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 1–34 of 34 results for author: <span class="mathjax">Marchi, F</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=Marchi%2C+F">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="Marchi, F"> </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=Marchi%2C+F&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="Marchi, F"> <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> <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/2309.14436">arXiv:2309.14436</a> <span> [<a href="https://arxiv.org/pdf/2309.14436">pdf</a>, <a href="https://arxiv.org/format/2309.14436">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/10.1051/0004-6361/202346293">10.1051/0004-6361/202346293 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS ESO public spectroscopic survey: The spectroscopic measurements catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+C">C. Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=Moresco%2C+M">M. Moresco</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J+P+U">J. P. U. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R">R. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Pompei%2C+E">E. Pompei</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+G">G. Vietri</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R+O">R. O. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a> , et al. (14 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.14436v1-abstract-short" style="display: inline;"> VANDELS is a deep spectroscopic survey, performed with the VIMOS instrument at VLT, aimed at studying in detail the physical properties of high-redshift galaxies. VANDELS targeted about 2100 sources at 1<z<6.5 in the CANDELS Chandra Deep-Field South (CDFS) and Ultra-Deep Survey (UDS) fields. In this paper we present the public release of the spectroscopic measurement catalogues from this survey, f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.14436v1-abstract-full').style.display = 'inline'; document.getElementById('2309.14436v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.14436v1-abstract-full" style="display: none;"> VANDELS is a deep spectroscopic survey, performed with the VIMOS instrument at VLT, aimed at studying in detail the physical properties of high-redshift galaxies. VANDELS targeted about 2100 sources at 1<z<6.5 in the CANDELS Chandra Deep-Field South (CDFS) and Ultra-Deep Survey (UDS) fields. In this paper we present the public release of the spectroscopic measurement catalogues from this survey, featuring emission and absorption line centroids, fluxes, and rest-frame equivalent widths obtained through a Gaussian fit, as well as a number of atomic and molecular indices (e.g. Lick) and continuum breaks (e.g. D4000), and including a correction to be applied to the error spectra. We describe the measurement methods and the validation of the codes that were used. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.14436v1-abstract-full').style.display = 'none'; document.getElementById('2309.14436v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 September, 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">12 pages, 9 figures; accepted for publication in Astronomy & Astrophysics. The measurement catalogues are accessible through the survey database (http://vandels.inaf.it) where all information can be queried interactively, and at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/cgi-bin/qcat?J/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 678, A25 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.01915">arXiv:2212.01915</a> <span> [<a href="https://arxiv.org/pdf/2212.01915">pdf</a>, <a href="https://arxiv.org/format/2212.01915">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/acacff">10.3847/1538-4357/acacff <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Art of Measuring Physical Parameters in Galaxies: A Critical Assessment of Spectral Energy Distribution Fitting Techniques </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=Iyer%2C+K+G">Kartheik G. Iyer</a>, <a href="/search/astro-ph?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/astro-ph?searchtype=author&query=da+Cunha%2C+E">Elisabete da Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Acquaviva%2C+V">Viviana Acquaviva</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Rivera%2C+G+C">Gabriela Calistro Rivera</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">Adam C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+Y">Yu-Yen Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chartab%2C+N">Nima Chartab</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+K+C">Kevin C. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Fairhurst%2C+C">Ciaran Fairhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J">Jeyhan Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Malek%2C+K">Katarzyna Malek</a>, <a href="/search/astro-ph?searchtype=author&query=Salmon%2C+B">Brett Salmon</a>, <a href="/search/astro-ph?searchtype=author&query=Torelli%2C+M">Marianna Torelli</a>, <a href="/search/astro-ph?searchtype=author&query=Vidal-Garcia%2C+A">Alba Vidal-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G+G">Gabriel G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">Michael J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Capak%2C+P+L">Peter L. Capak</a>, <a href="/search/astro-ph?searchtype=author&query=Chevallard%2C+J">Jacopo Chevallard</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">Chiara Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Croton%2C+D">Darren Croton</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.01915v1-abstract-short" style="display: inline;"> The study of galaxy evolution hinges on our ability to interpret multi-wavelength galaxy observations in terms of their physical properties. To do this, we rely on spectral energy distribution (SED) models which allow us to infer physical parameters from spectrophotometric data. In recent years, thanks to the wide and deep multi-waveband galaxy surveys, the volume of high quality data have signifi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.01915v1-abstract-full').style.display = 'inline'; document.getElementById('2212.01915v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.01915v1-abstract-full" style="display: none;"> The study of galaxy evolution hinges on our ability to interpret multi-wavelength galaxy observations in terms of their physical properties. To do this, we rely on spectral energy distribution (SED) models which allow us to infer physical parameters from spectrophotometric data. In recent years, thanks to the wide and deep multi-waveband galaxy surveys, the volume of high quality data have significantly increased. Alongside the increased data, algorithms performing SED fitting have improved, including better modeling prescriptions, newer templates, and more extensive sampling in wavelength space. We present a comprehensive analysis of different SED fitting codes including their methods and output with the aim of measuring the uncertainties caused by the modeling assumptions. We apply fourteen of the most commonly used SED fitting codes on samples from the CANDELS photometric catalogs at z~1 and z~3. We find agreement on the stellar mass, while we observe some discrepancies in the star formation rate (SFR) and dust attenuation results. To explore the differences and biases among the codes, we explore the impact of the various modeling assumptions as they are set in the codes (e.g., star formation histories, nebular, dust, and AGN models) on the derived stellar masses, SFRs, and A_V values. We then assess the difference among the codes on the SFR-stellar mass relation and we measure the contribution to the uncertainties by the modeling choices (i.e., the modeling uncertainties) in stellar mass (~0.1dex), SFR (~0.3dex), and dust attenuation (~0.3mag). Finally, we present some resources summarizing best practices in SED fitting. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.01915v1-abstract-full').style.display = 'none'; document.getElementById('2212.01915v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 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">25 pages, 11 figures. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.00660">arXiv:2107.00660</a> <span> [<a href="https://arxiv.org/pdf/2107.00660">pdf</a>, <a href="https://arxiv.org/format/2107.00660">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/10.1051/0004-6361/202141651">10.1051/0004-6361/202141651 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS survey: global properties of CIII]$位$1908脜 emitting star-forming galaxies at z$\sim$3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">M. Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">R. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R">R. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A">A. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Montero%2C+E">E. P茅rez-Montero</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+D+J">D. J. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hibon%2C+P">P. Hibon</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+A">A. Saxena</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</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="2107.00660v2-abstract-short" style="display: inline;"> We study the mean properties of a large representative sample of 217 galaxies showing CIII] emission at $2<z<4$, selected from a parent sample of $\sim$750 main-sequence star-forming galaxies in the VANDELS survey. These CIII] emitters have a broad range of UV luminosities, thus allowing a detailed stacking analysis to characterize their stellar mass, star formation rate (SFR) and stellar metallic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.00660v2-abstract-full').style.display = 'inline'; document.getElementById('2107.00660v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.00660v2-abstract-full" style="display: none;"> We study the mean properties of a large representative sample of 217 galaxies showing CIII] emission at $2<z<4$, selected from a parent sample of $\sim$750 main-sequence star-forming galaxies in the VANDELS survey. These CIII] emitters have a broad range of UV luminosities, thus allowing a detailed stacking analysis to characterize their stellar mass, star formation rate (SFR) and stellar metallicity, as a function of the UV emission line ratios, EWs, and the carbon-to-oxygen (C/O) abundance ratio. Reliable CIII] detections represent $\sim$30% of the parent sample. Extreme CIII] emitters (EW(CIII])$\gtrsim$8脜) are exceedingly rare ($\sim$3%) in VANDELS. The UV line ratios of the sample suggest no ionization source other than massive stars. Stacks with larger EW(CIII]) show larger EW(Ly$伪$) and lower metallicity, but not all CIII] emitters are Ly$伪$ emitters. The stellar metallicities of CIII] emitters are not significantly different from that of the parent sample, increasing from $\sim$10% to $\sim$40% solar for stellar masses $\log$(M$_{\star}$/M$_{\odot})\sim$9-10.5. The stellar mass-metallicity relation of the CIII] emitters is consistent with previous works showing strong evolution from $z=0$ to $z\sim3$. The C/O abundances of the sample range 35%-150% solar, with a noticeable increase with FUV luminosity and a smooth decrease with the CIII] EW. We discuss the CIII] emitters in the C/O-Fe/H and the C/O-O/H planes and find they follow stellar and nebular abundance trends consistent with those of Milky Way halo and thick disc stars and local HII galaxies, respectively. A qualitative agreement is also found with chemical evolution models, which suggests that CIII] emitters at $z\sim$3 are experiencing an active phase of chemical enrichment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.00660v2-abstract-full').style.display = 'none'; document.getElementById('2107.00660v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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 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 659, A16 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.06615">arXiv:2011.06615</a> <span> [<a href="https://arxiv.org/pdf/2011.06615">pdf</a>, <a href="https://arxiv.org/format/2011.06615">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/10.1051/0004-6361/202039244">10.1051/0004-6361/202039244 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS survey: the relation between UV continuum slope and stellar metallicity in star-forming galaxies at z~3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">F. Fontanot</a>, <a href="/search/astro-ph?searchtype=author&query=Menci%2C+N">N. Menci</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R">R. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">R. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lucia%2C+G">G. De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J">J. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">M. Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hibon%2C+P">P. Hibon</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">M. Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+A">A. Saxena</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+L">L. Xie</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="2011.06615v1-abstract-short" style="display: inline;"> The estimate of stellar metallicities (Z*) of high-z galaxies are of paramount importance in order to understand the complexity of dust effects and the reciprocal interrelations among stellar mass, dust attenuation, stellar age, and metallicity. Benefiting from uniquely deep FUV spectra of >500 star-forming galaxies at redshifts 2<z<5 extracted from the VANDELS survey and stacked in bins of stella… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06615v1-abstract-full').style.display = 'inline'; document.getElementById('2011.06615v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.06615v1-abstract-full" style="display: none;"> The estimate of stellar metallicities (Z*) of high-z galaxies are of paramount importance in order to understand the complexity of dust effects and the reciprocal interrelations among stellar mass, dust attenuation, stellar age, and metallicity. Benefiting from uniquely deep FUV spectra of >500 star-forming galaxies at redshifts 2<z<5 extracted from the VANDELS survey and stacked in bins of stellar mass (M*) and UV continuum slope (beta), we estimate their stellar metallicities Z* from stellar photospheric absorption features at 1501 and 1719 Angstrom, which are calibrated with Starburst99 models and are largely unaffected by stellar age, dust, IMF, nebular continuum or interstellar absorption. Comparing them to photometric based spectral slopes in the range 1250-1750 Angstrom, we find that the stellar metallicity increases by ~0.5 dex from beta ~ -2 to beta ~ -1 (1 < A(1600) < 3.2), and a dependence with beta holds at fixed UV absolute luminosity M(UV) and stellar mass up to 10^(9.65) Msun. As a result, the metallicity is a fundamental ingredient for properly rescaling dust corrections based on M(UV) and M*. Using the same absorption features, we analyze the mass-metallicity relation (MZR) and find it is consistent with the previous VANDELS estimation based on a global fit of the FUV spectra. Similarly, we do not find a significant evolution between z=2 and z=3.5. Finally, the slopes of our MZR and Z*-beta relation are in agreement with the predictions of well-studied semi-analytic models of galaxy formation (SAM), while some tensions with observations remain as to the absolute metallicity normalization. The relation between UV slope and stellar metallicity is fundamental for the exploitation of large volume surveys with next-generation telescopes and for the physical characterization of galaxies in the first billion years of our Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06615v1-abstract-full').style.display = 'none'; document.getElementById('2011.06615v1-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 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">25 pages, 4 tables, 16 figures, and 5 Appendix subsections; 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, 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/1911.12532">arXiv:1911.12532</a> <span> [<a href="https://arxiv.org/pdf/1911.12532">pdf</a>, <a href="https://arxiv.org/format/1911.12532">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201935925">10.1051/0004-6361/201935925 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Intergalactic medium transmission towards z>4 galaxies with VANDELS and the impact of dust attenuation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+R">R. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%A8vre%2C+O+L">O. Le F猫vre</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">F. Fontanot</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Hibon%2C+P">P. Hibon</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">N. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J+P+U">J. P. U. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Khusanova%2C+Y">Y. Khusanova</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+D">D. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">R. J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+A">A. Saxena</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</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="1911.12532v1-abstract-short" style="display: inline;"> Aims. Our aim is to estimate the intergalactic medium transmission towards UV-selected star-forming galaxies at redshift 4 and above and study the effect of the dust attenuation on these measurements. Methods. The ultra-violet spectrum of high redshift galaxies is a combination of their intrinsic emission and the effect of the Inter-Galactic medium (IGM) absorption along their line of sight. Usi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.12532v1-abstract-full').style.display = 'inline'; document.getElementById('1911.12532v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.12532v1-abstract-full" style="display: none;"> Aims. Our aim is to estimate the intergalactic medium transmission towards UV-selected star-forming galaxies at redshift 4 and above and study the effect of the dust attenuation on these measurements. Methods. The ultra-violet spectrum of high redshift galaxies is a combination of their intrinsic emission and the effect of the Inter-Galactic medium (IGM) absorption along their line of sight. Using data coming from the unprecedented deep spectroscopy from the VANDELS ESO public survey carried out with the VIMOS instrument we compute both the dust extinction and the mean transmission of the IGM as well as its scatter from a set of 281 galaxies at z>3.87. Because of a degeneracy between the dust content of the galaxy and the IGM, we first estimate the stellar dust extinction parameter E(B-V) and study the result as a function of the dust prescription. Using these measurements as constraint for the spectral fit we estimate the IGM transmission Tr(Lyalpha). Both photometric and spectroscopic SED fitting are done using the SPectroscopy And photometRy fiTting tool for Astronomical aNalysis (SPARTAN) that is able to fit the spectral continuum of the galaxies as well as photometric data. Results. Using the classical Calzetti's attenuation law we find that E(B-V) goes from 0.11 at z=3.99 to 0.08 at z=5.15. These results are in very good agreement with previous measurements from the literature. We estimate the IGM transmission and find that the transmission is decreasing with increasing redshift from Tr(Lyalpha)=0.53 at z=3.99 to 0.28 at z=5.15. We also find a large standard deviation around the average transmission that is more than 0.1 at every redshift. Our results are in very good agreement with both previous measurements from AGN studies and with theoretical models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.12532v1-abstract-full').style.display = 'none'; document.getElementById('1911.12532v1-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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 634, A110 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.09999">arXiv:1911.09999</a> <span> [<a href="https://arxiv.org/pdf/1911.09999">pdf</a>, <a href="https://arxiv.org/format/1911.09999">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/10.1051/0004-6361/201937170">10.1051/0004-6361/201937170 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The properties of He II 1640 emitters at z ~ 2.5-5 from the VANDELS survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+A">A. Saxena</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabelli%2C+M">M. Mirabelli</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+R">R. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J+P+U">J. P. U. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">A. Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">T. A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+D+J">D. J. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">R. J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">C. Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a> , et al. (2 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="1911.09999v2-abstract-short" style="display: inline;"> Strong He II emission is produced by low-metallicity stellar populations. Here, we aim to identify and study a sample of He II $位1640$-emitting galaxies at redshifts of $z \sim 2.5-5$ in the deep VANDELS spectroscopic survey.. We identified a total of 33 Bright He II emitters (S/N > 2.5) and 17 Faint emitters (S/N < 2.5) in the VANDELS survey and used the available deep multi-wavelength data to st… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.09999v2-abstract-full').style.display = 'inline'; document.getElementById('1911.09999v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.09999v2-abstract-full" style="display: none;"> Strong He II emission is produced by low-metallicity stellar populations. Here, we aim to identify and study a sample of He II $位1640$-emitting galaxies at redshifts of $z \sim 2.5-5$ in the deep VANDELS spectroscopic survey.. We identified a total of 33 Bright He II emitters (S/N > 2.5) and 17 Faint emitters (S/N < 2.5) in the VANDELS survey and used the available deep multi-wavelength data to study their physical properties. After identifying seven potential AGNs in our sample and discarding them from further analysis, we divided the sample of \emph{Bright} emitters into 20 \emph{Narrow} (FWHM < 1000 km s$^{-1}$) and 6 \emph{Broad} (FWHM > 1000 km s$^{-1}$) He II emitters. We created stacks of Faint, Narrow, and Broad emitters and measured other rest-frame UV lines such as O III] and C III] in both individual galaxies and stacks. We then compared the UV line ratios with the output of stellar population-synthesis models to study the ionising properties of He II emitters. We do not see a significant difference between the stellar masses, star-formation rates, and rest-frame UV magnitudes of galaxies with He II and no He II emission. The stellar population models reproduce the observed UV line ratios from metals in a consistent manner, however they under-predict the total number of \heii ionising photons, confirming earlier studies and suggesting that additional mechanisms capable of producing He II are needed, such as X-ray binaries or stripped stars. The models favour subsolar metallicities ($\sim0.1Z_\odot$) and young stellar ages ($10^6 - 10^7$ years) for the He II emitters. However, the metallicity measured for He II emitters is comparable to that of non-He II emitters at similar redshifts. We argue that galaxies with He II emission may have undergone a recent star-formation event, or may be powered by additional sources of He II ionisation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.09999v2-abstract-full').style.display = 'none'; document.getElementById('1911.09999v2-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 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 11 figures (including appendix), 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 636, A47 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.11082">arXiv:1903.11082</a> <span> [<a href="https://arxiv.org/pdf/1903.11082">pdf</a>, <a href="https://arxiv.org/format/1903.11082">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz2544">10.1093/mnras/stz2544 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS survey: the star-formation histories of massive quiescent galaxies at 1.0 < z < 1.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">R. J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">J. S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+D+J">D. J. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=Wild%2C+V">V. Wild</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+B+D">B. D. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Appleby%2C+S">S. Appleby</a>, <a href="/search/astro-ph?searchtype=author&query=Dav%C3%A9%2C+R">R. Dav茅</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">A. Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+C">C. Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</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="1903.11082v2-abstract-short" style="display: inline;"> We present a Bayesian full-spectral-fitting analysis of 75 massive ($M_* > 10^{10.3} M_\odot$) UVJ-selected galaxies at redshifts of $1.0 < z < 1.3$, combining extremely deep rest-frame ultraviolet spectroscopy from VANDELS with multi-wavelength photometry. By the use of a sophisticated physical plus systematic uncertainties model, constructed within the Bagpipes code, we place strong constraints… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.11082v2-abstract-full').style.display = 'inline'; document.getElementById('1903.11082v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.11082v2-abstract-full" style="display: none;"> We present a Bayesian full-spectral-fitting analysis of 75 massive ($M_* > 10^{10.3} M_\odot$) UVJ-selected galaxies at redshifts of $1.0 < z < 1.3$, combining extremely deep rest-frame ultraviolet spectroscopy from VANDELS with multi-wavelength photometry. By the use of a sophisticated physical plus systematic uncertainties model, constructed within the Bagpipes code, we place strong constraints on the star-formation histories (SFHs) of individual objects. We firstly constrain the stellar mass vs stellar age relationship, finding a steep trend towards earlier average formation with increasing stellar mass of $1.48^{+0.34}_{-0.39}$ Gyr per decade in mass, although this shows signs of flattening at $M_* > 10^{11} M_\odot$. We show that this is consistent with other spectroscopic studies from $0 < z < 2$. This relationship places strong constraints on the AGN-feedback models used in cosmological simulations. We demonstrate that, although the relationships predicted by Simba and IllustrisTNG agree well with observations at $z=0.1$, they are too shallow at $z=1$, predicting an evolution of $<0.5$ Gyr per decade in mass. Secondly, we consider the connections between green-valley, post-starburst and quiescent galaxies, using our inferred SFH shapes and the distributions of galaxy physical properties on the UVJ diagram. The majority of our lowest-mass galaxies ($M_* \sim 10^{10.5} M_\odot$) are consistent with formation in recent ($z<2$), intense starburst events, with timescales of $\lesssim500$ Myr. A second class of objects experience extended star-formation epochs before rapidly quenching, passing through both green-valley and post-starburst phases. The most massive galaxies in our sample are extreme systems: already old by $z=1$, they formed at $z\sim5$ and quenched by $z=3$. However, we find evidence for their continued evolution through both AGN and rejuvenated star-formation activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.11082v2-abstract-full').style.display = 'none'; document.getElementById('1903.11082v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 13 figures, MNRAS accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.11081">arXiv:1903.11081</a> <span> [<a href="https://arxiv.org/pdf/1903.11081">pdf</a>, <a href="https://arxiv.org/format/1903.11081">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/stz1402">10.1093/mnras/stz1402 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS survey: the stellar metallicities of star-forming galaxies at 2.5 < z < 5.0 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">R. J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">J. S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Khochfar%2C+S">S. Khochfar</a>, <a href="/search/astro-ph?searchtype=author&query=Dav%C3%A9%2C+R">R. Dav茅</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cirasuolo%2C+M">M. Cirasuolo</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J+P+U">J. P. U. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">F. Fontanot</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">A. Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">N. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hibon%2C+P">P. Hibon</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+D+J">D. J. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Shapley%2C+A+E">A. E. Shapley</a> , et al. (2 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="1903.11081v2-abstract-short" style="display: inline;"> We present the results of a study utilising ultra-deep, rest-frame UV, spectroscopy to quantify the relationship between stellar mass and stellar metallicity for 681 star-forming galaxies at $2.5<z<5.0$ ($\langle z \rangle = 3.5 \pm 0.6$) drawn from the VANDELS survey. Via a comparison with high-resolution stellar population models, we determine stellar metallicities for a set of composite spectra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.11081v2-abstract-full').style.display = 'inline'; document.getElementById('1903.11081v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.11081v2-abstract-full" style="display: none;"> We present the results of a study utilising ultra-deep, rest-frame UV, spectroscopy to quantify the relationship between stellar mass and stellar metallicity for 681 star-forming galaxies at $2.5<z<5.0$ ($\langle z \rangle = 3.5 \pm 0.6$) drawn from the VANDELS survey. Via a comparison with high-resolution stellar population models, we determine stellar metallicities for a set of composite spectra formed from subsamples selected by mass and redshift. Across the stellar mass range $8.5 < \mathrm{log}(\langle M_{\ast} \rangle/\rm{M}_{\odot}) < 10.2$ we find a strong correlation between stellar metallicity and stellar mass, with stellar metallicity monotonically increasing from $Z_{\ast}/\mathrm{Z}_{\odot} < 0.09$ at $\langle M_{\ast} \rangle = 3.2 \times 10^{8} \rm{M}_{\odot}$ to $Z_{\ast}/Z_{\odot} = 0.27$ at $\langle M_{\ast} \rangle = 1.7 \times 10^{10} \rm{M}_{\odot}$. In contrast, at a given stellar mass, we find no evidence for significant metallicity evolution across the redshift range of our sample. However, comparing our results to the $z=0$ stellar mass-metallicity relation, we find that the $\langle z \rangle = 3.5$ relation is consistent with being shifted to lower metallicities by $\simeq 0.6$ dex. Contrasting our derived stellar metallicities with estimates of gas-phase metallicities at similar redshifts, we find evidence for enhanced $\rm{O}/\rm{Fe}$ ratios of the order (O/Fe) $\gtrsim 1.8$ $\times$ (O/Fe)$_{\odot}$. Finally, by comparing our results to simulation predictions, we find that the $\langle z \rangle = 3.5$ stellar mass-metallicity relation is consistent with current predictions for how outflow strength scales with galaxy mass. This conclusion is supported by an analysis of analytic models, and suggests that the mass loading parameter ($畏=\dot{M}_{\mathrm{outflow}}/M_{\ast}$) scales as $畏\propto M_{\ast}^尾$ with $尾\simeq -0.4$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.11081v2-abstract-full').style.display = 'none'; document.getElementById('1903.11081v2-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 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages (+ appendix), 13 figures, MNRAS accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.08593">arXiv:1903.08593</a> <span> [<a href="https://arxiv.org/pdf/1903.08593">pdf</a>, <a href="https://arxiv.org/format/1903.08593">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/10.1051/0004-6361/201935495">10.1051/0004-6361/201935495 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS survey: the role of ISM and galaxy physical properties on the escape of Ly伪 emission in z $\sim$ 3.5 star-forming galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">N. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Charlot%2C+S">S. Charlot</a>, <a href="/search/astro-ph?searchtype=author&query=Chevallard%2C+J">J. Chevallard</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">F. Fontanot</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Hibon%2C+P">P. Hibon</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+D">D. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">R. J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">C. Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+A">A. Saxena</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="1903.08593v1-abstract-short" style="display: inline;"> We investigate the physical properties of a sample of 52 Ly伪 emitting galaxies in the VANDELS survey, with particular focus on the role of kinematics and neutral hydrogen column density in the escape and spatial distribution of Ly伪 photons. For these galaxies, we derive different physical properties and characterize the Ly伪 emission in terms of kinematics, EW, FWHM and spatial extension and then e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.08593v1-abstract-full').style.display = 'inline'; document.getElementById('1903.08593v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.08593v1-abstract-full" style="display: none;"> We investigate the physical properties of a sample of 52 Ly伪 emitting galaxies in the VANDELS survey, with particular focus on the role of kinematics and neutral hydrogen column density in the escape and spatial distribution of Ly伪 photons. For these galaxies, we derive different physical properties and characterize the Ly伪 emission in terms of kinematics, EW, FWHM and spatial extension and then estimate the velocity of the neutral outflowing gas. We reproduce some of the well known correlations between Ly伪 EW and stellar mass, dust extinction and UV \b{eta} slope, in the sense that the emission line appears brighter in lower mass, less dusty and bluer galaxies. We do not find any correlation with the SED-derived star formation rate, while we find that galaxies with brighter Ly伪 tend to be more compact both in UV and in Ly伪. Our data reveal a new interesting correlation between the Ly伪 velocity and the offset of the inter-stellar absorption lines with respect to the systemic redshift, in the sense that galaxies with larger inter-stellar medium (ISM) out-flow velocities show smaller Ly伪 velocity shifts. We interpret this relation in the context of the shell-model scenario, where the velocity of the ISM and the HI column density contribute together in determining the Ly伪 kinematics. In support to our interpretation, we observe that galaxies with high HI column densities have much more extended Ly伪 spatial profiles, a sign of increased scattering. However, we do not find any evidence that the HI column density is related to any other physical properties of the galaxies, although this might be due in part to the limited range of parameters that our sample spans. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.08593v1-abstract-full').style.display = 'none'; document.getElementById('1903.08593v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to 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 631, A19 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.01884">arXiv:1903.01884</a> <span> [<a href="https://arxiv.org/pdf/1903.01884">pdf</a>, <a href="https://arxiv.org/format/1903.01884">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/10.1051/0004-6361/201935400">10.1051/0004-6361/201935400 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The UV and Ly$伪$ Luminosity Functions of galaxies and the Star Formation Rate Density at the end of HI reionization from the VIMOS Ultra-Deep Survey (VUDS) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Khusanova%2C+Y">Y. Khusanova</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%A8vre%2C+O+L">O. Le F猫vre</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">P. Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">B. C. Lemaux</a>, <a href="/search/astro-ph?searchtype=author&query=Tasca%2C+L+A+M">L. A. M. Tasca</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+R">R. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+V+L">V. Le Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+D">D. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">R. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cassar%C3%A0%2C+L+P">L. P. Cassar脿</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Ilbert%2C+O">O. Ilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pforr%2C+J">J. Pforr</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+B">B. Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a> , et al. (3 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="1903.01884v1-abstract-short" style="display: inline;"> We establish a robust statistical description of the star-forming galaxy population at the end of cosmic HI reionization ($5.0\le{}z\le6.6$) from a large sample of 52 galaxies with spectroscopically confirmed redshifts from the VIMOS UltraDeep Survey. We identify galaxies with Ly$伪$ either in absorption or in emission, at variance with most spectroscopic samples in the literature where Ly$伪$ emitt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.01884v1-abstract-full').style.display = 'inline'; document.getElementById('1903.01884v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.01884v1-abstract-full" style="display: none;"> We establish a robust statistical description of the star-forming galaxy population at the end of cosmic HI reionization ($5.0\le{}z\le6.6$) from a large sample of 52 galaxies with spectroscopically confirmed redshifts from the VIMOS UltraDeep Survey. We identify galaxies with Ly$伪$ either in absorption or in emission, at variance with most spectroscopic samples in the literature where Ly$伪$ emitters dominate. We find that star-forming galaxies at these redshifts are distributed along a main sequence in the stellar mass vs. SFR plane. We report a flat evolution of the sSFR(z) in 3<z<6 compared to lower redshift measurements. UV-continuum slopes vary with luminosity, with a large dispersion. We determing UV and Ly$伪$ luminosity functions using V$_{max}$ method and use them to derive star formation rate densities (SFRD). We find that both UV-derived and Ly$伪$-derived SFRDs are in excellent agreement after correcting Ly$伪$ luminosity density for IGM absorption. Our new SFRD measurements at a mean redshift z=5.6 confirm the steep decline of the SFRD at z>2. The bright end of the Ly$伪$ luminosity function has a high number density, indicating a significant star formation activity concentrated in the brightest Ly$伪$ emitters (LAE) at these redshifts. LAE with EW>25脜~contribute to about 75\% of the total UV-derived SFRD. While our analysis favors a low dust content in 5.0<z<6.6, uncertainties on the dust extinction correction and associated degeneracies in spectral fitting will remain an issue to estimate the total SFRD until future survey extending spectroscopy to the NIR rest-frame spectral domain, e.g. with JWST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.01884v1-abstract-full').style.display = 'none'; document.getElementById('1903.01884v1-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 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, submitted to 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 634, A97 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.01847">arXiv:1808.01847</a> <span> [<a href="https://arxiv.org/pdf/1808.01847">pdf</a>, <a href="https://arxiv.org/format/1808.01847">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/10.1051/0004-6361/201732465">10.1051/0004-6361/201732465 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CANDELSz7: a large spectroscopic survey of CANDELS galaxies in the reionization epoch </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=De+Barros%2C+S">S. De Barros</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">M. Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S">S. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">A. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Tilvi%2C+V">V. Tilvi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1808.01847v1-abstract-short" style="display: inline;"> We present the results of CANDELSz7, an ESO large program aimed at confirming spectroscopically a homogeneous sample of z~6 and z~7 star forming galaxies. The candidates were selected in the GOODS-South, UDS and COSMOS fields using the official CANDELS catalogs based on H160-band detections. Standard color criteria, which were tailored depending on the ancillary multi-wavelength data available for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.01847v1-abstract-full').style.display = 'inline'; document.getElementById('1808.01847v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.01847v1-abstract-full" style="display: none;"> We present the results of CANDELSz7, an ESO large program aimed at confirming spectroscopically a homogeneous sample of z~6 and z~7 star forming galaxies. The candidates were selected in the GOODS-South, UDS and COSMOS fields using the official CANDELS catalogs based on H160-band detections. Standard color criteria, which were tailored depending on the ancillary multi-wavelength data available for each field, were applied to select more than 160 candidate galaxies at z~6 and z~7. Deep medium resolution FORS2 spectroscopic observations were then conducted with integration times ranging from 12 to 20 hours, to reach a Lyalpha flux limit of approximately 1-3x 10-18 erg/s/cm^2 at 3sigma. For about 40% of the galaxies we could determine a spectroscopic redshift, mainly through the detection of a single emission line that we interpret as Lyalpha emission, or for some of the brightest objects (H160< 25.5) from the presence of faint continuum and sharp drop that we interpret as a Lyman break. In this paper we present the redshifts and main properties of 65 newly confirmed high redshift galaxies. Adding previous proprietary and archival data we assemble a sample of ~260 galaxies that we use to explore the evolution of the Lyalpha fraction in Lyman break galaxies and the change in the shape of the emission line between z~6 and z~7. We also discuss the accuracy of the CANDELS photometric redshifts in this redshift range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.01847v1-abstract-full').style.display = 'none'; document.getElementById('1808.01847v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.09277">arXiv:1807.09277</a> <span> [<a href="https://arxiv.org/pdf/1807.09277">pdf</a>, <a href="https://arxiv.org/ps/1807.09277">ps</a>, <a href="https://arxiv.org/format/1807.09277">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aad59b">10.3847/2041-8213/aad59b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic investigation of a reionized galaxy overdensity at z=7 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Dayal%2C+P">P. Dayal</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrara%2C+A">A. Ferrara</a>, <a href="/search/astro-ph?searchtype=author&query=Hutter%2C+A">A. Hutter</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Gallerani%2C+S">S. Gallerani</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">D. Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Pilo%2C+S">S. Pilo</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1807.09277v1-abstract-short" style="display: inline;"> We present deep spectroscopic follow-up observations of the Bremer Deep Field (BDF) where the two $z\sim$7 bright Ly$伪$ emitters (LAE) BDF521 and BDF3299 were previously discovered by Vanzella et al. (2011) and where a factor of $\sim$3-4 overdensity of faint LBGs has been found by Castellano et al. (2016). We confirm a new bright Ly$伪$ emitter, BDF2195, at the same redshift of BDF521, $z=7.008$,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.09277v1-abstract-full').style.display = 'inline'; document.getElementById('1807.09277v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.09277v1-abstract-full" style="display: none;"> We present deep spectroscopic follow-up observations of the Bremer Deep Field (BDF) where the two $z\sim$7 bright Ly$伪$ emitters (LAE) BDF521 and BDF3299 were previously discovered by Vanzella et al. (2011) and where a factor of $\sim$3-4 overdensity of faint LBGs has been found by Castellano et al. (2016). We confirm a new bright Ly$伪$ emitter, BDF2195, at the same redshift of BDF521, $z=7.008$, and at only $\sim$90 kpc physical distance from it, confirming that the BDF area is likely an overdense, reionized region. A quantitative assessment of the Ly$伪$ fraction shows that the number of detected bright emitters is much higher than the average found at z$\sim$7, suggesting a high Ly$伪$ transmission through the inter-galactic medium (IGM). However, the line visibility from fainter galaxies is at odds with this finding, since no Ly$伪$ emission is found in any of the observed candidates with $M_{UV}>$-20.25. This discrepancy can be understood either if some mechanism prevents Ly$伪$ emission from fainter galaxies within the ionized bubbles from reaching the observer, or if faint galaxies are located outside the reionized area and bright LAEs are solely responsible for the creation of their own HII regions. A thorough assessment of the nature of the BDF region and of its sources of re-ionizing radiation will be made possible by JWST spectroscopic capabilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.09277v1-abstract-full').style.display = 'none'; document.getElementById('1807.09277v1-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal Letters. 6 pages, 3 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/1806.01191">arXiv:1806.01191</a> <span> [<a href="https://arxiv.org/pdf/1806.01191">pdf</a>, <a href="https://arxiv.org/format/1806.01191">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/sty1996">10.1093/mnras/sty1996 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a radio galaxy at z = 5.72 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+A">A. Saxena</a>, <a href="/search/astro-ph?searchtype=author&query=Marinello%2C+M">M. Marinello</a>, <a href="/search/astro-ph?searchtype=author&query=Overzier%2C+R+A">R. A. Overzier</a>, <a href="/search/astro-ph?searchtype=author&query=Best%2C+P+N">P. N. Best</a>, <a href="/search/astro-ph?searchtype=author&query=Rottgering%2C+H+J+A">H. J. A Rottgering</a>, <a href="/search/astro-ph?searchtype=author&query=Duncan%2C+K+J">K. J. Duncan</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Magliocchetti%2C+M">M. Magliocchetti</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">D. Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Intema%2C+H+T">H. T. Intema</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G+K">G. K. Miley</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="1806.01191v2-abstract-short" style="display: inline;"> We report the discovery of the most distant radio galaxy to date, TGSS1530 at a redshift of $z=5.72$ close to the presumed end of the Epoch of Reionisation. The radio galaxy was selected from the TGSS ADR1 survey at 150 MHz for having to an ultra-steep spectral index, $伪^{\textrm{150 MHz}}_{\textrm{1.4 GHz}} = -1.4$ and a compact morphology obtained using VLA imaging at 1.4 GHz. No optical or infr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.01191v2-abstract-full').style.display = 'inline'; document.getElementById('1806.01191v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.01191v2-abstract-full" style="display: none;"> We report the discovery of the most distant radio galaxy to date, TGSS1530 at a redshift of $z=5.72$ close to the presumed end of the Epoch of Reionisation. The radio galaxy was selected from the TGSS ADR1 survey at 150 MHz for having to an ultra-steep spectral index, $伪^{\textrm{150 MHz}}_{\textrm{1.4 GHz}} = -1.4$ and a compact morphology obtained using VLA imaging at 1.4 GHz. No optical or infrared counterparts for it were found in publicly available sky surveys. Follow-up optical spectroscopy at the radio position using GMOS on Gemini North revealed the presence of a single emission line. We identify this line as Lyman alpha at $z=5.72$, because of its asymmetric line profile, the absence of other optical/UV lines in the spectrum and a high equivalent width. With a Ly$伪$ luminosity of $5.7 \times 10^{42}$ erg s$^{-1}$ and a FWHM of $370$ km s$^{-1}$, TGSS1530 is comparable to `non-radio' Lyman alpha emitters (LAEs) at a similar redshift. However, with a radio luminosity of $\log L_{\textrm{150 MHz}} = 29.1$ W Hz$^{-1}$ and a deconvolved physical size $3.5$ kpc, its radio properties are similar to other known radio galaxies at $z>4$. Subsequent $J$ and $K$ band imaging using LUCI on the Large Binocular Telescope resulted in non-detection of the host galaxy down to $3蟽$ limits of $J>24.4$ and $K>22.4$ (Vega). The $K$ band limit is consistent with $z>5$ from the $K-z$ relation for radio galaxies, suggesting stellar mass limits using simple stellar population models of $M_{\textrm{stars}}< 10^{10.5}$ $M_\odot$. Its high redshift coupled with relatively small radio and Ly$伪$ sizes suggest that TGSS1530 may be a radio galaxy in an early phase of its evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.01191v2-abstract-full').style.display = 'none'; document.getElementById('1806.01191v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures. Latest published version 10 October 2018</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2018, Monthly Notices of the Royal Astronomical Society, Volume 480, Issue 2, p.2733-2742 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.07414">arXiv:1803.07414</a> <span> [<a href="https://arxiv.org/pdf/1803.07414">pdf</a>, <a href="https://arxiv.org/format/1803.07414">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/sty1213">10.1093/mnras/sty1213 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS ESO public spectroscopic survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">R. J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">J. S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cirasuolo%2C+M">M. Cirasuolo</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=De+Barros%2C+S">S. De Barros</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">F. Fontanot</a>, <a href="/search/astro-ph?searchtype=author&query=Franzetti%2C+P">P. Franzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Fumana%2C+M">M. Fumana</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">A. Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W+G">W. G. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Iovino%2C+A">A. Iovino</a> , et al. (70 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="1803.07414v2-abstract-short" style="display: inline;"> VANDELS is a uniquely-deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO's Very Large Telescope (VLT). The survey has obtained ultra-deep optical (0.48 < lambda < 1.0 micron) spectroscopy of ~2100 galaxies within the redshift interval 1.0 < z < 7.0, over a total area of ~0.2 sq. degrees centred on the CANDELS UDS and CDFS fields. Based on accurate photometric re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.07414v2-abstract-full').style.display = 'inline'; document.getElementById('1803.07414v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.07414v2-abstract-full" style="display: none;"> VANDELS is a uniquely-deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO's Very Large Telescope (VLT). The survey has obtained ultra-deep optical (0.48 < lambda < 1.0 micron) spectroscopy of ~2100 galaxies within the redshift interval 1.0 < z < 7.0, over a total area of ~0.2 sq. degrees centred on the CANDELS UDS and CDFS fields. Based on accurate photometric redshift pre-selection, 85% of the galaxies targeted by VANDELS were selected to be at z>=3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < t_int < 80 hours), the VANDELS survey targeted: a) bright star-forming galaxies at 2.4 < z < 5.5, b) massive quiescent galaxies at 1.0 < z < 2.5, c) fainter star-forming galaxies at 3.0 < z < 7.0 and d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multi-wavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design and target selection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.07414v2-abstract-full').style.display = 'none'; document.getElementById('1803.07414v2-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 9 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/1803.07373">arXiv:1803.07373</a> <span> [<a href="https://arxiv.org/pdf/1803.07373">pdf</a>, <a href="https://arxiv.org/format/1803.07373">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/10.1051/0004-6361/201833047">10.1051/0004-6361/201833047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS ESO public spectroscopic survey: observations and first data release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+R+J+M+B">R. J. McLure B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Franzetti%2C+P">P. Franzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Iovino%2C+A">A. Iovino</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cirasuolo%2C+M">M. Cirasuolo</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=DeBarros%2C+S">S. DeBarros</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">J. S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S">S. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">F. Fontanot</a>, <a href="/search/astro-ph?searchtype=author&query=Fumana%2C+M">M. Fumana</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">A. Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W">W. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</a> , et al. (71 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="1803.07373v1-abstract-short" style="display: inline;"> This paper describes the observations and the first data release (DR1) of the ESO public spectroscopic survey "VANDELS, a deep VIMOS survey of the CANDELS CDFS and UDS fields". VANDELS' main targets are star-forming galaxies at 2.4<z<5.5 and massive passive galaxies at 1<z<2.5. By adopting a strategy of ultra-long exposure times, from 20 to 80 hours per source, VANDELS is designed to be the deepes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.07373v1-abstract-full').style.display = 'inline'; document.getElementById('1803.07373v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.07373v1-abstract-full" style="display: none;"> This paper describes the observations and the first data release (DR1) of the ESO public spectroscopic survey "VANDELS, a deep VIMOS survey of the CANDELS CDFS and UDS fields". VANDELS' main targets are star-forming galaxies at 2.4<z<5.5 and massive passive galaxies at 1<z<2.5. By adopting a strategy of ultra-long exposure times, from 20 to 80 hours per source, VANDELS is designed to be the deepest ever spectroscopic survey of the high-redshift Universe. Exploiting the red sensitivity of the VIMOS spectrograph, the survey has obtained ultra-deep spectra covering the wavelength 4800-10000 A with sufficient signal-to-noise to investigate the astrophysics of high-redshift galaxy evolution via detailed absorption line studies. The VANDELS-DR1 is the release of all spectra obtained during the first season of observations and includes data for galaxies for which the total (or half of the total) scheduled integration time was completed. The release contains 879 individual objects with a measured redshift and includes fully wavelength and flux-calibrated 1D spectra, the associated error spectra, sky spectra and wavelength-calibrated 2D spectra. We also provide a catalog with the essential galaxy parameters, including spectroscopic redshifts and redshift quality flags. In this paper we present the survey layout and observations, the data reduction and redshift measurement procedure and the general properties of the VANDELS-DR1 sample. We also discuss the spectroscopic redshift distribution, the accuracy of the photometric redshifts and we provide some examples of data products. All VANDELS-DR1 data are publicly available and can be retrieved from the ESO archive. Two further data releases are foreseen in the next 2 years with a final release scheduled for June 2020 which will include improved re-reduction of the entire spectroscopic data set. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.07373v1-abstract-full').style.display = 'none'; document.getElementById('1803.07373v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to 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/1712.01292">arXiv:1712.01292</a> <span> [<a href="https://arxiv.org/pdf/1712.01292">pdf</a>, <a href="https://arxiv.org/format/1712.01292">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/sty469">10.1093/mnras/sty469 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VANDELS survey: Dust attenuation in star-forming galaxies at $\mathbf{z=3-4}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">R. J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Khochfar%2C+S">S. Khochfar</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">J. S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Vecchia%2C+C+D">C. Dalla Vecchia</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Bourne%2C+N">N. Bourne</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cirasuolo%2C+M">M. Cirasuolo</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J+P+U">J. P. U. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">A. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</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="1712.01292v2-abstract-short" style="display: inline;"> We present the results of a new study of dust attenuation at redshifts $3 < z < 4$ based on a sample of $236$ star-forming galaxies from the VANDELS spectroscopic survey. Motivated by results from the First Billion Years (FiBY) simulation project, we argue that the intrinsic spectral energy distributions (SEDs) of star-forming galaxies at these redshifts have a self-similar shape across the mass r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.01292v2-abstract-full').style.display = 'inline'; document.getElementById('1712.01292v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.01292v2-abstract-full" style="display: none;"> We present the results of a new study of dust attenuation at redshifts $3 < z < 4$ based on a sample of $236$ star-forming galaxies from the VANDELS spectroscopic survey. Motivated by results from the First Billion Years (FiBY) simulation project, we argue that the intrinsic spectral energy distributions (SEDs) of star-forming galaxies at these redshifts have a self-similar shape across the mass range $8.2 \leq$ log$(M_{\star}/M_{\odot}) \leq 10.6$ probed by our sample. Using FiBY data, we construct a set of intrinsic SED templates which incorporate both detailed star formation and chemical abundance histories, and a variety of stellar population synthesis (SPS) model assumptions. With this set of intrinsic SEDs, we present a novel approach for directly recovering the shape and normalization of the dust attenuation curve. We find, across all of the intrinsic templates considered, that the average attenuation curve for star-forming galaxies at $z\simeq3.5$ is similar in shape to the commonly-adopted Calzetti starburst law, with an average total-to-selective attenuation ratio of $R_{V}=4.18\pm0.29$. We show that the optical attenuation ($A_V$) versus stellar mass ($M_{\star}$) relation predicted using our method is consistent with recent ALMA observations of galaxies at $2<z<3$ in the \emph{Hubble} \emph{Ultra} \emph{Deep} \emph{Field} (HUDF), as well as empirical $A_V - M_{\star}$ relations predicted by a Calzetti-like law. Our results, combined with other literature data, suggest that the $A_V - M_{\star}$ relation does not evolve over the redshift range $0<z<5$, at least for galaxies with log$(M_{\star}/M_{\odot}) \gtrsim 9.5$. Finally, we present tentative evidence which suggests that the attenuation curve may become steeper at log$(M_{\star}/M_{\odot}) \lesssim 9.0$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.01292v2-abstract-full').style.display = 'none'; document.getElementById('1712.01292v2-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 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 12 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/1710.10715">arXiv:1710.10715</a> <span> [<a href="https://arxiv.org/pdf/1710.10715">pdf</a>, <a href="https://arxiv.org/ps/1710.10715">ps</a>, <a href="https://arxiv.org/format/1710.10715">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/10.1051/0004-6361/201732197">10.1051/0004-6361/201732197 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VIMOS Ultra-Deep Survey: evidence for AGN feedback in galaxies with CIII]-$位$1908脜~emission 10.8 to 12.5 Gyr ago </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=F%C3%A8vre%2C+O+L">O. Le F猫vre</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">B. C. Lemaux</a>, <a href="/search/astro-ph?searchtype=author&query=Nakajima%2C+K">K. Nakajima</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">P. Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+D">D. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Tasca%2C+L+A+M">L. A. M. Tasca</a>, <a href="/search/astro-ph?searchtype=author&query=Zucca%2C+E">E. Zucca</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Vergani%2C+D">D. Vergani</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J">J. Dunlop</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1710.10715v1-abstract-short" style="display: inline;"> We analyze the CIII]-1908脜emission properties in a sample of 3899 star-forming galaxies (SFGs) at 2<z<3.8 from the VIMOS Ultra-Deep Survey (VUDS). We find a median EW(CIII])=2.0$\pm$0.2 to 2.2$\pm$0.2脜~for the SFG population at 2<z<3 and 3<z<4, resp. About 24% of SFGs are showing EW(CIII])>3脜, including 20% with 3<EW(CIII])<10脜~and 4% with strong emission EW(CIII])>10脜. A significant fraction of 1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.10715v1-abstract-full').style.display = 'inline'; document.getElementById('1710.10715v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.10715v1-abstract-full" style="display: none;"> We analyze the CIII]-1908脜emission properties in a sample of 3899 star-forming galaxies (SFGs) at 2<z<3.8 from the VIMOS Ultra-Deep Survey (VUDS). We find a median EW(CIII])=2.0$\pm$0.2 to 2.2$\pm$0.2脜~for the SFG population at 2<z<3 and 3<z<4, resp. About 24% of SFGs are showing EW(CIII])>3脜, including 20% with 3<EW(CIII])<10脜~and 4% with strong emission EW(CIII])>10脜. A significant fraction of 1.2% of SFGs presents strong CIII] emission 20<EW(CIII])<40脜. This makes CIII] the second most-frequent emission line in the UV-rest spectra of SFGs after Lyman-$伪$. We find a large dispersion in the weak EW(CIII]) - EW(Ly伪) correlation, with galaxies showing strong CIII] and no Ly$伪$, and vice-versa. SFGs with 10<EW(CIII])<0脜~present strong emission lines including CIV-1549, HeII-1640, OIII-1664, but also weaker emission of highly ionized elements SiIV-1403, NIV-1485, NIII-1750, or SiIII-1888, indicating a hard radiation field. We present a broad range of observational evidence supporting the presence of AGN in the strong CIII] emitting population. As EW(CIII]) is rising, we identify powerful outflows with velocities up to 1014 km/s. The strongest CIII] emitters are preferentially located below the SFGs main sequence, with the SFR reduced by x2. In addition, the median stellar age of the strongest emitters is ~0.8 Gyr, three times that of galaxies with EW(CIII])<10脜. Spectral line analysis presented in a joint paper by Nakajima et al. (2017) confirms that the strongest emitters require an AGN. We conclude that these properties are indicative of AGN feedback in SFGs at 2<z<3.8, contributing to star-formation quenching. We find that quenching timescales of 0.25-0.5x10^9 years are necessary for such AGN feedback to turn part of the star-forming galaxy population with Mstar>10^10 MSun at z~3 into the population of quiescent galaxies observed at redshift z~1-2. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.10715v1-abstract-full').style.display = 'none'; document.getElementById('1710.10715v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 14 figures, submitted to 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 625, A51 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.10184">arXiv:1710.10184</a> <span> [<a href="https://arxiv.org/pdf/1710.10184">pdf</a>, <a href="https://arxiv.org/format/1710.10184">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/10.1051/0004-6361/201732133">10.1051/0004-6361/201732133 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ly$伪$-Lyman Continuum connection in 3.5 < z < 4.3 star-forming galaxies from the VUDS survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Verhamme%2C+A">A. Verhamme</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+B">B. Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%A8vre%2C+O+L">O. Le F猫vre</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">P. Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Durkalec%2C+A">A. Durkalec</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">B. C. Lemaux</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+D">D. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Zucca%2C+E">E. Zucca</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1710.10184v2-abstract-short" style="display: inline;"> To identify the galaxies responsible for the reionization of the Universe, we must rely on the investigation of the Lyman Continuum (LyC) properties of z<5 star-forming galaxies, where we can still directly observe their ionizing radiation. We selected a sample of 201 star-forming galaxies from the Vimos Ultra Deep Survey at 3.5<z<4.3 to explore the validity of some of the proposed indirect indica… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.10184v2-abstract-full').style.display = 'inline'; document.getElementById('1710.10184v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.10184v2-abstract-full" style="display: none;"> To identify the galaxies responsible for the reionization of the Universe, we must rely on the investigation of the Lyman Continuum (LyC) properties of z<5 star-forming galaxies, where we can still directly observe their ionizing radiation. We selected a sample of 201 star-forming galaxies from the Vimos Ultra Deep Survey at 3.5<z<4.3 to explore the validity of some of the proposed indirect indicators of LyC radiation. We created subsamples of galaxies with EWLya>70脜, Lya(ext)<5.7kpc, rUV<0.3kpc and |Dv Lya|<200km/s, stacked all the galaxies in each subsample and measured the flux density ratio fnu(895)/fnu(1470), that we consider to be a proxy for LyC emission. We compared these ratios to those obtained for the complementary samples. We find that the stacks of galaxies which are UV compact (rUV<0.3kpc) and have bright Lya emission (EWLya>70脜), have much higher LyC fluxes compared to the rest of the galaxy population in agreement with theoretical studies and previous observational works. We also find that galaxies with low Lya(ext) have the highest LyC flux: this new correlation seems even stronger than the correlations with high EWLya and small rUV. These results assume that the stacks from all the subsamples present the same statistical contamination from lower redshift interlopers. If we subtract a statistical contamination from low redshift interlopers obtained with dedicated Monte Carlo simulations, from the flux density ratios (fnu(895)/fnu(1470)) of the significant subsamples we find that these samples contain real LyC leaking flux with a very high probability, but the true average escape fractions remain uncertain. Our work indicates that galaxies with very high EWLya, small Lya(ext) and small rUV are very likely the best candidates to show LyC radiation at z=4 and could therefore be the galaxies that contributed more to reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.10184v2-abstract-full').style.display = 'none'; document.getElementById('1710.10184v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by 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 614, A11 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.01443">arXiv:1707.01443</a> <span> [<a href="https://arxiv.org/pdf/1707.01443">pdf</a>, <a href="https://arxiv.org/format/1707.01443">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/10.1051/0004-6361/201730603">10.1051/0004-6361/201730603 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VIMOS Ultra Deep Survey: The role of HI kinematics and HI column density on the escape of Lyalpha photons in star-forming galaxies at 2<z<4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Verhamme%2C+A">A. Verhamme</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">P. Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">B. C. Lemaux</a>, <a href="/search/astro-ph?searchtype=author&query=Orlitova%2C+I">I. Orlitova</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+B">B. Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+V+L">V. Le Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Fevre%2C+O+L">O. Le Fevre</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+D">D. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Tasca%2C+L+A+M">L. A. M. Tasca</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+R">R. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Zucca%2C+E">E. Zucca</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">A. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.01443v1-abstract-short" style="display: inline;"> We selected a sample of 76 Lya emitting galaxies from the VIMOS Ultra Deep Survey (VUDS) at 2<z<4. We estimated the velocity of the neutral gas flowing out of the interstellar medium as the velocity offset, Deltav, between the systemic redshift (zsys) and the center of low-ionization absorption line systems (LIS). To increase the SN of VUDS spectra, we stacked subsamples. We measured the systemic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01443v1-abstract-full').style.display = 'inline'; document.getElementById('1707.01443v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.01443v1-abstract-full" style="display: none;"> We selected a sample of 76 Lya emitting galaxies from the VIMOS Ultra Deep Survey (VUDS) at 2<z<4. We estimated the velocity of the neutral gas flowing out of the interstellar medium as the velocity offset, Deltav, between the systemic redshift (zsys) and the center of low-ionization absorption line systems (LIS). To increase the SN of VUDS spectra, we stacked subsamples. We measured the systemic redshift from the rest-frame UV spectroscopic data using the CIII]1908 nebular emission line, and we considered SiII1526 as the highest signal-to-noise LIS line. We calculated the Lya peak shift with respect to the zsys, the EW(Lya), and the Lya spatial extension, Ext(Lya-C), from the profiles in the 2D stacked spectra. The galaxies that are faint in the rest-frame UV continuum, strong in Lya and CIII], with compact UV morphology, and localized in an underdense environment are characterized by outflow velocities of the order of a few hundreds of km/sec. The subsamples with smaller Deltav are characterized by larger Lya peak shifts, larger Ext(Lya-C), and smaller EW(Lya). In general we find that EW(Lya) anti-correlates with Ext(Lya-C) and Lya peak shift. We interpret these trends using a radiative-transfer shell model. The model predicts that an HI gas with a column density larger than 10^20/cm^2 is able to produce Lya peak shifts larger than >300km/sec. An ISM with this value of NHI would favour a large amount of scattering events, especially when the medium is static, so it can explain large values of Ext(Lya-C) and small EW(Lya). On the contrary, an ISM with a lower NHI, but large velocity outflows would lead to a Lya spatial profile peaked at the galaxy center (i.e. low values of Ext(Lya-C)) and to a large EW(Lya), as we see in our data. Our results and their interpretation via radiative-transfer models tell us that it is possible to use Lya to study the properties of the HI gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01443v1-abstract-full').style.display = 'none'; document.getElementById('1707.01443v1-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 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted on May 2017</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.00354">arXiv:1703.00354</a> <span> [<a href="https://arxiv.org/pdf/1703.00354">pdf</a>, <a href="https://arxiv.org/ps/1703.00354">ps</a>, <a href="https://arxiv.org/format/1703.00354">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/10.1051/0004-6361/201730447">10.1051/0004-6361/201730447 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Lyman Continuum escape fraction of faint galaxies at z~3.3 in the CANDELS/GOODS-North, EGS, and COSMOS fields with LBC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">D. Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Boutsia%2C+K">K. Boutsia</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">R. A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">R. A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">S. H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Ashcraft%2C+T+A">T. A. Ashcraft</a>, <a href="/search/astro-ph?searchtype=author&query=Scarlata%2C+C">C. Scarlata</a>, <a href="/search/astro-ph?searchtype=author&query=Rutkowski%2C+M+J">M. J. Rutkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">H. C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">A. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pedichini%2C+F">F. Pedichini</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a> , et al. (19 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="1703.00354v1-abstract-short" style="display: inline;"> The reionization of the Universe is one of the most important topics of present day astrophysical research. The most plausible candidates for the reionization process are star-forming galaxies, which according to the predictions of the majority of the theoretical and semi-analytical models should dominate the HI ionizing background at z~3. We aim at measuring the Lyman continuum escape fraction, w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.00354v1-abstract-full').style.display = 'inline'; document.getElementById('1703.00354v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.00354v1-abstract-full" style="display: none;"> The reionization of the Universe is one of the most important topics of present day astrophysical research. The most plausible candidates for the reionization process are star-forming galaxies, which according to the predictions of the majority of the theoretical and semi-analytical models should dominate the HI ionizing background at z~3. We aim at measuring the Lyman continuum escape fraction, which is one of the key parameters to compute the contribution of star-forming galaxies to the UV background. We have used ultra-deep U-band imaging (U=30.2mag at 1sigma) by LBC/LBT in the CANDELS/GOODS-North field, as well as deep imaging in COSMOS and EGS fields, in order to estimate the Lyman continuum escape fraction of 69 star-forming galaxies with secure spectroscopic redshifts at 3.27<z<3.40 to faint magnitude limits (L=0.2L*, or equivalently M1500~-19). We have measured through stacks a stringent upper limit (<1.7% at 1sigma) for the relative escape fraction of HI ionizing photons from bright galaxies (L>L*), while for the faint population (L=0.2L*) the limit to the escape fraction is ~10%. We have computed the contribution of star-forming galaxies to the observed UV background at z~3 and we have found that it is not enough to keep the Universe ionized at these redshifts, unless their escape fraction increases significantly (>10%) at low luminosities (M1500>-19). We compare our results on the Lyman continuum escape fraction of high-z galaxies with recent estimates in the literature and discuss future prospects to shed light on the end of the Dark Ages. In the future, strong gravitational lensing will be fundamental to measure the Lyman continuum escape fraction down to faint magnitudes (M1500~-16) which are inaccessible with the present instrumentation on blank fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.00354v1-abstract-full').style.display = 'none'; document.getElementById('1703.00354v1-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 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 16 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 602, A18 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.05882">arXiv:1611.05882</a> <span> [<a href="https://arxiv.org/pdf/1611.05882">pdf</a>, <a href="https://arxiv.org/format/1611.05882">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/10.1051/0004-6361/201630054">10.1051/0004-6361/201630054 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New constraints on the average escape fraction of Lyman continuum radiation in z~4 galaxies from the VIMOS Ultra Deep Survey (VUDS) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Guaita%2C+L">L. Guaita</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+B">B. Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">B. C. Lemaux</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Fevre%2C+O+L">O. Le Fevre</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+D">D. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">P. Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+V+L">V. Le Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Tasca%2C+L+A+M">L. A. M. Tasca</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+R">R. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Zucca%2C+E">E. Zucca</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1611.05882v2-abstract-short" style="display: inline;"> Determining the average fraction of Lyman continuum (LyC) photons escaping high redshift galaxies is essential for understanding how reionization proceeded in the z>6 Universe. We want to measure the LyC signal from a sample of sources in the Chandra Deep Field South (CDFS) and COSMOS fields for which ultra-deep VIMOS spectroscopy as well as multi-wavelength Hubble Space Telescope (HST) imaging ar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.05882v2-abstract-full').style.display = 'inline'; document.getElementById('1611.05882v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.05882v2-abstract-full" style="display: none;"> Determining the average fraction of Lyman continuum (LyC) photons escaping high redshift galaxies is essential for understanding how reionization proceeded in the z>6 Universe. We want to measure the LyC signal from a sample of sources in the Chandra Deep Field South (CDFS) and COSMOS fields for which ultra-deep VIMOS spectroscopy as well as multi-wavelength Hubble Space Telescope (HST) imaging are available. We select a sample of 46 galaxies at $z\sim 4$ from the VIMOS Ultra Deep Survey (VUDS) database, such that the VUDS spectra contain the LyC part of the spectra, that is, the rest-frame range $880-910脜$. Taking advantage of the HST imaging, we apply a careful cleaning procedure and reject all the sources showing nearby clumps with different colours, that could potentially be lower-redshift interlopers. After this procedure, the sample is reduced to 33 galaxies. We measure the ratio between ionizing flux (LyC at $895脜$) and non-ionizing emission (at $\sim 1500 脜$) for all individual sources. We also produce a normalized stacked spectrum of all sources. Assuming an intrinsic average $L_谓(1470)/L_谓(895)$ of 3, we estimate the individual and average relative escape fraction. We do not detect ionizing radiation from any individual source, although we identify a possible LyC emitter with very high Ly$伪$ equivalent width (EW). From the stacked spectrum and assuming a mean transmissivity for the sample, we measure a relative escape fraction $f_{esc}^{rel}=0.09\pm0.04$. We also look for correlations between the limits in the LyC flux and source properties and find a tentative correlation between LyC flux and the EW of the Ly$伪$ emission line. Our results imply that the LyC flux emitted by $V=25-26$ star-forming galaxies at z$\sim$4 is at most very modest, in agreement with previous upper limits from studies based on broad and narrow band imaging. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.05882v2-abstract-full').style.display = 'none'; document.getElementById('1611.05882v2-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 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted by A&A updated fesc,rel value</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.00369">arXiv:1606.00369</a> <span> [<a href="https://arxiv.org/pdf/1606.00369">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> B.R.N.O. Contributions #39 Times of minima </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ho%C5%88kov%C3%A1%2C+K">K. Ho艌kov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Jury%C5%A1ek%2C+J">J. Jury拧ek</a>, <a href="/search/astro-ph?searchtype=author&query=Lehk%C3%BD%2C+M">M. Lehk媒</a>, <a href="/search/astro-ph?searchtype=author&query=%C5%A0melcer%2C+L">L. 艩melcer</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%C5%A1ek%2C+M">M. Ma拧ek</a>, <a href="/search/astro-ph?searchtype=author&query=Mazanec%2C+J">J. Mazanec</a>, <a href="/search/astro-ph?searchtype=author&query=Han%C5%BEl%2C+D">D. Han啪l</a>, <a href="/search/astro-ph?searchtype=author&query=Urban%C3%ADk%2C+M">M. Urban铆k</a>, <a href="/search/astro-ph?searchtype=author&query=Magris%2C+M">M. Magris</a>, <a href="/search/astro-ph?searchtype=author&query=Vra%C5%A1t%C3%A1k%2C+M">M. Vra拧t谩k</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Hlad%C3%ADk%2C+B">B. Hlad铆k</a>, <a href="/search/astro-ph?searchtype=author&query=Medulka%2C+T">T. Medulka</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%ADlek%2C+F">F. B铆lek</a>, <a href="/search/astro-ph?searchtype=author&query=Trnka%2C+J">J. Trnka</a>, <a href="/search/astro-ph?searchtype=author&query=Jacobsen%2C+J">J. Jacobsen</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%A1%C4%8Dek%2C+J">J. Ben谩膷ek</a>, <a href="/search/astro-ph?searchtype=author&query=Kuch%C5%A5%C3%A1k%2C+B">B. Kuch钮谩k</a>, <a href="/search/astro-ph?searchtype=author&query=Audejean%2C+M">M. Audejean</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%96gmen%2C+Y">Y. 脰gmen</a>, <a href="/search/astro-ph?searchtype=author&query=Z%C3%ADbar%2C+M">M. Z铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Fatka%2C+P">P. Fatka</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Poddan%C3%BD%2C+S">S. Poddan媒</a>, <a href="/search/astro-ph?searchtype=author&query=Quinones%2C+C">C. Quinones</a> , et al. (21 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="1606.00369v1-abstract-short" style="display: inline;"> This paper presents 1463 times of minima for 455 objects acquired by 46 members and cooperating observers of the Variable Star and Exoplanet Section of the Czech Astronomical Society (B.R.N.O. Observing project). Observations were carried out between October 2013 - September 2014. Some neglected southern eclipsing binaries and newly discovered stars by the observers of project B.R.N.O. are include… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.00369v1-abstract-full').style.display = 'inline'; document.getElementById('1606.00369v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.00369v1-abstract-full" style="display: none;"> This paper presents 1463 times of minima for 455 objects acquired by 46 members and cooperating observers of the Variable Star and Exoplanet Section of the Czech Astronomical Society (B.R.N.O. Observing project). Observations were carried out between October 2013 - September 2014. Some neglected southern eclipsing binaries and newly discovered stars by the observers of project B.R.N.O. are included in the list. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.00369v1-abstract-full').style.display = 'none'; document.getElementById('1606.00369v1-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in OEJV, 66 pages, 1 figure</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2015OEJV..168....1H </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.05949">arXiv:1602.05949</a> <span> [<a href="https://arxiv.org/pdf/1602.05949">pdf</a>, <a href="https://arxiv.org/format/1602.05949">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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/10.1103/PhysRevD.93.102003">10.1103/PhysRevD.93.102003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing the Strong Equivalence Principle with spacecraft ranging towards the nearby Lagrangian points </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">Giuseppe Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">Fabrizio De Marchi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1602.05949v2-abstract-short" style="display: inline;"> General relativity is supported by great experimental evidence. Yet there is a lot of interest in precisely setting its limits with on going and future experiments. A question to answer is about the validity of the Strong Equivalence Principle. Ground experiments and Lunar Laser Ranging have provided the best upper limit on the Nordtvedt parameter $蟽[畏]=4.4\times 10^{-4}$. With the future planetar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.05949v2-abstract-full').style.display = 'inline'; document.getElementById('1602.05949v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.05949v2-abstract-full" style="display: none;"> General relativity is supported by great experimental evidence. Yet there is a lot of interest in precisely setting its limits with on going and future experiments. A question to answer is about the validity of the Strong Equivalence Principle. Ground experiments and Lunar Laser Ranging have provided the best upper limit on the Nordtvedt parameter $蟽[畏]=4.4\times 10^{-4}$. With the future planetary mission BepiColombo, this parameter will be further improved by at least an order of magnitude. In this paper we envisage yet another possible testing environment with spacecraft ranging towards the nearby Sun-Earth collinear Lagrangian points. Neglecting errors in planetary masses and ephemerides, we forecast $蟽[畏]=6.4\,(2.0)\times10^{-4}$ (5 yr integration time) via ranging towards $L_1$ in a realistic (optimistic) scenario depending on current (future) range capabilities and knowledge of the Earth's ephemerides. A combined measurement, $L_1$+$L_2$, gives instead $4.8\,(1.7)\times10^{-4}$. In the optimistic scenario a single measurement of one year would be enough to reach $\approx3\times10^{-4}$. All figures are comparable with Lunar Laser Ranging, but worse than BepiColombo. Performances could be much improved if data were integrated over time and over the number of satellites flying around either of the two Lagrangian points. We point out that some systematics (gravitational perturbations of other planets or figure effects) are much more in control compared to other experiments. We do not advocate a specific mission to constrain the Strong Equivalence Principle, but we do suggest analysing ranging data of present and future spacecrafts flying around $L_1$/$L_2$ (one key mission is, for instance, LISA Pathfinder). This spacecraft ranging would be a new and complementary probe to constrain the Strong Equivalence Principle in space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.05949v2-abstract-full').style.display = 'none'; document.getElementById('1602.05949v2-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 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 2 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 93, 102003 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1306.4487">arXiv:1306.4487</a> <span> [<a href="https://arxiv.org/pdf/1306.4487">pdf</a>, <a href="https://arxiv.org/ps/1306.4487">ps</a>, <a href="https://arxiv.org/format/1306.4487">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> State space modelling and data analysis exercises in LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nofrarias%2C+M">M Nofrarias</a>, <a href="/search/astro-ph?searchtype=author&query=Antonucci%2C+F">F Antonucci</a>, <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Auger%2C+G">G Auger</a>, <a href="/search/astro-ph?searchtype=author&query=Benedetti%2C+M">M Benedetti</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Bogenstahl%2C+J">J Bogenstahl</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+N">N Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Caleno%2C+M">M Caleno</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+M">M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Aguilo%2C+M">M Diaz-Aguilo</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Dunbar%2C+N">N Dunbar</a>, <a href="/search/astro-ph?searchtype=author&query=Fauste%2C+J">J Fauste</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Fichter%2C+V+F+W">V Ferroni W Fichter</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E">E Fitzsimons</a> , et al. (61 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1306.4487v2-abstract-short" style="display: inline;"> LISA Pathfinder is a mission planned by the European Space Agency to test the key technologies that will allow the detection of gravitational waves in space. The instrument on-board, the LISA Technology package, will undergo an exhaustive campaign of calibrations and noise characterisation campaigns in order to fully describe the noise model. Data analysis plays an important role in the mission an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.4487v2-abstract-full').style.display = 'inline'; document.getElementById('1306.4487v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1306.4487v2-abstract-full" style="display: none;"> LISA Pathfinder is a mission planned by the European Space Agency to test the key technologies that will allow the detection of gravitational waves in space. The instrument on-board, the LISA Technology package, will undergo an exhaustive campaign of calibrations and noise characterisation campaigns in order to fully describe the noise model. Data analysis plays an important role in the mission and for that reason the data analysis team has been developing a toolbox which contains all the functionalities required during operations. In this contribution we give an overview of recent activities, focusing on the improvements in the modelling of the instrument and in the data analysis campaigns performed both with real and simulated data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.4487v2-abstract-full').style.display = 'none'; document.getElementById('1306.4487v2-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 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Plenary talk presented at the 9th International LISA Symposium, 21-25 May 2012, Paris</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2013ASPC..467..161N </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1202.5112">arXiv:1202.5112</a> <span> [<a href="https://arxiv.org/pdf/1202.5112">pdf</a>, <a href="https://arxiv.org/ps/1202.5112">ps</a>, <a href="https://arxiv.org/format/1202.5112">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/201118655">10.1051/0004-6361/201118655 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An HST search for planets in the lower Main Sequence of the globular cluster NGC 6397 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nascimbeni%2C+V">V. Nascimbeni</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F. De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. M. Rich</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="1202.5112v2-abstract-short" style="display: inline;"> Searches for planetary transits carried out in open and globular clusters have yielded to date only a handful of weak, unconfirmed candidates. These results have been interpreted either as being insignificant, or as evidence that the cluster chemical or dynamical environment inhibits the planetary formation or survival. Most campaigns were limited by small sample statistics or systematics from gro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.5112v2-abstract-full').style.display = 'inline'; document.getElementById('1202.5112v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.5112v2-abstract-full" style="display: none;"> Searches for planetary transits carried out in open and globular clusters have yielded to date only a handful of weak, unconfirmed candidates. These results have been interpreted either as being insignificant, or as evidence that the cluster chemical or dynamical environment inhibits the planetary formation or survival. Most campaigns were limited by small sample statistics or systematics from ground-based photometry. In this work we performed a search for transiting planets and variables in a deep stellar field of NGC 6397 imaged by HST-ACS for 126 orbits. We analyzed 5,078 light curves, including a pure sample of 2,215 cluster-member M0-M9 dwarfs. The light curves have been corrected for systematic trends and inspected with several tools. No high-significance planetary candidate is detected. We compared this null detection with the most recent results from Kepler, showing that no conclusive evidence of lower planet incidence can be drawn. However, a very small photometric jitter is measured for early-M cluster members (<~2 mmag on 98% of them), which may be worth targeting in the near future with more optimized campaigns. Twelve variable stars are reported for the first time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.5112v2-abstract-full').style.display = 'none'; document.getElementById('1202.5112v2-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 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </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, 6 figures, 1 table; accepted for publication in A&A on February 16, 2012. Typos corrected. One figure and a short final note added</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1108.0865">arXiv:1108.0865</a> <span> [<a href="https://arxiv.org/pdf/1108.0865">pdf</a>, <a href="https://arxiv.org/format/1108.0865">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Non-linear parameter estimation for the LTP experiment: analysis of an operational exercise </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G. Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F. De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Hueller%2C+M">M. Hueller</a>, <a href="/search/astro-ph?searchtype=author&query=Vitale%2C+S">S. Vitale</a>, <a href="/search/astro-ph?searchtype=author&query=Hewitson%2C+M">M. Hewitson</a>, <a href="/search/astro-ph?searchtype=author&query=Nofrarias%2C+M">M. Nofrarias</a>, <a href="/search/astro-ph?searchtype=author&query=Monsky%2C+A">A. Monsky</a>, <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Grynagier%2C+A">A. Grynagier</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Aguilo%2C+M">M. Diaz-Aguilo</a>, <a href="/search/astro-ph?searchtype=author&query=Plagnol%2C+E">E. Plagnol</a>, <a href="/search/astro-ph?searchtype=author&query=Rais%2C+B">B. Rais</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="1108.0865v1-abstract-short" style="display: inline;"> The precursor ESA mission LISA-Pathfinder, to be flown in 2013, aims at demonstrating the feasibility of the free-fall, necessary for LISA, the upcoming space-born gravitational wave observatory. LISA Technology Package (LTP) is planned to carry out a number of experiments, whose main targets are to identify and measure the disturbances on each test-mass, in order to reach an unprecedented low-lev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1108.0865v1-abstract-full').style.display = 'inline'; document.getElementById('1108.0865v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1108.0865v1-abstract-full" style="display: none;"> The precursor ESA mission LISA-Pathfinder, to be flown in 2013, aims at demonstrating the feasibility of the free-fall, necessary for LISA, the upcoming space-born gravitational wave observatory. LISA Technology Package (LTP) is planned to carry out a number of experiments, whose main targets are to identify and measure the disturbances on each test-mass, in order to reach an unprecedented low-level residual force noise. To fulfill this plan, it is then necessary to correctly design, set-up and optimize the experiments to be performed on-flight and do a full system parameter estimation. Here we describe the progress on the non-linear analysis using the methods developed in the framework of the \textit{LTPDA Toolbox}, an object-oriented MATLAB Data Analysis environment: the effort is to identify the critical parameters and remove the degeneracy by properly combining the results of different experiments coming from a closed-loop system like LTP. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1108.0865v1-abstract-full').style.display = 'none'; document.getElementById('1108.0865v1-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 August, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 2 figures, 1 table, Proceedings of the 8th International LISA Symposium</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1108.0862">arXiv:1108.0862</a> <span> [<a href="https://arxiv.org/pdf/1108.0862">pdf</a>, <a href="https://arxiv.org/format/1108.0862">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.85.122004">10.1103/PhysRevD.85.122004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Time domain maximum likelihood parameter estimation in LISA Pathfinder Data Analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G. Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Hueller%2C+M">M. Hueller</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F. De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Vitale%2C+S">S. Vitale</a>, <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Hewitson%2C+M">M. Hewitson</a>, <a href="/search/astro-ph?searchtype=author&query=Nofrarias%2C+M">M. Nofrarias</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="1108.0862v1-abstract-short" style="display: inline;"> LISA is the upcoming space-based Gravitational Wave telescope. LISA Pathfinder, to be launched in the coming years, will prove and verify the detection principle of the fundamental Doppler link of LISA on a flight hardware identical in design to that of LISA. LISA Pathfinder will collect a picture of all noise disturbances possibly affecting LISA, achieving the unprecedented pureness of geodesic m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1108.0862v1-abstract-full').style.display = 'inline'; document.getElementById('1108.0862v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1108.0862v1-abstract-full" style="display: none;"> LISA is the upcoming space-based Gravitational Wave telescope. LISA Pathfinder, to be launched in the coming years, will prove and verify the detection principle of the fundamental Doppler link of LISA on a flight hardware identical in design to that of LISA. LISA Pathfinder will collect a picture of all noise disturbances possibly affecting LISA, achieving the unprecedented pureness of geodesic motion necessary for the detection of gravitational waves. The first steps of both missions will crucially depend on a very precise calibration of the key system parameters. Moreover, robust parameters estimation is of fundamental importance in the correct assessment of the residual force noise, an essential part of the data processing for LISA. In this paper we present a maximum likelihood parameter estimation technique in time domain being devised for this calibration and show its proficiency on simulated data and validation through Monte Carlo realizations of independent noise runs. We discuss its robustness to non-standard scenarios possibly arising during the real-life mission, as well as its independence to the initial guess and non-gaussianities. Furthermore, we apply the same technique to data produced in mission-like fashion during operational exercises with a realistic simulator provided by ESA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1108.0862v1-abstract-full').style.display = 'none'; document.getElementById('1108.0862v1-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 August, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages (two columns), 15 figures, 5 tables, submitted to Phys. Rev. D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 85, 122004 (2012) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1012.5968">arXiv:1012.5968</a> <span> [<a href="https://arxiv.org/pdf/1012.5968">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0264-9381/28/9/094002">10.1088/0264-9381/28/9/094002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> From laboratory experiments to LISA Pathfinder: achieving LISA geodesic motion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Antonucci%2C+F">F Antonucci</a>, <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Auger%2C+G">G Auger</a>, <a href="/search/astro-ph?searchtype=author&query=Benedetti%2C+M">M Benedetti</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Boatella%2C+C">C Boatella</a>, <a href="/search/astro-ph?searchtype=author&query=Bogenstahl%2C+J">J Bogenstahl</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Bosetti%2C+P">P Bosetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+N">N Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Caleno%2C+M">M Caleno</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesa%2C+M">M Cesa</a>, <a href="/search/astro-ph?searchtype=author&query=Chmeissani%2C+M">M Chmeissani</a>, <a href="/search/astro-ph?searchtype=author&query=Ciani%2C+G">G Ciani</a>, <a href="/search/astro-ph?searchtype=author&query=Conchillo%2C+A">A Conchillo</a>, <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=Cristofolini%2C+I">I Cristofolini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+M">M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Aguilo%2C+M">M Diaz-Aguilo</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G Dixon</a> , et al. (76 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="1012.5968v3-abstract-short" style="display: inline;"> This paper presents a quantitative assessment of the performance of the upcoming LISA Pathfinder geodesic explorer mission. The findings are based on the results of extensive ground testing and simulation campaigns using flight hardware and flight control and operations algorithms. The results show that, for the central experiment of measuring the stray differential acceleration between the LISA t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1012.5968v3-abstract-full').style.display = 'inline'; document.getElementById('1012.5968v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1012.5968v3-abstract-full" style="display: none;"> This paper presents a quantitative assessment of the performance of the upcoming LISA Pathfinder geodesic explorer mission. The findings are based on the results of extensive ground testing and simulation campaigns using flight hardware and flight control and operations algorithms. The results show that, for the central experiment of measuring the stray differential acceleration between the LISA test masses, LISA Pathfinder will be able to verify the overall acceleration noise to within a factor two of the LISA requirement at 1 mHz and within a factor 6 at 0.1 mHz. We also discuss the key elements of the physical model of disturbances, coming from LISA Pathfinder and ground measurement, that will guarantee the LISA performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1012.5968v3-abstract-full').style.display = 'none'; document.getElementById('1012.5968v3-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 January, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 December, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings of the 8th LISA Symposium. To appear Class. Quantum Grav. 28 (2011)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1002.0489">arXiv:1002.0489</a> <span> [<a href="https://arxiv.org/pdf/1002.0489">pdf</a>, <a href="https://arxiv.org/format/1002.0489">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10569-010-9256-8">10.1007/s10569-010-9256-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Effects of Interplanetary Dust on the LISA drag-free Constellation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cerdonio%2C+M">Massimo Cerdonio</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">Fabrizio De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=De+Pietri%2C+R">Roberto De Pietri</a>, <a href="/search/astro-ph?searchtype=author&query=Jetzer%2C+P">Philippe Jetzer</a>, <a href="/search/astro-ph?searchtype=author&query=Marzari%2C+F">Francesco Marzari</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzolo%2C+G">Giulio Mazzolo</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolan%2C+A">Antonello Ortolan</a>, <a href="/search/astro-ph?searchtype=author&query=Sereno%2C+M">Mauro Sereno</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="1002.0489v1-abstract-short" style="display: inline;"> The analysis of non-radiative sources of static or time-dependent gravitational fields in the Solar System is crucial to accurately estimate the free-fall orbits of the LISA space mission. In particular, we take into account the gravitational effects of Interplanetary Dust (ID) on the spacecraft trajectories. The perturbing gravitational field has been calculated for some ID density distribution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.0489v1-abstract-full').style.display = 'inline'; document.getElementById('1002.0489v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1002.0489v1-abstract-full" style="display: none;"> The analysis of non-radiative sources of static or time-dependent gravitational fields in the Solar System is crucial to accurately estimate the free-fall orbits of the LISA space mission. In particular, we take into account the gravitational effects of Interplanetary Dust (ID) on the spacecraft trajectories. The perturbing gravitational field has been calculated for some ID density distributions that fit the observed zodiacal light. Then we integrated the Gauss planetary equations to get the deviations from the LISA keplerian orbits around the Sun. This analysis can be eventually extended to Local Dark Matter (LDM), as gravitational fields are expected to be similar for ID and LDM distributions. Under some strong assumptions on the displacement noise at very low frequency, the Doppler data collected during the whole LISA mission could provide upper limits on ID and LDM densities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.0489v1-abstract-full').style.display = 'none'; document.getElementById('1002.0489v1-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 February, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 figures, to be published on the special issue of "Celestial Mechanics and Dynamical Astronomy" on the CELMEC V conference</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0912.2286">arXiv:0912.2286</a> <span> [<a href="https://arxiv.org/pdf/0912.2286">pdf</a>, <a href="https://arxiv.org/format/0912.2286">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/200912563">10.1051/0004-6361/200912563 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The first search for variable stars in the open cluster NGC 6253 and its surrounding field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">Fabrizio De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Poretti%2C+E">Ennio Poretti</a>, <a href="/search/astro-ph?searchtype=author&query=Montalto%2C+M">Marco Montalto</a>, <a href="/search/astro-ph?searchtype=author&query=Desidera%2C+S">Silvano Desidera</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">Giampaolo Piotto</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="0912.2286v1-abstract-short" style="display: inline;"> This work presents the first high-precision variability survey in the field of the intermediate-age, metal--rich open cluster NGC 6253. Clusters of this type are benchmarks for stellar evolution models. Continuous photometric monitoring of the cluster and its surrounding field was performed over a time span of ten nights using the Wide Field Imager mounted at the ESO-MPI 2.2m telescope. High-qua… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.2286v1-abstract-full').style.display = 'inline'; document.getElementById('0912.2286v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0912.2286v1-abstract-full" style="display: none;"> This work presents the first high-precision variability survey in the field of the intermediate-age, metal--rich open cluster NGC 6253. Clusters of this type are benchmarks for stellar evolution models. Continuous photometric monitoring of the cluster and its surrounding field was performed over a time span of ten nights using the Wide Field Imager mounted at the ESO-MPI 2.2m telescope. High-quality timeseries, each composed of about 800 datapoints, were obtained for 250,000 stars using ISIS and DAOPHOT packages. Candidate members were selected by using the colour-magnitude diagrams and period-luminosity-colour relations. Membership probabilities based on the proper motions were also used. The membership of all the variables discovered within a radius of 8 arcmin from the centre is discussed by comparing the incidence of the classes in the cluster direction and in the surrounding field. We discovered 595 variables and we also characterized most of them providing their variability classes, periods, and amplitudes. The sample is complete for short periods: we classified 20 pulsating variables, 225 contact systems, 99 eclipsing systems (22 Beta Lyr type, 59 Beta Per type, 18 RS CVn type), and 77 rotational variables. The time-baseline hampered the precise characterization of 173 variables with periods longer than 4-5 days. Moreover, we found a cataclysmic system undergoing an outburst of about 2.5 mag. We propose a list of 35 variable stars (8 contact systems, 2 eclipsing systems, 15 rotational variables, 9 long-period variables and the cataclysmic variable) as probable members of NGC 6253. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.2286v1-abstract-full').style.display = 'none'; document.getElementById('0912.2286v1-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 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2009. </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">Astronomy and Astrophysics, in press. Extended version with tables and light curves</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0907.5148">arXiv:0907.5148</a> <span> [<a href="https://arxiv.org/pdf/0907.5148">pdf</a>, <a href="https://arxiv.org/ps/0907.5148">ps</a>, <a href="https://arxiv.org/format/0907.5148">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/10.1051/0004-6361/200810708">10.1051/0004-6361/200810708 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BVRIJHK photometry and proper motion analysis of NGC 6253 and the surrounding field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montalto%2C+M">M. Montalto</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/astro-ph?searchtype=author&query=Platais%2C+I">I. Platais</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Momany%2C+Y">Y. Momany</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F. De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</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="0907.5148v1-abstract-short" style="display: inline;"> Context. We present a photometric and astrometric catalog of 187963 stars located in the field around the old super-metal-rich Galactic open cluster NGC 6253. The total field-of-view covered by the catalog is 34' x 33'. In this field, we provide CCD BVRI photometry. For a smaller region close to the cluster's center, we also provide near-infrared JHK photometry. Aims. We analyze the properties o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.5148v1-abstract-full').style.display = 'inline'; document.getElementById('0907.5148v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.5148v1-abstract-full" style="display: none;"> Context. We present a photometric and astrometric catalog of 187963 stars located in the field around the old super-metal-rich Galactic open cluster NGC 6253. The total field-of-view covered by the catalog is 34' x 33'. In this field, we provide CCD BVRI photometry. For a smaller region close to the cluster's center, we also provide near-infrared JHK photometry. Aims. We analyze the properties of NGC 6253 by using our new photometric data and astrometric membership. Methods. In June 2004, we targeted the cluster during a 10 day multi-site campaign, which involved the MPG/ESO 2.2m telescope with its wide-field imager and the Anglo-Australian 3.9m telescope, equipped with the IRIS2 near-infrared imager. Archival CCD images of NGC 6253 were used to derive relative proper motions and to calculate the cluster membership probabilities. Results. We have refined the cluster's fundamental parameters, deriving (V_0-M_v)=11.15, E(B - V)=0.15, E(V - I)=0.25, E(V - J)=0.50, and E(V - H)=0.55. The color excess ratios obtained using both the optical and near infrared colors indicate a normal reddening law in the direction of NGC 6253. The age of NGC 6253 at 3.5 Gyr, determined from our best-fitting isochrone appears to be slightly older than the previous estimates. Finally, we estimated the binary fraction among the cluster members to be \sim20%-30% and identified 11 blue straggler candidates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.5148v1-abstract-full').style.display = 'none'; document.getElementById('0907.5148v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 13 figures, 11 tables. Accepted for publication in A&A. Catalog avaiable via CDS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0706.2962">arXiv:0706.2962</a> <span> [<a href="https://arxiv.org/pdf/0706.2962">pdf</a>, <a href="https://arxiv.org/format/0706.2962">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1051/0004-6361:20077386">10.1051/0004-6361:20077386 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variable stars in the open cluster NGC 6791 and its surrounding field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F. De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/astro-ph?searchtype=author&query=Montalto%2C+M">M. Montalto</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferro%2C+A+A">A. Arellano Ferro</a>, <a href="/search/astro-ph?searchtype=author&query=Bruntt%2C+H">H. Bruntt</a>, <a href="/search/astro-ph?searchtype=author&query=Stetson%2C+P+B">P. B. Stetson</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="0706.2962v1-abstract-short" style="display: inline;"> Aims: This work presents a high--precision variability survey in the field of the old, super metal-rich open cluster NGC 6791. Methods: The data sample consists of more than 75,000 high-precision CCD time series measurements in the V band obtained mainly at the Canada-France-Hawaii Telescope, with additional data from S. Pedro Martir and Loiano observatories, over a time span of ten nights. Th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0706.2962v1-abstract-full').style.display = 'inline'; document.getElementById('0706.2962v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0706.2962v1-abstract-full" style="display: none;"> Aims: This work presents a high--precision variability survey in the field of the old, super metal-rich open cluster NGC 6791. Methods: The data sample consists of more than 75,000 high-precision CCD time series measurements in the V band obtained mainly at the Canada-France-Hawaii Telescope, with additional data from S. Pedro Martir and Loiano observatories, over a time span of ten nights. The field covers an area of 42x28 arcmin^2. Results: We have discovered 260 new variables and re-determined periods and amplitudes of 70 known variable stars. By means of a photometric evaluation of the membership in NGC 6791, and a preliminary membership based on the proper motions, we give a full description of the variable content of the cluster and surrounding field in the range 16<V<23.5. Accurate periods can be given for the variables with P<4.0 d, while for ones with longer periods the limited time-baseline hampered precise determinations. We categorized the entire sample as follows: 6 pulsating, 3 irregular, 3 cataclysmic, 89 rotational variables and 61 eclipsing systems; moreover, we detected 168 candidate variables for which we cannot give a variability class since their periods are much longer than our time baseline. Conclusions: On the basis of photometric considerations, and of the positions of the stars with respect to the center of the cluster, we inferred that 11 new variable stars are likely members of the cluster, for 22 stars the membership is doubtful and 137 are likely non-members. We also detected an outburst of about 3 mag in the light curve of a very faint blue star belonging to the cluster and we suggest that this star could be a new U Gem (dwarf nova) cataclysmic variable. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0706.2962v1-abstract-full').style.display = 'none'; document.getElementById('0706.2962v1-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 June, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2007. </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">24 pages, 19 Figures, A&A accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0704.1668">arXiv:0704.1668</a> <span> [<a href="https://arxiv.org/pdf/0704.1668">pdf</a>, <a href="https://arxiv.org/ps/0704.1668">ps</a>, <a href="https://arxiv.org/format/0704.1668">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1051/0004-6361:20066199">10.1051/0004-6361:20066199 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new search for planet transits in NGC 6791 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montalto%2C+M">M. Montalto</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F. De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bruntt%2C+H">H. Bruntt</a>, <a href="/search/astro-ph?searchtype=author&query=Stetson%2C+P+B">P. B. Stetson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferro%2C+A+A">A. Arellano Ferro</a>, <a href="/search/astro-ph?searchtype=author&query=Momany%2C+Y">Y. Momany</a>, <a href="/search/astro-ph?searchtype=author&query=Gratton%2C+R+G">R. G. Gratton</a>, <a href="/search/astro-ph?searchtype=author&query=Poretti%2C+E">E. Poretti</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Barbieri%2C+M">M. Barbieri</a>, <a href="/search/astro-ph?searchtype=author&query=Claudi%2C+R+U">R. U. Claudi</a>, <a href="/search/astro-ph?searchtype=author&query=Grundahl%2C+G">G. Grundahl</a>, <a href="/search/astro-ph?searchtype=author&query=Rosenberg%2C+A">A. Rosenberg</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="0704.1668v1-abstract-short" style="display: inline;"> Context. Searching for planets in open clusters allows us to study the effects of dynamical environment on planet formation and evolution. Aims. Considering the strong dependence of planet frequency on stellar metallicity, we studied the metal rich old open cluster NGC 6791 and searched for close-in planets using the transit technique. Methods. A ten-night observational campaign was performe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0704.1668v1-abstract-full').style.display = 'inline'; document.getElementById('0704.1668v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0704.1668v1-abstract-full" style="display: none;"> Context. Searching for planets in open clusters allows us to study the effects of dynamical environment on planet formation and evolution. Aims. Considering the strong dependence of planet frequency on stellar metallicity, we studied the metal rich old open cluster NGC 6791 and searched for close-in planets using the transit technique. Methods. A ten-night observational campaign was performed using the Canada-France-Hawaii Telescope (3.6m), the San Pedro M谩rtir telescope (2.1m), and the Loiano telescope (1.5m). To increase the transit detection probability we also made use of the Bruntt et al. (2003) eight-nights observational campaign. Adequate photometric precision for the detection of planetary transits was achieved. Results. Should the frequency and properties of close-in planets in NGC 6791 be similar to those orbiting field stars of similar metallicity, then detailed simulations foresee the presence of 2-3 transiting planets. Instead, we do not confirm the transit candidates proposed by Bruntt et al. (2003). The probability that the null detection is simply due to chance coincidence is estimated to be 3%-10%, depending on the metallicity assumed for the cluster. Conclusions. Possible explanations of the null-detection of transits include: (i) a lower frequency of close-in planets in star clusters; (ii) a smaller planetary radius for planets orbiting super metal rich stars; or (iii) limitations in the basic assumptions. More extensive photometry with 3-4m class telescopes is required to allow conclusive inferences about the frequency of planets in NGC 6791. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0704.1668v1-abstract-full').style.display = 'none'; document.getElementById('0704.1668v1-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 April, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2007. </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, 23 figures, A&A accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0608464">arXiv:astro-ph/0608464</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0608464">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0608464">ps</a>, <a href="https://arxiv.org/format/astro-ph/0608464">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1051/0004-6361:20064898">10.1051/0004-6361:20064898 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search and analysis of blue straggler stars in open clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+F">F. De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+M+B">M. B. Davies</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="astro-ph/0608464v1-abstract-short" style="display: inline;"> Aims: This paper presents a new homogeneous catalogue of blue straggler stars (BSS) in Galactic open clusters. Methods: Photometric data for 216 clusters were collected from the literature and 2782 BSS candidates were extracted from 76 of them. Results: We found that the anticorrelation of BSS frequency vs. total magnitude identified in similar studies conducted on Galactic globular clusters ext… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0608464v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0608464v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0608464v1-abstract-full" style="display: none;"> Aims: This paper presents a new homogeneous catalogue of blue straggler stars (BSS) in Galactic open clusters. Methods: Photometric data for 216 clusters were collected from the literature and 2782 BSS candidates were extracted from 76 of them. Results: We found that the anticorrelation of BSS frequency vs. total magnitude identified in similar studies conducted on Galactic globular clusters extends to the open cluster regime: clusters with smaller total magnitude tend to have higher BSS frequencies. Moreover, a clear correlation between the BSS frequency (obtained normalising the total number of BSS either to the total cluster mass or, for the older clusters, to the total number of clump stars) and the age of the clusters was found. A simple model is developed here to try to explain this last and new result. The model allows us to ascertain the important effect played by mass loss in the evolution of open clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0608464v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0608464v1-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, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2006. </p> </li> </ol> <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