10.1093/mnras/stx1357 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ($-71.0^{\circ}< \ell < 67.0^{\circ}$) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Elia%2C+D">D. Elia</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+S">S. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Schisano%2C+E">E. Schisano</a>, <a href="/search/astro-ph?searchtype=author&query=Pestalozzi%2C+M">M. Pestalozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pezzuto%2C+S">S. Pezzuto</a>, <a href="/search/astro-ph?searchtype=author&query=Merello%2C+M">M. Merello</a>, <a href="/search/astro-ph?searchtype=author&query=Noriega-Crespo%2C+A">A. Noriega-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Moore%2C+T+J+T">T. J. T. Moore</a>, <a href="/search/astro-ph?searchtype=author&query=Russeil%2C+D">D. Russeil</a>, <a href="/search/astro-ph?searchtype=author&query=Mottram%2C+J+C">J. C. Mottram</a>, <a href="/search/astro-ph?searchtype=author&query=Paladini%2C+R">R. Paladini</a>, <a href="/search/astro-ph?searchtype=author&query=Strafella%2C+F">F. Strafella</a>, <a href="/search/astro-ph?searchtype=author&query=Benedettini%2C+M">M. Benedettini</a>, <a href="/search/astro-ph?searchtype=author&query=Bernard%2C+J+P">J. P. Bernard</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Giorgio%2C+A">A. Di Giorgio</a>, <a href="/search/astro-ph?searchtype=author&query=Eden%2C+D+J">D. J. Eden</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+Y">Y. Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Plume%2C+R">R. Plume</a>, <a href="/search/astro-ph?searchtype=author&query=Bally%2C+J">J. Bally</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+P+G">P. G. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Ragan%2C+S+E">S. E. Ragan</a>, <a href="/search/astro-ph?searchtype=author&query=Jaffa%2C+S+E">S. E. Jaffa</a>, <a href="/search/astro-ph?searchtype=author&query=Motte%2C+F">F. Motte</a>, <a href="/search/astro-ph?searchtype=author&query=Olmi%2C+L">L. Olmi</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+N">N. Schneider</a> , et al. (61 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="1706.01046v1-abstract-short" style="display: inline;"> Hi-GAL is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 $渭$m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogs presented in Molinari et al. (2016a), covering the port… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.01046v1-abstract-full').style.display = 'inline'; document.getElementById('1706.01046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.01046v1-abstract-full" style="display: none;"> Hi-GAL is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 $渭$m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogs presented in Molinari et al. (2016a), covering the portion of Galactic plane $-71.0^{\circ}< \ell < 67.0^{\circ}$. The band-merged catalogue contains 100922 sources with a regular SED, 24584 of which show a 70 $渭$m counterpart and are thus considered proto-stellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterise different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in proto-stellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to proto-stellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between "on-arm" and "inter-arm" positions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.01046v1-abstract-full').style.display = 'none'; document.getElementById('1706.01046v1-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> 4 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 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/1705.09877">arXiv:1705.09877</a> <span> [<a href="https://arxiv.org/pdf/1705.09877">pdf</a>, <a href="https://arxiv.org/format/1705.09877">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/10.1051/0004-6361/201629963">10.1051/0004-6361/201629963 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spatial distribution of star formation related to ionized regions throughout the inner Galactic plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Palmeirim%2C+P">P. Palmeirim</a>, <a href="/search/astro-ph?searchtype=author&query=Zavagno%2C+A">A. Zavagno</a>, <a href="/search/astro-ph?searchtype=author&query=Elia%2C+D">D. Elia</a>, <a href="/search/astro-ph?searchtype=author&query=Moore%2C+T+J+T">T. J. T. Moore</a>, <a href="/search/astro-ph?searchtype=author&query=Whitworth%2C+A">A. Whitworth</a>, <a href="/search/astro-ph?searchtype=author&query=Tremblin%2C+P">P. Tremblin</a>, <a href="/search/astro-ph?searchtype=author&query=Traficante%2C+A">A. Traficante</a>, <a href="/search/astro-ph?searchtype=author&query=Merello%2C+M">M. Merello</a>, <a href="/search/astro-ph?searchtype=author&query=Russeil%2C+D">D. Russeil</a>, <a href="/search/astro-ph?searchtype=author&query=Pezzuto%2C+S">S. Pezzuto</a>, <a href="/search/astro-ph?searchtype=author&query=Cambr%C3%A9sy%2C+L">L. Cambr茅sy</a>, <a href="/search/astro-ph?searchtype=author&query=Baldeschi%2C+A">A. Baldeschi</a>, <a href="/search/astro-ph?searchtype=author&query=Bandieramonte%2C+M">M. Bandieramonte</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">U. Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Benedettini%2C+M">M. Benedettini</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Bulpitt%2C+A">A. Bulpitt</a>, <a href="/search/astro-ph?searchtype=author&query=Butora%2C+R">R. Butora</a>, <a href="/search/astro-ph?searchtype=author&query=Carey%2C+D">D. Carey</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+A">A. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Deharveng%2C+L">L. Deharveng</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Giorgio%2C+A">A. Di Giorgio</a>, <a href="/search/astro-ph?searchtype=author&query=Eden%2C+D">D. Eden</a>, <a href="/search/astro-ph?searchtype=author&query=Hajnal%2C+A">A. Hajnal</a> , et al. (13 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="1705.09877v1-abstract-short" style="display: inline;"> We present a comprehensive statistical analysis of star-forming objects located in the vicinities of 1 360 bubble structures throughout the Galactic Plane and their local environments. The compilation of ~70 000 star-forming sources, found in the proximity of the ionized (Hii) regions and detected in both Hi-GAL and GLIMPSE surveys, provided a broad overview of the different evolutionary stages of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.09877v1-abstract-full').style.display = 'inline'; document.getElementById('1705.09877v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.09877v1-abstract-full" style="display: none;"> We present a comprehensive statistical analysis of star-forming objects located in the vicinities of 1 360 bubble structures throughout the Galactic Plane and their local environments. The compilation of ~70 000 star-forming sources, found in the proximity of the ionized (Hii) regions and detected in both Hi-GAL and GLIMPSE surveys, provided a broad overview of the different evolutionary stages of star-formation in bubbles, from prestellar objects to more evolved young stellar objects (YSOs). Surface density maps of star-forming objects clearly reveal an evolutionary trend where more evolved star-forming objects are found spatially located near the center, while younger star-forming objects are found at the edge of the bubbles. We derived dynamic ages for a subsample of 182 Hii regions for which kinematic distances and radio continuum flux measurements were available. We detect ~80% more star-forming sources per unit area in the direction of bubbles than in the surrounding fields. We estimate ~10% clump formation efficiency (CFE) of Hi-GAL clumps in bubbles, twice the CFE in fields not affected by feedback. We find higher CFE of protostellar clumps in younger bubbles, whose density of the bubble shells is higher. We argue that the formation rate from prestellar to protostellar phase is probably higher during the early stages of the bubble expansion. Evaluation of the fragmentation time inside the shell of bubbles advocates the preexistence of clumps in the medium before the bubble, as supported by numerical simulations. Approximately 23% of the Hi-GAL clumps are found located in the direction of a bubble, with 15% for prestellar clumps and 41% for protostellar clumps. We argue that the high fraction of protostellar clumps may be due to the acceleration of the star-formation process cause by the feedback of the (Hii) bubbles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.09877v1-abstract-full').style.display = 'none'; document.getElementById('1705.09877v1-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 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">15 pages, 12 figures. Accepted for publication by Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 605, A35 (2017) </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=Umana%2C+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Umana%2C+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Umana%2C+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Umana%2C+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Umana%2C+G&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </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