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 91 results for author: <span class="mathjax">Spavone, M</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=Spavone%2C+M">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="Spavone, M"> </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=Spavone%2C+M&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="Spavone, M"> <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=Spavone%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Spavone%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Spavone%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </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/2501.16192">arXiv:2501.16192</a> <span> [<a href="https://arxiv.org/pdf/2501.16192">pdf</a>, <a href="https://arxiv.org/format/2501.16192">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"> Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra I cluster III. Untangling UDG 32 from the stripped filaments of NGC 3314A with multi-wavelength data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">J. Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Gullieuszik%2C+M">M. Gullieuszik</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">M. Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Buttitta%2C+C">C. Buttitta</a>, <a href="/search/astro-ph?searchtype=author&query=Doll%2C+G">G. Doll</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Casa%2C+C+C">C. C. de la Casa</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Kotulla%2C+R">R. Kotulla</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B">B. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Corsini%2C+E+M">E. M. Corsini</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">J. Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">D. A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">M. Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">S. Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</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="2501.16192v1-abstract-short" style="display: inline;"> UDG 32 is an ultra-diffuse galaxy (UDG) candidate in the Hydra I cluster that was discovered in the extended network of stellar filaments of the jellyfish galaxy NGC 3314A. This galaxy is affected by ram pressure stripping and it is hypothesised that UDG 32 may have formed from its stripped material. In this paper, we address whether UDG 32 can be associated with the stripped material of NGC 3314A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16192v1-abstract-full').style.display = 'inline'; document.getElementById('2501.16192v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.16192v1-abstract-full" style="display: none;"> UDG 32 is an ultra-diffuse galaxy (UDG) candidate in the Hydra I cluster that was discovered in the extended network of stellar filaments of the jellyfish galaxy NGC 3314A. This galaxy is affected by ram pressure stripping and it is hypothesised that UDG 32 may have formed from its stripped material. In this paper, we address whether UDG 32 can be associated with the stripped material of NGC 3314A and constrain its formation scenario in relation to its environment. We use new integral-field spectroscopic data from the MUSE large programme `LEWIS' in conjunction with deep multi-band photometry to constrain the kinematics and stellar populations of UDG 32. The new MUSE data allow us to reveal that the stripped material from NGC 3314A, traced by emission lines such as H$伪$, extends much further from its parent galaxy than previously known, completely overlapping with UDG 32 in projection, and with ram pressure induced star formation. We determine the line-of-sight velocity of UDG 32 ($v_{\rm LOS} = 3080\pm120$ km/s) and confirm that UDG 32 is part of the same kinematic structure as NGC 3314A, the Hydra I cluster south-east subgroup. By fitting the UV and optical spectral energy distribution, we constrain the stellar population properties of UDG 32. We determine its mass-weighted age to be $7.7^{+2.9}_{-2.8}$ Gyr and its metallicity to be [M/H] = $0.07^{+0.19}_{-0.32}$ dex. We confirm the presence of two globular clusters (GCs) in the MUSE field of view, bound to the Hydra I cluster rather than to UDG 32, thus part of the Hydra I intracluster GC population. The metal-rich and intermediate-age nature of UDG 32 points towards its formation from pre-enriched material in the south-east group of the Hydra I cluster that was liberated from a more massive galaxy via tidal or ram-pressure stripping, but we cannot establish a direct link to the ram-pressure stripped material from NGC 3314A. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16192v1-abstract-full').style.display = 'none'; document.getElementById('2501.16192v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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, 16 figures, accepted for publication in Astronomy and Astrophysics, abstract abridged for arxiv submission</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.16190">arXiv:2501.16190</a> <span> [<a href="https://arxiv.org/pdf/2501.16190">pdf</a>, <a href="https://arxiv.org/format/2501.16190">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/10.1051/0004-6361/202452915">10.1051/0004-6361/202452915 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra-I cluster II. Stellar kinematics and dynamical masses </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Buttitta%2C+C">Chiara Buttitta</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Doll%2C+G">Goran Doll</a>, <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">Johanna Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Corsini%2C+E+M">Enrico M. Corsini</a>, <a href="/search/astro-ph?searchtype=author&query=Rossi%2C+L">Luca Rossi</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Falcon-Barroso%2C+J">Jesus Falcon-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Gullieuszik%2C+M">Marco Gullieuszik</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">Chiara Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Sarzi%2C+M">Marc Sarzi</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="2501.16190v1-abstract-short" style="display: inline;"> Context: This paper focuses on a class of galaxies characterised by an extremely low surface brightness: the ultra-diffuse galaxies (UDGs). We used new integral-field spectroscopic data from the ESO Large Programme Looking into the faintEst WIth MUSE (LEWIS) project. Aims: Our main goals are addressing the formation channels and investigating possible correlations of their observational properties… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16190v1-abstract-full').style.display = 'inline'; document.getElementById('2501.16190v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.16190v1-abstract-full" style="display: none;"> Context: This paper focuses on a class of galaxies characterised by an extremely low surface brightness: the ultra-diffuse galaxies (UDGs). We used new integral-field spectroscopic data from the ESO Large Programme Looking into the faintEst WIth MUSE (LEWIS) project. Aims: Our main goals are addressing the formation channels and investigating possible correlations of their observational properties. In particular, we derive their stellar kinematics and dynamical properties. Methods: We extract the 1D stacked spectrum inside the effective radius to obtain an unbiased measure of $蟽_{\rm eff}$. To derive the spatially-resolved stellar kinematics, we first apply the Voronoi tessellation algorithm to bin the spaxels in the datacube and then follow the same prescription adopted for the 1D case. In addition, we extract the velocity profiles along the galaxy's major and minor axes. Results: We find that 7 out of 18 UDGs in LEWIS show a mild rotation, 5 do not have evidence of any rotation, and the remaining 6 UDGs are unconstrained cases. This is the first large census of velocity profiles for UDGs. On average, UDGs in LEWIS are characterised by low values of $蟽_{\rm eff}$, comparable with available values from the literature. In the Faber-Jackson relation plane, we found a group of UDGs consistent with the relation within the errorbars, whereas outliers are objects with non-negligible rotation components. UDGs and LSBs in LEWIS have larger dark matter content than dwarf galaxies with similar total luminosity. We do not find clear correlations between the derived properties and the local environment. Conclusions: Based on the stellar kinematics, two classes of UDGs are found in the Hydra I cluster: the rotating and non-rotating systems. This result, combined with other structural properties, can help to discriminate between the several formation scenarios proposed for UDGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16190v1-abstract-full').style.display = 'none'; document.getElementById('2501.16190v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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 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 694, A276 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.18015">arXiv:2412.18015</a> <span> [<a href="https://arxiv.org/pdf/2412.18015">pdf</a>, <a href="https://arxiv.org/format/2412.18015">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/10.1051/0004-6361/202452206">10.1051/0004-6361/202452206 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VEGAS-SSS: An intra-group component in the globular cluster system of NGC 5018 group of galaxies using VST data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lonare%2C+P">Pratik Lonare</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Hazra%2C+N">Nandini Hazra</a>, <a href="/search/astro-ph?searchtype=author&query=Riccio%2C+G">Gabriele Riccio</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="2412.18015v1-abstract-short" style="display: inline;"> Globular clusters (GCs) are fossil tracer of formation and evolution of galaxies and studying their properties provides crucial insights into past formation and interaction events. We study the properties of GC candidates in 1.25 $\times$ 1.03 sq. degrees area centred on NGC 5018 group of galaxies using deep, wide field and multi-band observations obtained with VST. We derived photometric catalogu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18015v1-abstract-full').style.display = 'inline'; document.getElementById('2412.18015v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.18015v1-abstract-full" style="display: none;"> Globular clusters (GCs) are fossil tracer of formation and evolution of galaxies and studying their properties provides crucial insights into past formation and interaction events. We study the properties of GC candidates in 1.25 $\times$ 1.03 sq. degrees area centred on NGC 5018 group of galaxies using deep, wide field and multi-band observations obtained with VST. We derived photometric catalogues of compact and extended sources and identified GC candidates using a set of photometric and morphometric selection parameters. A GC candidates catalogue is inspected using a statistical background decontamination technique. The 2D distribution map of GC candidates reveals an overdensity of sources on brightest member of group, NGC 5018. No significant GC overdensities are observed in other bright galaxies of group. We report discovery of a candidate local nucleated LSB dwarf galaxy possibly in tidal interaction with NGC 5018. The 2D map also reveals an intra-group GC population aligning with bright galaxies and along intra-group light component. Radial density profile of GC candidates in NGC 5018 follows galaxy surface brightness profile. Colour profile of GC candidates centred on this galaxy shows no evidence of well-known colour bimodality, which is instead observed in intra-group population. From GC luminosity function (GCLF) analysis, we find a low specific frequency $S_{\!\rm N}=0.59 \pm 0.27$ for NGC 5018, consistent with previous results. This relatively low $S_{\!\rm N}$ and lack of colour bimodality might be due to a combination of observational data limitations and the post-merger status of NGC 5018, which might host a population of relatively young GCs. For intra-group GC population, we obtain a lower limit of $S_{\!\rm {N,gr}}\sim0.6$. Using GCLF as a distance indicator, we estimate that NGC 5018 is located $38.0 \pm 7.9$ Mpc away, consistent with values in the literature.. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18015v1-abstract-full').style.display = 'none'; document.getElementById('2412.18015v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 694, A231 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.10663">arXiv:2411.10663</a> <span> [<a href="https://arxiv.org/pdf/2411.10663">pdf</a>, <a href="https://arxiv.org/format/2411.10663">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"> Stellar Halos of Bright Central Galaxies: A View from the FEGA Semi-Analytic Model of Galaxy Formation and VEGAS Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Contini%2C+E">Emanuele Contini</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Yi%2C+S+K">Sukyoung K. Yi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.10663v2-abstract-short" style="display: inline;"> We present theoretical predictions and extrapolations from observed data of the stellar halos surrounding central group/cluster galaxies and the transition radius between them and the intracluster or diffuse light. Leveraging the state-of-the-art semi-analytic model of galaxy formation, {\small FEGA} (\citealt{contini2024c}), applied to two dark matter-only cosmological simulations, we derive both… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10663v2-abstract-full').style.display = 'inline'; document.getElementById('2411.10663v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10663v2-abstract-full" style="display: none;"> We present theoretical predictions and extrapolations from observed data of the stellar halos surrounding central group/cluster galaxies and the transition radius between them and the intracluster or diffuse light. Leveraging the state-of-the-art semi-analytic model of galaxy formation, {\small FEGA} (\citealt{contini2024c}), applied to two dark matter-only cosmological simulations, we derive both the stellar halo mass and its radius. Using theoretical assumptions about the diffuse light distribution and halo concentration, we extrapolate the same information for observed data from the {\small VEGAS} survey (\citealt{capaccioli2015,iodice2021}). Our model, supported by observational data and independent simulation results, predicts an increasing transition radius with halo mass, a constant stellar halo-to-intracluster light ratio, and a stable stellar halo mass fraction with increasing halo mass. Specifically, we find that the transition radius between the stellar halo and the diffuse light ranges from 20 to 250 kpc, from Milky Way-like halos to large clusters, while the stellar halo mass comprises only a small fraction, between 7\% and 18\%, of the total stellar mass within the virial radius. These results support the idea that the stellar halo can be viewed as a transition region between the stars bound to the galaxy and those belonging to the intracluster light, consistent with recent observations and theoretical predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10663v2-abstract-full').style.display = 'none'; document.getElementById('2411.10663v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">5 pages, 3 figures. Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.09608">arXiv:2411.09608</a> <span> [<a href="https://arxiv.org/pdf/2411.09608">pdf</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"> VST-SMASH: the VST Survey of Mass Assembly and Structural Hierarchy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">Crescenzo Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Gatto%2C+M">Massimiliano Gatto</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L">Leslie Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">Vincenzo Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Dall%27Ora%2C+M">Massimo Dall'Ora</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">Francesca Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Baes%2C+M">Maarten Baes</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F+M+C">Francesco Michel Concetto Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bellucco%2C+N">Nicola Bellucco</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">Micol Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Dimauro%2C+P">Paola Dimauro</a>, <a href="/search/astro-ph?searchtype=author&query=Kluge%2C+M">Mathias Kluge</a>, <a href="/search/astro-ph?searchtype=author&query=Lelli%2C+F">Federico Lelli</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">Nicola R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Nucita%2C+A">Achille Nucita</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">Mario Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Scaramella%2C+R">Roberto Scaramella</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Testa%2C+V">Vincenzo Testa</a>, <a href="/search/astro-ph?searchtype=author&query=Unni%2C+A">Aiswarya Unni</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.09608v1-abstract-short" style="display: inline;"> The VLT Survey Telescope Survey of Mass Assembly and Structural Hierarchy (VST-SMASH) aims to detect tidal features and remnants around very nearby galaxies, a unique and essential diagnostic of the hierarchical nature of galaxy formation. Leveraging optimal sky conditions at ESO's Paranal Observatory, combined with the VST's multi-band optical filters, VST-SMASH aims to be the definitive survey o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09608v1-abstract-full').style.display = 'inline'; document.getElementById('2411.09608v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.09608v1-abstract-full" style="display: none;"> The VLT Survey Telescope Survey of Mass Assembly and Structural Hierarchy (VST-SMASH) aims to detect tidal features and remnants around very nearby galaxies, a unique and essential diagnostic of the hierarchical nature of galaxy formation. Leveraging optimal sky conditions at ESO's Paranal Observatory, combined with the VST's multi-band optical filters, VST-SMASH aims to be the definitive survey of stellar streams and tidal remnants in the Local Volume, targeting a low surface-brightness limit of $渭\sim$ 30 mag arcsec$^{-2}$ in the g and r bands, and $渭\sim$ 28 mag arcsec$^{-2}$ in the i band, in a volume-limited sample of local galaxies within 11 Mpc and the Euclid footprint. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09608v1-abstract-full').style.display = 'none'; document.getElementById('2411.09608v1-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 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">4 pages, 2 figures, 1 table, published in the ESO Messenger 193</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Messenger 193, 31 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.01501">arXiv:2408.01501</a> <span> [<a href="https://arxiv.org/pdf/2408.01501">pdf</a>, <a href="https://arxiv.org/format/2408.01501">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"> Galaxy populations in the Hydra I cluster from the VEGAS survey III. The realm of low surface brightness features and intra-cluster light </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Lohmann%2C+F+S">Felipe S. Lohmann</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Calvi%2C+R">Rosa Calvi</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Corsini%2C+E+M">Enrico M. Corsini</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</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="2408.01501v1-abstract-short" style="display: inline;"> In this paper, we analyse the light distribution in the Hydra I cluster of galaxies to explore their low surface brightness features, measure the intra-cluster light, and address the assembly history of the cluster. For this purpose, we used deep wide-field g- and r-band images obtained with the VST as part of the VEGAS project. The VST mosaic covers ~0.4 times the virial radius around the core of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01501v1-abstract-full').style.display = 'inline'; document.getElementById('2408.01501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.01501v1-abstract-full" style="display: none;"> In this paper, we analyse the light distribution in the Hydra I cluster of galaxies to explore their low surface brightness features, measure the intra-cluster light, and address the assembly history of the cluster. For this purpose, we used deep wide-field g- and r-band images obtained with the VST as part of the VEGAS project. The VST mosaic covers ~0.4 times the virial radius around the core of the cluster, which enabled us to map the light distribution down to faint surface brightness levels of mu_g ~ 28 mag/arcsec^2. In this region of the cluster, 44 cluster members are brighter than m_B<16 mag, and the region includes more than 300 dwarf galaxies. Similar to the projected distribution of all cluster members (bright galaxies and dwarfs), we find that the bulk of the galaxy light is concentrated in the cluster core, which also emits in the X-rays, and there are two overdensities: in the north (N) and south-east (SE) with respect to the cluster core. We present the analysis of the light distribution of all the bright cluster members. After removing foreground stars and other objects, we measured the diffuse intra-cluster light and compared its distribution with that of the globular clusters and dwarf galaxies in the cluster. We find that most of the diffuse light low surface brightness features, and signs of possible gravitational interaction between galaxies reside in the core and in the group in the N, while ram-pressure stripping is frequently found to affect galaxies within the SE group. All these features confirm that the mass assembly in this cluster is still ongoing. By combining the projected phase-space with these observed properties, we trace the different stages of the assembly history. We also address the main formation channels for the intra-cluster light detected in the cluster, which contributes ~ 12% to the total luminosity of the cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01501v1-abstract-full').style.display = 'none'; document.getElementById('2408.01501v1-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 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">18 pages, 13 figures, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.21620">arXiv:2407.21620</a> <span> [<a href="https://arxiv.org/pdf/2407.21620">pdf</a>, <a href="https://arxiv.org/format/2407.21620">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/10.1051/0004-6361/202451273">10.1051/0004-6361/202451273 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VEGAS-SSS: Tracing Globular Cluster Populations in the Interacting NGC3640 Galaxy Group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Lonare%2C+P">Pratik Lonare</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Hazra%2C+N">Nandini Hazra</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Riccio%2C+G">Gabriele Riccio</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R+A">Rebecca A. Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Brocato%2C+E">Enzo Brocato</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Grado%2C+A">Aniello Grado</a>, <a href="/search/astro-ph?searchtype=author&query=Limatola%2C+L">Luca Limatola</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="2407.21620v1-abstract-short" style="display: inline;"> Globular clusters (GCs) are among the oldest stellar systems in the universe. As such, GCs population are valuable fossil tracers of galaxy formation and interaction history. We use the multi-band wide-field images obtained with the VST to study the properties of the GC population in an interacting pair of galaxies. We derived ugri photometry over $1.5x1.5deg^2$ centred on the galaxy group compose… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21620v1-abstract-full').style.display = 'inline'; document.getElementById('2407.21620v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.21620v1-abstract-full" style="display: none;"> Globular clusters (GCs) are among the oldest stellar systems in the universe. As such, GCs population are valuable fossil tracers of galaxy formation and interaction history. We use the multi-band wide-field images obtained with the VST to study the properties of the GC population in an interacting pair of galaxies. We derived ugri photometry over $1.5x1.5deg^2$ centred on the galaxy group composed by two elliptical galaxies: NGC3640 and its fainter companion NGC3641. We studied the GC system properties from both the ugri and gri matched catalogs GC candidates were identified based on a combination of photometric properties (colors, magnitudes) and morphometric criteria (concentration index, elongation, FWHM), using sources with well-defined classifications from spectroscopic or imaging data available in the literature and numerical simulations as references. The selection criteria were also applied to empty fields to determine a statistical background correction for the number of identified GC candidates. The 2D density maps of GCs appear to align with the diffuse light patches resulting from merging events of the galaxies. The highest density peak of GCs is observed to be on NGC3641 rather than NGC3640, despite the latter being the more massive galaxy. The azimuthal averaged radial density profiles in both galaxies reveal that the GC population extends beyond the galaxy light profile and indicate the likely presence of an intra-group GC component. A color bimodality in (u-r) and (g-i) is observed for NGC3641, whereas NGC3640 shows a broad unimodal distribution. Analysis of the GC Luminosity Function indicates that both galaxies are roughly located at the same distance (~27Mpc). We provide an estimate of the total number of GCs, and determine the specific frequency for NGC3640, $S_N =2.0\pm0.6$, which aligns with expectations, while for NGC3641 we find a large $S_N=4.5\pm1.6$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21620v1-abstract-full').style.display = 'none'; document.getElementById('2407.21620v1-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> 31 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">37 pages, 23 figures, 13 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A104 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.07163">arXiv:2407.07163</a> <span> [<a href="https://arxiv.org/pdf/2407.07163">pdf</a>, <a href="https://arxiv.org/format/2407.07163">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/10.1051/0004-6361/202450642">10.1051/0004-6361/202450642 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The YMCA (Yes, Magellanic Clouds Again) survey: probing the outer regions of the Magellanic system with VST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gatto%2C+M">Massimiliano Gatto</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">Vincenzo Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">Michele Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Tosi%2C+M">Monica Tosi</a>, <a href="/search/astro-ph?searchtype=author&query=Cignoni%2C+M">Michele Cignoni</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">Crescenzo Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">Marcella Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Dall%27Ora%2C+M">Massimo Dall'Ora</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+L">Maria-Rosa L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Musella%2C+I">Ilaria Musella</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</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="2407.07163v1-abstract-short" style="display: inline;"> The Magellanic Clouds (MCs) are the Milky Way's most massive dwarf satellites. As they also represent the closest pair of galaxies in an ongoing tidal interaction, while simultaneously infalling into the Milky Way halo, they provide a unique opportunity to study in detail an ongoing three-body encounter. We present the ``YMCA (Yes, Magellanic Clouds Again) survey: probing the outer regions of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07163v1-abstract-full').style.display = 'inline'; document.getElementById('2407.07163v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.07163v1-abstract-full" style="display: none;"> The Magellanic Clouds (MCs) are the Milky Way's most massive dwarf satellites. As they also represent the closest pair of galaxies in an ongoing tidal interaction, while simultaneously infalling into the Milky Way halo, they provide a unique opportunity to study in detail an ongoing three-body encounter. We present the ``YMCA (Yes, Magellanic Clouds Again) survey: probing the outer regions of the Magellanic system with VST'' based on deep optical photometry carried out with the VLT Survey Telescope (VST). YMCA targeted 110 square degrees, in the g and i filters, in the periphery of both the MCs, including a long strip in between the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC). The photometry of YMCA is sufficiently deep (50\% complete down to $g \simeq 23.5-24.0$~mag) to allow for a detailed analysis of main-sequence stars in regions of the MCs remained relatively unexplored at these faint magnitudes. The resulting colour-magnitude diagrams reveal that the outskirts of the MCs are predominantly characterized by intermediate-age and old stellar populations, with limited or negligible evidence of recent star formation. The analysis of the age distribution of star clusters (SCs) within the surveyed area, both already known and newly discovered candidates, hints at a close fly-by between the LMC and SMC that occurred $\simeq 2.5-3.0$~Gyr ago, in agreement with previous results. We also report the discovery of candidate SCs with ages within the so-called ``age-gap'', questioning its real existence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07163v1-abstract-full').style.display = 'none'; document.getElementById('2407.07163v1-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 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">28 pages, 21 figures. Accepted for publication on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A164 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.17000">arXiv:2405.17000</a> <span> [<a href="https://arxiv.org/pdf/2405.17000">pdf</a>, <a href="https://arxiv.org/format/2405.17000">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/10.1051/0004-6361/202449441">10.1051/0004-6361/202449441 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MHONGOOSE discovery of a gas-rich low-surface brightness galaxy in the Dorado Group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Pi%C3%B1a%2C+P+E+M">P. E. Mancera Pi帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">R. Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=McGaugh%2C+S">S. McGaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Oman%2C+K+A">K. A. Oman</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</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=Kim%2C+M">M. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Amram%2C+P">P. Amram</a>, <a href="/search/astro-ph?searchtype=author&query=Bosma%2C+A">A. Bosma</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Brinks%2C+E">E. Brinks</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=Gibson%2C+B">B. Gibson</a>, <a href="/search/astro-ph?searchtype=author&query=Healy%2C+J">J. Healy</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">S. Kurapati</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.17000v1-abstract-short" style="display: inline;"> We present the discovery of a low-mass gas-rich low-surface brightness galaxy in the Dorado Group, at a distance of 17.7 Mpc. Combining deep MeerKAT 21-cm observations from the MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters (MHONGOOSE) survey with deep photometric images from the VST Early-type Galaxy Survey (VEGAS) we find a stellar and neutral atomic hydrogen (HI… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17000v1-abstract-full').style.display = 'inline'; document.getElementById('2405.17000v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17000v1-abstract-full" style="display: none;"> We present the discovery of a low-mass gas-rich low-surface brightness galaxy in the Dorado Group, at a distance of 17.7 Mpc. Combining deep MeerKAT 21-cm observations from the MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters (MHONGOOSE) survey with deep photometric images from the VST Early-type Galaxy Survey (VEGAS) we find a stellar and neutral atomic hydrogen (HI) gas mass of $M_\star = 2.23\times10^6$ M$_\odot$ and $M_{\rm HI}=1.68\times10^6$ M$_\odot$, respectively. This low-surface brightness galaxy is the lowest mass HI detection found in a group beyond the Local Universe ($D\gtrsim 10$ Mpc). The dwarf galaxy has the typical overall properties of gas-rich low surface brightness galaxies in the Local group, but with some striking differences. Namely, the MHONGOOSE observations reveal a very low column density ($\sim 10^{18-19}$ cm$^{-2}$) HI disk with asymmetrical morphology possibly supported by rotation and higher velocity dispersion in the centre. There, deep optical photometry and UV-observations suggest a recent enhancement of the star formation. Found at galactocentric distances where in the Local Group dwarf galaxies are depleted of cold gas (at $390$ projected-kpc distance from the group centre), this galaxy is likely on its first orbit within the Dorado group. We discuss the possible environmental effects that may have caused the formation of the HI disk and the enhancement of star formation, highlighting the short-lived phase (a few hundreds of Myr) of the gaseous disk, before either SF or hydrodynamical forces will deplete the gas of the galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17000v1-abstract-full').style.display = 'none'; document.getElementById('2405.17000v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 14 figures, 5 tables; accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A69 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.12966">arXiv:2309.12966</a> <span> [<a href="https://arxiv.org/pdf/2309.12966">pdf</a>, <a href="https://arxiv.org/format/2309.12966">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> INSPIRE: INvestigating Stellar Population In RElics V. A catalogue of ultra-compact massive galaxies outside the local Universe and their degree of relicness </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">J. Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Pulsoni%2C+C">C. Pulsoni</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">M. Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Maksymowicz-Maciata%2C+M">M. Maksymowicz-Maciata</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bevacqua%2C+D">D. Bevacqua</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L+K">L. K. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn-Navarro%2C+I">I. Mart铆n-Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Saracco%2C+P">P. Saracco</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</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="2309.12966v2-abstract-short" style="display: inline;"> This paper presents the third data release of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 52 ultra-compact massive galaxies (UCMGs) observed with the X-Shooter spectrograph. We measure integrated stellar velocity dispersion, [Mg/Fe] abundances, ages, and metallicities for all the INSPIRE objects. We thus infer star formation histories and confirm the existence of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12966v2-abstract-full').style.display = 'inline'; document.getElementById('2309.12966v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.12966v2-abstract-full" style="display: none;"> This paper presents the third data release of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 52 ultra-compact massive galaxies (UCMGs) observed with the X-Shooter spectrograph. We measure integrated stellar velocity dispersion, [Mg/Fe] abundances, ages, and metallicities for all the INSPIRE objects. We thus infer star formation histories and confirm the existence of a degree of relicness (DoR), defined in terms of the fraction of stellar mass formed by $z=2$, the time at which a galaxy has assembled 75\% of its mass, and the final assembly time. Objects with a high DoR assembled their stellar mass at early epochs, while low-DoR objects show a non-negligible fraction of later-formed populations and hence a spread in ages and metallicities. A higher DoR correlates with larger [Mg/Fe], super-solar metallicity, and larger velocity dispersion values. The 52 UMCGs span a large range of DoR from 0.83 to 0.06, with 38 of them having formed more than 75\% of their mass by $z=2$. Of these, nine are extreme relics (DoR$>0.7$), since they formed the totality ($>99\%$) of their stellar mass by redshift $z=2$. The remaining 14 UCMGs cannot be considered relics, as they are characterised by more extended star formation histories. With INSPIRE, we built the first sizeable sample of relics outside the local Universe, up to $z\sim0.4$, increasing the number of confirmed relics by a factor of $>10$, and opening up an important window to explain the mass assembly of massive galaxies in the high-z Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12966v2-abstract-full').style.display = 'none'; document.getElementById('2309.12966v2-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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 on MNRAS, 20 pages, 15 figures, 3 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/2308.11496">arXiv:2308.11496</a> <span> [<a href="https://arxiv.org/pdf/2308.11496">pdf</a>, <a href="https://arxiv.org/format/2308.11496">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Ultra diffuse galaxies in the Hydra I cluster from the LEWIS Project: Phase-Space distribution and globular cluster richness </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D">Duncan Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Gannon%2C+J">Jonah Gannon</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Doll%2C+G">Goran Doll</a>, <a href="/search/astro-ph?searchtype=author&query=Buttitta%2C+C">Chiara Buttitta</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Barroso%2C+J+F">Jesus Falcon Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Greggio%2C+L">Laura Greggio</a>, <a href="/search/astro-ph?searchtype=author&query=Gullieuszik%2C+M">Marco Gullieuszik</a>, <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">Johanna Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">Roberto Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">Chiara Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+G">Giulio Capasso</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="2308.11496v1-abstract-short" style="display: inline;"> Although ultra diffuse galaxies (UDGs) are found in large numbers in clusters of galaxies, the role of the cluster environment in shaping their low surface brightness and large sizes is still uncertain. Here we examine a sample of UDGs in the Hydra I cluster (D = 51 Mpc) with new radial velocities obtained as part of the LEWIS (Looking into the faintest with MUSE) project using VLT/MUSE data. Usin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11496v1-abstract-full').style.display = 'inline'; document.getElementById('2308.11496v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.11496v1-abstract-full" style="display: none;"> Although ultra diffuse galaxies (UDGs) are found in large numbers in clusters of galaxies, the role of the cluster environment in shaping their low surface brightness and large sizes is still uncertain. Here we examine a sample of UDGs in the Hydra I cluster (D = 51 Mpc) with new radial velocities obtained as part of the LEWIS (Looking into the faintest with MUSE) project using VLT/MUSE data. Using a phase-space, or infall diagnostic, diagram we compare the UDGs to other known galaxies in the Hydra I cluster and to UDGs in other clusters. The UDGs, along with the bulk of regular Hydra I galaxies, have low relative velocities and are located near the cluster core, and thus consistent with very early infall into the cluster. Combining with literature data, we do not find the expected trend of GC-rich UDGs associated with earlier infall times. This result suggests that quenching mechanisms other than cluster infall should be further considered, e.g. quenching by strong feedback or in cosmic sheets and filaments. Tidal stripping of GCs in the cluster environment also warrants further modelling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11496v1-abstract-full').style.display = 'none'; document.getElementById('2308.11496v1-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 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">6 pages, 2 figures, MNRAS, 525, 93</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.11493">arXiv:2308.11493</a> <span> [<a href="https://arxiv.org/pdf/2308.11493">pdf</a>, <a href="https://arxiv.org/format/2308.11493">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/10.1051/0004-6361/202347129">10.1051/0004-6361/202347129 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Looking into the faintEst WIth MUSE (LEWIS): on the nature of ultra-diffuse galaxies in the Hydra-I cluster.I. Project description and preliminary results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Doll%2C+G">Goran Doll</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Buttitta%2C+C">Chiara Buttitta</a>, <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">Johanna Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Gullieuszik%2C+M">Marco Gullieuszik</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">Chiara Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Corsini%2C+E+M">Enrico M. Corsini</a>, <a href="/search/astro-ph?searchtype=author&query=Greggio%2C+L">Laura Greggio</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">Jesus Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Fahrion%2C+K">Katja Fahrion</a>, <a href="/search/astro-ph?searchtype=author&query=Fritz%2C+J">Jacopo Fritz</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">Maria Angela Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">Roberto Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Sarzi%2C+M">Marc Sarzi</a> , et al. (1 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="2308.11493v1-abstract-short" style="display: inline;"> Looking into the faintEst WIth MUSE (LEWIS) is an ESO large observing programme aimed at obtaining the first homogeneous integral-field spectroscopic survey of 30 extremely low-surface brightness (LSB) galaxies in the Hydra I cluster of galaxies, with MUSE at ESO-VLT. The majority of LSB galaxies in the sample (22 in total) are ultra-diffuse galaxies (UDGs). The distribution of systemic velocities… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11493v1-abstract-full').style.display = 'inline'; document.getElementById('2308.11493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.11493v1-abstract-full" style="display: none;"> Looking into the faintEst WIth MUSE (LEWIS) is an ESO large observing programme aimed at obtaining the first homogeneous integral-field spectroscopic survey of 30 extremely low-surface brightness (LSB) galaxies in the Hydra I cluster of galaxies, with MUSE at ESO-VLT. The majority of LSB galaxies in the sample (22 in total) are ultra-diffuse galaxies (UDGs). The distribution of systemic velocities Vsys ranges between 2317 km/s and 5198 km/s and is centred on the mean velocity of Hydra I (Vsys = 3683 $\pm$ 46 km/s). Considering the mean velocity and the velocity dispersion of the cluster, 17 out of 20 targets are confirmed cluster members. To assess the quality of the data and demonstrate the feasibility of the science goals, we report the preliminary results obtained for one of the sample galaxies, UDG11. For this target, we derived the stellar kinematics, including the 2-dimensional maps of line-of-sight velocity and velocity dispersion, constrained age and metallicity, and studied the globular cluster (GC) population hosted by the UDG. Results are compared with the available measurements for UDGs and dwarf galaxies in literature. By fitting the stacked spectrum inside one effective radius, we find that UDG11 has a velocity dispersion $蟽= 20 \pm 8$ km/s, it is old ($10\pm1$ Gyr), metal-poor ([M/H]=-1.17$\pm$0.11 dex) and has a total dynamical mass-to-light ratio M$/L_V\sim 14$, comparable to those observed for classical dwarf galaxies. The spatially resolved stellar kinematics maps suggest that UDG11 does not show a significant velocity gradient along either major or minor photometric axes. We find two GCs kinematically associated with UDG11. The estimated total number of GCs in UDG11, corrected for the spectroscopic completeness limit, is $N_{GC}= 5.9^{+2.2}_ {-1.8}$, which corresponds to a GC specific frequency of $S_N = 8.4^{+3.2}_{-2.7}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11493v1-abstract-full').style.display = 'none'; document.getElementById('2308.11493v1-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 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 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 679, A69 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.01075">arXiv:2305.01075</a> <span> [<a href="https://arxiv.org/pdf/2305.01075">pdf</a>, <a href="https://arxiv.org/format/2305.01075">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/10.1051/0004-6361/202346521">10.1051/0004-6361/202346521 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The AGN fuelling/feedback cycle in nearby radio galaxies - V. The cold atomic gas of NGC 3100 and its group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">I. Ruffa</a>, <a href="/search/astro-ph?searchtype=author&query=Loni%2C+A">A. Loni</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">R. Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</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="2305.01075v1-abstract-short" style="display: inline;"> We present Australia Compact Telescope Array (ATCA) 21-cm observations of the nearby low-excitation radio galaxy (LERG) NGC 3100. This is the brightest galaxy of a loose group and hosts a young ($\sim 2$ Myr) radio source. The ATCA observations reveal for the first time the presence of neutral hydrogen (HI) gas in absorption in the centre of this radio galaxy, and in emission in two low-mass galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.01075v1-abstract-full').style.display = 'inline'; document.getElementById('2305.01075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.01075v1-abstract-full" style="display: none;"> We present Australia Compact Telescope Array (ATCA) 21-cm observations of the nearby low-excitation radio galaxy (LERG) NGC 3100. This is the brightest galaxy of a loose group and hosts a young ($\sim 2$ Myr) radio source. The ATCA observations reveal for the first time the presence of neutral hydrogen (HI) gas in absorption in the centre of this radio galaxy, and in emission in two low-mass galaxies of the group and in a diffuse dark cloud in the proximity of NGC 3100. The sensitivity to low-column density gas ($N_{\rm HI}\sim 10^{19}$ cm$^{-2}$) allows us to reveal asymmetries in the periphery of most the HI-detected galaxies, suggesting that tidal interactions may be on-going. The diffuse cloud does not show a stellar counterpart down to $27$ mag/arcsec$^2$ and could be the remnant of these interactions. The analysis of the HI absorption complex in NGC 3100 indicates that the atomic phase of the hydrogen is distributed as its molecular phase (observed at arcsecond resolution through several carbon monoxide emission lines). We suggest that the interactions occurring within the group are causing turbulent cold gas clouds in the intra-group medium to be slowly accreted towards the centre of NGC 3100. This caused the recent formation of the cold circum-nuclear disk which is likely sustaining the young nuclear activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.01075v1-abstract-full').style.display = 'none'; document.getElementById('2305.01075v1-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">10 pages, 7 figures; submitted to 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 675, A59 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.06533">arXiv:2302.06533</a> <span> [<a href="https://arxiv.org/pdf/2302.06533">pdf</a>, <a href="https://arxiv.org/format/2302.06533">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/stad503">10.1093/mnras/stad503 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> INSPIRE: INvestigating Stellar Population In RElics IV. The Initial Mass Function slope in relics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martin-Navarro%2C+I">I. Martin-Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Ferre-Mateu%2C+A">A. Ferre-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Pulsoni%2C+C">C. Pulsoni</a>, <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">J. Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L">L. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</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="2302.06533v1-abstract-short" style="display: inline;"> In the last decade, growing evidence has emerged supporting a non-universal stellar Initial Mass Function (IMF) in massive galaxies, with a larger number of dwarf stars with respect to the Milky-Way (bottom-heavy IMF). However, a consensus about the mechanisms that cause IMF variations is yet to be reached. Recently, it has been suggested that stars formed early-on in cosmic time, via a star forma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.06533v1-abstract-full').style.display = 'inline'; document.getElementById('2302.06533v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.06533v1-abstract-full" style="display: none;"> In the last decade, growing evidence has emerged supporting a non-universal stellar Initial Mass Function (IMF) in massive galaxies, with a larger number of dwarf stars with respect to the Milky-Way (bottom-heavy IMF). However, a consensus about the mechanisms that cause IMF variations is yet to be reached. Recently, it has been suggested that stars formed early-on in cosmic time, via a star formation burst, could be characterised by a bottom-heavy IMF. A promising way to confirm this is to use relics, ultra-compact massive galaxies, almost entirely composed by these "pristine" stars. The INSPIRE Project aims at assembling a large sample of confirmed relics, that can serve as laboratory to investigate on the conditions of star formation in the first 1-3 Gyr of the Universe. In this third INSPIRE paper, we build a high signal-to-noise spectrum from five relics and one from five galaxies with similar sizes, masses, and kinematical properties, but characterised by a more extended star formation history (non-relics). Our detailed stellar population analysis suggests a systematically bottom-heavier IMF slope for relics than for non-relics, adding new observational evidence for the non-universality of the IMF at various redshifts and further supporting the above proposed physical scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.06533v1-abstract-full').style.display = 'none'; document.getElementById('2302.06533v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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. 8 pages, 5 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/2212.06164">arXiv:2212.06164</a> <span> [<a href="https://arxiv.org/pdf/2212.06164">pdf</a>, <a href="https://arxiv.org/format/2212.06164">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/10.1051/0004-6361/202245530">10.1051/0004-6361/202245530 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Does the virial mass drive the intra-cluster light? The relationship between the ICL and M$_{vir}$ from VEGAS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+M">Mireia Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</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="2212.06164v1-abstract-short" style="display: inline;"> In this Letter we revisit the relationship between the fraction of the intra-cluster light (ICL) and both the virial mass and the fraction of Early Type Galaxies in the host halo. This is based on a statistically significant and homogeneous sample of 22 groups and clusters of galaxies in the local Universe ($z \leq 0.05$), obtained with the VST Early-type GAlaxy Survey (VEGAS). Taking advantage of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06164v1-abstract-full').style.display = 'inline'; document.getElementById('2212.06164v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.06164v1-abstract-full" style="display: none;"> In this Letter we revisit the relationship between the fraction of the intra-cluster light (ICL) and both the virial mass and the fraction of Early Type Galaxies in the host halo. This is based on a statistically significant and homogeneous sample of 22 groups and clusters of galaxies in the local Universe ($z \leq 0.05$), obtained with the VST Early-type GAlaxy Survey (VEGAS). Taking advantage of the long integration time and large area of the VEGAS images, we are able to map the galaxy outskirts and ICL down to $渭_g$ $\geq$ 29-30 mag/arcsec$^2$ and out to hundreds of kpc. With this data-set, we have expanded the sample of ICL measurements, doubling the previous measures available from the literature for z $\leq$ 0.05. The main result of this work is the lack of any significant trend between the fraction of ICL and the virial mass of the host environment, covering a wide range of virial masses ( $\sim$ $10^{12.5} \leq M_{vir} \leq 10^{15.5} M_{\odot}$), in agreement with some theoretical studies. Since the new data points are all derived with the same methodology and from the same observational setup, and all have comparable depth, the large observed scatter indicates an intrinsic variation in the ICL fraction.On the other hand, there is a weak relation between the fraction of ICL and the fraction of Early Type Galaxies in the host halo, where a larger fraction of ICL is found in groups and clusters of galaxies dominated by earlier morphological types, indicating a connection between the ICL and the dynamical state of the host system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06164v1-abstract-full').style.display = 'none'; document.getElementById('2212.06164v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 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">Letter to the editor, accepted for publication in A&A. 8 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 670, L20 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.05525">arXiv:2209.05525</a> <span> [<a href="https://arxiv.org/pdf/2209.05525">pdf</a>, <a href="https://arxiv.org/format/2209.05525">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/stac2606">10.1093/mnras/stac2606 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SAMI -- Fornax Dwarfs Survey II: The Stellar Mass Fundamental Plane and the Dark Matter fraction of Dwarf Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eftekhari%2C+F+S">F. Sara Eftekhari</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R+F">Reynier F. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+N">Nicholas Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+J+J">Julia J. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Croom%2C+S+M">Scott M. Croom</a>, <a href="/search/astro-ph?searchtype=author&query=Drinkwater%2C+M+J">Michael J. Drinkwater</a>, <a href="/search/astro-ph?searchtype=author&query=Falcon-Barroso%2C+J">Jesus Falcon-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">Nicola R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Valentijn%2C+E+A">Edwin A. Valentijn</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">Aku Venhola</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.05525v1-abstract-short" style="display: inline;"> We explore the kinematic scaling relations of 38 dwarf galaxies in the Fornax Cluster using observations from the SAMI integral field spectrograph. We focus on the Fundamental Plane (FP), defined by the physical properties of the objects (scale length, surface brightness and velocity dispersion) and the Stellar Mass (Fundamental) Plane, where surface brightness is replaced by stellar mass, and inv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05525v1-abstract-full').style.display = 'inline'; document.getElementById('2209.05525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.05525v1-abstract-full" style="display: none;"> We explore the kinematic scaling relations of 38 dwarf galaxies in the Fornax Cluster using observations from the SAMI integral field spectrograph. We focus on the Fundamental Plane (FP), defined by the physical properties of the objects (scale length, surface brightness and velocity dispersion) and the Stellar Mass (Fundamental) Plane, where surface brightness is replaced by stellar mass, and investigate their dynamical-to-stellar-mass ratio. We confirm earlier results that the Fornax dEs are significantly offset above the FP defined by massive, hot stellar systems. For the Stellar Mass (Fundamental) Plane, which shows much lower scatter, we find that young and old dwarf galaxies lie at about the same distance from the plane, all with comparable scatter. We introduce the perpendicular deviation of dwarf galaxies from the Stellar Mass Plane defined by giant early-types as a robust estimate of their DM fraction, and find that the faintest dwarfs are systematically offset above the plane, implying that they have a higher dark matter fraction. This result is confirmed when estimating the dynamical mass of our dEs using a virial mass estimator, tracing the onset of dark matter domination in low mass stellar systems. We find that the position of our galaxies on the Stellar Mass FP agrees with the galaxies in the Local Group. This seems to imply that the processes determining the position of dwarf galaxies on the FP depend on the environment in the same way, whether the galaxy is situated in the Local Group or in the Fornax Cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05525v1-abstract-full').style.display = 'none'; document.getElementById('2209.05525v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 14 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/2207.09478">arXiv:2207.09478</a> <span> [<a href="https://arxiv.org/pdf/2207.09478">pdf</a>, <a href="https://arxiv.org/format/2207.09478">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/10.1051/0004-6361/202243993">10.1051/0004-6361/202243993 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMHK 1762: Another star cluster in the Large Magellanic Cloud age gap </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gatto%2C+M">M. Gatto</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">M. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Tosi%2C+M">M. Tosi</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Cignoni%2C+M">M. Cignoni</a>, <a href="/search/astro-ph?searchtype=author&query=Dall%27Ora%2C+M">M. Dall'Ora</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+-+L">M. -R. L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Longo%2C+G">G. Longo</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">M. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Musella%2C+I">I. Musella</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">P. Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</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="2207.09478v1-abstract-short" style="display: inline;"> The star cluster (SC) age distribution of the Large Magellanic Cloud (LMC) exhibits a gap from $\sim$ 4 to 10 Gyr ago, with an almost total absence of SCs. Within this age gap, only two confirmed SCs have been identified hitherto. Nonetheless, the star field counterpart does not show the same characteristics, making the LMC a peculiar galaxy where star formation history and cluster formation histo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09478v1-abstract-full').style.display = 'inline'; document.getElementById('2207.09478v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.09478v1-abstract-full" style="display: none;"> The star cluster (SC) age distribution of the Large Magellanic Cloud (LMC) exhibits a gap from $\sim$ 4 to 10 Gyr ago, with an almost total absence of SCs. Within this age gap, only two confirmed SCs have been identified hitherto. Nonetheless, the star field counterpart does not show the same characteristics, making the LMC a peculiar galaxy where star formation history and cluster formation history appear to differ significantly. We re-analyzed the color-magnitude diagram (CMD) of the KMHK 1762 SC by using the deep optical photometry provided by the "Yes, Magellanic Clouds Again" survey, to robustly assess its age. First, we partially removed foreground and/or field stars by means of parallaxes and proper motions obtained from the {\it Gaia} Early Data Release 3. Then, we applied the Automated Stellar Cluster Analysis package to the cleaned photometric catalogue to identify the isochrone that best matches the CMD of KMHK 1762. The estimated age of KMHK 1762 is $\log (t) = 9.74 \pm 0.15$ dex ($\sim$5.5 Gyr), that is more than 2 Gyr older than the previous estimation which was obtained with shallower photometry. This value makes KMHK 1762 the third confirmed age gap SC of the LMC. The physical existence of a quiescent period of the LMC SC formation is questioned. We suggest it can be the result of an observational bias, originated by the combination of shallow photometry and limited investigation of the LMC periphery. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09478v1-abstract-full').style.display = 'none'; document.getElementById('2207.09478v1-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, 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">6 pages, 4 figures. Accepted for publication in A&A Letter</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, L12 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.14207">arXiv:2206.14207</a> <span> [<a href="https://arxiv.org/pdf/2206.14207">pdf</a>, <a href="https://arxiv.org/format/2206.14207">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 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/10.1051/0004-6361/202142894">10.1051/0004-6361/202142894 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Properties of intra-cluster low-mass X-ray binaries in Fornax globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riccio%2C+G">G. Riccio</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">M. Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+R+D+X">R. D'Abrusco X. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Z. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T">T. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">S. Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Prole%2C+D+J">D. J. Prole</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Gatto%2C+M">M. Gatto</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</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="2206.14207v1-abstract-short" style="display: inline;"> We present a study of the intra-cluster population of low-mass X-ray binaries (LMXB) residing in globular clusters (GC) in the central 1 $deg^2$ of the Fornax galaxy cluster. Differently from previous studies, which were restricted to the innermost regions of individual galaxies, this work is aimed at comparing the properties of the intra-cluster population of GC-LMXBs with those of the host galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.14207v1-abstract-full').style.display = 'inline'; document.getElementById('2206.14207v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.14207v1-abstract-full" style="display: none;"> We present a study of the intra-cluster population of low-mass X-ray binaries (LMXB) residing in globular clusters (GC) in the central 1 $deg^2$ of the Fornax galaxy cluster. Differently from previous studies, which were restricted to the innermost regions of individual galaxies, this work is aimed at comparing the properties of the intra-cluster population of GC-LMXBs with those of the host galaxy. We use VLT Survey Telescope (VST) and Chandra observations. We identify 168 LMXBs residing in GCs and divide it into host-galaxy and intra-cluster objects based on their distance from the nearest galaxy in terms of effective radius. We found 82 intra-cluster GC-LMXBs and 86 objects that are hosted in galaxies. We perform a Gaussian mixture model to divide the population into red and blue GCs. As has been found for the innermost regions of galaxies, LMXBs tend to form in red and bright GCs in intra-cluster space as well. We find, however, that the likelihood of a red GC to host an LMXB decreases with galactocentric distance, but it remains approximately constant for the blue GC population. Investigating the X-ray properties of the LMXBs residing in GCs, we find a difference in the X-ray luminosity function between the intra-cluster and host-galaxy sample: both follow a power-law down to $\sim 8.5\times 10^{37}$ erg s$^{-1}$, which is consistent with field LMXBs for the intra-cluster sample, while the latter agree with previous estimates for LMXBs in GCs. We detect a tentative difference in the hardness ratio of two populations, where the intra-cluster GC-LMXBs appear to have harder spectra than the host-galaxy objects. We find the same trend when we compare red and blue GC-LMXBs: the spectra of the blue sample are harder spectra than those of the red sample. This result could suggest a relation between the spectral properties of LMXBs and the host GC colour and therefore its metallicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.14207v1-abstract-full').style.display = 'none'; document.getElementById('2206.14207v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 by 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/2206.07385">arXiv:2206.07385</a> <span> [<a href="https://arxiv.org/pdf/2206.07385">pdf</a>, <a href="https://arxiv.org/format/2206.07385">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/10.1051/0004-6361/202142367">10.1051/0004-6361/202142367 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy populations in the Hydra I cluster from the VEGAS survey II. The ultra-diffuse galaxy population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Greggio%2C+L">Laura Greggio</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">Chiara Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">Aku Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">Maria Angela Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">Roberto Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">Reynier Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Challapa%2C+N+C">Nelvy Choque Challapa</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</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="2206.07385v1-abstract-short" style="display: inline;"> In this work, we extend the catalog of low-surface brightness (LSB) galaxies, including Ultra-Diffuse Galaxy (UDG) candidates, within $\approx 0.4R_{vir}$ of the Hydra I cluster of galaxies, based on deep images from the VST Early-type GAlaxy Survey (VEGAS). The new galaxies are found by applying an automatic detection tool and carrying out additional visual inspections of $g$ and $r$ band images.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.07385v1-abstract-full').style.display = 'inline'; document.getElementById('2206.07385v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.07385v1-abstract-full" style="display: none;"> In this work, we extend the catalog of low-surface brightness (LSB) galaxies, including Ultra-Diffuse Galaxy (UDG) candidates, within $\approx 0.4R_{vir}$ of the Hydra I cluster of galaxies, based on deep images from the VST Early-type GAlaxy Survey (VEGAS). The new galaxies are found by applying an automatic detection tool and carrying out additional visual inspections of $g$ and $r$ band images. This led to the detection of 11 UDGs and 8 more LSB galaxies. For all of them, the cluster membership has been assessed using the color-magnitude relation derived for early-type giant and dwarf galaxies in Hydra I. The UDGs and new LSB galaxies found in Hydra I span a wide range of central surface brightness ($22.7 \lesssim 渭_{0,g} \lesssim 26.5$ mag/arcsec$^2$), effective radius ($0.6 \lesssim R_e \lesssim 4.0$ kpc) and color ($0.4 \leq g-r \leq 0.9$ mag), and have stellar masses in the range $\sim 5\times 10^6 - 2\times 10^8$M$_{\odot}$. The 2D projected distribution of both galaxy types is similar to the spatial distribution of dwarf galaxies, with over-densities in the cluster core and north of the cluster centre. They have similar color distribution and comparable stellar masses to the red dwarf galaxies. Based on photometric selection, we identify a total of 9 globular cluster candidates associated to the UDGs and 4 to the LSB galaxies, with the highest number of candidates in an individual UDG being three. We find that there are no relevant differences between dwarfs, LSB galaxies and UDGs: the structural parameters (that is surface brightness, size, colors, n-index) and GCs content of the three classes have similar properties and trends. This finding is consistent with UDGs being the extreme LSB tail of the size-luminosity distribution of dwarfs in this environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.07385v1-abstract-full').style.display = 'none'; document.getElementById('2206.07385v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 A&A. 30 pages, 22 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, A105 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.01578">arXiv:2206.01578</a> <span> [<a href="https://arxiv.org/pdf/2206.01578">pdf</a>, <a href="https://arxiv.org/format/2206.01578">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/10.1051/0004-6361/202243726">10.1051/0004-6361/202243726 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dorado and its member galaxies. III. Mapping star formation with FUV imaging from UVIT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">R. Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzei%2C+P">P. Mazzei</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A">A. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+L">L. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Postma%2C+J">J. Postma</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">R. Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Held%2C+E+V">E. V. Held</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="2206.01578v1-abstract-short" style="display: inline;"> We are investigating the SF in galaxies of the actively evolving Dorado group where signatures of interactions and merging events are revealed by optical and radio observations in both ETGs and LTGs. Our previous Ha+[NII] study, probing ~10 Myrs timescales, suggested that SF is still ongoing in ETGs. In this work, we use far-UV (FUV) imaging to map recent SF on times scales of about 100 Myrs. We u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.01578v1-abstract-full').style.display = 'inline'; document.getElementById('2206.01578v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.01578v1-abstract-full" style="display: none;"> We are investigating the SF in galaxies of the actively evolving Dorado group where signatures of interactions and merging events are revealed by optical and radio observations in both ETGs and LTGs. Our previous Ha+[NII] study, probing ~10 Myrs timescales, suggested that SF is still ongoing in ETGs. In this work, we use far-UV (FUV) imaging to map recent SF on times scales of about 100 Myrs. We used the Ultraviolet telescope UVIT on board Astrosat to image the Dorado backbone galaxies previously observed in Ha+[NII], with the far-UV filter FUV.CaF2 (1300-1800A). The sample includes NGC1536, NGC1546, NGC1549, [CMI2001]4136-01, NGC1553, IC2058, PGC75125,NGC1566, NGC1596 and NGC1602. FUV.CaF2 emission is revealed in all galaxies, tracing young stellar populations in rings and showing tidal distortions. The Sersic index, derived by fitting the luminosity profiles, is always n<3 suggesting that the FUV.CaF2 emission originates from a disk also in ETGs. The SFR ranges from 0.004+-0.001 M_sol yr^{-1} of [CMI2001]4136-01 to 2.455+-0.027 M_sol yr^{-1} of NGC 1566. Most of the recent SF is found at the periphery of the Dorado group where most of LTGs are located. For these galaxies, the ratio SFR_Ha/SFR_FUV.CaF2 is close to 1, except for the edge-on IC 2058, similarly to previously reported relations for Local Volume samples. For ETGs, however, SFR_Ha is about 15 times higher than SFR_FUV. The Dorado's ETGs define a separate locus in SFR_FUV, SFR_Ha space with respect to the LTGs, which is well represented by the relation log (SFR_FUV.CaF2) = 0.70xlog (SFR_{Ha})-1.26.The disk structure of the FUV.CaF2 emitting populations discovered in all the ETGs implies dissipative processes and wet merging events. The systematic discrepancy between SFRs derived from Ha and FUV fluxes suggests that rejuvenation episodes in ETGs cannot sustain constant SF over ~100 Myrs timescales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.01578v1-abstract-full').style.display = 'none'; document.getElementById('2206.01578v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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, 16 figures, accepted for publication in Astronomy & Astrophysics Main 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/2205.15331">arXiv:2205.15331</a> <span> [<a href="https://arxiv.org/pdf/2205.15331">pdf</a>, <a href="https://arxiv.org/format/2205.15331">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/10.1051/0004-6361/202243290">10.1051/0004-6361/202243290 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fornax3D project: The assembly history of massive early-type galaxies in the Fornax cluster from deep imaging and integral field spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">G. van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Morelli%2C+L">L. Morelli</a>, <a href="/search/astro-ph?searchtype=author&query=Corsini%2C+E+M">E. M. Corsini</a>, <a href="/search/astro-ph?searchtype=author&query=Sarzi%2C+M">M. Sarzi</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=Fahrion%2C+K">K. Fahrion</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">J. Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Gadotti%2C+D+A">D. A. Gadotti</a>, <a href="/search/astro-ph?searchtype=author&query=Lyubenova%2C+M">M. Lyubenova</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn-Navarro%2C+I">I. Mart铆n-Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=McDermid%2C+R+M">R. M. McDermid</a>, <a href="/search/astro-ph?searchtype=author&query=Pinna%2C+F">F. Pinna</a>, <a href="/search/astro-ph?searchtype=author&query=Pizzella%2C+A">A. Pizzella</a>, <a href="/search/astro-ph?searchtype=author&query=Poci%2C+A">A. Poci</a>, <a href="/search/astro-ph?searchtype=author&query=de+Zeeuw%2C+P+T">P. T. de Zeeuw</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">L. Zhu</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="2205.15331v1-abstract-short" style="display: inline;"> This work is based on high quality integral-field spectroscopic data obtained with the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (VLT). The 21 brightest ($m_B\leq 15$ mag) early-type galaxies (ETGs) inside the virial radius of the Fornax cluster are observed out to distances of $\sim2-3\ R_{\rm e}$. Deep imaging from the VLT Survey Telescope (VST) is also available for t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.15331v1-abstract-full').style.display = 'inline'; document.getElementById('2205.15331v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.15331v1-abstract-full" style="display: none;"> This work is based on high quality integral-field spectroscopic data obtained with the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (VLT). The 21 brightest ($m_B\leq 15$ mag) early-type galaxies (ETGs) inside the virial radius of the Fornax cluster are observed out to distances of $\sim2-3\ R_{\rm e}$. Deep imaging from the VLT Survey Telescope (VST) is also available for the sample ETGs. We investigate the variation of the galaxy structural properties as a function of the total stellar mass and cluster environment. Moreover, we correlate the size scales of the luminous components derived from a multi-component decomposition of the VST surface-brightness radial profiles of the sample ETGs with the MUSE radial profiles of stellar kinematic and population properties. The results are compared with both theoretical predictions and previous observational studies and used to address the assembly history of the massive ETGs of the Fornax cluster. We find that galaxies in the core and north-south clump of the cluster, which have the highest accreted mass fraction, show milder metallicity gradients in their outskirts than the galaxies infalling into the cluster. We also find a segregation in both age and metallicity between the galaxies belonging to the core and north-south clump and the infalling galaxies. The new findings fit well within the general framework for the assembly history of the Fornax cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.15331v1-abstract-full').style.display = 'none'; document.getElementById('2205.15331v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">23 pages, 7 figures, 3 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 663, A135 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.02420">arXiv:2204.02420</a> <span> [<a href="https://arxiv.org/pdf/2204.02420">pdf</a>, <a href="https://arxiv.org/format/2204.02420">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/ac6421">10.3847/2041-8213/ac6421 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep VLT photometry of the faint stellar system in the Large Magellanic Cloud periphery YMCA-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gatto%2C+M">M. Gatto</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">M. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Dall%27Ora%2C+M">M. Dall'Ora</a>, <a href="/search/astro-ph?searchtype=author&query=Tosi%2C+M">M. Tosi</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Cignoni%2C+M">M. Cignoni</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+-+L">M. -R. L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Longo%2C+G">G. Longo</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">M. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Musella%2C+I">I. Musella</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">P. Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</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="2204.02420v1-abstract-short" style="display: inline;"> We present FORS2@VLT follow-up photometry of YMCA-1, a recently discovered stellar system located 13\degr~from the Large Magellanic Cloud (LMC) center. The deep color-magnitude diagram (CMD) reveals a well-defined main sequence (MS) and a handful of stars in the post-MS evolutionary phases. We analyse the YMCA-1 CMD by means of the automated isochrone matching package {\tt ASteCA} and model its ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.02420v1-abstract-full').style.display = 'inline'; document.getElementById('2204.02420v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.02420v1-abstract-full" style="display: none;"> We present FORS2@VLT follow-up photometry of YMCA-1, a recently discovered stellar system located 13\degr~from the Large Magellanic Cloud (LMC) center. The deep color-magnitude diagram (CMD) reveals a well-defined main sequence (MS) and a handful of stars in the post-MS evolutionary phases. We analyse the YMCA-1 CMD by means of the automated isochrone matching package {\tt ASteCA} and model its radial density profile with a Plummer function. We find that YMCA-1 is an old ($11.7^{+1.7}_{-1.3}$~Gyr), metal-intermediate ([Fe/H] $\simeq -1.12^{+0.21}_{-0.13}$~dex), compact (r$_{\rm h} = 3.5 \pm 0.5$ pc), low-mass (M $= 10^{2.45 \pm 0.02} M_{\odot}$) and low-luminosity (M$_V = -0.47 \pm 0.57$~mag) stellar system. The estimated distance modulus ($渭_0 = 18.72^{+0.15}_{-0.17}$~mag), corresponding to about 55~kpc, suggests that YMCA-1 is associated to the LMC, but we cannot discard the scenario in which it is a Milky Way satellite. The structural parameters of YMCA-1 are remarkably different compared with those of the 15 known old LMC globular clusters. In particular, it resides in a transition region of the M$_V$-r$_h$ plane, in between the ultra-faint dwarf galaxies and the classical old clusters, and close to SMASH-1, another faint stellar system recently discovered in the LMC surroundings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.02420v1-abstract-full').style.display = 'none'; document.getElementById('2204.02420v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures, Accepted for publication in The Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07675">arXiv:2203.07675</a> <span> [<a href="https://arxiv.org/pdf/2203.07675">pdf</a>, <a href="https://arxiv.org/format/2203.07675">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/stac1003">10.1093/mnras/stac1003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Preparing for low surface brightness science with the Vera C. Rubin Observatory: characterisation of tidal features from mock images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martin%2C+G">G. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Bazkiaei%2C+A+E">A. E. Bazkiaei</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. C. Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+M">M. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Benavides%2C+J+A">J. A. Benavides</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">S. Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Carlin%2C+J+L">J. L. Carlin</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+C+A">C. A. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+A">P. A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+F+A">F. A. G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Galaz%2C+G">G. Galaz</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez-Toledo%2C+H+M">H. M. Hern谩ndez-Toledo</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+A">R. A. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Kaviraj%2C+S">S. Kaviraj</a>, <a href="/search/astro-ph?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez-Lombilla%2C+C">C. Mart铆nez-Lombilla</a>, <a href="/search/astro-ph?searchtype=author&query=McGee%2C+S">S. McGee</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Ryan%2C+D">D. O'Ryan</a>, <a href="/search/astro-ph?searchtype=author&query=Prole%2C+D+J">D. J. Prole</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. M. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n%2C+J">J. Rom谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+E+A">E. A. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+T+K">T. K. Starkenburg</a> , et al. (28 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="2203.07675v2-abstract-short" style="display: inline;"> Tidal features in the outskirts of galaxies yield unique information about their past interactions and are a key prediction of the hierarchical structure formation paradigm. The Vera C. Rubin Observatory is poised to deliver deep observations for potentially of millions of objects with visible tidal features, but the inference of galaxy interaction histories from such features is not straightforwa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07675v2-abstract-full').style.display = 'inline'; document.getElementById('2203.07675v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07675v2-abstract-full" style="display: none;"> Tidal features in the outskirts of galaxies yield unique information about their past interactions and are a key prediction of the hierarchical structure formation paradigm. The Vera C. Rubin Observatory is poised to deliver deep observations for potentially of millions of objects with visible tidal features, but the inference of galaxy interaction histories from such features is not straightforward. Utilising automated techniques and human visual classification in conjunction with realistic mock images produced using the NEWHORIZON cosmological simulation, we investigate the nature, frequency and visibility of tidal features and debris across a range of environments and stellar masses. In our simulated sample, around 80 per cent of the flux in the tidal features around Milky Way or greater mass galaxies is detected at the 10-year depth of the Legacy Survey of Space and Time (30-31 mag / sq. arcsec), falling to 60 per cent assuming a shallower final depth of 29.5 mag / sq. arcsec. The fraction of total flux found in tidal features increases towards higher masses, rising to 10 per cent for the most massive objects in our sample (M*~10^{11.5} Msun). When observed at sufficient depth, such objects frequently exhibit many distinct tidal features with complex shapes. The interpretation and characterisation of such features varies significantly with image depth and object orientation, introducing significant biases in their classification. Assuming the data reduction pipeline is properly optimised, we expect the Rubin Observatory to be capable of recovering much of the flux found in the outskirts of Milky Way mass galaxies, even at intermediate redshifts (z<0.2). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07675v2-abstract-full').style.display = 'none'; document.getElementById('2203.07675v2-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 25 figures; accepted for publication in MNRAS following minor corrections</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, Volume 513, Issue 1, June 2022, Pages 1459-1487, </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.08193">arXiv:2202.08193</a> <span> [<a href="https://arxiv.org/pdf/2202.08193">pdf</a>, <a href="https://arxiv.org/format/2202.08193">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 intra-group baryons in the LEO I pair from the VST Early-type GAlaxy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</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="2202.08193v1-abstract-short" style="display: inline;"> In this paper we present the deep, wide-field and multi-band imaging of the LEO I pair NGC~3379-NGC~3384, from the VST Early-type GAlaxy Survey (VEGAS). The main goal of this study is to map the intra-group baryons in the pair, in the form of diffuse light and globular clusters (GCs). Taking advantage from the large covered area, which extends for $\sim$ 3.9 square degrees around the pair, and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08193v1-abstract-full').style.display = 'inline'; document.getElementById('2202.08193v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.08193v1-abstract-full" style="display: none;"> In this paper we present the deep, wide-field and multi-band imaging of the LEO I pair NGC~3379-NGC~3384, from the VST Early-type GAlaxy Survey (VEGAS). The main goal of this study is to map the intra-group baryons in the pair, in the form of diffuse light and globular clusters (GCs). Taking advantage from the large covered area, which extends for $\sim$ 3.9 square degrees around the pair, and the long integration time, we can map the light distribution out to $\sim$ 63 kpc and down to $\sim$ 30 mag/arcsec$^2$ in the $g$ band and $\sim$ 29 mag/arcsec$^2$ in the $r$ band, deeper than previous data available for this target. The map of the intra-group light (IGL) presents two very faint ($渭_g \sim$ 28-29 mag/arcsec$^2$) streams protruding from the brightest group member NGC~3379 and elongated toward North-West and South. We estimate that the fraction of the stellar halo around NGC~3379 plus the IGL is $\sim 17 \pm 2\%$ in both $g$ and $r$ bands, with an average color $g$-$r$= $0.75 \pm 0.04$~mag. The color distribution of the GCs appears multi-modal, with two dominant peaks at (u-r) = 1.8 mag and (u-r) = 2.1 mag, respectively. The GC population stretches from North-East to South-West and from North-West to South of the pair, in the last case overlapping with the streams of IGL, as well as the PNe distribution found by \citet{Hartke2020} and \citet{Hartke2022arXiv220108710H}. Since these structures are elongated in the direction of the two nearby galaxies M96 and NGC~3338, they could be the remnant of a past gravitational interactions with the pair. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08193v1-abstract-full').style.display = 'none'; document.getElementById('2202.08193v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">30 pages 9 figures 6 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/2112.00711">arXiv:2112.00711</a> <span> [<a href="https://arxiv.org/pdf/2112.00711">pdf</a>, <a href="https://arxiv.org/format/2112.00711">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/10.1051/0004-6361/202141901">10.1051/0004-6361/202141901 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy populations in the Hydra I cluster from the VEGAS survey I. Optical properties of a large sample of dwarf galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">Reynier Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Challapa%2C+N+C">Nelvy Choque Challapa</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">Aku Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">Maria Angela Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">Roberto Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">Chiara Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</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="2112.00711v2-abstract-short" style="display: inline;"> At ~50 Mpc, the Hydra I cluster of galaxies is among the closest cluster in the z=0 Universe, and an ideal environment to study dwarf galaxy properties in a cluster environment. We exploit deep imaging data of the Hydra I cluster to construct a new photometric catalog of dwarf galaxies in the cluster core, which is then used to derive properties of the Hydra I cluster dwarf galaxies population as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.00711v2-abstract-full').style.display = 'inline'; document.getElementById('2112.00711v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.00711v2-abstract-full" style="display: none;"> At ~50 Mpc, the Hydra I cluster of galaxies is among the closest cluster in the z=0 Universe, and an ideal environment to study dwarf galaxy properties in a cluster environment. We exploit deep imaging data of the Hydra I cluster to construct a new photometric catalog of dwarf galaxies in the cluster core, which is then used to derive properties of the Hydra I cluster dwarf galaxies population as well as to compare with other clusters. Moreover, we investigate the dependency of dwarf galaxy properties on their surrounding environment. The new Hydra I dwarf catalog contains 317 galaxies with luminosity between -18.5<$M_r$<-11.5 mag, a semi-major axis larger than ~200 pc (a=0.84 arcsec), of which 202 are new detections, previously unknown dwarf galaxies in the Hydra I central region. We estimate that our detection efficiency reaches 50% at the limiting magnitude $M_r$=-11.5 mag, and at the mean effective surface brightness $\overline渭_{e,r}$=26.5 mag/$arcsec^2$. We present the standard scaling relations for dwarf galaxies and compare them with other nearby clusters. We find that there are no observational differences for dwarfs scaling relations in clusters of different sizes. We study the spatial distribution of galaxies, finding evidence for the presence of substructures within half the virial radius. We also find that mid- and high-luminosity dwarfs ($M_r$<-14.5 mag) become on average redder toward the cluster center, and that they have a mild increase in $R_e$ with increasing clustercentric distance, similar to what is observed for the Fornax cluster. No clear clustercentric trends are reported with surface brightness and S茅rsic index. Considering galaxies in the same magnitude-bins, we find that for high and mid-luminosity dwarfs ($M_r$<-13.5 mag) the g-r color is redder for the brighter surface brightness and higher S茅rsic n index objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.00711v2-abstract-full').style.display = 'none'; document.getElementById('2112.00711v2-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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 A&A. 25 pages, 21 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A92 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.01855">arXiv:2111.01855</a> <span> [<a href="https://arxiv.org/pdf/2111.01855">pdf</a>, <a href="https://arxiv.org/format/2111.01855">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 Fornax Deep Survey (FDS) with VST XII: Low surface brightness dwarf galaxies in the Fornax cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">Aku Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R+F">Reynier F. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Salo%2C+H">Heikki Salo</a>, <a href="/search/astro-ph?searchtype=author&query=Laurikainen%2C+E">Eija Laurikainen</a>, <a href="/search/astro-ph?searchtype=author&query=Janz%2C+J">Joachim Janz</a>, <a href="/search/astro-ph?searchtype=author&query=Haigh%2C+C">Caroline Haigh</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkinson%2C+M+H+F">Michael H. F. Wilkinson</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</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="2111.01855v1-abstract-short" style="display: inline;"> In this work we use Max-Tree Objects, (MTO) on the FDS data in order to detect previously undetected Low surface brightness (LSB) galaxies. After extending the existing Fornax dwarf galaxy catalogs with this sample, our goal is to understand the evolution of LSB dwarfs in the cluster. We also study the contribution of the newly detected galaxies to the faint end of the luminosity function. We test… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.01855v1-abstract-full').style.display = 'inline'; document.getElementById('2111.01855v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.01855v1-abstract-full" style="display: none;"> In this work we use Max-Tree Objects, (MTO) on the FDS data in order to detect previously undetected Low surface brightness (LSB) galaxies. After extending the existing Fornax dwarf galaxy catalogs with this sample, our goal is to understand the evolution of LSB dwarfs in the cluster. We also study the contribution of the newly detected galaxies to the faint end of the luminosity function. We test the detection completeness and parameter extraction accuracy of MTO. We then apply MTO to the FDS images to identify LSB candidates. The identified objects are fitted with 2D S茅rsic models using GALFIT and classified based on their morphological appearance, colors, and structure. With MTO, we are able to increase the completeness of our earlier FDS dwarf catalog (FDSDC) 0.5-1 mag deeper in terms of total magnitude and surface brightness. Due to the increased accuracy in measuring sizes of the detected objects, we also add many small galaxies to the catalog that were previously excluded as their outer parts had been missed in detection. We detect 265 new LSB dwarf galaxies in the Fornax cluster, which increases the total number of known dwarfs in Fornax to 821. Using the extended catalog, we show that the luminosity function has a faint-end slope of -1.38+/-0.02. We compare the obtained luminosity function with different environments studied earlier using deep data but do not find any significant differences. On the other hand, the Fornax-like simulated clusters in the IllustrisTNG cosmological simulation have shallower slopes than found in the observational data. We also find several trends in the galaxy colors, structure, and morphology that support the idea that the number of LSB galaxies is higher in the cluster center due to tidal forces and the age dimming of the stellar populations. The same result also holds for the subgroup of large LSB galaxies, so-called ultra-diffuse galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.01855v1-abstract-full').style.display = 'none'; document.getElementById('2111.01855v1-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics. 29 pages, 27 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/2109.08695">arXiv:2109.08695</a> <span> [<a href="https://arxiv.org/pdf/2109.08695">pdf</a>, <a href="https://arxiv.org/format/2109.08695">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/10.1051/0004-6361/202141872">10.1051/0004-6361/202141872 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fornax Cluster VLT Spectroscopic Survey IV -- Cold kinematical substructures in the Fornax core from COSTA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Gatto%2C+M">M. Gatto</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">M. Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Chaturvedi%2C+A">A. Chaturvedi</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Abrusco%2C+R">R. D'Abrusco</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+R">R. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">M. Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">R. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">A. Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Pota%2C+V">V. Pota</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">M. Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Longo%2C+G">G. Longo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.08695v3-abstract-short" style="display: inline;"> The COld STream finder Algorithm (COSTA) is a novel algorithm to find streams in the phase space of planetary nebulae (PNe) and globular cluster (GCs) populations. COSTA isolates groups of particles with small velocity dispersion, using an iterative sigma-clipping over a defined number of neighbor particles. We have applied COSTA to a catalog of about 2000 PNe and GCs from the Fornax Cluster VLT S… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08695v3-abstract-full').style.display = 'inline'; document.getElementById('2109.08695v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.08695v3-abstract-full" style="display: none;"> The COld STream finder Algorithm (COSTA) is a novel algorithm to find streams in the phase space of planetary nebulae (PNe) and globular cluster (GCs) populations. COSTA isolates groups of particles with small velocity dispersion, using an iterative sigma-clipping over a defined number of neighbor particles. We have applied COSTA to a catalog of about 2000 PNe and GCs from the Fornax Cluster VLT Spectroscopic Survey (FVSS), within 200 kpc from the cluster core, to detect cold substructures and characterize their kinematics. We have found 13 cold substructures, with velocity dispersion ranging from 20 to 100 kms^{-1}, which are likely associated either to large galaxies or to ultra-compact dwarf (UCD) galaxies in the Fornax core. These streams show a clear correlation of their luminosity with the internal velocity dispersion, and their surface brightness with size and distance from the cluster center that are compatible with dissipative processes producing them. However, we cannot exclude that some of these substructures have formed by violent relaxation of massive satellites finally merged into the central galaxy. Among these substructures we have: a stream connecting NGC1387 to the central galaxy, NGC1399, previously reported in literature; a new giant stream produced by the interaction of NGC1382 with NGC1380 and possibly NGC1381; a series of streams kinematically connected to nearby ultra compact dwarf galaxies; clumps of tracers with no clear kinematical association to close cluster members. We show evidence for a variety of cold substructure predicted in simulations. Most of the streams are kinematically connected to UCDs, supporting the scenario that they can be remnants of disrupted dwarf systems. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08695v3-abstract-full').style.display = 'none'; document.getElementById('2109.08695v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 Pages, 15 Figures. Accepted for publication in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.10312">arXiv:2107.10312</a> <span> [<a href="https://arxiv.org/pdf/2107.10312">pdf</a>, <a href="https://arxiv.org/format/2107.10312">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/10.3847/2515-5172/ac14bf">10.3847/2515-5172/ac14bf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> YMCA-1: a new remote star cluster of the Milky Way? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gatto%2C+M">M. Gatto</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">M. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Tosi%2C+M">M. Tosi</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Cignoni%2C+M">M. Cignoni</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Dall%27ora%2C+M">M. Dall'ora</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Longo%2C+G">G. Longo</a>, <a href="/search/astro-ph?searchtype=author&query=Musella%2C+I">I. Musella</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">M. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">P. Schipani</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="2107.10312v1-abstract-short" style="display: inline;"> We report the possible discovery of a new stellar system (YMCA-1), identified during a search for small scale overdensities in the photometric data of the YMCA survey. The object's projected position lies on the periphery of the Large Magellanic Cloud about $13^\circ$ apart from its center. The most likely interpretation of its color-magnitude diagram, as well as of its integrated properties, is t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10312v1-abstract-full').style.display = 'inline'; document.getElementById('2107.10312v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10312v1-abstract-full" style="display: none;"> We report the possible discovery of a new stellar system (YMCA-1), identified during a search for small scale overdensities in the photometric data of the YMCA survey. The object's projected position lies on the periphery of the Large Magellanic Cloud about $13^\circ$ apart from its center. The most likely interpretation of its color-magnitude diagram, as well as of its integrated properties, is that YMCA-1 may be an old and remote star cluster of the Milky Way at a distance of 100 kpc from the Galactic center. If this scenario could be confirmed, then the cluster would be significantly fainter and more compact than most of the known star clusters residing in the extreme outskirts of the Galactic halo, but quite similar to Laevens~3. However, much deeper photometry is needed to firmly establish the actual nature of the cluster and the distance to the system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10312v1-abstract-full').style.display = 'none'; document.getElementById('2107.10312v1-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, 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">5 Pages, 3 figures. Published on Research Notes of the AAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Res. Notes AAS 5 159 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.04486">arXiv:2107.04486</a> <span> [<a href="https://arxiv.org/pdf/2107.04486">pdf</a>, <a href="https://arxiv.org/format/2107.04486">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/10.1051/0004-6361/202141086">10.1051/0004-6361/202141086 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Formation of an ultra-diffuse galaxy in the stellar filaments of NGC3314A: caught in act? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Gullieuszik%2C+M">Marco Gullieuszik</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">Chiara Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Greggio%2C+L">Laura Greggio</a>, <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">Roberto Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</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="2107.04486v1-abstract-short" style="display: inline;"> The VEGAS imaging survey of the Hydra I cluster reveals an extended network of stellar filaments to the south-west of the spiral galaxy NGC3314A. Within these filaments, at a projected distance of ~40 kpc from the galaxy, we discover an ultra-diffuse galaxy (UDG) with a central surface brightness of $渭_{0,g}\sim26$ mag arcsec$^{-2}$ and effective radius $R_e\sim3.8$ kpc. This UDG, named UDG32, is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.04486v1-abstract-full').style.display = 'inline'; document.getElementById('2107.04486v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.04486v1-abstract-full" style="display: none;"> The VEGAS imaging survey of the Hydra I cluster reveals an extended network of stellar filaments to the south-west of the spiral galaxy NGC3314A. Within these filaments, at a projected distance of ~40 kpc from the galaxy, we discover an ultra-diffuse galaxy (UDG) with a central surface brightness of $渭_{0,g}\sim26$ mag arcsec$^{-2}$ and effective radius $R_e\sim3.8$ kpc. This UDG, named UDG32, is one of the faintest and most diffuse low-surface brightness galaxies in the Hydra~I cluster. Based on the available data, we cannot exclude that this object is just seen in projection on top of the stellar filaments, thus being instead a foreground or background UDG in the cluster. However, the clear spatial coincidence of UDG32 with the stellar filaments of NGC3314A suggests that it might have formed from the material in the filaments, becoming a detached, gravitationally bound system. In this scenario, the origin of UDG32 depends on the nature of the stellar filaments in NGC3314A, which is still unknown. They could result from ram-pressure stripping or have a tidal origin. In this letter, we focus on the comparison of the observed properties of the stellar filaments and UDG32, and speculate about their possible origin. The relatively red color ($g-r=0.54 \pm 0.14$~mag) of the UDG, similar to that of the disk in NGC3314A, combined with an age older than 1Gyr, and the possible presence of a few compact stellar systems, all point towards a tidal formation scenario inferred for the UDG32. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.04486v1-abstract-full').style.display = 'none'; document.getElementById('2107.04486v1-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 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 Astronomy & Astrophysics Letter</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 652, L11 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.06448">arXiv:2106.06448</a> <span> [<a href="https://arxiv.org/pdf/2106.06448">pdf</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/10.18727/0722-6691/5232">10.18727/0722-6691/5232 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VST Early-type GAlaxy Survey: Exploring the Outskirts and Intra-cluster Regions of Galaxies in the Low-surface-brightness Regime </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">Massimo Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=De+Cicco%2C+D">Demetra De Cicco</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Greggio%2C+L">Laura Greggio</a>, <a href="/search/astro-ph?searchtype=author&query=Krajnovic%2C+D">Davor Krajnovic</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">Nicola R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">Maria Angela Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">Roberto Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</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="2106.06448v1-abstract-short" style="display: inline;"> The VST Early-type GAlaxy Survey (VEGAS) is a deep, multi-band (u, g, r, i) imaging survey, carried out with the 2.6-metre VLT Survey Telescope (VST) at ESO's Paranal Observatory in Chile. VEGAS combines the wide (1-square-degree) OmegaCAM imager and long integration times, together with a specially designed observing strategy. It has proven to be a gold mine for studies of features at very low su… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.06448v1-abstract-full').style.display = 'inline'; document.getElementById('2106.06448v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.06448v1-abstract-full" style="display: none;"> The VST Early-type GAlaxy Survey (VEGAS) is a deep, multi-band (u, g, r, i) imaging survey, carried out with the 2.6-metre VLT Survey Telescope (VST) at ESO's Paranal Observatory in Chile. VEGAS combines the wide (1-square-degree) OmegaCAM imager and long integration times, together with a specially designed observing strategy. It has proven to be a gold mine for studies of features at very low surface brightness, down to levels of mu_g~27-30 magnitudes arcsec^(-2), over 5-8 magnitudes fainter than the dark sky at Paranal. In this article we highlight the main science results obtained with VEGAS observations of galaxies across different environments, from dense clusters of galaxies to unexplored poor groups and in the field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.06448v1-abstract-full').style.display = 'none'; document.getElementById('2106.06448v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Published in The Messenger, vol. 183, p. 25-29</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.06970">arXiv:2105.06970</a> <span> [<a href="https://arxiv.org/pdf/2105.06970">pdf</a>, <a href="https://arxiv.org/format/2105.06970">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/10.1051/0004-6361/202039921">10.1051/0004-6361/202039921 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VEGAS: A VST Early-type GAlaxy Survey.VI. The diffuse light in HCG 86 from the ultra-deep VEGAS images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">Maria Angela Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Ago%2C+G+D">Giuseppe D Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">Roberto Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</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="2105.06970v1-abstract-short" style="display: inline;"> Context. In this paper we present ultra deep images of the compact group of galaxies HCG 86 as part of the VEGAS survey. Aims. Our main goals are to estimate the amount of intragroup light (IGL), to study the light and color distributions in order to address the main formation process of the IGL component in groups of galaxies. Methods. We derived the azimuthally averaged surface brightness profil… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06970v1-abstract-full').style.display = 'inline'; document.getElementById('2105.06970v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.06970v1-abstract-full" style="display: none;"> Context. In this paper we present ultra deep images of the compact group of galaxies HCG 86 as part of the VEGAS survey. Aims. Our main goals are to estimate the amount of intragroup light (IGL), to study the light and color distributions in order to address the main formation process of the IGL component in groups of galaxies. Methods. We derived the azimuthally averaged surface brightness profiles in the g,r and i bands with g - r and r - i average colors and color profiles for all group members. By fitting the light distribution, we have extrapolated the contribution of the stellar halos plus the diffuse light from the brightest component of each galaxy. The results are compared with theoretical predictions. Results. The long integration time and wide area covered make our data deeper than previous literature studies of the IGL in compact groups of galaxies and allow us to produce an extended (~160 kpc) map of the IGL, down to a surface brightness level of about 30 mag/arcsec^2 in the g band. The IGL in HCG 86 is mainly in diffuse form and has average colors of g - r ~ 0.8 mag and r - i ~ 0.4 mag. The fraction of IGL in HCG 86 is ~ 16% of the total luminosity of the group, and this is consistent with estimates available for other compact groups and loose groups of galaxies of similar virial masses. A weak trend is present between the amount of IGL and the early-type to late-type galaxy ratio. Conclusions. By comparing the IGL fraction and colors with those predicted by simulations, the amount of IGL in HCG 86 would be the result of the disruption of satellites at an epoch of z ~ 0.4. At this redshift, observed colors are consistent with the scenario where the main contribution to the mass of the IGL comes from the intermediate-massive galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06970v1-abstract-full').style.display = 'none'; document.getElementById('2105.06970v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 651, A39 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.13417">arXiv:2103.13417</a> <span> [<a href="https://arxiv.org/pdf/2103.13417">pdf</a>, <a href="https://arxiv.org/format/2103.13417">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/10.3847/2515-5172/abf050">10.3847/2515-5172/abf050 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photometric Redshifts in the W-CDF-S and ELAIS-S1 Fields Based on Forced Photometry from 0.36 -- 4.5 Microns </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zou%2C+F">Fan Zou</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Ni%2C+Q">Qingling Ni</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Covone%2C+G">Giovanni Covone</a>, <a href="/search/astro-ph?searchtype=author&query=Lacy%2C+M">Mark Lacy</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">Nicola R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Nyland%2C+K">Kristina Nyland</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">Mario Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Vaccari%2C+M">Mattia Vaccari</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="2103.13417v1-abstract-short" style="display: inline;"> The W-CDF-S and ELAIS-S1 fields will be two of the LSST Deep Drilling fields, but the availability of spectroscopic redshifts within these two fields is still limited on deg^2 scales. To prepare for future science, we use EAZY to estimate photometric redshifts (photo-zs) in these two fields based on forced-photometry catalogs. Our photo-z catalog consists of ~0.8 million sources covering 4.9 deg^2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.13417v1-abstract-full').style.display = 'inline'; document.getElementById('2103.13417v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.13417v1-abstract-full" style="display: none;"> The W-CDF-S and ELAIS-S1 fields will be two of the LSST Deep Drilling fields, but the availability of spectroscopic redshifts within these two fields is still limited on deg^2 scales. To prepare for future science, we use EAZY to estimate photometric redshifts (photo-zs) in these two fields based on forced-photometry catalogs. Our photo-z catalog consists of ~0.8 million sources covering 4.9 deg^2 in W-CDF-S and ~0.8 million sources covering 3.4 deg^2 in ELAIS-S1, among which there are ~0.6 (W-CDF-S) and ~0.4 (ELAIS-S1) million sources having signal-to-noise-ratio (SNR) > 5 detections in more than 5 bands. By comparing photo-zs and available spectroscopic redshifts, we demonstrate the general reliability of our photo-z measurements. Our photo-z catalog is publicly available at \doi{10.5281/zenodo.4603178}. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.13417v1-abstract-full').style.display = 'none'; document.getElementById('2103.13417v1-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">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> Res. Notes AAS 5 56 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.12086">arXiv:2103.12086</a> <span> [<a href="https://arxiv.org/pdf/2103.12086">pdf</a>, <a href="https://arxiv.org/format/2103.12086">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140856">10.1051/0004-6361/202140856 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> INSPIRE: INvestigating Stellar Population In RElics II. First Data Release (DR1) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Pulsoni%2C+C">C. Pulsoni</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L">L. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</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="2103.12086v2-abstract-short" style="display: inline;"> The INvestigating Stellar Population In RElics is an on-going project targeting 52 ultra-compact massive galaxies at 0.1<z<0.5 with the X-Shooter@VLT spectrograph (XSH). These objects are the perfect candidates to be 'relics', massive red-nuggets formed at high-z (z>2) through a short and intense star formation burst, that evolved passively and undisturbed until the present-day. Relics provide a u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12086v2-abstract-full').style.display = 'inline'; document.getElementById('2103.12086v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.12086v2-abstract-full" style="display: none;"> The INvestigating Stellar Population In RElics is an on-going project targeting 52 ultra-compact massive galaxies at 0.1<z<0.5 with the X-Shooter@VLT spectrograph (XSH). These objects are the perfect candidates to be 'relics', massive red-nuggets formed at high-z (z>2) through a short and intense star formation burst, that evolved passively and undisturbed until the present-day. Relics provide a unique opportunity to study the mechanisms of star formation at high-z. In this paper, we present the first INSPIRE Data Release, comprising 19 systems with observations completed in 2020. We use the methods already presented in the INSPIRE Pilot, but revisiting the 1D spectral extraction. For these 19 systems, we obtain an estimate of the stellar velocity dispersion, fitting separately the two UVB and VIS XSH arms at their original resolution. We estimate [Mg/Fe] abundances via line-index strength and mass-weighted integrated stellar ages and metallicities with full spectral fitting on the combined spectrum. Ages are generally old, in agreement with the photometric ones, and metallicities are almost always super-solar, confirming the mass-metallicity relation. The [Mg/Fe] ratio is also larger than solar for the great majority of the galaxies, as expected. We find that 10 objects have formed more than 75% of their stellar mass (M*) within 3 Gyr from the Big Bang and classify them as relics. Among these, we identify 4 galaxies which had already fully assembled their M* by that time. They are therefore `extreme relics' of the ancient Universe. The INSPIRE DR1 catalogue of 10 known relics to-date augment by a factor of 3.3 the total number of confirmed relics, also enlarging the redshift window. It is therefore the largest publicly available collection. Thanks to the larger number of systems, we can also better quantify the existence of a 'degree of relicness', already hinted at the Pilot Paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12086v2-abstract-full').style.display = 'none'; document.getElementById('2103.12086v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">(Abstract abridged) 21 pages, 12 figures and 5 tables in the main body, plus 3 figure and 1 table in the appendix, accepted for publication on A&A. The associated data are available via the ESO Phase 3 Science Portal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, A136 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.11219">arXiv:2103.11219</a> <span> [<a href="https://arxiv.org/pdf/2103.11219">pdf</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/10.18727/0722-6691/5216">10.18727/0722-6691/5216 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MAORY: A Multi-conjugate Adaptive Optics RelaY for ELT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ciliegi%2C+P">Paolo Ciliegi</a>, <a href="/search/astro-ph?searchtype=author&query=Agapito%2C+G">Guido Agapito</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">Matteo Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">Francesca Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Arcidiacono%2C+C">Carmelo Arcidiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+A">Andrea Balestra</a>, <a href="/search/astro-ph?searchtype=author&query=Baruffolo%2C+A">Andrea Baruffolo</a>, <a href="/search/astro-ph?searchtype=author&query=Bergomi%2C+M">Maria Bergomi</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+A">Andrea Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Bonaglia%2C+M">Marco Bonaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Busoni%2C+L">Lorenzo Busoni</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Cascone%2C+E">Enrico Cascone</a>, <a href="/search/astro-ph?searchtype=author&query=Chauvin%2C+G">Gael Chauvin</a>, <a href="/search/astro-ph?searchtype=author&query=Chinellato%2C+S">Simonetta Chinellato</a>, <a href="/search/astro-ph?searchtype=author&query=Cianniello%2C+V">Vincenzo Cianniello</a>, <a href="/search/astro-ph?searchtype=author&query=Correira%2C+J+J">Jean Jacques Correira</a>, <a href="/search/astro-ph?searchtype=author&query=Cosentino%2C+G">Giuseppe Cosentino</a>, <a href="/search/astro-ph?searchtype=author&query=Dall%27Ora%2C+M">Massimo Dall'Ora</a>, <a href="/search/astro-ph?searchtype=author&query=De+Caprio%2C+V">Vincenzo De Caprio</a>, <a href="/search/astro-ph?searchtype=author&query=Devaney%2C+N">Nicholas Devaney</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Antonio%2C+I">Ivan Di Antonio</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Cianno%2C+A">Amico Di Cianno</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Giammatteo%2C+U">Ugo Di Giammatteo</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">Valentina D'Orazi</a> , et al. (51 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="2103.11219v1-abstract-short" style="display: inline;"> MAORY is the adaptive optics module for ELT providing two gravity invariant ports with the same optical quality for two different client instruments. It enable high angular resolution observations in the near infrared over a large field of view (~1 arcmin2 ) by real time compensation of the wavefront distortions due to atmospheric turbulence. Wavefront sensing is performed by laser and natural gui… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.11219v1-abstract-full').style.display = 'inline'; document.getElementById('2103.11219v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.11219v1-abstract-full" style="display: none;"> MAORY is the adaptive optics module for ELT providing two gravity invariant ports with the same optical quality for two different client instruments. It enable high angular resolution observations in the near infrared over a large field of view (~1 arcmin2 ) by real time compensation of the wavefront distortions due to atmospheric turbulence. Wavefront sensing is performed by laser and natural guide stars while the wavefront sensor compensation is performed by an adaptive deformable mirror in MAORY which works together with the telescope's adaptive and tip tilt mirrors M4 and M5 respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.11219v1-abstract-full').style.display = 'none'; document.getElementById('2103.11219v1-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">4 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Messenger 182 (March 2021): 13-16 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.07478">arXiv:2103.07478</a> <span> [<a href="https://arxiv.org/pdf/2103.07478">pdf</a>, <a href="https://arxiv.org/format/2103.07478">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/10.1051/0004-6361/202040186">10.1051/0004-6361/202040186 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the assembly history of massive galaxies. A pilot project with VEGAS deep imaging and M3G integral field spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Krajnovi%C4%87%2C+D">Davor Krajnovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+M+d">Mark den Brok</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="2103.07478v1-abstract-short" style="display: inline;"> In this paper we present the new deep images from the VEGAS survey of three massive ($M_{*} \simeq 10^{12}$~M$_\odot$) galaxies from the MUSE Most Massive Galaxies (M3G) project, with distances in the range $151\leq D \leq 183$ Mpc: PGC007748, PGC015524 and PGC049940. The long integration time and the wide field of view of OmegaCam@VST allowed us to map the light and color distributions down to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.07478v1-abstract-full').style.display = 'inline'; document.getElementById('2103.07478v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.07478v1-abstract-full" style="display: none;"> In this paper we present the new deep images from the VEGAS survey of three massive ($M_{*} \simeq 10^{12}$~M$_\odot$) galaxies from the MUSE Most Massive Galaxies (M3G) project, with distances in the range $151\leq D \leq 183$ Mpc: PGC007748, PGC015524 and PGC049940. The long integration time and the wide field of view of OmegaCam@VST allowed us to map the light and color distributions down to $渭_g\simeq30$~mag/arcsec$^2$ and out to $\sim 2R_e$. The deep data are crucial to estimate the contribution of the different galaxy's components, in particular the accreted fraction in the stellar halo. The available integral-field observations with MUSE cover a limited portion of each galaxy (out to $\sim 1R_e$), but, from the imaging analysis we find that they map the kinematics and stellar population beyond the first transition radius, where the contribution of the accreted component starts to dominate. The main goal of this work is to correlate the scales of the different components derived from the image analysis with the kinematics and stellar population profiles from the MUSE data. Results were used to address the assembly history of the three galaxies with the help of the theoretical predictions. Our results suggest that PGC049940 has the lowest accreted mass fraction of 77%. The higher accreted mass fraction estimated for PGC007748 and PGC015524 (86% and 89%, respectively), combined with the flat $位_R$ profiles suggest that a great majority of the mass has been acquired through major mergers, which have also shaped the shallower metallicity profiles observed at larger radii. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.07478v1-abstract-full').style.display = 'none'; document.getElementById('2103.07478v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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 A&A. 12 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A161 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.11892">arXiv:2102.11892</a> <span> [<a href="https://arxiv.org/pdf/2102.11892">pdf</a>, <a href="https://arxiv.org/format/2102.11892">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/10.3847/2515-5172/abe769">10.3847/2515-5172/abe769 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Multi-Band Forced-Photometry Catalog in the ELAIS-S1 Field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zou%2C+F">Fan Zou</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Lacy%2C+M">Mark Lacy</a>, <a href="/search/astro-ph?searchtype=author&query=Ni%2C+Q">Qingling Ni</a>, <a href="/search/astro-ph?searchtype=author&query=Nyland%2C+K">Kristina Nyland</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Covone%2C+G">Giovanni Covone</a>, <a href="/search/astro-ph?searchtype=author&query=Grado%2C+A">Aniello Grado</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">Nicola R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">Mario Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Vaccari%2C+M">Mattia Vaccari</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="2102.11892v1-abstract-short" style="display: inline;"> The ELAIS-S1 field will be an LSST Deep Drilling field, and it also has extensive multiwavelength coverage. To improve the utility of the existing data, we use The Tractor to perform forced-photometry measurements in this field. We compile data in 16 bands from the DeepDrill, VIDEO, DES, ESIS, and VOICE surveys. Using a priori information from the high-resolution fiducial images in VIDEO, we model… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11892v1-abstract-full').style.display = 'inline'; document.getElementById('2102.11892v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.11892v1-abstract-full" style="display: none;"> The ELAIS-S1 field will be an LSST Deep Drilling field, and it also has extensive multiwavelength coverage. To improve the utility of the existing data, we use The Tractor to perform forced-photometry measurements in this field. We compile data in 16 bands from the DeepDrill, VIDEO, DES, ESIS, and VOICE surveys. Using a priori information from the high-resolution fiducial images in VIDEO, we model the images in other bands and generate a forced-photometry catalog. This technique enables consistency throughout different surveys, deblends sources from low-resolution images, extends photometric measurements to a fainter magnitude regime, and improves photometric-redshift estimates. Our catalog contains over 0.8 million sources covering a 3.4 deg2 area in the VIDEO footprint and is available at 10.5281/zenodo.4540178. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11892v1-abstract-full').style.display = 'none'; document.getElementById('2102.11892v1-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, 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">8 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Res. Notes AAS 5 31 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.04950">arXiv:2102.04950</a> <span> [<a href="https://arxiv.org/pdf/2102.04950">pdf</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> <p class="title is-5 mathjax"> The VST Early-type GAlaxy Survey (VEGAS) data release 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">M. A. Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">M. Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=team%2C+V+s">VEGAS science team</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="2102.04950v1-abstract-short" style="display: inline;"> We present the first data release (DR1) of the VST Early-type GAlaxy Survey (VEGAS). This is a deep multi-band (u'g'r'i') imaging survey, carried out with the ESO VLT Survey Telescope (VST). To date, using about 90% of the total observing time, VEGAS has already collected 43 targets (groups and clusters of galaxies) covering a total area on the sky of about 95 square degrees. Taking advantage of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.04950v1-abstract-full').style.display = 'inline'; document.getElementById('2102.04950v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.04950v1-abstract-full" style="display: none;"> We present the first data release (DR1) of the VST Early-type GAlaxy Survey (VEGAS). This is a deep multi-band (u'g'r'i') imaging survey, carried out with the ESO VLT Survey Telescope (VST). To date, using about 90% of the total observing time, VEGAS has already collected 43 targets (groups and clusters of galaxies) covering a total area on the sky of about 95 square degrees. Taking advantage of the wide (1 deg^2) field-of-view of OmegaCAM@VST, the long integration time and the wide variety of targets, VEGAS has proven to be a gold mine to explore the structure of galaxies down to the faintest surface brightness levels of about 27-30 mag/arcsec^2 in the SDSS g' band, for the dense clusters of galaxies and for the unexplored poor groups of galaxies. Based on the analysed data, VEGAS allowed us to i) study the galaxy outskirts, detect the intra-cluster light and low-surface brightness features in the intra-cluster/group space, ii) trace the mass assembly in galaxies, by estimating the accreted mass fraction in the stellar halos and provide results that can be directly compared with the predictions of galaxy formation models, iii) trace the spatial distribution of candidate globular clusters, and iv) detect the ultra-diffuse galaxies. With the DR1, we provide the reduced VST mosaics of 10 targets, which have been presented in the VEGAS publications. The data products are available via the ESO Science Portal (see http://www.eso.org/sci/observing/phase3/news.html#VEGAS-DR1). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.04950v1-abstract-full').style.display = 'none'; document.getElementById('2102.04950v1-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.05699">arXiv:2101.05699</a> <span> [<a href="https://arxiv.org/pdf/2101.05699">pdf</a>, <a href="https://arxiv.org/format/2101.05699">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/10.1051/0004-6361/202039633">10.1051/0004-6361/202039633 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fornax Deep Survey (FDS) with the VST XI. The search for signs of preprocessing between the Fornax main cluster and Fornax A group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Su%2C+A+H">Alan H. Su</a>, <a href="/search/astro-ph?searchtype=author&query=Salo%2C+H">Heikki Salo</a>, <a href="/search/astro-ph?searchtype=author&query=Janz%2C+J">Joachim Janz</a>, <a href="/search/astro-ph?searchtype=author&query=Laurikainen%2C+E">Eija Laurikainen</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">Aku Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R+F">Reynier F. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrica Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N">Nicola Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">Maria A. Raj</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen. Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">Massimo Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Valentijn%2C+E+A">Edwin A. Valentijn</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+A+E">Aaron E. Watkins</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="2101.05699v1-abstract-short" style="display: inline;"> We investigate the structural properties of cluster and group galaxies by studying the Fornax main cluster and the infalling Fornax A group, exploring the effects of galaxy preprocessing in this showcase example. Additionally, we compare the structural complexity of Fornax galaxies to those in the Virgo cluster and in the field. Our sample consists of 582 galaxies from the Fornax main cluster and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05699v1-abstract-full').style.display = 'inline'; document.getElementById('2101.05699v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05699v1-abstract-full" style="display: none;"> We investigate the structural properties of cluster and group galaxies by studying the Fornax main cluster and the infalling Fornax A group, exploring the effects of galaxy preprocessing in this showcase example. Additionally, we compare the structural complexity of Fornax galaxies to those in the Virgo cluster and in the field. Our sample consists of 582 galaxies from the Fornax main cluster and Fornax A group. We quantified the light distributions of each galaxy based on a combination of aperture photometry, S茅rsic+PSF (point spread function) and multi-component decompositions, and non-parametric measures of morphology (Concentration $C$; Asymmetry $A$, Clumpiness $S$; Gini $G$; second order moment of light $M_{20}$), and structural complexity based on multi-component decompositions. These quantities were then compared between the Fornax main cluster and Fornax A group. The structural complexity of Fornax galaxies were also compared to those in Virgo and in the field. Overall, we find significant differences in the distributions of quantities derived from S茅rsic profiles ($g'-r'$, $r'-i'$, $R_e$, and $\bar渭_{e,r'}$), and non-parametric indices ($A$ and $S$) between the Fornax main cluster and Fornax A group. Moreover, we find significant cluster-centric trends with $r'-i'$, $R_e$, and $\bar渭_{e,r'}$, as well as $A$, $S$, $G$, and $M_{20}$ for galaxies in the Fornax main cluster. We find the structural complexity of galaxies increases as a function of the absolute $r'$-band magnitude (and stellar mass), with the largest change occurring between -14 mag $\lesssim M_{r'}\lesssim$ -19 mag. This same trend was observed for galaxies in the Virgo cluster and in the field, which suggests that the formation or maintenance of morphological structures (e.g. bulges, bar) is largely dependent on the stellar mass of the galaxies, rather than their environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05699v1-abstract-full').style.display = 'none'; document.getElementById('2101.05699v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 January, 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">Submitted to A&A 9th October 2020, accepted 11th January 2021. For decompositions see https://www.oulu.fi/astronomy/FDS_DECOMP/main/index.html (username=password=sundial)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 647, A100 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.10306">arXiv:2012.10306</a> <span> [<a href="https://arxiv.org/pdf/2012.10306">pdf</a>, <a href="https://arxiv.org/format/2012.10306">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/10.1007/s12036-021-09690-x">10.1007/s12036-021-09690-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dorado and its member galaxies II. A UVIT picture of the NGC 1533 substructure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">R. Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzei%2C+P">P. Mazzei</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A">A. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+L">L. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Held%2C+E+V">E. V. Held</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Postma%2C+J">J. Postma</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan-Weber%2C+E">E. Ryan-Weber</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Uslenghi%2C+M">M. Uslenghi</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="2012.10306v1-abstract-short" style="display: inline;"> Dorado is a nearby (17.69 Mpc) strongly evolving galaxy group in the Southern Hemisphere. We are investigating the star formation in this group. This paper provides a FUV imaging of NGC 1533, IC 2038 and IC 2039, which form a substructure, south west of the Dorado group barycentre. FUV CaF2-1 UVIT-Astrosat images enrich our knowledge of the system provided by GALEX. In conjunction with deep optica… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.10306v1-abstract-full').style.display = 'inline'; document.getElementById('2012.10306v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.10306v1-abstract-full" style="display: none;"> Dorado is a nearby (17.69 Mpc) strongly evolving galaxy group in the Southern Hemisphere. We are investigating the star formation in this group. This paper provides a FUV imaging of NGC 1533, IC 2038 and IC 2039, which form a substructure, south west of the Dorado group barycentre. FUV CaF2-1 UVIT-Astrosat images enrich our knowledge of the system provided by GALEX. In conjunction with deep optical wide-field, narrow-band Halpha and 21-cm radio images we search for signatures of the interaction mechanisms looking in the FUV morphologies and derive the star formation rate. The shape of the FUV luminosity profile suggests the presence of a disk in all three galaxies. FUV emission is detected out to the optical size for IC 2038, and in compact structures corresponding to Halpha and HII bright features in NGC 1533. A faint FUV emission, without an optical counterpart, reminiscent of the HI structure that surrounds the outskirts of NGC 1533 and extends up to IC 2038/2039, is revealed above the local background noise. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.10306v1-abstract-full').style.display = 'none'; document.getElementById('2012.10306v1-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 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">13 pages, 8 figures, 3 tables, accepted for publication in The Journal of Astrophysics and Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.05347">arXiv:2011.05347</a> <span> [<a href="https://arxiv.org/pdf/2011.05347">pdf</a>, <a href="https://arxiv.org/format/2011.05347">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038936">10.1051/0004-6361/202038936 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> INSPIRE: INvestigating Stellar Population In RElics -- I. Survey presentation and pilot program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L">L. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Moehler%2C+S">S. Moehler</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</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="2011.05347v2-abstract-short" style="display: inline;"> Massive ETGs are thought to form through a two-phase process. At early times, an intense and fast starburst forms blue and disk-dominated galaxies. After quenching, the remaining structures become red, compact and massive, i.e., 'red nuggets'. Then, a time-extended second phase which is dominated by mergers, causes structural evolution and size growth. Given the stochastic nature of mergers, a sma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.05347v2-abstract-full').style.display = 'inline'; document.getElementById('2011.05347v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.05347v2-abstract-full" style="display: none;"> Massive ETGs are thought to form through a two-phase process. At early times, an intense and fast starburst forms blue and disk-dominated galaxies. After quenching, the remaining structures become red, compact and massive, i.e., 'red nuggets'. Then, a time-extended second phase which is dominated by mergers, causes structural evolution and size growth. Given the stochastic nature of mergers, a small fraction of red nuggets survives, without any interaction, massive and compact until today: relic galaxies. Since this fraction depends on the processes dominating the size growth, counting relics at low-z is a valuable way to disentangle between different galaxy evolution models. In this paper, we introduce the INvestigating Stellar Population In RElics (INSPIRE) Project, that aims at spectroscopically confirming and fully characterizing a large number of relics at 0.1<z<0.5. We focus here on the first results based on a pilot program targeting three systems, representative of the whole sample. For these, we extract 1D optical spectra over an aperture comprising ~30 % of the galaxies light, and obtain line-of-sight integrated stellar velocity and velocity dispersion. We also infer the stellar [$伪$/Fe] abundance from line-index measurements and mass-weighted age and metallicity from full-spectral fitting with single stellar population models. Two galaxies have large integrated stellar velocity dispersion values, confirming their massive nature. They are populated by stars with super-solar metallicity and [$伪$/Fe]. Both objects have formed >80 % of their stellar mass within a short (0.5 - 1.0 Gyrs) initial star formation episode occurred only ~1 Gyr after the Big Bang. The third galaxy has a more extended star formation history and a lower velocity dispersion. Thus we confirm two out of three candidates as relics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.05347v2-abstract-full').style.display = 'none'; document.getElementById('2011.05347v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">19 pages, 14 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 646, A28 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.14731">arXiv:2009.14731</a> <span> [<a href="https://arxiv.org/pdf/2009.14731">pdf</a>, <a href="https://arxiv.org/format/2009.14731">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/10.1051/0004-6361/202038996">10.1051/0004-6361/202038996 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dorado and its member galaxies. Ha imaging of the group backbone </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">R. Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzei%2C+P">P. Mazzei</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mille%2C+F">F. Di Mille</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">E. Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Cattapan%2C+A">A. Cattapan</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+L">L. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A">A. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Plana%2C+H">H. Plana</a>, <a href="/search/astro-ph?searchtype=author&query=Postma%2C+J">J. Postma</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</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="2009.14731v1-abstract-short" style="display: inline;"> ABRIDGED: Dorado is a nearby, rich and clumpy galaxy group that extends for several degrees in the Southern Hemisphere. For the first time, we map the Ha distribution as a possible indicator of star formation (SF) activity of Dorado members a large fraction of which show interaction and merging signatures. With the 2.5m du Pont and the 1m Swope telescopes we obtained narrow-band, calibrated images… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.14731v1-abstract-full').style.display = 'inline'; document.getElementById('2009.14731v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.14731v1-abstract-full" style="display: none;"> ABRIDGED: Dorado is a nearby, rich and clumpy galaxy group that extends for several degrees in the Southern Hemisphere. For the first time, we map the Ha distribution as a possible indicator of star formation (SF) activity of Dorado members a large fraction of which show interaction and merging signatures. With the 2.5m du Pont and the 1m Swope telescopes we obtained narrow-band, calibrated images of 14 galaxies, forming the backbone of the group, mapping Ha+[N II] down to few 10$^{-17}$ erg~cm$^{-2}$~s$^{-1}$~arcsec$^{-2}$. We estimated the galaxy star formation rate (SFR) from the Ha fluxes, corrected for Galaxy foreground extinction and [N II] contamination. Ha+[N II] emission has been detected in all galaxies. HII regions clearly emerge in late-type galaxies (LTGs) , while in early-type galaxies (ETGs) the Ha+[N II] emission is dominated by [N II], especially in the central regions. However, HII complexes are also revealed in four ETGs. Considering the Dorado group as a whole, we notice that the Ha+[N II] equivalent width, a measure of the specific SF, increases with the morphological type, from early to late-type members, although it remains lower that what observed in similar surveys of spiral galaxies. The SFR of the spiral members is in the range of what observed in similar galaxies surveys James+ (2004), although, in three spirals the SFR is well below the median for their morphological classes. The SFR of some early-type members tends, at odds, to be higher than the average derived from Ha+[N II] surveys of this morphological family. We detected in Ha+[N II] all the ETGs observed and half of them show HII regions. These findings suggest that ETGs in this group are not dead galaxies: their SF has not shut down yet. Mechanisms such as gas stripping and gas accretion, through galaxy-galaxy interaction, seem relevant in modifying the SF in this evolutionary phase of Dorado. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.14731v1-abstract-full').style.display = 'none'; document.getElementById('2009.14731v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 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">21 figures, 4 tables, accepted for publication on 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/2008.12633">arXiv:2008.12633</a> <span> [<a href="https://arxiv.org/pdf/2008.12633">pdf</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> <p class="title is-5 mathjax"> The Fornax Deep Survey data release 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">Reynier Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">Aku Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">Massimo Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Abrusco%2C+R">Raffaele D'Abrusco</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">Jes煤s Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Grado%2C+A">Aniello Grado</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Limatola%2C+L">Luca Limatola</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N">Nicola Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Valentijn%2C+E">Edwin Valentijn</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Kleijn%2C+G+V">Gijs Verdoes Kleijn</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="2008.12633v1-abstract-short" style="display: inline;"> We present the first data release of the Fornax Deep Survey (FDS), an imaging survey using using the wide-field imager OmegaCAM mounted on the VST in the SDSS u', g', r', and i'-bands covering the Fornax Galaxy Cluster and the infalling Fornax A Group. FDS is a joint project between NOVA (previously called FOCUS - PI: R. F. Peletier) and INAF (as part of VEGAS - PIs: M. Capaccioli and E. Iodice).… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.12633v1-abstract-full').style.display = 'inline'; document.getElementById('2008.12633v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.12633v1-abstract-full" style="display: none;"> We present the first data release of the Fornax Deep Survey (FDS), an imaging survey using using the wide-field imager OmegaCAM mounted on the VST in the SDSS u', g', r', and i'-bands covering the Fornax Galaxy Cluster and the infalling Fornax A Group. FDS is a joint project between NOVA (previously called FOCUS - PI: R. F. Peletier) and INAF (as part of VEGAS - PIs: M. Capaccioli and E. Iodice). With exposure times of about 9 hours over an area of ~28 square degrees, this survey is a legacy dataset for studies of members of the Fornax Galaxy Cluster and the infalling Fornax A Group down to a surface brightness limit of ~28 mag/arcsec^2 (1-sigma surface brightness over a 1 arcsecond^2 area) and opens a new parameter regime to investigate the role of the cluster environment in shaping the properties of its galaxy population. After the Virgo cluster,Fornax is the second nearest galaxy cluster to us, and with its different mass and evolutionary state, it provides a valuable comparison that makes it possible to understand the various evolutionary effects on galaxies and galaxy clusters. Details about the survey can be found in A. Venhola, R. F. Peletier, E. Laurikainen et al., 2018, A&A 620, 165. In this release, 181 Gb of (compressed) fits files reduced using the system are present. Catalogues with the complete sample of sources including dwarf galaxies part of the cluster, globular clusters, and background galaxies will be provided in forthcoming releases. The data products are available via the ESO Science Portal at https://archive.eso.org/scienceportal/home?publ_date=2020-08-26 <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.12633v1-abstract-full').style.display = 'none'; document.getElementById('2008.12633v1-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 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">arXiv admin note: substantial text overlap with arXiv:1810.00550</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.11533">arXiv:2007.11533</a> <span> [<a href="https://arxiv.org/pdf/2007.11533">pdf</a>, <a href="https://arxiv.org/format/2007.11533">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/10.1051/0004-6361/202038523">10.1051/0004-6361/202038523 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The first detection of ultra-diffuse galaxies in the Hydra I cluster from VEGAS survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">M. Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Greggio%2C+L">L. Greggio</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">D. A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">S. Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">A. La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Rampazzo%2C+R">R. Rampazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">M. Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">M. Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">P. Schipani</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.11533v1-abstract-short" style="display: inline;"> In this paper we report on the discovery of 27 low-surface brightness galaxies, of which 12 are candidate ultra-diffuse galaxy (UDG) in the Hydra I cluster, based on deep observations taken as part of the VST Early-type Galaxy Survey (VEGAS). This first sample of UDG candidates in the Hydra I cluster represents an important step in our project that aims to enlarge the number of confirmed UDGs and,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.11533v1-abstract-full').style.display = 'inline'; document.getElementById('2007.11533v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.11533v1-abstract-full" style="display: none;"> In this paper we report on the discovery of 27 low-surface brightness galaxies, of which 12 are candidate ultra-diffuse galaxy (UDG) in the Hydra I cluster, based on deep observations taken as part of the VST Early-type Galaxy Survey (VEGAS). This first sample of UDG candidates in the Hydra I cluster represents an important step in our project that aims to enlarge the number of confirmed UDGs and, through study of statistically relevant samples, constrain the nature and formation of UDGs. This study presents the main properties of this class of galaxies in the Hydra I cluster. For all UDGs, we analyse the light and colour distribution, and provide a census of the globular cluster (GC) systems around them. Given the limitations of a reliable GC selection based on two relatively close optical bands only, we find that half of the UDG candidates have a total GC population consistent with zero. Of the other half, two galaxies have a total population larger than zero at 2$蟽$ level. We estimate the stellar mass, the total number of GCs and the GC specific frequency ($S_N$). Most of the candidates span a range of stellar masses of $10^7-10^8$~M$_{\odot}$. Based on the GC population of these newly discovered UDGs, we conclude that most of these galaxies have a standard or low dark matter content, with a halo mass of $\leq 10^{10}$~M$_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.11533v1-abstract-full').style.display = 'none'; document.getElementById('2007.11533v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 642, A48 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.04492">arXiv:2007.04492</a> <span> [<a href="https://arxiv.org/pdf/2007.04492">pdf</a>, <a href="https://arxiv.org/format/2007.04492">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/staa2042">10.1093/mnras/staa2042 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SAMI -- Fornax Dwarfs Survey I: Sample, observations and the specific stellar angular momentum of dwarf elliptical galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scott%2C+N">Nicholas Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Eftekhari%2C+F+S">F. Sara Eftekhari</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R+F">Reynier F. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+J+J">Julia J. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">Massimo Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Croom%2C+S+M">Scott M. Croom</a>, <a href="/search/astro-ph?searchtype=author&query=Drinkwater%2C+M">Michael Drinkwater</a>, <a href="/search/astro-ph?searchtype=author&query=Falcon-Barroso%2C+J">Jesus Falcon-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Lorente%2C+N+F+P">Nuria F. P. Lorente</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">Aku Venhola</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.04492v1-abstract-short" style="display: inline;"> Dwarf ellipticals are the most common galaxy type in cluster environments, however the challenges associated with their observation mean their formation mechanisms are still poorly understood. To address this, we present deep integral field observations of a sample of 31 low-mass ($10^{7.5} <$ M$_\star < 10^{9.5}$ M$_\odot$) early-type galaxies in the Fornax cluster with the SAMI instrument. For 2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.04492v1-abstract-full').style.display = 'inline'; document.getElementById('2007.04492v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.04492v1-abstract-full" style="display: none;"> Dwarf ellipticals are the most common galaxy type in cluster environments, however the challenges associated with their observation mean their formation mechanisms are still poorly understood. To address this, we present deep integral field observations of a sample of 31 low-mass ($10^{7.5} <$ M$_\star < 10^{9.5}$ M$_\odot$) early-type galaxies in the Fornax cluster with the SAMI instrument. For 21 galaxies our observations are sufficiently deep to construct spatially resolved maps of the stellar velocity and velocity dispersion - for the remaining galaxies we extract global velocities and dispersions from aperture spectra only. From the kinematic maps we measure the specific stellar angular momentum $位_R$ of the lowest mass dE galaxies to date. Combining our observations with early-type galaxy data from the literature spanning a large range in stellar mass, we find that $位_R$ decreases towards lower stellar mass, with a corresponding increase in the proportion of slowly rotating galaxies in this regime. The decrease of $位_R$ with mass in our sample dE galaxies is consistent with a similar trend seen in somewhat more massive spiral galaxies from the CALIFA survey. This suggests that the degree of dynamical heating required to produce dEs from low-mass starforming progenitors may be relatively modest, and consistent with a broad range of formation mechanisms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.04492v1-abstract-full').style.display = 'none'; document.getElementById('2007.04492v1-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 10 figures and an additional 10 pages of appendices. 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/2006.13235">arXiv:2006.13235</a> <span> [<a href="https://arxiv.org/pdf/2006.13235">pdf</a>, <a href="https://arxiv.org/format/2006.13235">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/10.1051/0004-6361/202038373">10.1051/0004-6361/202038373 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nature versus nurture: relic nature and environment of the most massive passive galaxies at $z < 0.5$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L">L. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+N">N. Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">L. Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</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=D%60Ago%2C+G">G. D`Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Longo%2C+G">G. Longo</a>, <a href="/search/astro-ph?searchtype=author&query=Bellagamba%2C+F">F. Bellagamba</a>, <a href="/search/astro-ph?searchtype=author&query=Maturi%2C+M">M. Maturi</a>, <a href="/search/astro-ph?searchtype=author&query=Roncarelli%2C+M">M. Roncarelli</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="2006.13235v1-abstract-short" style="display: inline;"> Relic galaxies are thought to be the progenitors of high-redshift red nuggets that for some reason missed the channels of size growth and evolved passively and undisturbed since the first star formation burst (at $z>2$). These local ultracompact old galaxies are unique laboratories for studying the star formation processes at high redshift and thus the early stage of galaxy formation scenarios. Co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.13235v1-abstract-full').style.display = 'inline'; document.getElementById('2006.13235v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.13235v1-abstract-full" style="display: none;"> Relic galaxies are thought to be the progenitors of high-redshift red nuggets that for some reason missed the channels of size growth and evolved passively and undisturbed since the first star formation burst (at $z>2$). These local ultracompact old galaxies are unique laboratories for studying the star formation processes at high redshift and thus the early stage of galaxy formation scenarios. Counterintuitively, theoretical and observational studies indicate that relics are more common in denser environments, where merging events predominate. To verify this scenario, we compared the number counts of a sample of ultracompact massive galaxies (UCMGs) selected within the third data release of the Kilo Degree Survey, that is, systems with sizes $R_{\rm e} < 1.5 \, \rm kpc$ and stellar masses $M_{\rm \star} > 8 \times 10^{10}\, \rm M_{\odot}$, with the number counts of galaxies with the same masses but normal sizes in field and cluster environments. Based on their optical and near-infrared colors, these UCMGs are likely to be mainly old, and hence representative of the relic population. We find that both UCMGs and normal-size galaxies are more abundant in clusters and their relative fraction depends only mildly on the global environment, with denser environments penalizing the survival of relics. Hence, UCMGs (and likely relics overall) are not special because of the environment effect on their nurture, but rather they are just a product of the stochasticity of the merging processes regardless of the global environment in which they live. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.13235v1-abstract-full').style.display = 'none'; document.getElementById('2006.13235v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on Astronomy & Astrophysics Letters, 6 pages, 1 figure</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.11828">arXiv:2006.11828</a> <span> [<a href="https://arxiv.org/pdf/2006.11828">pdf</a>, <a href="https://arxiv.org/format/2006.11828">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/10.1051/0004-6361/202038043">10.1051/0004-6361/202038043 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fornax Deep Survey with VST. X. The assembly history of the bright galaxies and intra-group light in the Fornax A subgroup </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">M. A. Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">M. Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R+F">R. F. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+H">H-S. Su</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">J. Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">G. van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">A. Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">S. Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">M. Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">M. Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">P. Schipani</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="2006.11828v2-abstract-short" style="display: inline;"> We present the study of the south-west group in the Fornax cluster centred on the brightest group galaxy (BGG) Fornax A, observed as part of the Fornax Deep Survey (FDS). This includes the analysis of the bright group members (mB < 16 mag) and the intra-group light (IGL). The main objective of this work is to investigate the assembly history of the Fornax A group and to compare its physical quanti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.11828v2-abstract-full').style.display = 'inline'; document.getElementById('2006.11828v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.11828v2-abstract-full" style="display: none;"> We present the study of the south-west group in the Fornax cluster centred on the brightest group galaxy (BGG) Fornax A, observed as part of the Fornax Deep Survey (FDS). This includes the analysis of the bright group members (mB < 16 mag) and the intra-group light (IGL). The main objective of this work is to investigate the assembly history of the Fornax A group and to compare its physical quantities as a function of the environment to that of the Fornax cluster core. For all galaxies, we extract the azimuthally averaged surface brightness profiles in three optical bands (g, r, i) by modelling the galaxy's isophotes. We derive their colour profiles and structural parameters in all respective bands. The long integration time and large covered area of the FDS allow us to also estimate the amount of IGL. The majority of galaxies in the Fornax A group are late-type galaxies (LTGs), spanning a range of stellar mass of $8 < log (M_* M_{\odot}) < 10.5$. Six out of nine LTGs show a Type III (up-bending) break in their light profiles, which is either suggestive of strangulation halting star-formation in their outskirts or their HI-richness causing enhanced star-formation in their outer-discs. The estimated luminosity of the IGL is $6 \pm 2 \times 10^{10} L_{\odot}$ in g-band, which corresponds to about 16% of the total light in the group. The Fornax A group appears to be in an early stage of assembly with respect to the cluster core. The environment of the Fornax A group is not as dense as that of the cluster core, with all galaxies except the BGG showing similar morphology, comparable colours and stellar masses, and Type III disc-breaks, without any clear trend of these properties with group-centric distances. The main contribution to the IGL is from the minor merging in the outskirts of the BGG NGC1316 and, probably, the disrupted dwarf galaxies close to the group centre. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.11828v2-abstract-full').style.display = 'none'; document.getElementById('2006.11828v2-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Published in A&A. Replaced version: corrected typos and title (series number X)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 640, A137 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.12085">arXiv:2005.12085</a> <span> [<a href="https://arxiv.org/pdf/2005.12085">pdf</a>, <a href="https://arxiv.org/format/2005.12085">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/10.1051/0004-6361/202038137">10.1051/0004-6361/202038137 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fornax Deep Survey with VST. IX. The catalog of sources in the FDS area, with an example study for globular clusters and background galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">Aku Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Grado%2C+A">Aniello Grado</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Abrusco%2C+R">Raffaele D'Abrusco</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">Gabriella Raimondo</a>, <a href="/search/astro-ph?searchtype=author&query=Quintini%2C+M">Massimo Quintini</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">Crescenzo Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">Massimo Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrica Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">Reynier Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Barroso%2C+J+F">Jesus Falcon Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Limatola%2C+L">Luca Limatola</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N">Nicola Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Gentile%2C+F">Fabrizio Gentile</a>, <a href="/search/astro-ph?searchtype=author&query=Covone%2C+G">Giovanni Covone</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.12085v2-abstract-short" style="display: inline;"> This paper continues the series of the Fornax Deep Survey (FDS). Following the previous studies dedicated to extended Fornax cluster members, we present the catalogs of compact stellar systems in the Fornax cluster as well as extended background sources and point-like sources. We derive ugri photometry of ~1.7 million sources over the $\sim$21 sq. degree area of FDS centered on NGC1399. For a wide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12085v2-abstract-full').style.display = 'inline'; document.getElementById('2005.12085v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.12085v2-abstract-full" style="display: none;"> This paper continues the series of the Fornax Deep Survey (FDS). Following the previous studies dedicated to extended Fornax cluster members, we present the catalogs of compact stellar systems in the Fornax cluster as well as extended background sources and point-like sources. We derive ugri photometry of ~1.7 million sources over the $\sim$21 sq. degree area of FDS centered on NGC1399. For a wider area, of $\sim$27 sq. degs extending in the direction of NGC1316, we provide gri data for ~3.1 million sources. To improve the morphological characterization of sources we generate multi-band image stacks by coadding the best seeing gri-band single exposures with a cut at FWHM<=0.9 arcsec. We use the multi-band stacks as detection frames. The identification of compact sources is obtained from a combination of photometric and morphometric selection criteria taking as reference the properties of sources with well-defined classification from the literature. We present a preliminary analysis of globular cluster (GC) distributions in the Fornax area. The study confirms and extends further previous results. We observe the inter-galactic population of GCs, a population of mainly blue GCs centered on NGC1399, extends over $\sim$0.9Mpc, with an ellipticity $\sim$0.65. Several sub-structures extend over $\sim$0.5Mpc along various directions. Two of these structures do not cross any bright galaxy; one of them appears to be connected to NGC1404, a bright galaxy close to the cluster core and particularly poor of GCs. Using the gri catalogs we analyze the GC distribution over the extended FDS area, and do not find any obvious GC sub-structure bridging the two brightest cluster galaxies, NGC1316 and NGC1399. Although NGC1316 is twice brighter of NGC1399 in optical bands we estimate a factor of 3-4 richer GC population around NGC1399 compared to NGC1316, out to galactocentric distances of 40 arcmin <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12085v2-abstract-full').style.display = 'none'; document.getElementById('2005.12085v2-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 18 figures, A&A accepted, tables 3-6 available on line</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 639, A136 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.00025">arXiv:2005.00025</a> <span> [<a href="https://arxiv.org/pdf/2005.00025">pdf</a>, <a href="https://arxiv.org/format/2005.00025">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/10.1051/0004-6361/202038015">10.1051/0004-6361/202038015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fornax Deep Survey with VST. VIII. Connecting the accretion history with the cluster density </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">G. van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">J. Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">M. A. Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">M. Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R+P">R. P. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">M. Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">S. Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">A. Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">M. Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">P. Schipani</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.00025v1-abstract-short" style="display: inline;"> This work is based on deep multi-band (g, r, i) data from the Fornax Deep Survey with VST. We analyse the surface brightness profiles of the 19 bright ETGs inside the virial radius of the Fornax cluster. The main aim of this work is to identify signatures of accretion onto galaxies by studying the presence of outer stellar halos, and understand their nature and occurrence. Our analysis also provid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00025v1-abstract-full').style.display = 'inline'; document.getElementById('2005.00025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.00025v1-abstract-full" style="display: none;"> This work is based on deep multi-band (g, r, i) data from the Fornax Deep Survey with VST. We analyse the surface brightness profiles of the 19 bright ETGs inside the virial radius of the Fornax cluster. The main aim of this work is to identify signatures of accretion onto galaxies by studying the presence of outer stellar halos, and understand their nature and occurrence. Our analysis also provides a new and accurate estimate of the intra-cluster light inside the virial radius of Fornax. We performed multi-component fits to the azimuthally averaged surface brightness profiles available for all sample galaxies. This allows to quantify the relative weight of all components in the galaxy structure that contribute to the total light. In addition, we derived the average g-i colours in each component identified by the fit, as well as the azimuthally averaged g-i colour profiles, to correlate them with the stellar mass of each galaxy and the location inside the cluster. We find that in the most massive and reddest ETGs the fraction of light in, probably accreted, halos is much larger than in the other galaxies. Less-massive galaxies have an accreted mass fraction lower than 30%, bluer colours and reside in the low-density regions of the cluster. Inside the virial radius of the cluster, the total luminosity of the intra-cluster light, compared with the total luminosity of all cluster members, is about 34%. Inside the Fornax cluster there is a clear correlation between the amount of accreted material in the stellar halos of galaxies and the density of the environment in which those galaxies reside. By comparing this quantity with theoretical predictions and previous observational estimates, there is a clear indication that the driving factor for the accretion process is the total stellar mass of the galaxy, in agreement with the hierarchical accretion scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00025v1-abstract-full').style.display = 'none'; document.getElementById('2005.00025v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 10 figures. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 639, A14 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.10855">arXiv:2004.10855</a> <span> [<a href="https://arxiv.org/pdf/2004.10855">pdf</a>, <a href="https://arxiv.org/format/2004.10855">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/staa1111">10.1093/mnras/staa1111 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultra Diffuse Galaxies in the IC1459 Group from the VEGAS Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Dullo%2C+B+T">Bililign T. Dullo</a>, <a href="/search/astro-ph?searchtype=author&query=Gannon%2C+J">Jonah Gannon</a>, <a href="/search/astro-ph?searchtype=author&query=Couch%2C+W+J">Warrick J. Couch</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</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="2004.10855v1-abstract-short" style="display: inline;"> Using deep g,r,i imaging from the VEGAS survey, we have searched for ultra diffuse galaxies (UDGs) in the IC 1459 group. Assuming they are group members, we identify 9 galaxies with physical sizes and surface brightnesses that match the UDG criteria within our measurement uncertainties. They have mean colours of g--i = 0.6 and stellar masses of $\sim$10$^8$ M$_{\odot}$. Several galaxies appear to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10855v1-abstract-full').style.display = 'inline'; document.getElementById('2004.10855v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.10855v1-abstract-full" style="display: none;"> Using deep g,r,i imaging from the VEGAS survey, we have searched for ultra diffuse galaxies (UDGs) in the IC 1459 group. Assuming they are group members, we identify 9 galaxies with physical sizes and surface brightnesses that match the UDG criteria within our measurement uncertainties. They have mean colours of g--i = 0.6 and stellar masses of $\sim$10$^8$ M$_{\odot}$. Several galaxies appear to have associated systems of compact objects, e.g. globular clusters. Two UDGs contain a central bright nucleus, with a third UDG revealing a remarkable double nucleus. This appears to be the first reported detection of a double nucleus in a UDG - its origin is currently unclear. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10855v1-abstract-full').style.display = 'none'; document.getElementById('2004.10855v1-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 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">6 pages, 4 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/2002.12922">arXiv:2002.12922</a> <span> [<a href="https://arxiv.org/pdf/2002.12922">pdf</a>, <a href="https://arxiv.org/format/2002.12922">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/ab7db3">10.3847/1538-4357/ab7db3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Building the largest spectroscopic sample of ultra-compact massive galaxies with the Kilo Degree Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">Diana Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">Crescenzo Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">Chiara Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">Nicola R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">Francesco La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Getman%2C+F">Fedor Getman</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+N">Nivya Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">Maria Angela Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">Mario Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">Massimo Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">Stefano Cavuoti</a>, <a href="/search/astro-ph?searchtype=author&query=Koopmans%2C+L+V+E">Leon V. E. Koopmans</a>, <a href="/search/astro-ph?searchtype=author&query=Kuijken%2C+K+H">Koen H. Kuijken</a>, <a href="/search/astro-ph?searchtype=author&query=Longo%2C+G">Giuseppe Longo</a>, <a href="/search/astro-ph?searchtype=author&query=Petrillo%2C+C+E">Carlo Enrico Petrillo</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="2002.12922v1-abstract-short" style="display: inline;"> Ultra-compact massive galaxies UCMGs, i.e. galaxies with stellar masses $M_{*} > 8 \times 10^{10} M_{\odot}$ and effective radii $R_{e} < 1.5$ kpc, are very rare systems, in particular at low and intermediate redshifts. Their origin as well as their number density across cosmic time are still under scrutiny, especially because of the paucity of spectroscopically confirmed samples. We have started… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.12922v1-abstract-full').style.display = 'inline'; document.getElementById('2002.12922v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.12922v1-abstract-full" style="display: none;"> Ultra-compact massive galaxies UCMGs, i.e. galaxies with stellar masses $M_{*} > 8 \times 10^{10} M_{\odot}$ and effective radii $R_{e} < 1.5$ kpc, are very rare systems, in particular at low and intermediate redshifts. Their origin as well as their number density across cosmic time are still under scrutiny, especially because of the paucity of spectroscopically confirmed samples. We have started a systematic census of UCMG candidates within the ESO Kilo Degree Survey, together with a large spectroscopic follow-up campaign to build the largest possible sample of confirmed UCMGs. This is the third paper of the series and the second based on the spectroscopic follow-up program. Here, we present photometrical and structural parameters of 33 new candidates at redshifts $0.15 \lesssim z \lesssim 0.5$ and confirm 19 of them as UCMGs, based on their nominal spectroscopically inferred $M_{*}$ and $R_{e}$. This corresponds to a success rate of $\sim 58\%$, nicely consistent with our previous findings. The addition of these 19 newly confirmed objects, allows us to fully assess the systematics on the system selection, and finally reduce the number density uncertainties. Moreover, putting together the results from our current and past observational campaigns and some literature data, we build the largest sample of UCMGs ever collected, comprising 92 spectroscopically confirmed objects at $0.1 \lesssim z \lesssim 0.5$. This number raises to 116, allowing for a $3蟽$ tolerance on the $M_{*}$ and $R_{e}$ thresholds for the UCMG definition. For all these galaxies we have estimated the velocity dispersion values at the effective radii which have been used to derive a preliminary mass-velocity dispersion correlation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.12922v1-abstract-full').style.display = 'none'; document.getElementById('2002.12922v1-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 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">Journal ref:</span> The Astrophysical Journal 893:4 (2020) pp22 </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=Spavone%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Spavone%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Spavone%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </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