Search | arXiv e-print repository

<!DOCTYPE html> <html lang="en"> <head> <meta charset="utf-8"/> <meta name="viewport" content="width=device-width, initial-scale=1"/>  <link rel="apple-touch-icon" sizes="180x180" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/apple-touch-icon.png"> <link rel="icon" type="image/png" sizes="32x32" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-32x32.png"> <link rel="icon" type="image/png" sizes="16x16" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-16x16.png"> <link rel="manifest" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/site.webmanifest"> <link rel="mask-icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/safari-pinned-tab.svg" color="#b31b1b"> <link rel="shortcut icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon.ico"> <meta name="msapplication-TileColor" content="#b31b1b"> <meta name="msapplication-config" content="images/icons/browserconfig.xml"> <meta name="theme-color" content="#b31b1b">  <title>Search | arXiv e-print repository</title> <script defer src="https://static.arxiv.org/static/base/1.0.0a5/fontawesome-free-5.11.2-web/js/all.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/base/1.0.0a5/css/arxivstyle.css" /> <script type="text/x-mathjax-config"> MathJax.Hub.Config({ messageStyle: "none", extensions: ["tex2jax.js"], jax: ["input/TeX", "output/HTML-CSS"], tex2jax: { inlineMath: [ ['$','$'], ["\$","\$"] ], displayMath: [ ['$$','$$'], ["\\[","\\]"] ], processEscapes: true, ignoreClass: '.*', processClass: 'mathjax.*' }, TeX: { extensions: ["AMSmath.js", "AMSsymbols.js", "noErrors.js"], noErrors: { inlineDelimiters: ["$","$"], multiLine: false, style: { "font-size": "normal", "border": "" } } }, "HTML-CSS": { availableFonts: ["TeX"] } }); </script> <script src='//static.arxiv.org/MathJax-2.7.3/MathJax.js'></script> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/notification.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/bulma-tooltip.min.css" /> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/search.css" /> <script src="https://code.jquery.com/jquery-3.2.1.slim.min.js" integrity="sha256-k2WSCIexGzOj3Euiig+TlR8gA0EmPjuc79OEeY5L45g=" crossorigin="anonymous"></script> <script src="https://static.arxiv.org/static/search/0.5.6/js/fieldset.js"></script> <style> radio#cf-customfield_11400 { display: none; } </style> </head> <body> <header><a href="#main-container" class="is-sr-only">Skip to main content</a>  <div class="attribution level is-marginless" role="banner"> <div class="level-left"> <a class="level-item" href="https://cornell.edu/"><img src="https://static.arxiv.org/static/base/1.0.0a5/images/cornell-reduced-white-SMALL.svg" alt="Cornell University" width="200" aria-label="logo" /></a> </div> <div class="level-right is-marginless"><p class="sponsors level-item is-marginless"><span id="support-ack-url">We gratefully acknowledge support from<br /> the Simons Foundation, <a href="https://info.arxiv.org/about/ourmembers.html">member institutions</a>, and all contributors. <a href="https://info.arxiv.org/about/donate.html">Donate</a></span></p></div> </div>  <div class="identity level is-marginless"> <div class="level-left"> <div class="level-item"> <a class="arxiv" href="https://arxiv.org/" aria-label="arxiv-logo"> <img src="https://static.arxiv.org/static/base/1.0.0a5/images/arxiv-logo-one-color-white.svg" aria-label="logo" alt="arxiv logo" width="85" style="width:85px;"/> </a> </div> </div> <div class="search-block level-right"> <form class="level-item mini-search" method="GET" action="https://arxiv.org/search"> <div class="field has-addons"> <div class="control"> <input class="input is-small" type="text" name="query" placeholder="Search..." aria-label="Search term or terms" /> <p class="help"><a href="https://info.arxiv.org/help">Help</a> | <a href="https://arxiv.org/search/advanced">Advanced Search</a></p> </div> <div class="control"> <div class="select is-small"> <select name="searchtype" aria-label="Field to search"> <option value="all" selected="selected">All fields</option> <option value="title">Title</option> <option value="author">Author</option> <option value="abstract">Abstract</option> <option value="comments">Comments</option> <option value="journal_ref">Journal reference</option> <option value="acm_class">ACM classification</option> <option value="msc_class">MSC classification</option> <option value="report_num">Report number</option> <option value="paper_id">arXiv identifier</option> <option value="doi">DOI</option> <option value="orcid">ORCID</option> <option value="author_id">arXiv author ID</option> <option value="help">Help pages</option> <option value="full_text">Full text</option> </select> </div> </div> <input type="hidden" name="source" value="header"> <button class="button is-small is-cul-darker">Search</button> </div> </form> </div> </div>  <div class="container"> <div class="user-tools is-size-7 has-text-right has-text-weight-bold" role="navigation" aria-label="User menu"> <a href="https://arxiv.org/login">Login</a> </div> </div> </header> <main class="container" id="main-container"> <div class="level is-marginless"> <div class="level-left"> <h1 class="title is-clearfix"> Showing 1–50 of 176 results for author: <span class="mathjax">Alfaro, J</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=Alfaro%2C+J">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="Alfaro, J"> </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=Alfaro%2C+J&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="Alfaro, J"> <ul id="abstracts"><li><input checked id="abstracts-0" name="abstracts" type="radio" value="show"> <label for="abstracts-0">Show abstracts</label></li><li><input id="abstracts-1" name="abstracts" type="radio" value="hide"> <label for="abstracts-1">Hide abstracts</label></li></ul> </div> <div class="box field is-grouped is-grouped-multiline level-item"> <div class="control"> <span class="select is-small"> <select id="size" name="size"><option value="25">25</option><option selected value="50">50</option><option value="100">100</option><option value="200">200</option></select> </span> <label for="size">results per page</label>. </div> <div class="control"> <label for="order">Sort results by</label> <span class="select is-small"> <select id="order" name="order"><option selected value="-announced_date_first">Announcement date (newest first)</option><option value="announced_date_first">Announcement date (oldest first)</option><option value="-submitted_date">Submission date (newest first)</option><option value="submitted_date">Submission date (oldest first)</option><option value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.07022">arXiv:2406.07022</a> <span> [<a href="https://arxiv.org/pdf/2406.07022">pdf</a>, <a href="https://arxiv.org/format/2406.07022">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: No sign of multiple stellar populations in open clusters from their sodium and oxygen abundances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Martell%2C+S">S. Martell</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvaisiene%2C+G">G. Tautvaisiene</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</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="2406.07022v2-abstract-short" style="display: inline;"> Context: The light element (anti-)correlations shown by globular clusters (GCs) are the main spectroscopic signature of multiple stellar populations. These internal abundance variations provide us with fundamental constraints on the formation mechanism of stellar clusters. Aims: Using Gaia-ESO, the largest and most homogeneous survey of open clusters (OCs), we intend to check whether these stellar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07022v2-abstract-full').style.display = 'inline'; document.getElementById('2406.07022v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.07022v2-abstract-full" style="display: none;"> Context: The light element (anti-)correlations shown by globular clusters (GCs) are the main spectroscopic signature of multiple stellar populations. These internal abundance variations provide us with fundamental constraints on the formation mechanism of stellar clusters. Aims: Using Gaia-ESO, the largest and most homogeneous survey of open clusters (OCs), we intend to check whether these stellar aggregates display the same patterns. Based on previous studies of many GCs, several young and massive clusters in the Magellanic Clouds, as well as a few OCs, we do not expect to find any anti-correlation, given the low mass of Milky Way OCs. Methods: We used the results based on UVES spectra of stars in Gaia-ESO to derive the distribution of Na and O abundances and seevwhether they show an unexplained dispersion or whether they are anti-correlated. By selecting only high-probability members with high-precision stellar parameters, we ended up with more than 700 stars in 74 OCs. We examined the O-Na distribution in 28 OCsvwith at least 4 stars available as well as the Na distribution in 24 OCs, with at least 10 stars available. Results: We find that the distribution of Na abundances is compatible with a single-value population, within the errors. The fewvapparent exceptions can be explained by differences in the evolutionary phase (main sequence and giant post first dredge-up episode) or by difficulties in analysing low gravity giants. We did not find any indication of an Na-O anti-correlation in any of the clusters for which O has been derived. Conclusions: Based on the very small spread we find, OCs maintain the status of single stellar populations. However, a definitive answer requires studying more elements and larger samples covering different evolutionary phases. This will be possible with the next generation of large surveys <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07022v2-abstract-full').style.display = 'none'; document.getElementById('2406.07022v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Based on the Gaia-ESO Survey. In press on Astronomy & Astrophysics. Figure A.2 updated</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.08859">arXiv:2404.08859</a> <span> [<a href="https://arxiv.org/pdf/2404.08859">pdf</a>, <a href="https://arxiv.org/format/2404.08859">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> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Calibrating the lithium-age relation with open clusters and associations. II. Expanded cluster sample and final membership selection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albarr%C3%A1n%2C+M+L+G">M. L. Guti茅rrez Albarr谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Tabernero%2C+H+M">H. M. Tabernero</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Marfil%2C+E">E. Marfil</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Klutsch%2C+A">A. Klutsch</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+A">A. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Feltzing%2C+S">S. Feltzing</a>, <a href="/search/astro-ph?searchtype=author&query=Fran%C3%A7ois%2C+P">P. Fran莽ois</a>, <a href="/search/astro-ph?searchtype=author&query=Esteban%2C+F+J">F. Jim茅nez Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.08859v1-abstract-short" style="display: inline;"> The Li abundance observed in pre-main sequence and main sequence late-type stars is strongly age-dependent, but also shows a complex pattern depending on several parameters, such as rotation, chromospheric activity and metallicity. The best way to calibrate these effects, with the aim of studying Li as an age indicator for FGK stars, is to calibrate coeval groups of stars, such as open clusters (O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08859v1-abstract-full').style.display = 'inline'; document.getElementById('2404.08859v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.08859v1-abstract-full" style="display: none;"> The Li abundance observed in pre-main sequence and main sequence late-type stars is strongly age-dependent, but also shows a complex pattern depending on several parameters, such as rotation, chromospheric activity and metallicity. The best way to calibrate these effects, with the aim of studying Li as an age indicator for FGK stars, is to calibrate coeval groups of stars, such as open clusters (OCs) and associations. We present a considerable target sample of 42 OCs and associations, ranging from 1 Myr to 5 Gyr, observed within the Gaia-ESO survey (GES), and using the latest data provided by GES iDR6 and the most recent release of Gaia that was then available, EDR3. As part of this study, we update and improve the membership analysis for all 20 OCs presented in our previous article. We perform detailed membership analyses for all target clusters to identify likely candidates, using all available parameters provided by GES and based on numerous criteria: from radial velocity distributions, to the astrometry and photometry provided by Gaia, to gravity indicators, [Fe/H] metallicity, and Li content. We obtain updated lists of cluster members for the whole target sample, as well as a selection of Li-rich giant contaminants obtained as an additional result of the membership process. Each selection of cluster candidates was thoroughly contrasted with numerous existing membership studies using data from Gaia to ensure the most robust results. These final cluster selections will be used in the third and last paper of this series, which reports the results of a comparative study characterising the observable Li dispersion in each cluster and analysing its dependence on several parameters, allowing us to calibrate a Li-age relation and obtain a series of empirical Li envelopes for key ages in our sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08859v1-abstract-full').style.display = 'none'; document.getElementById('2404.08859v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">83 pages, 246 figures. To be published in A&A, accepted January 27, 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.04857">arXiv:2403.04857</a> <span> [<a href="https://arxiv.org/pdf/2403.04857">pdf</a>, <a href="https://arxiv.org/format/2403.04857">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/07/047">10.1088/1475-7516/2024/07/047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dark Matter Line Searches with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/astro-ph?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Angel%2C+L">L. Angel</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arnesen%2C+T+T+H">T. T. H. Arnesen</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a> , et al. (540 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="2403.04857v2-abstract-short" style="display: inline;"> Monochromatic gamma-ray signals constitute a potential smoking gun signature for annihilating or decaying dark matter particles that could relatively easily be distinguished from astrophysical or instrumental backgrounds. We provide an updated assessment of the sensitivity of the Cherenkov Telescope Array (CTA) to such signals, based on observations of the Galactic centre region as well as of sele… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04857v2-abstract-full').style.display = 'inline'; document.getElementById('2403.04857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.04857v2-abstract-full" style="display: none;"> Monochromatic gamma-ray signals constitute a potential smoking gun signature for annihilating or decaying dark matter particles that could relatively easily be distinguished from astrophysical or instrumental backgrounds. We provide an updated assessment of the sensitivity of the Cherenkov Telescope Array (CTA) to such signals, based on observations of the Galactic centre region as well as of selected dwarf spheroidal galaxies. We find that current limits and detection prospects for dark matter masses above 300 GeV will be significantly improved, by up to an order of magnitude in the multi-TeV range. This demonstrates that CTA will set a new standard for gamma-ray astronomy also in this respect, as the world's largest and most sensitive high-energy gamma-ray observatory, in particular due to its exquisite energy resolution at TeV energies and the adopted observational strategy focussing on regions with large dark matter densities. Throughout our analysis, we use up-to-date instrument response functions, and we thoroughly model the effect of instrumental systematic uncertainties in our statistical treatment. We further present results for other potential signatures with sharp spectral features, e.g.~box-shaped spectra, that would likewise very clearly point to a particle dark matter origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04857v2-abstract-full').style.display = 'none'; document.getElementById('2403.04857v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages JCAP style (excluding author list and references), 19 figures; minor changes to match published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 07 (2024) 047 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.06076">arXiv:2402.06076</a> <span> [<a href="https://arxiv.org/pdf/2402.06076">pdf</a>, <a href="https://arxiv.org/format/2402.06076">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D+K">D. K. Feuillet</a>, <a href="/search/astro-ph?searchtype=author&query=Tabernero%2C+H+M">H. M. Tabernero</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">S. Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Mikolaitis%2C+%C5%A0">艩. Mikolaitis</a>, <a href="/search/astro-ph?searchtype=author&query=Lind%2C+K">K. Lind</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+A+R">A. R. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">P. Bonifacio</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Caffau%2C+E">E. Caffau</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Merle%2C+T">T. Merle</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Fran%C3%A7ois%2C+P">P. Fran莽ois</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a> , et al. (20 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="2402.06076v1-abstract-short" style="display: inline;"> The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted $10^5$ stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high ($R\sim47,000$) and GIRAFFE medium ($R\sim20,000$) resolution spectra. The analysis of the Gaia-ESO spectra was the work of mult… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.06076v1-abstract-full').style.display = 'inline'; document.getElementById('2402.06076v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.06076v1-abstract-full" style="display: none;"> The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted $10^5$ stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high ($R\sim47,000$) and GIRAFFE medium ($R\sim20,000$) resolution spectra. The analysis of the Gaia-ESO spectra was the work of multiple analysis teams (nodes) within five working groups (WG). The homogenisation of the stellar parameters within WG11 (high resolution observations of FGK stars) and the homogenisation of the stellar parameters within WG10 (medium resolution observations of FGK stars) is described here. In both cases, the homogenisation was carried out using a bayesian Inference method developed specifically for the Gaia-ESO Survey by WG11. The WG10 homogenisation primarily used the cross-match of stars with WG11 as the reference set in both the stellar parameter and chemical abundance homogenisation. In this way the WG10 homogenised results have been placed directly onto the WG11 stellar parameter and chemical abundance scales. The reference set for the metal-poor end was sparse which limited the effectiveness of the homogenisation in that regime. For WG11, the total number of stars for which stellar parameters were derived was 6,231 with typical uncertainties for Teff, log g and [Fe/H] of 32~K, 0.05 and 0.05 respectively. One or more chemical abundances out of a possible 39 elements were derived for 6,188 of the stars. For WG10, the total number of stars for which stellar parameters were derived was 76,675 with typical uncertainties for Teff, log g and [Fe/H] of 64~K, 0.15 and 0.07 respectively. One or more chemical abundances out of a possible 30 elements were derived for 64,177 of the stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.06076v1-abstract-full').style.display = 'none'; document.getElementById('2402.06076v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 19 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/2402.01315">arXiv:2402.01315</a> <span> [<a href="https://arxiv.org/pdf/2402.01315">pdf</a>, <a href="https://arxiv.org/format/2402.01315">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The evolution of lithium in FGK dwarf stars. Influence of planets and Galactic migration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Andr%C3%A9s%2C+F+L">F. Llorente de Andr茅s</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Reza%2C+R">R. de la Reza</a>, <a href="/search/astro-ph?searchtype=author&query=Cruz%2C+P">P. Cruz</a>, <a href="/search/astro-ph?searchtype=author&query=Cuenda-Mu%C3%B1oz%2C+D">D. Cuenda-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Chavero%2C+C">C. Chavero</a>, <a href="/search/astro-ph?searchtype=author&query=Cifuentes%2C+C">C. Cifuentes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.01315v1-abstract-short" style="display: inline;"> This work aims to investigate the behaviour of the lithium abundance in stars with and without detected planets. Our study is based on a sample of 1332 FGK main-sequence stars with measured lithium abundances, for 257 of which planets were detected. Our method reviews the sample statistics and is addressed specifically to the influence of tides and orbital decay, with special attention to planets… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.01315v1-abstract-full').style.display = 'inline'; document.getElementById('2402.01315v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.01315v1-abstract-full" style="display: none;"> This work aims to investigate the behaviour of the lithium abundance in stars with and without detected planets. Our study is based on a sample of 1332 FGK main-sequence stars with measured lithium abundances, for 257 of which planets were detected. Our method reviews the sample statistics and is addressed specifically to the influence of tides and orbital decay, with special attention to planets on close orbits, whose stellar rotational velocity is higher than the orbital period of the planet. In this case, tidal effects are much more pronounced. The analysis also covers the orbital decay on a short timescale, with planets spiralling into their parent star. Furthermore, the sample allows us to study the relation between the presence of planets and the physical properties of their host stars, such as the chromospheric activity, metallicity, and lithium abundance. In the case of a strong tidal influence, we cannot infer from any of the studies described that the behaviour of Li differs between stars that host planets and those that do not. Our sample includes stars with super-solar metallicity ([Fe/H]>0.15 dex) and a low lithium abundance (A(Li) <1.0 dex). This enabled us to analyse scenarios of the origin and existence of these stars. Considering the possible explanation of the F dip, we show that it is not a plausible scenario. Our analysis is based on a kinematic study and concludes that the possible time that elapsed in the travel from their birth places in the central regions of the Galaxy to their current positions in the solar neighbourhood is not enough to explain the high lithium depletion. It is remarkable that those of our high-metallicity low-lithium stars with the greatest eccentricity (e>0.2) are closest to the Galactic centre. A dedicated study of a set of high-metallicity low-Li stars is needed to test the migration-depletion scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.01315v1-abstract-full').style.display = 'none'; document.getElementById('2402.01315v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 9 figures, accepted for publication in A\&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.07413">arXiv:2310.07413</a> <span> [<a href="https://arxiv.org/pdf/2310.07413">pdf</a>, <a href="https://arxiv.org/format/2310.07413">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Chasing Gravitational Waves with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Green%2C+J+G">Jarred Gershon Green</a>, <a href="/search/astro-ph?searchtype=author&query=Carosi%2C+A">Alessandro Carosi</a>, <a href="/search/astro-ph?searchtype=author&query=Nava%2C+L">Lara Nava</a>, <a href="/search/astro-ph?searchtype=author&query=Patricelli%2C+B">Barbara Patricelli</a>, <a href="/search/astro-ph?searchtype=author&query=Sch%C3%BCssler%2C+F">Fabian Sch眉ssler</a>, <a href="/search/astro-ph?searchtype=author&query=Seglar-Arroyo%2C+M">Monica Seglar-Arroyo</a>, <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+C">Cta Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">Kazuki Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">Shotaro Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">Atreya Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">Remi Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">Arnau Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">Nuria Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">Rafael Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J">Jean-Philippe Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">Elena Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosino%2C+F">Filippo Ambrosino</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">Ekrem Oguzhan Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">Lucio Angelo Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">Cornelia Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">Luisa Arrabito</a> , et al. (545 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="2310.07413v3-abstract-short" style="display: inline;"> The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.07413v3-abstract-full').style.display = 'inline'; document.getElementById('2310.07413v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.07413v3-abstract-full" style="display: none;"> The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very-high-energy (VHE, > 100GeV) photons which have yet to be detected in coincidence with a gravitational wave signal. The Cherenkov Telescope Array (CTA) is a next-generation VHE observatory which aims to be indispensable in this search, with an unparalleled sensitivity and ability to slew anywhere on the sky within a few tens of seconds. New observing modes and follow-up strategies are being developed for CTA to rapidly cover localization areas of gravitational wave events that are typically larger than the CTA field of view. This work will evaluate and provide estimations on the expected number of of gravitational wave events that will be observable with CTA, considering both on- and off-axis emission. In addition, we will present and discuss the prospects of potential follow-up strategies with CTA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.07413v3-abstract-full').style.display = 'none'; document.getElementById('2310.07413v3-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Presented at the 38th International Cosmic Ray Conference (ICRC 2023), 2023 (arXiv:2309.08219)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> CTA-ICRC/2023/30 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03712">arXiv:2309.03712</a> <span> [<a href="https://arxiv.org/pdf/2309.03712">pdf</a>, <a href="https://arxiv.org/format/2309.03712">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-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/10.1088/1475-7516/2024/10/004">10.1088/1475-7516/2024/10/004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for $纬$-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Araya%2C+M">M. Araya</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a> , et al. (542 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="2309.03712v1-abstract-short" style="display: inline;"> Galaxy clusters are expected to be dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at gamma-ray energies and are predicted to be sources of large-scale gamma-ray emission due to hadronic interactions in the intracluster med… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03712v1-abstract-full').style.display = 'inline'; document.getElementById('2309.03712v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03712v1-abstract-full" style="display: none;"> Galaxy clusters are expected to be dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at gamma-ray energies and are predicted to be sources of large-scale gamma-ray emission due to hadronic interactions in the intracluster medium. We estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse gamma-ray emission from the Perseus galaxy cluster. We perform a detailed spatial and spectral modelling of the expected signal for the DM and the CRp components. For each, we compute the expected CTA sensitivity. The observing strategy of Perseus is also discussed. In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio within the radius $R_{500}$ down to about $X_{500}<3\times 10^{-3}$, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index $伪_{\rm CRp}=2.3$. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure $伪_{\rm CRp}$ down to about $螖伪_{\rm CRp}\simeq 0.1$ and the CRp spatial distribution with 10% precision. Regarding DM, CTA should improve the current ground-based gamma-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to $\sim 5$, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with $蟿_蠂>10^{27}$s for DM masses above 1 TeV. These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03712v1-abstract-full').style.display = 'none'; document.getElementById('2309.03712v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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">93 pages (including author list, appendix and references), 143 figures. Submitted to JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP10(2024)004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15007">arXiv:2303.15007</a> <span> [<a href="https://arxiv.org/pdf/2303.15007">pdf</a>, <a href="https://arxiv.org/format/2303.15007">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2023.102850">10.1016/j.astropartphys.2023.102850 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+%C3%81">N. 脕lvarez Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a> , et al. (334 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="2303.15007v1-abstract-short" style="display: inline;"> The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3~PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The pote… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15007v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15007v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15007v1-abstract-full" style="display: none;"> The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3~PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy $纬$-ray spectral signatures for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods for the identification of PeVatrons are introduced, and realistic Monte--Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a $纬$-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 hours of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations with $\mathcal{O}(100)$ hours of exposure per source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15007v1-abstract-full').style.display = 'none'; document.getElementById('2303.15007v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">34 pages, 16 figures, Accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.00366">arXiv:2302.00366</a> <span> [<a href="https://arxiv.org/pdf/2302.00366">pdf</a>, <a href="https://arxiv.org/ps/2302.00366">ps</a>, <a href="https://arxiv.org/format/2302.00366">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Image and Video Processing">eess.IV</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/stad2852">10.1093/mnras/stad2852 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CzSL: Learning from citizen science, experts and unlabelled data in astronomical image classification </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jimenez%2C+M">Manuel Jimenez</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Torres%2C+M+T">Mercedes Torres Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Triguero%2C+I">Isaac Triguero</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.00366v4-abstract-short" style="display: inline;"> Citizen science is gaining popularity as a valuable tool for labelling large collections of astronomical images by the general public. This is often achieved at the cost of poorer quality classifications made by amateur participants, which are usually verified by employing smaller data sets labelled by professional astronomers. Despite its success, citizen science alone will not be able to handle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00366v4-abstract-full').style.display = 'inline'; document.getElementById('2302.00366v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.00366v4-abstract-full" style="display: none;"> Citizen science is gaining popularity as a valuable tool for labelling large collections of astronomical images by the general public. This is often achieved at the cost of poorer quality classifications made by amateur participants, which are usually verified by employing smaller data sets labelled by professional astronomers. Despite its success, citizen science alone will not be able to handle the classification of current and upcoming surveys. To alleviate this issue, citizen science projects have been coupled with machine learning techniques in pursuit of a more robust automated classification. However, existing approaches have neglected the fact that, apart from the data labelled by amateurs, (limited) expert knowledge of the problem is also available along with vast amounts of unlabelled data that have not yet been exploited within a unified learning framework. This paper presents an innovative learning methodology for citizen science capable of taking advantage of expert- and amateur-labelled data, featuring a transfer of labels between experts and amateurs. The proposed approach first learns from unlabelled data with a convolutional autoencoder and then exploits amateur and expert labels via the pre-training and fine-tuning of a convolutional neural network, respectively. We focus on the classification of galaxy images from the Galaxy Zoo project, from which we test binary, multi-class, and imbalanced classification scenarios. The results demonstrate that our solution is able to improve classification performance compared to a set of baseline approaches, deploying a promising methodology for learning from different confidence levels in data labelling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00366v4-abstract-full').style.display = 'none'; document.getElementById('2302.00366v4-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 526(2), 2023, 1742 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.08310">arXiv:2301.08310</a> <span> [<a href="https://arxiv.org/pdf/2301.08310">pdf</a>, <a href="https://arxiv.org/format/2301.08310">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245335">10.1051/0004-6361/202245335 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia-ESO Survey: massive stars in the Carina Nebula. A new census of OB stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Berlanas%2C+S+R">S. R. Berlanas</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Dorda%2C+R">R. Dorda</a>, <a href="/search/astro-ph?searchtype=author&query=Comer%C3%B3n%2C+F">F. Comer贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Gosset%2C+E">E. Gosset</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Lera%2C+J+A+M">J. A. Molina Lera</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=Furst%2C+T">T. Furst</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Drew%2C+J+E">J. E. Drew</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Vink%2C+J+S">J. S. Vink</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.08310v2-abstract-short" style="display: inline;"> The Gaia-ESO survey sample of massive OB stars in the Carina Nebula consists of 234 stars. The addition of brighter sources from the Galactic O-Star Spectroscopic Survey and additional sources from the literature allows us to create the most complete census of massive OB stars done so far in the region. It contains a total of 316 stars, being 18 of them in the background and four in the foreground… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.08310v2-abstract-full').style.display = 'inline'; document.getElementById('2301.08310v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.08310v2-abstract-full" style="display: none;"> The Gaia-ESO survey sample of massive OB stars in the Carina Nebula consists of 234 stars. The addition of brighter sources from the Galactic O-Star Spectroscopic Survey and additional sources from the literature allows us to create the most complete census of massive OB stars done so far in the region. It contains a total of 316 stars, being 18 of them in the background and four in the foreground. Of the 294 stellar systems in Car OB1, 74 are of O type, 214 are of non-supergiant B type and 6 are of WR or non-O supergiant (II to Ia) spectral class. We identify 20 spectroscopic binary systems with an O-star primary, of which 6 are reported for the first time, and another 18 with a B-star primary, of which 13 are new detections. The average observed double-lined binary fraction of O-type stars in the surveyed region is 0.35, which represents a lower limit. We find a good correlation between the spectroscopic n-qualifier and the projected rotational velocity of the stars. The fraction of candidate runaways among the stars with and without the n-qualifier is 4.4% and 2.4%, respectively, although non resolved double-lined binaries can be contaminating the fast rotators sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.08310v2-abstract-full').style.display = 'none'; document.getElementById('2301.08310v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 62 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A20 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.03981">arXiv:2212.03981</a> <span> [<a href="https://arxiv.org/pdf/2212.03981">pdf</a>, <a href="https://arxiv.org/format/2212.03981">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad557">10.1093/mnras/stad557 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shoko Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Trager%2C+S+C">Scott C. Trager</a>, <a href="/search/astro-ph?searchtype=author&query=Dalton%2C+G+B">Gavin B. Dalton</a>, <a href="/search/astro-ph?searchtype=author&query=Aguerri%2C+J+A+L">J. Alfonso L. Aguerri</a>, <a href="/search/astro-ph?searchtype=author&query=Drew%2C+J+E">J. E. Drew</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">Jes煤s Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A4nsicke%2C+B+T">Boris T. G盲nsicke</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Iovino%2C+A">Angela Iovino</a>, <a href="/search/astro-ph?searchtype=author&query=Pieri%2C+M+M">Matthew M. Pieri</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B+M">Bianca M. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+J+B">D. J. B. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">Antonella Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Abrams%2C+D+C">Don Carlos Abrams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+D+S">David S. Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">Teresa Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=Arag%C3%B3n-Salamanca%2C+A">Alfonso Arag贸n-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Yago Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">Carine Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Balcells%2C+M">Marc Balcells</a>, <a href="/search/astro-ph?searchtype=author&query=Barrena%2C+R">R. Barrena</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+G">Giuseppina Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Belokurov%2C+V">Vasily Belokurov</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">Thomas Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">Piercarlo Bonifacio</a> , et al. (190 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="2212.03981v2-abstract-short" style="display: inline;"> WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrogr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03981v2-abstract-full').style.display = 'inline'; document.getElementById('2212.03981v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.03981v2-abstract-full" style="display: none;"> WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366$-$959\,nm at $R\sim5000$, or two shorter ranges at $R\sim20\,000$. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for $\sim$3 million stars and detailed abundances for $\sim1.5$ million brighter field and open-cluster stars; (ii) survey $\sim0.4$ million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey $\sim400$ neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in $z<0.5$ cluster galaxies; (vi) survey stellar populations and kinematics in $\sim25\,000$ field galaxies at $0.3\lesssim z \lesssim 0.7$; (vii) study the cosmic evolution of accretion and star formation using $>1$ million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at $z>2$. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03981v2-abstract-full').style.display = 'none'; document.getElementById('2212.03981v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">41 pages, 27 figures, accepted for publication by MNRAS; updated version including information on individual grants in a revised Acknowledgements section, corrections to the affiliation list, and an updated references list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.17133">arXiv:2210.17133</a> <span> [<a href="https://arxiv.org/pdf/2210.17133">pdf</a>, <a href="https://arxiv.org/format/2210.17133">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac3155">10.1093/mnras/stac3155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The miniJPAS survey: stellar atmospheric parameters from 56 optical filters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+H+-">H. -B. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+L">L. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Cruz%2C+P">P. Cruz</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F">F. Jim茅nez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Daflon%2C+S">S. Daflon</a>, <a href="/search/astro-ph?searchtype=author&query=Placco%2C+V+M">V. M. Placco</a>, <a href="/search/astro-ph?searchtype=author&query=Akras%2C+S">S. Akras</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Galarza%2C+C+A">C. Andr茅s Galarza</a>, <a href="/search/astro-ph?searchtype=author&query=Gon%C3%A7alves%2C+D+R">D. R. Gon莽alves</a>, <a href="/search/astro-ph?searchtype=author&query=Duan%2C+F+-">F. -Q. Duan</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+J+-">J. -F. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Laur%2C+J">J. Laur</a>, <a href="/search/astro-ph?searchtype=author&query=Solano%2C+E">E. Solano</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandes%2C+M+B">M. Borges Fernandes</a>, <a href="/search/astro-ph?searchtype=author&query=Cenarro%2C+A+J">A. J. Cenarro</a>, <a href="/search/astro-ph?searchtype=author&query=Mar%C3%ADn-Franch%2C+A">A. Mar铆n-Franch</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+J">J. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Sanjuan%2C+C">Carlos L贸pez-Sanjuan</a>, <a href="/search/astro-ph?searchtype=author&query=Abramo%2C+R">R. Abramo</a>, <a href="/search/astro-ph?searchtype=author&query=Alcaniz%2C+J">J. Alcaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+N">N. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Bonoli%2C+S">S. Bonoli</a>, <a href="/search/astro-ph?searchtype=author&query=Crist%C3%B3bal-Hornillos%2C+D">D. Crist贸bal-Hornillos</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.17133v1-abstract-short" style="display: inline;"> With a unique set of 54 overlapping narrow-band and two broader filters covering the entire optical range, the incoming Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will provide a great opportunity for stellar physics and near-field cosmology. In this work, we use the miniJPAS data in 56 J-PAS filters and 4 complementary SDSS-like filters to explore and prove the po… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.17133v1-abstract-full').style.display = 'inline'; document.getElementById('2210.17133v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.17133v1-abstract-full" style="display: none;"> With a unique set of 54 overlapping narrow-band and two broader filters covering the entire optical range, the incoming Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will provide a great opportunity for stellar physics and near-field cosmology. In this work, we use the miniJPAS data in 56 J-PAS filters and 4 complementary SDSS-like filters to explore and prove the potential of the J-PAS filter system in characterizing stars and deriving their atmospheric parameters. We obtain estimates for the effective temperature with a good precision (<150 K) from spectral energy distribution fitting. We have constructed the metallicity-dependent stellar loci in 59 colours for the miniJPAS FGK dwarf stars, after correcting certain systematic errors in flat-fielding. The very blue colours, including uJAVA-r, J0378-r, J0390-r, uJPAS-r, show the strongest metallicity dependence, around 0.25 mag/dex. The sensitivities decrease to about 0.1 mag/dex for the J0400-r, J0410-r, and J0420-r colours. The locus fitting residuals show peaks at the J0390, J0430, J0510, and J0520 filters, suggesting that individual elemental abundances such as [Ca/Fe], [C/Fe], and [Mg/Fe] can also be determined from the J-PAS photometry. Via stellar loci, we have achieved a typical metallicity precision of 0.1 dex. The miniJPAS filters also demonstrate strong potential in discriminating dwarfs and giants, particularly the J0520 and J0510 filters. Our results demonstrate the power of the J-PAS filter system in stellar parameter determinations and the huge potential of the coming J-PAS survey in stellar and Galactic studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.17133v1-abstract-full').style.display = 'none'; document.getElementById('2210.17133v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 16 figures, 3 tables, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.04721">arXiv:2210.04721</a> <span> [<a href="https://arxiv.org/pdf/2210.04721">pdf</a>, <a href="https://arxiv.org/format/2210.04721">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244854">10.1051/0004-6361/202244854 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Lithium measurements and new curves of growth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=de+Laverny%2C+P">P. de Laverny</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D+K">D. K. Feuillet</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Lind%2C+K">K. Lind</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Sanna%2C+N">N. Sanna</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">P. Bonifacio</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.04721v1-abstract-short" style="display: inline;"> The Gaia-ESO Survey (GES) is a large public spectroscopic survey that was carried out using the multi-object FLAMES spectrograph at the Very Large Telescope. The survey provides accurate radial velocities, stellar parameters, and elemental abundances for ~115,000 stars in all Milky Way components. In this paper we describe the method adopted in the final data release to derive lithium equivalent w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04721v1-abstract-full').style.display = 'inline'; document.getElementById('2210.04721v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.04721v1-abstract-full" style="display: none;"> The Gaia-ESO Survey (GES) is a large public spectroscopic survey that was carried out using the multi-object FLAMES spectrograph at the Very Large Telescope. The survey provides accurate radial velocities, stellar parameters, and elemental abundances for ~115,000 stars in all Milky Way components. In this paper we describe the method adopted in the final data release to derive lithium equivalent widths (EWs) and abundances. Lithium EWs were measured using two different approaches for FGK and M-type stars, to account for the intrinsic differences in the spectra. For FGK stars, we fitted the lithium line using Gaussian components, while direct integration over a predefined interval was adopted for M-type stars. Care was taken to ensure continuity between the two regimes. Abundances were derived using a new set of homogeneous curves of growth that were derived specifically for GES, and which were measured on a synthetic spectral grid consistently with the way the EWs were measured. The derived abundances were validated by comparison with those measured by other analysis groups using different methods. Lithium EWs were measured for ~40,000 stars, and abundances could be derived for ~38,000 of them. The vast majority of the measures (80%) have been obtained for stars in open cluster fields. The remaining objects are stars in globular clusters, or field stars in the Milky Way disc, bulge, and halo. The GES dataset of homogeneous lithium abundances described here will be valuable for our understanding of several processes, from stellar evolution and internal mixing in stars at different evolutionary stages to Galactic evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04721v1-abstract-full').style.display = 'none'; document.getElementById('2210.04721v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 15 figures. Accepted by Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A49 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.05432">arXiv:2208.05432</a> <span> [<a href="https://arxiv.org/pdf/2208.05432">pdf</a>, <a href="https://arxiv.org/format/2208.05432">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div 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/10.1051/0004-6361/202243134">10.1051/0004-6361/202243134 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J+R">J. R. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Francois%2C+P">P. Francois</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">S. E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eck%2C+S">S. Van Eck</a>, <a href="/search/astro-ph?searchtype=author&query=Zwitter%2C+T">T. Zwitter</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Flaccomio%2C+E">E. Flaccomio</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a> , et al. (143 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.05432v1-abstract-short" style="display: inline;"> The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100,000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.05432v1-abstract-full').style.display = 'inline'; document.getElementById('2208.05432v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.05432v1-abstract-full" style="display: none;"> The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100,000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper (arXiv:2206.02901) introduces the survey results. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. The Gaia-ESO Survey obtained 202,000 spectra of 115,000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.05432v1-abstract-full').style.display = 'none'; document.getElementById('2208.05432v1-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages. A&A in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, A120 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12792">arXiv:2207.12792</a> <span> [<a href="https://arxiv.org/pdf/2207.12792">pdf</a>, <a href="https://arxiv.org/format/2207.12792">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244112">10.1051/0004-6361/202244112 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO survey: A spectroscopic study of the young open cluster NGC 3293 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morel%2C+T">T. Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Blaz%C3%A8re%2C+A">A. Blaz猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Semaan%2C+T">T. Semaan</a>, <a href="/search/astro-ph?searchtype=author&query=Gosset%2C+E">E. Gosset</a>, <a href="/search/astro-ph?searchtype=author&query=Zorec%2C+J">J. Zorec</a>, <a href="/search/astro-ph?searchtype=author&query=Fr%C3%A9mat%2C+Y">Y. Fr茅mat</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Daflon%2C+S">S. Daflon</a>, <a href="/search/astro-ph?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Nieva%2C+M+F">M. F. Nieva</a>, <a href="/search/astro-ph?searchtype=author&query=Przybilla%2C+N">N. Przybilla</a>, <a href="/search/astro-ph?searchtype=author&query=Gebran%2C+M">M. Gebran</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+W">W. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</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="2207.12792v1-abstract-short" style="display: inline;"> We present a spectroscopic analysis of the GIRAFFE and UVES data collected by the Gaia-ESO survey for the young open cluster NGC 3293. Archive spectra from the same instruments obtained in the framework of the `VLT-FLAMES survey of massive stars' are also analysed. Atmospheric parameters, non-LTE chemical abundances for six elements, or variability information are reported for a total of about 160… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12792v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12792v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12792v1-abstract-full" style="display: none;"> We present a spectroscopic analysis of the GIRAFFE and UVES data collected by the Gaia-ESO survey for the young open cluster NGC 3293. Archive spectra from the same instruments obtained in the framework of the `VLT-FLAMES survey of massive stars' are also analysed. Atmospheric parameters, non-LTE chemical abundances for six elements, or variability information are reported for a total of about 160 B stars spanning a wide range in terms of spectral types (B1 to B9.5) and rotation rate (up to 350 km/s). We take advantage of the multi-epoch observations to detect several binary systems or intrinsically line-profile variables. A deconvolution algorithm is used to infer the current, true (deprojected) rotational velocity distribution. We find a broad, Gaussian-like distribution peaking around 200-250 km/s. Although some stars populate the high-velocity tail, most stars in the cluster appear to rotate far from critical. We discuss the chemical properties of the cluster, including the low occurrence of abundance peculiarities in the late B stars and the paucity of objects showing CN-cycle burning products at their surface. We argue that the former result can largely be explained by the inhibition of diffusion effects because of fast rotation, while the latter is generally in accord with the predictions of single-star evolutionary models under the assumption of a wide range of initial spin rates at the onset of main-sequence evolution. However, we find some evidence for a less efficient mixing in two quite rapidly rotating stars that are among the most massive objects in our sample. Finally, we obtain a cluster age of ~20 Myrs through a detailed, star-to-star correction of our results for the effect of stellar rotation. This is significantly older than previous estimates from turn-off fitting that fully relied on classical, non-rotating isochrones. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12792v1-abstract-full').style.display = 'none'; document.getElementById('2207.12792v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 24 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, A108 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.11313">arXiv:2206.11313</a> <span> [<a href="https://arxiv.org/pdf/2206.11313">pdf</a>, <a href="https://arxiv.org/ps/2206.11313">ps</a>, <a href="https://arxiv.org/format/2206.11313">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/ac8b0c">10.3847/1538-4357/ac8b0c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Topography of the Young Galactic Disk: Spatial and Kinematic Patterns of the Clustered Star Formation in the Solar Neighborhood </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez%2C+M">Manuel Jim茅nez</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Gil%2C+M+C">Mari Carmen S谩nchez-Gil</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+N">N茅stor S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M">Marta Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">Jes煤s Ma铆z Apell谩niz</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.11313v2-abstract-short" style="display: inline;"> The accuracy in determining the spatial-kinematical parameters of open clusters makes them ideal tracers of the Galactic structure. Young open clusters (YOCs) are the main representative of the clustered star formation mode, which identifies how most of the stars in the Galaxy form. We apply the Kriging technique to a sample of Gaia YOCs within a 3.5 kpc radius around the Sun and log(age) $\leq$ 7… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.11313v2-abstract-full').style.display = 'inline'; document.getElementById('2206.11313v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.11313v2-abstract-full" style="display: none;"> The accuracy in determining the spatial-kinematical parameters of open clusters makes them ideal tracers of the Galactic structure. Young open clusters (YOCs) are the main representative of the clustered star formation mode, which identifies how most of the stars in the Galaxy form. We apply the Kriging technique to a sample of Gaia YOCs within a 3.5 kpc radius around the Sun and log(age) $\leq$ 7.5, age in years, to obtain the $Z(X,Y)$ and $V_Z(X,Y)$ maps. The previous work by Alfaro et al. (1991) showed that Kriging can provide reliable results even with small data samples ($N \sim 100$). We approach the 3D spatial and vertical velocity field structure of the Galactic disk defined by YOCs and analyze the hierarchy of the stellar cluster formation, which shows a rich hierarchical structure, displaying complexes embedded within each other. We discuss the fundamental characteristics of the methodology used to perform the mapping and point out the main results obtained in phenomenological terms. Both the 3D spatial distribution and the vertical velocity field reveal a complex disk structure with a high degree of substructures. Their analysis provides clues about the main physical mechanisms that shape the phase space of the clustered star formation in this Galactic area. Warp, corrugations, and high local deviations in $Z$ and $V_Z$, appear intimately connected in a single but intricate scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.11313v2-abstract-full').style.display = 'none'; document.getElementById('2206.11313v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.04908">arXiv:2206.04908</a> <span> [<a href="https://arxiv.org/pdf/2206.04908">pdf</a>, <a href="https://arxiv.org/ps/2206.04908">ps</a>, <a href="https://arxiv.org/format/2206.04908">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The Gaia view on massive stars: EDR3 and what to expect from DR3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Weiler%2C+M">M. Weiler</a>, <a href="/search/astro-ph?searchtype=author&query=Reed%2C+B+C">B. C. Reed</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+R+F">R. Fern谩ndez Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+P+C">P. Crespo Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Lera%2C+J+A+M">J. A. Molina Lera</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.04908v1-abstract-short" style="display: inline;"> At the time of this meeting, the latest Gaia data release is EDR3, published on 3 December 2020, but the next one, DR3, will appear soon, on 13 June 2022. This contribution describes, on the one hand, Gaia EDR3 results on massive stars and young stellar clusters, placing special emphasis on how a correct treatment of the astrometric and photometric calibration yields results that are simultaneousl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.04908v1-abstract-full').style.display = 'inline'; document.getElementById('2206.04908v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.04908v1-abstract-full" style="display: none;"> At the time of this meeting, the latest Gaia data release is EDR3, published on 3 December 2020, but the next one, DR3, will appear soon, on 13 June 2022. This contribution describes, on the one hand, Gaia EDR3 results on massive stars and young stellar clusters, placing special emphasis on how a correct treatment of the astrometric and photometric calibration yields results that are simultaneously precise and accurate. On the other hand, it gives a brief description of the exciting results we can expect from Gaia DR3. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.04908v1-abstract-full').style.display = 'none'; document.getElementById('2206.04908v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in Massive Stars Near and Far, Proceedings IAU Symposium No. 361, 2022. N. St-Louis, J. S. Vink & J. Mackey, eds</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.02901">arXiv:2206.02901</a> <span> [<a href="https://arxiv.org/pdf/2206.02901">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202243141">10.1051/0004-6361/202243141 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=V%C3%A0zquez%2C+C+V">C. Viscasillas V脿zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J+R">J. R. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+T+B+R">T. Bensby R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Flaccomio%2C+E">E. Flaccomio</a>, <a href="/search/astro-ph?searchtype=author&query=Fran%C3%A7ois%2C+P">P. Fran莽ois</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">S. E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a> , et al. (139 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="2206.02901v1-abstract-short" style="display: inline;"> In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey (GES), the only one performed on a 8m class telescope, was designed to target 100,000 stars… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.02901v1-abstract-full').style.display = 'inline'; document.getElementById('2206.02901v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.02901v1-abstract-full" style="display: none;"> In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey (GES), the only one performed on a 8m class telescope, was designed to target 100,000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article (Gilmore et al.) reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. The GES has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110,000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by the Gaia-ESO consortium and the community, with many highlight results achieved. The final catalogue has been released through the ESO archive at the end of May 2022, including the complete set of advanced data products. In addition to these results, the Gaia-ESO Survey will leave a very important legacy, for several aspects and for many years to come. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.02901v1-abstract-full').style.display = 'none'; document.getElementById('2206.02901v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics. 30 pages, 30 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.05485">arXiv:2204.05485</a> <span> [<a href="https://arxiv.org/pdf/2204.05485">pdf</a>, <a href="https://arxiv.org/ps/2204.05485">ps</a>, <a href="https://arxiv.org/format/2204.05485">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2022.137080">10.1016/j.physletb.2022.137080 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Very Special Linear Gravity: A Gauge-Invariant Graviton Mass </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Santoni%2C+A">Alessandro Santoni</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.05485v2-abstract-short" style="display: inline;"> Linearized gravity in the Very Special Relativity (VSR) framework is considered. We prove that this theory allows for a non-zero graviton mass $m_g$ without breaking gauge invariance nor modifying the relativistic dispersion relation. We find the analytic solution for the new equations of motion in our gauge choice, verifying as expected the existence of only two physical degrees of freedom. Final… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05485v2-abstract-full').style.display = 'inline'; document.getElementById('2204.05485v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05485v2-abstract-full" style="display: none;"> Linearized gravity in the Very Special Relativity (VSR) framework is considered. We prove that this theory allows for a non-zero graviton mass $m_g$ without breaking gauge invariance nor modifying the relativistic dispersion relation. We find the analytic solution for the new equations of motion in our gauge choice, verifying as expected the existence of only two physical degrees of freedom. Finally, through the geodesic deviation equation, we confront some results for classic gravitational waves (GW) with the VSR ones: we see that the ratios between VSR effects and classical ones are proportional to $(m_g/E)^2$, $E$ being the energy of a graviton in the GW. For GW detectable by the interferometers LIGO and VIRGO this ratio is at most $10^{-20}$. However, for GW in the lower frequency range of future detectors, like LISA, the ratio increases significantly to $ 10^{-10}$, that combined with the anisotropic nature of VSR phenomena may lead to observable effects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05485v2-abstract-full').style.display = 'none'; document.getElementById('2204.05485v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex,6 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.00422">arXiv:2204.00422</a> <span> [<a href="https://arxiv.org/pdf/2204.00422">pdf</a>, <a href="https://arxiv.org/format/2204.00422">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142985">10.1051/0004-6361/202142985 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Westerlund 1 under the light of Gaia EDR3: Distance, isolation, extent, and a hidden population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">Ignacio Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Dorda%2C+R">Ricardo Dorda</a>, <a href="/search/astro-ph?searchtype=author&query=Marco%2C+A">Amparo Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">Jes煤s Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Fern%C3%A1ndez%2C+C">Carlos Gonz谩lez-Fern谩ndez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.00422v2-abstract-short" style="display: inline;"> (Abridged) We have used Gaia EDR3 data, together with spectra of a large sample of luminous stars in the field surrounding Westerlund 1, to explore the extent of the cluster. We carry out a non-parametric analysis of proper motions and membership determination. We investigate the reddening and proper motions of several dozen OB stars and red supergiants < 1 deg away from Wd 1. We identify a popula… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00422v2-abstract-full').style.display = 'inline'; document.getElementById('2204.00422v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.00422v2-abstract-full" style="display: none;"> (Abridged) We have used Gaia EDR3 data, together with spectra of a large sample of luminous stars in the field surrounding Westerlund 1, to explore the extent of the cluster. We carry out a non-parametric analysis of proper motions and membership determination. We investigate the reddening and proper motions of several dozen OB stars and red supergiants < 1 deg away from Wd 1. We identify a population of kinematic members of Wd 1 that largely includes the known spectroscopic members. From their EDR3 parallaxes, we derive a distance to the cluster of $4.23^{+0.23}_{-0.21}$kpc. Extinction in this direction increases by a large amount around 2.8 kpc, due to dark clouds associated to the Scutum-Crux arm. As a consequence, we hardly see any stars at distances comparable to that of the cluster. The proper motions of Wd 1, however, are very similar to those of stars in the field surrounding it, but distinct. We find a second, astrometrically well-defined population in the foreground ($d\approx2\:$kpc), likely connected to the possible open cluster BH197. Wd 1 is very elongated, an effect not driven by the very heavy extinction to the East and South. We find a low-density halo extending up to 10' from the cluster centre, mainly in the NW quadrant. A few OB stars at larger distances from the cluster, most notably the LBV MN48, share its proper motions, suggesting that Wd 1 has little or no peculiar motion with respect to the field population of the Norma arm. However, we are unable to find any red supergiant that could belong to an extended population related to the cluster, although we observe several dozen such objects in the foreground. We find a substantial population of luminous OB members obscured by several more magnitudes of extinction than most known members. These objects, mostly located in the central region of the cluster, increase the population of OB supergiants by about 25%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00422v2-abstract-full').style.display = 'none'; document.getElementById('2204.00422v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics. Figures have been converted to PNG and are of lower quality than in the version accepted. Three tables in the appendices will be published electronically; only table C1 is given here. 25 pages (including appendices),23 figures. V2 incorporates style and language edits and some comments</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A146 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.08662">arXiv:2202.08662</a> <span> [<a href="https://arxiv.org/pdf/2202.08662">pdf</a>, <a href="https://arxiv.org/format/2202.08662">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142349">10.1051/0004-6361/202142349 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: The analysis of the hot-star spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Daflon%2C+S">S. Daflon</a>, <a href="/search/astro-ph?searchtype=author&query=Gebran%2C+M">M. Gebran</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+F">F. Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Morel%2C+T">T. Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Berlanas%2C+S+R">S. R. Berlanas</a>, <a href="/search/astro-ph?searchtype=author&query=Blazere%2C+A">A. Blazere</a>, <a href="/search/astro-ph?searchtype=author&query=Fremat%2C+Y">Y. Fremat</a>, <a href="/search/astro-ph?searchtype=author&query=Gosset%2C+E">E. Gosset</a>, <a href="/search/astro-ph?searchtype=author&query=Apellaniz%2C+J+M">J. Maiz Apellaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+W">W. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Semaan%2C+T">T. Semaan</a>, <a href="/search/astro-ph?searchtype=author&query=Simon-Diaz%2C+S">S. Simon-Diaz</a>, <a href="/search/astro-ph?searchtype=author&query=Volpi%2C+D">D. Volpi</a>, <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Esteban%2C+F">F. Jimenez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Nieva%2C+M+F">M. F. Nieva</a>, <a href="/search/astro-ph?searchtype=author&query=Przybilla%2C+N">N. Przybilla</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a> , et al. (22 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="2202.08662v2-abstract-short" style="display: inline;"> The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of 6 years, spectra of ~ 10^5 stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08662v2-abstract-full').style.display = 'inline'; document.getElementById('2202.08662v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.08662v2-abstract-full" style="display: none;"> The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of 6 years, spectra of ~ 10^5 stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of the hottest stars (O, B and A type, with a formal cut-off of Teff > 7000 K) that were observed as part of GES. We present the procedures and techniques that have been applied to the reduced spectra, in order to determine the stellar parameters and abundances of these stars. The procedure used is similar to that of other working groups in GES. A number of groups (called `Nodes') each independently analyse the spectra, using their state-of-the-art techniques and codes. Specific for the analysis in WG13 is the large temperature range that is covered (Teff = 7000 - 50,000 K), requiring the use of different analysis codes. Most Nodes can therefore only handle part of the data. Quality checks are applied to the results of these Nodes by comparing them to benchmark stars, and by comparing them one to another. For each star the Node values are then homogenised into a single result: the recommended parameters and abundances. Eight Nodes each analysed (part of) the data. In total 17,693 spectra of 6462 stars were analysed, most of them in 37 open star clusters. The homogenisation led to stellar parameters for 5584 stars. Abundances were determined for a more limited number of stars. Elements studied are He, C, N, O, Ne, Mg, Al, Si and Sc. Abundances for at least one of those elements were determined for 292 stars. The hot-star data analysed here, as well as the Gaia-ESO Survey data in general, will be of considerable use in future studies of stellar evolution and open clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08662v2-abstract-full').style.display = 'none'; document.getElementById('2202.08662v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 14 figures, accepted for publication in Astronomy & Astrophysics; language-edited version; two appendices merged</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A120 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.01464">arXiv:2110.01464</a> <span> [<a href="https://arxiv.org/pdf/2110.01464">pdf</a>, <a href="https://arxiv.org/format/2110.01464">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/10.1051/0004-6361/202142364">10.1051/0004-6361/202142364 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Villafranca catalog of Galactic OB groups. II. From Gaia DR2 to EDR3 and ten new systems with O stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+R+F">R. Fern谩ndez Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+P+C">P. Crespo Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</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="2110.01464v2-abstract-short" style="display: inline;"> CONTEXT. This is the second paper of a series on Galactic OB groups that uses astrometric and photometric data from Gaia and spectral classifications from GOSSS and LiLiMaRlin. The previous paper was based on Gaia DR2, this is based on Gaia EDR3. AIMS. The two aims of this paper are to revise the results for the sample from paper I using Gaia EDR3 data and to expand the sample of analyzed stella… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01464v2-abstract-full').style.display = 'inline'; document.getElementById('2110.01464v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.01464v2-abstract-full" style="display: none;"> CONTEXT. This is the second paper of a series on Galactic OB groups that uses astrometric and photometric data from Gaia and spectral classifications from GOSSS and LiLiMaRlin. The previous paper was based on Gaia DR2, this is based on Gaia EDR3. AIMS. The two aims of this paper are to revise the results for the sample from paper I using Gaia EDR3 data and to expand the sample of analyzed stellar groups to 26, from Villafranca O-001 to Villafranca O-026. METHODS. We use GOSSS to select Galactic stellar groups with O stars and an updated version of the method in paper 0 of this series, combining Gaia EDR3 G+GBP+GRP photometry, positions, proper motions, and parallaxes to assign memberships and measure distances. We present 99 spectra from GOSSS and 32 from LiLiMaRlin for stars in the analyzed groups or in their foreground. RESULTS. We derive distances to the 26 stellar groups with unprecedented precision and accuracy, with total uncertainties <1% within 1 kpc and of ~3% around 3 kpc, values that are almost 4x better than for Gaia DR2. We provide homogeneous spectral types for 110 stars and correct a number of errors in the literature, especially for objects in the Orion nebula cluster. For each of the groups we discuss its membership and present possible runaway/walkaway stars. At least two groups, Villafranca O-O12 S and Villafranca O-014 NW, are orphan clusters in which the most massive stars have been ejected by dynamical interactions, leaving objects with a capped mass function. The existence of such clusters has important consequences for the study of the IMF, the distribution of SNe across the Galaxy, and the population and dynamics of isolated compact objects. We fit PMS isochrones to four clusters to derive ages of 2.0$\pm$0.5 Ma for the sigma Orionis cluster, 4$\pm$2 Ma for NGC 2264, 5.0$\pm$0.5 Ma for NGC 2362, and 8$\pm$2 Ma for the gamma Velorum cluster. [ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01464v2-abstract-full').style.display = 'none'; document.getElementById('2110.01464v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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. Original arXiv version was submitted prior to paper being accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 657, A131 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.09415">arXiv:2108.09415</a> <span> [<a href="https://arxiv.org/pdf/2108.09415">pdf</a>, <a href="https://arxiv.org/format/2108.09415">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202141360">10.1051/0004-6361/202141360 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Non-Sequential Neural Network for Simultaneous, Consistent Classification and Photometric Redshifts of OTELO Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Diego%2C+J+A">Jos茅 A. de Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Nadolny%2C+J">Jakub Nadolny</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiovanni%2C+%C3%81">脕ngel Bongiovanni</a>, <a href="/search/astro-ph?searchtype=author&query=Cepa%2C+J">Jordi Cepa</a>, <a href="/search/astro-ph?searchtype=author&query=Lara-L%C3%B3pez%2C+M+A">Maritza A. Lara-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Gallego%2C+J">Jes煤s Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Cervi%C3%B1o%2C+M">Miguel Cervi帽o</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Porta%2C+M">Miguel S谩nchez-Porta</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Serrano%2C+J+I">J. Ignacio Gonz谩lez-Serrano</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Povi%C4%87%2C+M">Mirjana Povi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+A+M+P">Ana Mar铆a P茅rez Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+R+P">Ricardo P茅rez Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Torres%2C+C+P+P">Carmen P. Padilla Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Cedr%C3%A9s%2C+B">Bernab茅 Cedr茅s</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Aguilar%2C+D">Diego Garc铆a-Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+J">J. Jes煤s Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Otero%2C+M">Mauro Gonz谩lez-Otero</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro-Mart%C3%ADnez%2C+R">Roc铆o Navarro-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Pintos-Castro%2C+I">Irene Pintos-Castro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.09415v1-abstract-short" style="display: inline;"> Context. Computational techniques are essential for mining large databases produced in modern surveys with value-added products. Aims. This paper presents a machine learning procedure to carry out simultaneously galaxy morphological classification and photometric redshift estimates. Currently, only spectral energy distribution (SED) fitting has been used to obtain these results all at once. Method… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.09415v1-abstract-full').style.display = 'inline'; document.getElementById('2108.09415v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.09415v1-abstract-full" style="display: none;"> Context. Computational techniques are essential for mining large databases produced in modern surveys with value-added products. Aims. This paper presents a machine learning procedure to carry out simultaneously galaxy morphological classification and photometric redshift estimates. Currently, only spectral energy distribution (SED) fitting has been used to obtain these results all at once. Methods. We used the ancillary data gathered in the OTELO catalog and designed a non-sequential neural network that accepts optical and near-infrared photometry as input. The network transfers the results of the morphological classification task to the redshift fitting process to ensure consistency between both procedures. Results. The results successfully recover the morphological classification and the redshifts of the test sample, reducing catastrophic redshift outliers produced by SED fitting and avoiding possible discrepancies between independent classification and redshift estimates. Our technique may be adapted to include galaxy images to improve the classification. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.09415v1-abstract-full').style.display = 'none'; document.getElementById('2108.09415v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy and Astrophysics (A&A) accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 655, A56 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.12213">arXiv:2106.12213</a> <span> [<a href="https://arxiv.org/pdf/2106.12213">pdf</a>, <a href="https://arxiv.org/ps/2106.12213">ps</a>, <a href="https://arxiv.org/format/2106.12213">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac0a7e">10.3847/2041-8213/ac0a7e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The OTELO survey: the star formation rate evolution of low-mass galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cedr%C3%A9s%2C+B">Bernab茅 Cedr茅s</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Garc%C3%ADa%2C+A+M">Ana Mar铆a P茅rez-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Mart%C3%ADnez%2C+R">Ricardo P茅rez-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Cervi%C3%B1o%2C+M">Miguel Cervi帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Gallego%2C+J">Jes煤s Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiovanni%2C+%C3%81">脕ngel Bongiovanni</a>, <a href="/search/astro-ph?searchtype=author&query=Cepa%2C+J">Jordi Cepa</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+R+N">Roc铆o Navarro Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Nadolny%2C+J">Jakub Nadolny</a>, <a href="/search/astro-ph?searchtype=author&query=Lara-L%C3%B3pez%2C+M+A">Maritza A. Lara-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Portal%2C+M">Miguel S谩nchez-Portal</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=de+Diego%2C+J+A">Jos茅 A. de Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Otero%2C+M">Mauro Gonz谩lez-Otero</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+J">J. Jes煤s Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Serrano%2C+J+I">J. Ignacio Gonz谩lez-Serrano</a>, <a href="/search/astro-ph?searchtype=author&query=Torres%2C+C+P+P">Carmen P. Padilla Torres</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.12213v1-abstract-short" style="display: inline;"> We present the analysis of a sample of \ha\,, \hb\ and \oii\ emission line galaxies from the \otelo\ survey, with masses typically below $log(M_*/M_\sun) \sim 9.4$ and redshifts between $z \sim 0.4$ and 1.43. We study the star formation rate, star formation rate density, and number density and their evolution with redshift. We obtain a robust estimate of the specific star formation rate -- stellar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.12213v1-abstract-full').style.display = 'inline'; document.getElementById('2106.12213v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.12213v1-abstract-full" style="display: none;"> We present the analysis of a sample of \ha\,, \hb\ and \oii\ emission line galaxies from the \otelo\ survey, with masses typically below $log(M_*/M_\sun) \sim 9.4$ and redshifts between $z \sim 0.4$ and 1.43. We study the star formation rate, star formation rate density, and number density and their evolution with redshift. We obtain a robust estimate of the specific star formation rate -- stellar mass relation based on the lowest mass sample published so far. We also determine a flat trend of the star formation rate density and number density with redshift. Our results suggest a scenario of no evolution of the number density of galaxies, regardless of their masses, up to redshift $z\sim1.4$. This implies a gradual change of the relative importance of the star forming processes, from high-mass galaxies to low-mass galaxies, with decreasing redshift. We also find little or no variation of the star formation rate density in the redshift range of $0.4<z<1.43$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.12213v1-abstract-full').style.display = 'none'; document.getElementById('2106.12213v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 3 figures, accepted for publication in ApJ letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.09451">arXiv:2106.09451</a> <span> [<a href="https://arxiv.org/pdf/2106.09451">pdf</a>, <a href="https://arxiv.org/format/2106.09451">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/stab1769">10.1093/mnras/stab1769 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GALANTE photometric survey of the northern Galactic plane: Project description and pipeline </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Rami%C3%B3%2C+H+V">H. V谩zquez Rami贸</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+J">J. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Lorenzo-Guti%C3%A9rrez%2C+A">A. Lorenzo-Guti茅rrez</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Lario%2C+P">P. Garc铆a-Lario</a>, <a href="/search/astro-ph?searchtype=author&query=Escudero%2C+H+G">H. Garc铆a Escudero</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+M">M. Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+P+R+T">P. R. T. Coelho</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.09451v1-abstract-short" style="display: inline;"> The GALANTE optical photometric survey is observing the northern Galactic plane and some adjacent regions using seven narrow- and intermediate-filters, covering a total of 1618 square degrees. The survey has been designed with multiple exposure times and at least two different air masses per field to maximize its photometric dynamic range, comparable to that of Gaia, and ensure the accuracy of its… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.09451v1-abstract-full').style.display = 'inline'; document.getElementById('2106.09451v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.09451v1-abstract-full" style="display: none;"> The GALANTE optical photometric survey is observing the northern Galactic plane and some adjacent regions using seven narrow- and intermediate-filters, covering a total of 1618 square degrees. The survey has been designed with multiple exposure times and at least two different air masses per field to maximize its photometric dynamic range, comparable to that of Gaia, and ensure the accuracy of its photometric calibration. The goal is to reach at least 1% accuracy and precision in the seven bands for all stars brighter than AB magnitude 17 while detecting fainter stars with lower values of the signal-to-noise ratio.The main purposes of GALANTE are the identification and study of extinguished O+B+WR stars, the derivation of their extinction characteristics, and the cataloguing of F and G stars in the solar neighbourhood. Its data will be also used for a variety of other stellar studies and to generate a high-resolution continuum-free map of the H伪 emission in the Galactic plane. We describe the techniques and the pipeline that are being used to process the data, including the basis of an innovative calibration system based on Gaia DR2 and 2MASS photometry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.09451v1-abstract-full').style.display = 'none'; document.getElementById('2106.09451v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.03859">arXiv:2104.03859</a> <span> [<a href="https://arxiv.org/pdf/2104.03859">pdf</a>, <a href="https://arxiv.org/format/2104.03859">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/stab2797">10.1093/mnras/stab2797 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pisces VII: Discovery of a possible satellite of Messier 33 in the DESI Legacy Imaging Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martinez-Delgado%2C+D">David Martinez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Karim%2C+N">Noushin Karim</a>, <a href="/search/astro-ph?searchtype=author&query=Charles%2C+E+J+E">Emily J. E. Charles</a>, <a href="/search/astro-ph?searchtype=author&query=Boschin%2C+W">Walter Boschin</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">Matteo Monelli</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+M+L+M">Michelle L. M. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Donatiello%2C+G">Giuseppe Donatiello</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</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="2104.03859v2-abstract-short" style="display: inline;"> We report deep imaging observations with DOLoRes@TNG of an ultra-faint dwarf satellite candidate of the Triangulum galaxy (M33) found by visual inspection of the public imaging data release of the DESI Legacy Imaging Surveys. Pisces VII/Triangulum (Tri) III is found at a projected distance of 72 kpc from M33, and using the tip of the red giant branch method we estimate a distance of D=1.0 +0.3,-0.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.03859v2-abstract-full').style.display = 'inline'; document.getElementById('2104.03859v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.03859v2-abstract-full" style="display: none;"> We report deep imaging observations with DOLoRes@TNG of an ultra-faint dwarf satellite candidate of the Triangulum galaxy (M33) found by visual inspection of the public imaging data release of the DESI Legacy Imaging Surveys. Pisces VII/Triangulum (Tri) III is found at a projected distance of 72 kpc from M33, and using the tip of the red giant branch method we estimate a distance of D=1.0 +0.3,-0.2 Mpc, meaning the galaxy could either be an isolated ultra-faint or the second known satellite of M33. We estimate an absolute magnitude of M_V=-6.1+/-0.2 if Pisces VII/Tri II is at the distance of M33, or as bright as M_V=-6.8+/-0.2 if the galaxy is isolated. At the isolated distance, it has a physical half-light radius of r_h=131+/-61 pc consistent with similarly faint galaxies around the Milky Way. As the tip of the red giant branch is sparsely populated, constraining a precision distance is not possible, but if Pisces VII/Tri III can be confirmed as a true satellite of M33 it is a significant finding. With only one potential satellite detected around M33 previously (Andromeda XXII/Tri I), it lacks a significant satellite population in stark contrast to the similarly massive Large Magellanic Cloud. The detection of more satellites in the outskirts of M33 could help to better illuminate if this discrepancy between expectation and observations is due to a poor understanding of the galaxy formation process, or if it is due to the low luminosity and surface brightness of the M33 satellite population which has thus far fallen below the detection limits of previous surveys. If it is truly isolated, it would be the faintest known field dwarf detected to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.03859v2-abstract-full').style.display = 'none'; document.getElementById('2104.03859v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">10 pages, 9 figures, 2 tables, accepted for publication in MNRAS. This final version includes a moderate revision after the referee's comments and a correct title</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.03645">arXiv:2103.03645</a> <span> [<a href="https://arxiv.org/pdf/2103.03645">pdf</a>, <a href="https://arxiv.org/ps/2103.03645">ps</a>, <a href="https://arxiv.org/format/2103.03645">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/10.1051/0004-6361/202039880">10.1051/0004-6361/202039880 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The OTELO survey: Faint end of the luminosity function of [OII] emitters at <z>= 1.43 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cedr%C3%A9s%2C+B">Bernab茅 Cedr茅s</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiovanni%2C+%C3%81">脕ngel Bongiovanni</a>, <a href="/search/astro-ph?searchtype=author&query=Cervi%C3%B1o%2C+M">Miguel Cervi帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Nadolny%2C+J">Jakub Nadolny</a>, <a href="/search/astro-ph?searchtype=author&query=Cepa%2C+J">Jordi Cepa</a>, <a href="/search/astro-ph?searchtype=author&query=de+Diego%2C+J+A">Jos茅 A. de Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+A+M+P">Ana Mar铆a P茅rez Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Gallego%2C+J">Jes煤s Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Lara-L%C3%B3pez%2C+M+A">Maritza A. Lara-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Portal%2C+M">Miguel S谩nchez-Portal</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Serrano%2C+J+I">J. Ignacio Gonz谩lez-Serrano</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+R+N">Roc铆o Navarro Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+R+P">Ricardo P茅rez Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+J">J. Jes煤s Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Torres%2C+C+P+P">Carmen P. Padilla Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Casta%C3%B1eda%2C+H+O">H茅ctor O. Casta帽eda</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M">Mauro Gonz谩lez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.03645v1-abstract-short" style="display: inline;"> In this paper, we aim to study the main properties and luminosity function (LF) of the [OII] emitters detected in the OTELO survey in order to characterise the star formation processes in low-mass galaxies at $z\sim1.43$ and to constrain the faint-end of the LF. Here, we describe the selection method and analysis of the emitters obtained from narrow-band scanning techniques. In addition, we pres… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.03645v1-abstract-full').style.display = 'inline'; document.getElementById('2103.03645v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.03645v1-abstract-full" style="display: none;"> In this paper, we aim to study the main properties and luminosity function (LF) of the [OII] emitters detected in the OTELO survey in order to characterise the star formation processes in low-mass galaxies at $z\sim1.43$ and to constrain the faint-end of the LF. Here, we describe the selection method and analysis of the emitters obtained from narrow-band scanning techniques. In addition, we present several relevant properties of the emitters and discuss the selection biases and uncertainties in the determination of the LF and the star formation rate density (SFRD). We confirmed a total of 60 sources from a preliminary list of 332 candidates as [OII] emitters. Approximately 93% of the emitters have masses in the range of $10^{8}<M_{*}/{\rm M_{\odot}}<10^{9}$. All of our emitters are classified as late-type galaxies, with a lower value of $(u-v)$\, when compared with the rest of the emitters of the OTELO survey. We find that the cosmic variance strongly affects the normalisation ($蠁^*$) of the LF and explains the discrepancy of our results when compared with those obtained from surveys of much larger volumes. However, we are able to determine the faint-end slope of the LF, namely, $伪=-1.42\pm0.06$, by sampling the LF down to $\sim1$\,dex lower than in previous works. We present our calculation of the SFRD of our sample and compare it to the value obtained in previous studies from the literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.03645v1-abstract-full').style.display = 'none'; document.getElementById('2103.03645v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 14 figures. Accepted 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 649, A73 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.12407">arXiv:2101.12407</a> <span> [<a href="https://arxiv.org/pdf/2101.12407">pdf</a>, <a href="https://arxiv.org/format/2101.12407">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140444">10.1051/0004-6361/202140444 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> J-PLUS: Systematic impact of metallicity on photometric calibration with the stellar locus </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Sanjuan%2C+C">C. L贸pez-Sanjuan</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+H">H. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Rami%C3%B3%2C+H+V">H. V谩zquez Rami贸</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+J">J. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Crist%C3%B3bal-Hornillos%2C+D">D. Crist贸bal-Hornillos</a>, <a href="/search/astro-ph?searchtype=author&query=Tremblay%2C+P+-">P. -E. Tremblay</a>, <a href="/search/astro-ph?searchtype=author&query=Mar%C3%ADn-Franch%2C+A">A. Mar铆n-Franch</a>, <a href="/search/astro-ph?searchtype=author&query=Cenarro%2C+A+J">A. J. Cenarro</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Candal%2C+A">A. Alvarez-Candal</a>, <a href="/search/astro-ph?searchtype=author&query=Daflon%2C+S">S. Daflon</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1n-Caballero%2C+A">A. Hern谩n-Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez-Monteagudo%2C+C">C. Hern谩ndez-Monteagudo</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F+M">F. M. Jim茅nez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Placco%2C+V+M">V. M. Placco</a>, <a href="/search/astro-ph?searchtype=author&query=Tempel%2C+E">E. Tempel</a>, <a href="/search/astro-ph?searchtype=author&query=Alcaniz%2C+J">J. Alcaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Angulo%2C+R+E">R. E. Angulo</a>, <a href="/search/astro-ph?searchtype=author&query=Dupke%2C+R+A">R. A. Dupke</a>, <a href="/search/astro-ph?searchtype=author&query=Moles%2C+M">M. Moles</a>, <a href="/search/astro-ph?searchtype=author&query=Sodr%C3%A9%2C+L">L. Sodr茅 Jr</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.12407v2-abstract-short" style="display: inline;"> We present the updated photometric calibration of the twelve optical passbands for the Javalambre Photometric Local Universe Survey (J-PLUS) second data release (DR2), comprising 1088 pointings of two square degrees, and study the systematic impact of metallicity in the stellar locus technique. The [Fe/H] metallicity from LAMOST DR5 for 146184 high-quality calibration stars, defined with S/N > 10… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12407v2-abstract-full').style.display = 'inline'; document.getElementById('2101.12407v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.12407v2-abstract-full" style="display: none;"> We present the updated photometric calibration of the twelve optical passbands for the Javalambre Photometric Local Universe Survey (J-PLUS) second data release (DR2), comprising 1088 pointings of two square degrees, and study the systematic impact of metallicity in the stellar locus technique. The [Fe/H] metallicity from LAMOST DR5 for 146184 high-quality calibration stars, defined with S/N > 10 in J-PLUS passbands and S/N > 3 in Gaia parallax, was used to compute the metallicity-dependent stellar locus (ZSL). The initial homogenization of J-PLUS photometry, performed with a unique stellar locus, was refined by including the metallicity effect in colours via the ZSL. The variation of the average metallicity along the Milky Way produces a systematic offset in J-PLUS calibration. This effect is well above 1% for the bluer passbands and amounts 0.07, 0.07, 0.05, 0.03, and 0.02 mag in u, J0378, J0395, J0410, and J0430, respectively. We modelled this effect with the Milky Way location of the J-PLUS pointing, providing also an updated calibration for those observations without LAMOST information. The estimated accuracy in the calibration after including the metallicity effect is at 1% level for the bluer J-PLUS passbands and below for the rest. We conclude that photometric calibration with the stellar locus technique is prone to significant systematic bias along the Milky Way location for passbands bluer than lambda = 4500 A. The updated calibration method for J-PLUS DR2 reaches 1-2% precision and 1% accuracy for twelve optical filters within an area of 2176 square degrees. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12407v2-abstract-full').style.display = 'none'; document.getElementById('2101.12407v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Astronomy & Astrophysics. 18 pages, 12 figures, 3 tables, 2 appendices</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, A61 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.05553">arXiv:2010.05553</a> <span> [<a href="https://arxiv.org/pdf/2010.05553">pdf</a>, <a href="https://arxiv.org/ps/2010.05553">ps</a>, <a href="https://arxiv.org/format/2010.05553">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa3082">10.1093/mnras/staa3082 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detailed Studies of IPHAS sources. II. Sab 19, a true planetary nebula and its mimic crossing the Perseus Arm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guerrero%2C+M+A">Martin A Guerrero</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+R">Roberto Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Sabin%2C+L">Laurence Sabin</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Larios%2C+G">Gerardo Ramos-Larios</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J Alfaro</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="2010.05553v1-abstract-short" style="display: inline;"> The INT Photometric H$伪$ Survey (IPHAS) has provided us with a number of new-emission line sources, among which planetary nebulae (PNe) constitute an important fraction. Here we present a detailed analysis of the IPHAS nebula Sab\,19 (IPHASX\,J055242.8+262116) based on radio, infrared, and optical images and intermediate- and high-dispersion longslit spectra. Sab\,19 consists of a roundish 0.10 pc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.05553v1-abstract-full').style.display = 'inline'; document.getElementById('2010.05553v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.05553v1-abstract-full" style="display: none;"> The INT Photometric H$伪$ Survey (IPHAS) has provided us with a number of new-emission line sources, among which planetary nebulae (PNe) constitute an important fraction. Here we present a detailed analysis of the IPHAS nebula Sab\,19 (IPHASX\,J055242.8+262116) based on radio, infrared, and optical images and intermediate- and high-dispersion longslit spectra. Sab\,19 consists of a roundish 0.10 pc in radius double-shell nebula surrounded by a much larger 2.8 pc in radius external shell with a prominent H-shaped filament. We confirm the nature of the main nebula as a PN whose sub-solar N/O ratio abundances, low ionized mass, peculiar radial velocity, and low-mass central star allow us to catalog it as a type III PN. Apparently, the progenitor star of Sab\,19 became a PN when crossing the Perseus Arm during a brief visit of a few Myr. The higher N/O ratio and velocity shift $\simeq$40 \kms\ of the external shell with respect to the main nebula and its large ionized mass suggest that it is not truly associated with Sab\,19, but it is rather dominated by a Str枚mgren zone in the interstellar medium ionized by the PN central star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.05553v1-abstract-full').style.display = 'none'; document.getElementById('2010.05553v1-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 8 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.01349">arXiv:2010.01349</a> <span> [<a href="https://arxiv.org/pdf/2010.01349">pdf</a>, <a href="https://arxiv.org/format/2010.01349">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2021/02/048">10.1088/1475-7516/2021/02/048 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=B%2C+R+A">R. Alves B</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Araudo%2C+A">A. Araudo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M">M. Ashley</a> , et al. (474 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.01349v2-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for $纬$-ray astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of $纬$-ray cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nucle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.01349v2-abstract-full').style.display = 'inline'; document.getElementById('2010.01349v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.01349v2-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for $纬$-ray astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of $纬$-ray cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nuclei (AGN) and of their relativistic jets. Observations of AGN with CTA will enable a measurement of $纬$-ray absorption on the extragalactic background light with a statistical uncertainty below 15% up to a redshift $z=2$ and to constrain or detect $纬$-ray halos up to intergalactic-magnetic-field strengths of at least 0.3pG. Extragalactic observations with CTA also show promising potential to probe physics beyond the Standard Model. The best limits on Lorentz invariance violation from $纬$-ray astronomy will be improved by a factor of at least two to three. CTA will also probe the parameter space in which axion-like particles could constitute a significant fraction, if not all, of dark matter. We conclude on the synergies between CTA and other upcoming facilities that will foster the growth of $纬$-ray cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.01349v2-abstract-full').style.display = 'none'; document.getElementById('2010.01349v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">71 pages (including affiliations and references), 13 figures, 6 tables. Accepted in JCAP; matches published version. Corresponding authors: Jonathan Biteau, Julien Lefaucheur, Humberto Martinez-Huerta, Manuel Meyer, Santiago Pita, Ievgen Vovk</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 02 (2021) 048 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.13305">arXiv:2009.13305</a> <span> [<a href="https://arxiv.org/pdf/2009.13305">pdf</a>, <a href="https://arxiv.org/format/2009.13305">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="General Relativity and Quantum Cosmology">gr-qc</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/abddc3">10.3847/1538-4357/abddc3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observational constraints in Delta Gravity: CMB and supernovas </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn%2C+M+S">Marco San Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Rubio%2C+C">Carlos Rubio</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.13305v1-abstract-short" style="display: inline;"> Delta Gravity is a gravitational model based on an extension of General Relativity given by a new symmetry called $\tilde未$. In this model, new matter fields are added to the original matter fields, motivated by the additional symmetry. We call them $\tilde未$ matter fields. This model predicts an accelerating Universe without the need to introduce a cosmological constant. In this work, we study th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.13305v1-abstract-full').style.display = 'inline'; document.getElementById('2009.13305v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.13305v1-abstract-full" style="display: none;"> Delta Gravity is a gravitational model based on an extension of General Relativity given by a new symmetry called $\tilde未$. In this model, new matter fields are added to the original matter fields, motivated by the additional symmetry. We call them $\tilde未$ matter fields. This model predicts an accelerating Universe without the need to introduce a cosmological constant. In this work, we study the Delta Gravity prediction about the scalar CMB TT power spectrum using an analytical hydrodynamical approach. To fit the Planck satellite's data with the DG model, we used a Markov Chain Monte Carlo analysis. We also include a study about the compatibility between SNe-Ia and CMB observations in the Delta Gravity Context. Finally, we obtain the scalar CMB TT power spectrum and the fitted parameters needed to explain both SNe-Ia Data and CMB measurements. The results are in a reasonable agreement with both observations considering the analytical approximation. We also discuss if the Hubble Constant and the Accelerating Universe are in concordance with the observational evidence in the Delta Gravity context. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.13305v1-abstract-full').style.display = 'none'; document.getElementById('2009.13305v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.01855">arXiv:2009.01855</a> <span> [<a href="https://arxiv.org/pdf/2009.01855">pdf</a>, <a href="https://arxiv.org/format/2009.01855">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div 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/staa2655">10.1093/mnras/staa2655 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A revised view of the Canis Major stellar overdensity with DECam and Gaia: new evidence of a stellar warp of blue stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carballo-Bello%2C+J+A">Julio A. Carballo-Bello</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez-Delgado%2C+D">David Mart铆nez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Corral-Santana%2C+J+M">Jes煤s M. Corral-Santana</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">Camila Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M谩rcio Catelan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.01855v1-abstract-short" style="display: inline;"> We present DECam imaging combined with Gaia DR2 data to study the Canis Major overdensity. The presence of the so-called Blue Plume stars in a low-pollution area of the color-magnitude diagram allows us to derive the distance and proper motions of this stellar feature along the line of sight of its hypothetical core. The stellar overdensity extends on a large area of the sky at low Galactic latitu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01855v1-abstract-full').style.display = 'inline'; document.getElementById('2009.01855v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.01855v1-abstract-full" style="display: none;"> We present DECam imaging combined with Gaia DR2 data to study the Canis Major overdensity. The presence of the so-called Blue Plume stars in a low-pollution area of the color-magnitude diagram allows us to derive the distance and proper motions of this stellar feature along the line of sight of its hypothetical core. The stellar overdensity extends on a large area of the sky at low Galactic latitudes, below the plane, and between 230$^\circ < \ell < 255^\circ$. According to the orbit derived for Canis Major, it presents an on-plane rotation around the Milky Way. Moreover, additional overdensities of Blue Plume stars are found around the plane and across the Galaxy, proving that these objects are not only associated with that structure. The spatial distribution of these stars, derived using Gaia astrometric data, confirms that the detection of the Canis Major overdensity results more from the warped structure of the Milky Way disk than from the accretion of a dwarf galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01855v1-abstract-full').style.display = 'none'; document.getElementById('2009.01855v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 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/2009.00610">arXiv:2009.00610</a> <span> [<a href="https://arxiv.org/pdf/2009.00610">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 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/10.1051/0004-6361/202037620">10.1051/0004-6361/202037620 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Calibrating the lithium-age relation with open clusters and associations. I. Cluster age range and initial membership selections </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albarr%C3%A1n%2C+M+L+G">M. L. Guti茅rrez Albarr谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Garrido%2C+M+G">M. G贸mez Garrido</a>, <a href="/search/astro-ph?searchtype=author&query=Tabernero%2C+H+M">H. M. Tabernero</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. G贸nzalez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Marfil%2C+E">E. Marfil</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Klutsch%2C+A">A. Klutsch</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito%2C+R">R. Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Mena%2C+E+D">E. Delgado Mena</a>, <a href="/search/astro-ph?searchtype=author&query=Feltzing%2C+S">S. Feltzing</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a> , et al. (11 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="2009.00610v1-abstract-short" style="display: inline;"> Previous studies of open clusters have shown that lithium depletion is not only strongly age dependent but also shows a complex pattern with other parameters that is not yet understood. For pre- and main-sequence late-type stars, these parameters include metallicity, mixing mechanisms, convection structure, rotation, and magnetic activity. We perform a thorough membership analysis for a large numb… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.00610v1-abstract-full').style.display = 'inline'; document.getElementById('2009.00610v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.00610v1-abstract-full" style="display: none;"> Previous studies of open clusters have shown that lithium depletion is not only strongly age dependent but also shows a complex pattern with other parameters that is not yet understood. For pre- and main-sequence late-type stars, these parameters include metallicity, mixing mechanisms, convection structure, rotation, and magnetic activity. We perform a thorough membership analysis for a large number of stars observed within the Gaia-ESO survey (GES) in the field of 20 open clusters, ranging in age from young clusters and associations, to intermediate-age and old open clusters. Based on the parameters derived from the GES spectroscopic observations, we obtained lists of candidate members for each of the clusters in the sample by deriving RV distributions and studying the position of the kinematic selections in the EW(Li) versus Teff plane to obtain lithium members. We used gravity indicators to discard field contaminants and studied [Fe/H] metallicity to further confirm the membership of the candidates. We also made use of studies using recent data from the Gaia DR1 and DR2 releases to assess our member selections. We identified likely member candidates for the sample of 20 clusters observed in GES (iDR4) with UVES and GIRAFFE, and conducted a comparative study that allowed us to characterize the properties of these members, as well as identify field contaminant stars, both lithium-rich giants and non-giant outliers. This work is the first step towards the calibration of the lithium-age relation and its dependence on other GES parameters. During this project we aim to use this relation to infer the ages of GES field stars, and identify their potential membership to young associations and stellar kinematic groups of different ages. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.00610v1-abstract-full').style.display = 'none'; document.getElementById('2009.00610v1-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 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">264 pages, 105 figures. To be published in A&A, accepted 29th July 2020</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 643, A71 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.16129">arXiv:2007.16129</a> <span> [<a href="https://arxiv.org/pdf/2007.16129">pdf</a>, <a href="https://arxiv.org/format/2007.16129">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-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/10.1088/1475-7516/2021/01/057">10.1088/1475-7516/2021/01/057 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Araudo%2C+A">A. Araudo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M">M. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a> , et al. (427 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="2007.16129v2-abstract-short" style="display: inline;"> We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models giv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.16129v2-abstract-full').style.display = 'inline'; document.getElementById('2007.16129v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.16129v2-abstract-full" style="display: none;"> We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models given a standard cuspy profile of the dark matter density distribution. Importantly, even for a cored profile, the projected sensitivity of CTA will be sufficient to probe various well-motivated models of thermally produced dark matter at the TeV scale. This is due to CTA's unprecedented sensitivity, angular and energy resolutions, and the planned observational strategy. The survey of the inner Galaxy will cover a much larger region than corresponding previous observational campaigns with imaging atmospheric Cherenkov telescopes. CTA will map with unprecedented precision the large-scale diffuse emission in high-energy gamma rays, constituting a background for dark matter searches for which we adopt state-of-the-art models based on current data. Throughout our analysis, we use up-to-date event reconstruction Monte Carlo tools developed by the CTA consortium, and pay special attention to quantifying the level of instrumental systematic uncertainties, as well as background template systematic errors, required to probe thermally produced dark matter at these energies. "Full likelihood tables complementing our analysis are provided here [ https://doi.org/10.5281/zenodo.4057987 ]" <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.16129v2-abstract-full').style.display = 'none'; document.getElementById('2007.16129v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">68 pages (including references) and 26 figures; text identical to the version published in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP01(2021)057 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.10189">arXiv:2007.10189</a> <span> [<a href="https://arxiv.org/pdf/2007.10189">pdf</a>, <a href="https://arxiv.org/format/2007.10189">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201936726">10.1051/0004-6361/201936726 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Spectroscopic-asteroseismic analysis of K2 stars in Gaia-ESO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Jofre%2C+P">P. Jofre</a>, <a href="/search/astro-ph?searchtype=author&query=Rendle%2C+B">B. Rendle</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">A. Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D">D. Feuillet</a>, <a href="/search/astro-ph?searchtype=author&query=Gavel%2C+A">A. Gavel</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Lind%2C+K">K. Lind</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A">A. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Francois%2C+P">P. Francois</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J">J. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G">G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Feltzing%2C+S">S. Feltzing</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M">M. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Solares%2C+E+G">E. Gonzalez Solares</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+D">D. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a> , et al. (11 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="2007.10189v2-abstract-short" style="display: inline;"> The extensive stellar spectroscopic datasets that are available for studies in Galactic Archeaology thanks to, for example, the Gaia-ESO Survey, now benefit from having a significant number of targets that overlap with asteroseismology projects such as Kepler, K2 and CoRoT. Combining the measurements from spectroscopy and asteroseismology allows us to attain greater accuracy with regard to the ste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.10189v2-abstract-full').style.display = 'inline'; document.getElementById('2007.10189v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.10189v2-abstract-full" style="display: none;"> The extensive stellar spectroscopic datasets that are available for studies in Galactic Archeaology thanks to, for example, the Gaia-ESO Survey, now benefit from having a significant number of targets that overlap with asteroseismology projects such as Kepler, K2 and CoRoT. Combining the measurements from spectroscopy and asteroseismology allows us to attain greater accuracy with regard to the stellar parameters needed to characterise the stellar populations of the Milky Way. The aim of this Gaia-ESO Survey special project is to produce a catalogue of self-consistent stellar parameters by combining measurements from high-resolution spectroscopy and precision asteroseismology. We carried out an iterative analysis of 90 K2@Gaia-ESO red giants. The spectroscopic values of Teff were used as input in the seismic analysis to obtain log(g) values. The seismic estimates of log(g) were then used to re-determine the spectroscopic values of Teff and [Fe/H]. Only one iteration was required to obtain parameters that are in good agreement for both methods and thus, to obtain the final stellar parameters. A detailed analysis of outliers was carried out to ensure a robust determination of the parameters. The results were then combined with Gaia DR2 data to compare the seismic log(g) with a parallax-based log(g) and to investigate instances of variations in the velocity and possible binaries within the dataset. This analysis produced a high-quality catalogue of stellar parameters for 90 red giant stars observed by both K2 and Gaia-ESO that were determined through iterations between spectroscopy and asteroseismology. We compared the seismic gravities with those based on Gaia parallaxes to find an offset which is similar to other studies that have used asteroseismology. Our catalogue also includes spectroscopic chemical abundances and radial velocities, as well as indicators for possible binary detections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.10189v2-abstract-full').style.display = 'none'; document.getElementById('2007.10189v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 26 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 643, A83 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.01910">arXiv:2007.01910</a> <span> [<a href="https://arxiv.org/pdf/2007.01910">pdf</a>, <a href="https://arxiv.org/format/2007.01910">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038841">10.1051/0004-6361/202038841 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The miniJPAS survey: a preview of the Universe in 56 colours </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bonoli%2C+S">S. Bonoli</a>, <a href="/search/astro-ph?searchtype=author&query=Mar%C3%ADn-Franch%2C+A">A. Mar铆n-Franch</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+J">J. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Rami%C3%B3%2C+H+V">H. V谩zquez Rami贸</a>, <a href="/search/astro-ph?searchtype=author&query=Abramo%2C+L+R">L. R. Abramo</a>, <a href="/search/astro-ph?searchtype=author&query=Cenarro%2C+A+J">A. J. Cenarro</a>, <a href="/search/astro-ph?searchtype=author&query=Dupke%2C+R+A">R. A. Dupke</a>, <a href="/search/astro-ph?searchtype=author&query=V%C3%ADlchez%2C+J+M">J. M. V铆lchez</a>, <a href="/search/astro-ph?searchtype=author&query=Crist%C3%B3bal-Hornillos%2C+D">D. Crist贸bal-Hornillos</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado%2C+R+M+G">R. M. Gonz谩lez Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez-Monteagudo%2C+C">C. Hern谩ndez-Monteagudo</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Sanjuan%2C+C">C. L贸pez-Sanjuan</a>, <a href="/search/astro-ph?searchtype=author&query=Muniesa%2C+D+J">D. J. Muniesa</a>, <a href="/search/astro-ph?searchtype=author&query=Civera%2C+T">T. Civera</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1n-Caballero%2C+A">A. Hern谩n-Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Marra%2C+V">V. Marra</a>, <a href="/search/astro-ph?searchtype=author&query=Baqui%2C+P+O">P. O. Baqui</a>, <a href="/search/astro-ph?searchtype=author&query=Cortesi%2C+A">A. Cortesi</a>, <a href="/search/astro-ph?searchtype=author&query=Cypriano%2C+E+S">E. S. Cypriano</a>, <a href="/search/astro-ph?searchtype=author&query=Daflon%2C+S">S. Daflon</a>, <a href="/search/astro-ph?searchtype=author&query=de+Amorim%2C+A+L">A. L. de Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-Garc%C3%ADa%2C+L+A">L. A. D铆az-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Diego%2C+J+M">J. M. Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez-Solaeche%2C+G">G. Mart铆nez-Solaeche</a> , et al. (144 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="2007.01910v2-abstract-short" style="display: inline;"> The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will soon start to scan thousands of square degrees of the northern extragalactic sky with a unique set of $56$ optical filters from a dedicated $2.55$m telescope, JST, at the Javalambre Astrophysical Observatory. Before the arrival of the final instrument (a 1.2 Gpixels, 4.2deg$^2$ field-of-view camera), the JST was… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.01910v2-abstract-full').style.display = 'inline'; document.getElementById('2007.01910v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.01910v2-abstract-full" style="display: none;"> The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will soon start to scan thousands of square degrees of the northern extragalactic sky with a unique set of $56$ optical filters from a dedicated $2.55$m telescope, JST, at the Javalambre Astrophysical Observatory. Before the arrival of the final instrument (a 1.2 Gpixels, 4.2deg$^2$ field-of-view camera), the JST was equipped with an interim camera (JPAS-Pathfinder), composed of one CCD with a 0.3deg$^2$ field-of-view and resolution of 0.23 arcsec pixel$^{-1}$. To demonstrate the scientific potential of J-PAS, with the JPAS-Pathfinder camera we carried out a survey on the AEGIS field (along the Extended Groth Strip), dubbed miniJPAS. We observed a total of $\sim 1$ deg$^2$, with the $56$ J-PAS filters, which include $54$ narrow band (NB, $\rm{FWHM} \sim 145$Angstrom) and two broader filters extending to the UV and the near-infrared, complemented by the $u,g,r,i$ SDSS broad band (BB) filters. In this paper we present the miniJPAS data set, the details of the catalogues and data access, and illustrate the scientific potential of our multi-band data. The data surpass the target depths originally planned for J-PAS, reaching $\rm{mag}_{\rm {AB}}$ between $\sim 22$ and $23.5$ for the NB filters and up to $24$ for the BB filters ($5蟽$ in a $3$~arcsec aperture). The miniJPAS primary catalogue contains more than $64,000$ sources extracted in the $r$ detection band with forced photometry in all other bands. We estimate the catalogue to be complete up to $r=23.6$ for point-like sources and up to $r=22.7$ for extended sources. Photometric redshifts reach subpercent precision for all sources up to $r=22.5$, and a precision of $\sim 0.3$% for about half of the sample. (Abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.01910v2-abstract-full').style.display = 'none'; document.getElementById('2007.01910v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">The miniJPAS data and associated value added catalogues are publicly accessible via this url: http://archive.cefca.es/catalogues/minijpas-pdr201912</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 653, A31 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.07228">arXiv:2005.07228</a> <span> [<a href="https://arxiv.org/pdf/2005.07228">pdf</a>, <a href="https://arxiv.org/format/2005.07228">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/10.1051/0004-6361/202037697">10.1051/0004-6361/202037697 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy classification: deep learning on the OTELO and COSMOS databases </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Diego%2C+J+A">Jos茅 A. de Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Nadolny%2C+J">Jakub Nadolny</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiovanni%2C+%C3%81">脕ngel Bongiovanni</a>, <a href="/search/astro-ph?searchtype=author&query=Cepa%2C+J">Jordi Cepa</a>, <a href="/search/astro-ph?searchtype=author&query=Povi%C4%87%2C+M">Mirjana Povi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+A+M+P">Ana Mar铆a P茅rez Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Torres%2C+C+P+P">Carmen P. Padilla Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Lara-L%C3%B3pez%2C+M+A">Maritza A. Lara-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Cervi%C3%B1o%2C+M">Miguel Cervi帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+R+P">Ricardo P茅rez Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Casta%C3%B1eda%2C+H+O">H茅ctor O. Casta帽eda</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Lorenzo%2C+M">Miriam Fern谩ndez-Lorenzo</a>, <a href="/search/astro-ph?searchtype=author&query=Gallego%2C+J">Jes煤s Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+J">J. Jes煤s Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Serrano%2C+J+I">J. Ignacio Gonz谩lez-Serrano</a>, <a href="/search/astro-ph?searchtype=author&query=Pintos-Castro%2C+I">Irene Pintos-Castro</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Portal%2C+M">Miguel S谩nchez-Portal</a>, <a href="/search/astro-ph?searchtype=author&query=Cedr%C3%A9s%2C+B">Bernab? Cedr茅s</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Otero%2C+M">Mauro Gonz谩lez-Otero</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+H">D. Heath Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.07228v1-abstract-short" style="display: inline;"> Context. The accurate classification of hundreds of thousands of galaxies observed in modern deep surveys is imperative if we want to understand the universe and its evolution. Aims. Here, we report the use of machine learning techniques to classify early- and late-type galaxies in the OTELO and COSMOS databases using optical and infrared photometry and available shape parameters: either the Sersi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.07228v1-abstract-full').style.display = 'inline'; document.getElementById('2005.07228v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.07228v1-abstract-full" style="display: none;"> Context. The accurate classification of hundreds of thousands of galaxies observed in modern deep surveys is imperative if we want to understand the universe and its evolution. Aims. Here, we report the use of machine learning techniques to classify early- and late-type galaxies in the OTELO and COSMOS databases using optical and infrared photometry and available shape parameters: either the Sersic index or the concentration index. Methods. We used three classification methods for the OTELO database: 1) u-r color separation , 2) linear discriminant analysis using u-r and a shape parameter classification, and 3) a deep neural network using the r magnitude, several colors, and a shape parameter. We analyzed the performance of each method by sample bootstrapping and tested the performance of our neural network architecture using COSMOS data. Results. The accuracy achieved by the deep neural network is greater than that of the other classification methods, and it can also operate with missing data. Our neural network architecture is able to classify both OTELO and COSMOS datasets regardless of small differences in the photometric bands used in each catalog. Conclusions. In this study we show that the use of deep neural networks is a robust method to mine the cataloged data <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.07228v1-abstract-full').style.display = 'none'; document.getElementById('2005.07228v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 tables, 14 figures, Astronomy and Astrophysics (in press)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 638, A134 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.08978">arXiv:2002.08978</a> <span> [<a href="https://arxiv.org/pdf/2002.08978">pdf</a>, <a href="https://arxiv.org/format/2002.08978">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/10.1051/0004-6361/201833656e">10.1051/0004-6361/201833656e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The OTELO survey. A case study of [O III]4959,5007 emitters at <z> = 0.83 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bongiovanni%2C+%C3%81">脕ngel Bongiovanni</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%B3n-P%C3%A9rez%2C+M">Marina Ram贸n-P茅rez</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+A+M+P">Ana Mar铆a P茅rez Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Cervi%C3%B1o%2C+M">Miguel Cervi帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Cepa%2C+J">Jordi Cepa</a>, <a href="/search/astro-ph?searchtype=author&query=Nadolny%2C+J">Jakub Nadolny</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+R+P">Ricardo P茅rez Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Casta%C3%B1eda%2C+H">H茅ctor Casta帽eda</a>, <a href="/search/astro-ph?searchtype=author&query=Cedr%C3%A9s%2C+B">Bernab茅 Cedr茅s</a>, <a href="/search/astro-ph?searchtype=author&query=de+Diego%2C+J+A">Jos茅 A. de Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">Alessandro Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Lorenzo%2C+M">Mirian Fern谩ndez-Lorenzo</a>, <a href="/search/astro-ph?searchtype=author&query=Gallego%2C+J">Jes煤s Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+J">J. Jes煤s Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Serrano%2C+J+I">J. Ignacio Gonz谩lez-Serrano</a>, <a href="/search/astro-ph?searchtype=author&query=Lara-L%C3%B3pez%2C+M+A">Maritza A. Lara-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+I+O">Iv谩n Oteo G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Torres%2C+C+P+P">Carmen P. Padilla Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Pintos-Castro%2C+I">Irene Pintos-Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Povi%C4%87%2C+M">Mirjana Povi膰</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Portal%2C+M">Miguel S谩nchez-Portal</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+H">D. Heath Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera-Lavers%2C+A">Antonio Cabrera-Lavers</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.08978v2-abstract-short" style="display: inline;"> The OTELO survey is a very deep, blind exploration of a selected region of the Extended Groth Strip and is designed for finding emission-line sources (ELSs). The survey design, observations, data reduction, astrometry, and photometry, as well as the correlation with ancillary data used to obtain a final catalogue, including photo-z estimates and a preliminary selection of ELS, were described in a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.08978v2-abstract-full').style.display = 'inline'; document.getElementById('2002.08978v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.08978v2-abstract-full" style="display: none;"> The OTELO survey is a very deep, blind exploration of a selected region of the Extended Groth Strip and is designed for finding emission-line sources (ELSs). The survey design, observations, data reduction, astrometry, and photometry, as well as the correlation with ancillary data used to obtain a final catalogue, including photo-z estimates and a preliminary selection of ELS, were described in a previous contribution. Here, we aim to determine the main properties and luminosity function (LF) of the [O III] ELS sample of OTELO as a scientific demonstration of its capabilities, advantages, and complementarity with respect to other surveys. The selection and analysis procedures of ELS candidates obtained using tunable filter (TF) pseudo-spectra are described. We performed simulations in the parameter space of the survey to obtain emission-line detection probabilities. Relevant characteristics of [O III] emitters and the LF([O III]), including the main selection biases and uncertainties, are presented. A total of 184 sources were confirmed as [O III] emitters at a mean redshift z=0.83. The minimum detectable line flux and equivalent width (EW) in this ELS sample are $\sim$5 $\times$ 10$^{-19}$ erg s$^{-1}$ cm$^{2}$ and $\sim$6 脜, respectively. We are able to constrain the faint-end slope ($伪= -1.03\pm0.08$) of the observed LF([O III]) at z=0.83. This LF reaches values that are approximately ten times lower than those from other surveys. The vast majority (84\%) of the morphologically classified [O III] ELSs are disc-like sources, and 87\% of this sample is comprised of galaxies with stellar masses of M$_\star$ $<$ 10$^{10}$ M$_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.08978v2-abstract-full').style.display = 'none'; document.getElementById('2002.08978v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">v1: 16 pages, 6 figures. Accepted in Astronomy \& Astrophysics. v2: Author added in metadata</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 637, C2 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.08354">arXiv:2001.08354</a> <span> [<a href="https://arxiv.org/pdf/2001.08354">pdf</a>, <a href="https://arxiv.org/format/2001.08354">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="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Cosmological Fluctuations in Delta Gravity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Rubio%2C+C">Carlos Rubio</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn%2C+M+S">Marco San Mart铆n</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="2001.08354v2-abstract-short" style="display: inline;"> About 70\% of the Universe is Dark Energy, but the physics community still does not know what it is. Delta Gravity (DG) is an alternative theory of gravitation that could solve this cosmological problem. Previously, we studied the Universe's accelerated expansion, where DG was able to explain the SNe-Ia data successfully. In this work, we explore the cosmological fluctuations that give rise to the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08354v2-abstract-full').style.display = 'inline'; document.getElementById('2001.08354v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08354v2-abstract-full" style="display: none;"> About 70\% of the Universe is Dark Energy, but the physics community still does not know what it is. Delta Gravity (DG) is an alternative theory of gravitation that could solve this cosmological problem. Previously, we studied the Universe's accelerated expansion, where DG was able to explain the SNe-Ia data successfully. In this work, we explore the cosmological fluctuations that give rise to the CMB through a hydrodynamic approximation. We calculate the gauge transformations for the metric and the perfect fluid to present the equations of the evolution of cosmological fluctuations, providing the necessary equations to solve in a semi-analytical way the scalar TT Power Spectrum. These equations will be useful for comparing the DG theory with astronomical observations and thus being able to constraint the DG cosmology, testing, in the future, the compatibility with the CMB Planck data, which are currently in controversy with SNe-Ia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08354v2-abstract-full').style.display = 'none'; document.getElementById('2001.08354v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">39 pages, latex</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.03179">arXiv:2001.03179</a> <span> [<a href="https://arxiv.org/pdf/2001.03179">pdf</a>, <a href="https://arxiv.org/format/2001.03179">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201937055">10.1051/0004-6361/201937055 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: a new approach to chemically characterising young open clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Tsantaki%2C+M">M. Tsantaki</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvaisiene%2C+G">G. Tautvaisiene</a>, <a href="/search/astro-ph?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">P. Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nes-Esteban%2C+F+M">F. M. Jim茅nes-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado-Mena%2C+E">E. Delgado-Mena</a>, <a href="/search/astro-ph?searchtype=author&query=Martell%2C+S">S. Martell</a>, <a href="/search/astro-ph?searchtype=author&query=Van+der+Swaelmen%2C+M">M. Van der Swaelmen</a>, <a href="/search/astro-ph?searchtype=author&query=Roccatagliata%2C+V">V. Roccatagliata</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a> , et al. (11 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="2001.03179v1-abstract-short" style="display: inline;"> Open clusters (OCs) are recognised as excellent tracers of Galactic thin-disc properties. At variance with intermediate-age and old OCs, for which a significant number of studies is now available, clusters younger than 150 Myr have been mostly overlooked in terms of their chemical composition, with few exceptions. On the other hand, previous investigations seem to indicate an anomalous behaviour o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03179v1-abstract-full').style.display = 'inline'; document.getElementById('2001.03179v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.03179v1-abstract-full" style="display: none;"> Open clusters (OCs) are recognised as excellent tracers of Galactic thin-disc properties. At variance with intermediate-age and old OCs, for which a significant number of studies is now available, clusters younger than 150 Myr have been mostly overlooked in terms of their chemical composition, with few exceptions. On the other hand, previous investigations seem to indicate an anomalous behaviour of young clusters, which includes slightly sub-solar iron (Fe) abundances and extreme, unexpectedly high barium (Ba) enhancements. In a series of papers, we plan to expand our understanding of this topic and investigate whether these chemical peculiarities are instead related to abundance analysis techniques. We present a new determination of the atmospheric parameters for 23 dwarf stars observed by the Gaia-ESO survey in five young OCs (younger than 150 Myr) and one star-forming region (NGC 2264). We exploit a new method based on titanium (Ti) lines to derive the spectroscopic surface gravity, and most importantly, the microturbulence parameter. A combination of Ti I and Fe I lines is used to obtain effective temperatures. We also infer the abundances of Fe II, Ti II, Na I, Mg I, Al I, Si I, Ca I, Cr I and Ni I. Our findings are in fair agreement with Gaia-ESO iDR5 results for effective temperatures and surface gravities, but suggest that for very young stars, the microturbulence parameter is over-estimated when Fe lines are employed. This affects the derived chemical composition and causes the metal content of very young clusters to be under-estimated. Our clusters display a metallicity [Fe/H] between +0.04 and +0.12; they are not more metal poor than the Sun. Although based on a relatively small sample size, our explorative study suggests that we may not need to call for ad hoc explanations to reconcile the chemical composition of young OCs with Galactic chemical evolution models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03179v1-abstract-full').style.display = 'none'; document.getElementById('2001.03179v1-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 11 figures, accepted by A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.09828">arXiv:1906.09828</a> <span> [<a href="https://arxiv.org/pdf/1906.09828">pdf</a>, <a href="https://arxiv.org/format/1906.09828">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201834636">10.1051/0004-6361/201834636 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: The inner disc, intermediate-age open cluster Pismis 18 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hatzidimitriou%2C+D">D. Hatzidimitriou</a>, <a href="/search/astro-ph?searchtype=author&query=Held%2C+E+V">E. V. Held</a>, <a href="/search/astro-ph?searchtype=author&query=Tognelli%2C+E">E. Tognelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Bravi%2C+L">L. Bravi</a>, <a href="/search/astro-ph?searchtype=author&query=Gazeas%2C+K">K. Gazeas</a>, <a href="/search/astro-ph?searchtype=author&query=Dapergolas%2C+A">A. Dapergolas</a>, <a href="/search/astro-ph?searchtype=author&query=Drazdauskas%2C+A">A. Drazdauskas</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado-Mena%2C+E">E. Delgado-Mena</a>, <a href="/search/astro-ph?searchtype=author&query=Friel%2C+E+D">E. D. Friel</a>, <a href="/search/astro-ph?searchtype=author&query=Minkeviciute%2C+R">R. Minkeviciute</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvaisiene%2C+G">G. Tautvaisiene</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Feltzing%2C+S">S. Feltzing</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Flaccomio%2C+E">E. Flaccomio</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a> , et al. (12 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="1906.09828v1-abstract-short" style="display: inline;"> Pismis 18 is a moderately populated, intermediate-age open cluster located within the solar circle at a Galactocentric distance of about 7 kpc. Few open clusters have been studied in detail in the inner disc region before the Gaia-ESO Survey. New data from the Gaia-ESO Survey allowed us to conduct an extended radial velocity membership study as well as spectroscopic metallicity and detailed chemic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.09828v1-abstract-full').style.display = 'inline'; document.getElementById('1906.09828v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.09828v1-abstract-full" style="display: none;"> Pismis 18 is a moderately populated, intermediate-age open cluster located within the solar circle at a Galactocentric distance of about 7 kpc. Few open clusters have been studied in detail in the inner disc region before the Gaia-ESO Survey. New data from the Gaia-ESO Survey allowed us to conduct an extended radial velocity membership study as well as spectroscopic metallicity and detailed chemical abundance measurements for this cluster. Gaia-ESO Survey data for 142 potential members, lying on the upper MS and on the red clump, yielded radial velocity measurements, which, together with proper motion measurements from the Gaia DR2, were used to determine the systemic velocity of the cluster and membership of individual stars. Photometry from Gaia DR2 was used to re-determine cluster parameters based on high confidence member stars only. Cluster abundance measurements of six radial-velocity member stars with UVES high-resolution spectroscopy are presented for 23 elements. According to the new estimates, based on high confidence members, Pismis 18 has an age of $700^{+40}_{-50}$ Myr, interstellar reddening of E(B-V) = $0.562^{+0.012}_{-0.026}$ mag and a de-reddened distance modulus of $DM_0 = 11.96^{+0.10}_{-0.24}$ mag. The median metallicity of the cluster (using the six UVES stars) is [Fe/H] = $+0.23 \pm 0.05$ dex, with [$伪$/Fe]= $0.07 \pm 0.13$ and a slight enhancement of s- and r- neutron-capture elements. With the present work, we fully characterized the open cluster Pismis 18, confirming its present location in the inner disc. We estimated a younger age than the previous literature values and gave, for the first time, its metallicity and its detailed abundances. Its [$伪$/Fe] and [s-process/Fe], both slightly super-solar, are in agreement with other inner-disc open clusters observed by the Gaia-ESO survey. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.09828v1-abstract-full').style.display = 'none'; document.getElementById('1906.09828v1-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 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 10 figures, 8 tables (Table 2 available at the CDS)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy & Astrophysics, 2019, Volume 626, id.A90, 14 pp </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.11385">arXiv:1904.11385</a> <span> [<a href="https://arxiv.org/pdf/1904.11385">pdf</a>, <a href="https://arxiv.org/format/1904.11385">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/10.1051/0004-6361/201935359">10.1051/0004-6361/201935359 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MONOS: Multiplicity Of Northern O-type Spectroscopic systems. I. Project description and spectral classifications and visual multiplicity of previously known objects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Lorenzo%2C+J">J. Lorenzo</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R+C">R. C. Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Fari%C3%B1a%2C+C">C. Fari帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Salas%2C+J">J. Salas</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N+I">N. I. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Pellerin%2C+A">A. Pellerin</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">J. I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Marco%2C+A">A. Marco</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.11385v1-abstract-short" style="display: inline;"> [ABRIDGED] AIMS. MONOS is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 1st paper we describe the sample and provide spectral classifications and additional information for objects with previous SB or EB orbits. In the future we will test the validity of previous solutions and calculate new SB orbits. METHODS.The spectra in this paper have 2 source… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.11385v1-abstract-full').style.display = 'inline'; document.getElementById('1904.11385v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.11385v1-abstract-full" style="display: none;"> [ABRIDGED] AIMS. MONOS is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 1st paper we describe the sample and provide spectral classifications and additional information for objects with previous SB or EB orbits. In the future we will test the validity of previous solutions and calculate new SB orbits. METHODS.The spectra in this paper have 2 sources: GOSSS, which is obtaining blue-violet R~2500 spectroscopy of thousands of massive stars, and LiLiMaRlin, a library of libraries of high-resolution spectroscopy of massive stars obtained from 4 different surveys and additional data from our own observing programs and public archives. We also use lucky images from AstraLux. RESULTS. We present homogeneous spectral classifications for 92 O-type spectroscopic multiple systems and 10 optical companions. We discuss the visual multiplicity of each system with the support of AstraLux images and additional sources. For 11 O-type objects and for 6 B-type objects we present their first GOSSS spectral classifications. For 2 known EBs we detect SB2/SB1 lines for the first time, to which we add a third system already reported by us recently. For 2 previous SB1 systems we detect their SB2 nature for the first time and give their first separate spectral classifications, something we also do for a 3rd object just recently identified as a SB2. We also detect 9 new astrometric companions and provide updated information on several others. For sigma Ori AaAbB we provide spectral classifications for the 3 components with a single observation for the first time thanks to a lucky spectroscopy observation obtained close to the Aa,Ab periastron and for theta^1 Ori CaCb we add it to the class of Galactic Of?p stars, raising the number of its members to 6. Our sample of O-type spectroscopic binaries contains more triple/higher-order systems than double systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.11385v1-abstract-full').style.display = 'none'; document.getElementById('1904.11385v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 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 626, A20 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.01577">arXiv:1904.01577</a> <span> [<a href="https://arxiv.org/pdf/1904.01577">pdf</a>, <a href="https://arxiv.org/format/1904.01577">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/stz842">10.1093/mnras/stz842 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GALANTE Photometric System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lorenzo-Guti%C3%A9rrez%2C+A">A. Lorenzo-Guti茅rrez</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Mar%C3%ADn-Franch%2C+A">A. Mar铆n-Franch</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Crist%C3%B3bal-Hornillos%2C+D">D. Crist贸bal-Hornillos</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+J">J. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Rami%C3%B3%2C+H+V">H. V谩zquez Rami贸</a>, <a href="/search/astro-ph?searchtype=author&query=Cenarro%2C+J">J. Cenarro</a>, <a href="/search/astro-ph?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Lario%2C+P">P. Garc铆a-Lario</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.01577v1-abstract-short" style="display: inline;"> This paper describes the characterization of the GALANTE photometric system, a seven intermediate- and narrow-band filter system with a wavelength coverage from 3000 $脜$ to 9000 $脜$ . We describe the photometric system presenting the full sensitivity curve as a product of the filter sensitivity, CCD, telescope mirror, and atmospheric transmission curves, as well as some first- and second-order mom… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01577v1-abstract-full').style.display = 'inline'; document.getElementById('1904.01577v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.01577v1-abstract-full" style="display: none;"> This paper describes the characterization of the GALANTE photometric system, a seven intermediate- and narrow-band filter system with a wavelength coverage from 3000 $脜$ to 9000 $脜$ . We describe the photometric system presenting the full sensitivity curve as a product of the filter sensitivity, CCD, telescope mirror, and atmospheric transmission curves, as well as some first- and second-order moments of this sensitivity function. The GALANTE photometric system is composed of four filters from the J-PLUS photometric system, a twelve broad-to-narrow filter system, and three exclusive filters, specifically designed to measure the physical parameters of stars such as effective temperature $T_{\rm eff}$, $\log(g)$, metallicity, colour excess $E(4405-5495)$, and extinction type $R_{5495}$. Two libraries, the Next Generation Spectral Library (NGSL) and the one presented in Ma铆z Apell谩niz & Weiler (2018), have been used to determine the transformation equations between the Sloan Digital Sky Survey ($\textit{SDSS}$) $\textit{ugriz}$ photometry and the GALANTE photometric system. We will use this transformation to calibrate the zero points of GALANTE images. To this end, a preliminary photometric calibration of GALANTE has been made based on two different $\textit{griz}$ libraries ($\textit{SDSS}$ DR12 and ATLAS All-Sky Stellar Reference Catalog, hereinafter $\textit{RefCat2}$). A comparison between both zero points is performed leading us to the choice of $\textit{RefCat2}$ as the base catalogue for this calibration, and applied to a field in the Cyg OB2 association. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01577v1-abstract-full').style.display = 'none'; document.getElementById('1904.01577v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.01426">arXiv:1904.01426</a> <span> [<a href="https://arxiv.org/pdf/1904.01426">pdf</a>, <a href="https://arxiv.org/format/1904.01426">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2019.04.001">10.1016/j.astropartphys.2019.04.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Barai%2C+P">P. Barai</a>, <a href="/search/astro-ph?searchtype=author&query=Barbano%2C+A">A. Barbano</a>, <a href="/search/astro-ph?searchtype=author&query=Barkov%2C+M">M. Barkov</a> , et al. (445 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.01426v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is the major next-generation observatory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01426v1-abstract-full').style.display = 'inline'; document.getElementById('1904.01426v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.01426v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is the major next-generation observatory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possible by using tens of imaging Cherenkov telescopes of three successive sizes. They will be arranged into two arrays, one per hemisphere, located on the La Palma island (Spain) and in Paranal (Chile). We present here the optimised and final telescope arrays for both CTA sites, as well as their foreseen performance, resulting from the analysis of three different large-scale Monte Carlo productions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01426v1-abstract-full').style.display = 'none'; document.getElementById('1904.01426v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">48 pages, 16 figures, accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.12176">arXiv:1903.12176</a> <span> [<a href="https://arxiv.org/pdf/1903.12176">pdf</a>, <a href="https://arxiv.org/ps/1903.12176">ps</a>, <a href="https://arxiv.org/format/1903.12176">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz870">10.1093/mnras/stz870 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Asymmetric expansion of the Lagoon Nebula cluster NGC 6530 from GES and Gaia DR2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wright%2C+N+J">Nicholas J. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito%2C+R">R. Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Kalari%2C+V">V. Kalari</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Parker%2C+R+J">R. J. Parker</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Vink%2C+J+S">J. S. Vink</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">P. Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">S. E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J">J. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</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="1903.12176v1-abstract-short" style="display: inline;"> The combination of precise radial velocities from multi-object spectroscopy and highly accurate proper motions from Gaia DR2 opens up the possibility for detailed 3D kinematic studies of young star forming regions and clusters. Here, we perform such an analysis by combining Gaia-ESO Survey spectroscopy with Gaia astrometry for ~900 members of the Lagoon Nebula cluster, NGC 6530. We measure the 3D… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.12176v1-abstract-full').style.display = 'inline'; document.getElementById('1903.12176v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.12176v1-abstract-full" style="display: none;"> The combination of precise radial velocities from multi-object spectroscopy and highly accurate proper motions from Gaia DR2 opens up the possibility for detailed 3D kinematic studies of young star forming regions and clusters. Here, we perform such an analysis by combining Gaia-ESO Survey spectroscopy with Gaia astrometry for ~900 members of the Lagoon Nebula cluster, NGC 6530. We measure the 3D velocity dispersion of the region to be $5.35^{+0.39}_{-0.34}$~km~s$^{-1}$, which is large enough to suggest the region is gravitationally unbound. The velocity ellipsoid is anisotropic, implying that the region is not sufficiently dynamically evolved to achieve isotropy, though the central part of NGC 6530 does exhibit velocity isotropy that suggests sufficient mixing has occurred in this denser part. We find strong evidence that the stellar population is expanding, though this is preferentially occurring in the declination direction and there is very little evidence for expansion in the right ascension direction. This argues against a simple radial expansion pattern, as predicted by models of residual gas expulsion. We discuss these findings in the context of cluster formation, evolution and disruption theories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.12176v1-abstract-full').style.display = 'none'; document.getElementById('1903.12176v1-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 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">18 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/1902.04550">arXiv:1902.04550</a> <span> [<a href="https://arxiv.org/pdf/1902.04550">pdf</a>, <a href="https://arxiv.org/format/1902.04550">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="General Relativity and Quantum Cosmology">gr-qc</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/s10714-020-02771-2">10.1007/s10714-020-02771-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A nontrivial footprint of standard cosmology in the future observations of low-frequency gravitational waves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Gamonal%2C+M">Mauricio Gamonal</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="1902.04550v4-abstract-short" style="display: inline;"> Recent research show that the cosmological components of the Universe should influence on the propagation of Gravitational Waves (GWs) and even it has been proposed a new way to measure the cosmological constant using Pulsar Timing Arrays (PTAs). However, these results have considered very particular cases (e.g. a de Sitter Universe or a mixing with non-relativistic matter). In this work we propos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.04550v4-abstract-full').style.display = 'inline'; document.getElementById('1902.04550v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.04550v4-abstract-full" style="display: none;"> Recent research show that the cosmological components of the Universe should influence on the propagation of Gravitational Waves (GWs) and even it has been proposed a new way to measure the cosmological constant using Pulsar Timing Arrays (PTAs). However, these results have considered very particular cases (e.g. a de Sitter Universe or a mixing with non-relativistic matter). In this work we propose an extension of these results, using the Hubble constant as the natural parameter that includes all the cosmological information and studying its effect on the propagation of GWs. Using linearized gravity we considered a mixture of perfect fluids permeating the spacetime and studied the propagation of GWs within the context of the LCDM model. We found from numerical simulations that the timing residual of local pulsars should present a distinguishable peak depending on the local value of the Hubble constant. As a consequence, when assuming the standard LCDM model, our result predicts that the region of maximum timing residual is determined by the redshift of the source. This framework represents a new test for the standard cosmological model, and it can be used to facilitate the measurements of gravitational wave by ongoing PTAs projects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.04550v4-abstract-full').style.display = 'none'; document.getElementById('1902.04550v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">19 pages, 7 figures, 3 tables. Initially submitted to ApJ on March 5, 2019</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Gen Relativ Gravit 52, 118 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.09589">arXiv:1901.09589</a> <span> [<a href="https://arxiv.org/pdf/1901.09589">pdf</a>, <a href="https://arxiv.org/ps/1901.09589">ps</a>, <a href="https://arxiv.org/format/1901.09589">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201834870">10.1051/0004-6361/201834870 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: age spread in the star forming region NGC6530 from the HR diagram and gravity indicators </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Kalari%2C+V">V. Kalari</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R">R. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito%2C+R">R. Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+N+J">N. J. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Tognelli%2C+E">E. Tognelli</a>, <a href="/search/astro-ph?searchtype=author&query=Guarcello%2C+M+G">M. G. Guarcello</a>, <a href="/search/astro-ph?searchtype=author&query=Vink%2C+J+S">J. S. Vink</a>, <a href="/search/astro-ph?searchtype=author&query=Klutsch%2C+A">A. Klutsch</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F+M">F. M. Jim茅nez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Roccatagliata%2C+V">V. Roccatagliata</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Flaccomio%2C+E">E. Flaccomio</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S">S. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A">A. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a> , et al. (11 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="1901.09589v1-abstract-short" style="display: inline;"> In very young clusters, stellar age distribution is the empirical proof of the duration of star formation (SF) and of the physical mechanisms involved in the process. We derived accurate stellar ages for the cluster NGC6530, associated with the Lagoon Nebula to infer its SF history. We use the Gaia-ESO survey observations and Gaia DR2 data, to derive cluster membership and fundamental stellar para… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.09589v1-abstract-full').style.display = 'inline'; document.getElementById('1901.09589v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.09589v1-abstract-full" style="display: none;"> In very young clusters, stellar age distribution is the empirical proof of the duration of star formation (SF) and of the physical mechanisms involved in the process. We derived accurate stellar ages for the cluster NGC6530, associated with the Lagoon Nebula to infer its SF history. We use the Gaia-ESO survey observations and Gaia DR2 data, to derive cluster membership and fundamental stellar parameters. We identified 652 confirmed and 9 probable members. The reddening inferred for members and non-members allows us to distinguish MS stars and giants, in agreement with the distances inferred from Gaia DR2 data. The foreground and background stars show a spatial pattern that traces the 3D structure of the nebular dust component. We derive stellar ages for 382 confirmed cluster members and we find that the gravity-sensitive gamma index distribution for M stars is correlated with stellar age. For all members with Teff<5500 K, the mean logarithmic age is 5.84 (units of years) with a dispersion of 0.36 dex. The age distribution of stars with accretion and/or disk (CTTSe) is similar to that of stars without accretion and without disk (WTTSp). We interpret this dispersion as evidence of a real age spread since the total uncertainties on age determinations, derived from Monte Carlo simulations, are significantly smaller than the observed spread. This conclusion is supported by the evidence of a decreasing of the gravity-sensitive gamma index as a function of stellar ages. The presence of the age spread is also supported by the spatial distribution and the kinematics of old and young members. In particular, members with accretion and/or disk, formed in the last 1 Myr, show evidence of subclustering around the cluster center, in the Hourglass Nebula and in the M8-E region, suggesting a possible triggering of star formation events by the O-type star ionization fronts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.09589v1-abstract-full').style.display = 'none'; document.getElementById('1901.09589v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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; 23 pages, 17 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 623, A159 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.10709">arXiv:1812.10709</a> <span> [<a href="https://arxiv.org/pdf/1812.10709">pdf</a>, <a href="https://arxiv.org/format/1812.10709">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/mnrasl/sly240">10.1093/mnrasl/sly240 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Two kinematically distinct old globular cluster populations in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Piatti%2C+A+E">Andr茅s E. Piatti</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">Tristan Cantat-Gaudin</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="1812.10709v1-abstract-short" style="display: inline;"> We report results of proper motions of 15 known Large Magellanic Cloud (LMC) old globular clusters (GCs) derived from the Gaia DR2 data sets. When these mean proper motions are gathered with existent radial velocity measurements to compose the GCs' velocity vectors, we found that the projection of the velocity vectors onto the LMC plane and those perpendicular to it tell us about two distinct kine… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.10709v1-abstract-full').style.display = 'inline'; document.getElementById('1812.10709v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.10709v1-abstract-full" style="display: none;"> We report results of proper motions of 15 known Large Magellanic Cloud (LMC) old globular clusters (GCs) derived from the Gaia DR2 data sets. When these mean proper motions are gathered with existent radial velocity measurements to compose the GCs' velocity vectors, we found that the projection of the velocity vectors onto the LMC plane and those perpendicular to it tell us about two distinct kinematic GC populations. Such a distinction becomes clear if the GCs are split at a perpendicular velocity of 10 km/s (absolute value). The two different kinematic groups also exhibit different spatial distributions. Those with smaller vertical velocities are part of the LMC disc, while those with larger values are closely distributed like a spherical component. Since GCs in both kinematic-structural components share similar ages and metallicities, we speculate with the possibility that their origins could have occurred through a fast collapse that formed halo and disc concurrently. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.10709v1-abstract-full').style.display = 'none'; document.getElementById('1812.10709v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures. Accepted for publication in Monthly Notices of the Royal Astronomical Society Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.05828">arXiv:1811.05828</a> <span> [<a href="https://arxiv.org/pdf/1811.05828">pdf</a>, <a href="https://arxiv.org/format/1811.05828">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="General Relativity and Quantum Cosmology">gr-qc</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/10.3390/universe5020051">10.3390/universe5020051 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Accelerating Universe without Lambda: Delta~Gravity Using Monte Carlo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+M+S">Marco San Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Sureda%2C+J">Joaquin Sureda</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1811.05828v2-abstract-short" style="display: inline;"> A gravitational field model based on two symmetric tensors, $g_{渭谓}$ and $\tilde{g}_{渭谓}$, is studied, using a Markov Chain Monte Carlo (MCMC) analysis with the most updated catalog of SN-Ia. In this model, new matter fields are added to the original matter fields, motivated by an additional symmetry ($\tilde未$~symmetry). We call them $\tilde未$ matter fields. This theory predicts an accelerating U… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.05828v2-abstract-full').style.display = 'inline'; document.getElementById('1811.05828v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.05828v2-abstract-full" style="display: none;"> A gravitational field model based on two symmetric tensors, $g_{渭谓}$ and $\tilde{g}_{渭谓}$, is studied, using a Markov Chain Monte Carlo (MCMC) analysis with the most updated catalog of SN-Ia. In this model, new matter fields are added to the original matter fields, motivated by an additional symmetry ($\tilde未$~symmetry). We call them $\tilde未$ matter fields. This theory predicts an accelerating Universe without the need to introduce a cosmological constant $螞$ by hand in the equations. We obtained a very good fit to the SN-Ia Data, and with this, we found the two free parameters of the theory called $C$ and $L_2$. With these values, we have fixed all the degrees of freedom in the model. The last $H_0$ local value measurement is in tension with the CMB Data from Planck. Based on an absolute magnitude $M_V = -19.23$ for the SN, Delta Gravity finds $H_0$ to be $74.47\pm 1.63$ km/(s Mpc). This value is in concordance with the last measurement of the $H_0$ local value, $73.83\pm 1.48$ km/(s Mpc). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.05828v2-abstract-full').style.display = 'none'; document.getElementById('1811.05828v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">latex, 27 pages,15 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Universe 2019, 5(2), 51 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.05273">arXiv:1811.05273</a> <span> [<a href="https://arxiv.org/pdf/1811.05273">pdf</a>, <a href="https://arxiv.org/format/1811.05273">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/sty3106">10.1093/mnras/sty3106 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hierarchical Bayesian approach for estimating physical properties in nearby galaxies: Age Maps (Paper II) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Gil%2C+M+C">M. Carmen S谩nchez-Gil</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">Emilio J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cervi%C3%B1o%2C+M">Miguel Cervi帽o</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez%2C+E">Enrique P茅rez</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+H">Heath Jones</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1811.05273v1-abstract-short" style="display: inline;"> One of the fundamental goals of modern astrophysics is to estimate the physical parameters of galaxies. We present a hierarchical Bayesian model to compute age maps from images in the \Ha\ line (taken with Taurus Tunable Filter, TTF), ultraviolet band (GALEX far UV, FUV), and infrared bands (Spitzer 24, 70, and 160 $渭$m). We present the burst ages for young stellar populations in a sample of nearb… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.05273v1-abstract-full').style.display = 'inline'; document.getElementById('1811.05273v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.05273v1-abstract-full" style="display: none;"> One of the fundamental goals of modern astrophysics is to estimate the physical parameters of galaxies. We present a hierarchical Bayesian model to compute age maps from images in the \Ha\ line (taken with Taurus Tunable Filter, TTF), ultraviolet band (GALEX far UV, FUV), and infrared bands (Spitzer 24, 70, and 160 $渭$m). We present the burst ages for young stellar populations in a sample of nearby and nearly face-on galaxies. The \Ha\ to FUV flux ratio is a good relative indicator of the very recent star formation history (SFH). As a nascent star-forming region evolves, the \Ha\ line emission declines earlier than the UV continuum, leading to a decrease in the \Ha/FUV ratio. Using star-forming galaxy models, sampled with a probabilistic formalism, and allowing for a variable fraction of ionizing photons in the clusters, we obtain the corresponding theoretical ratio \Ha/FUV to compare with our observed flux ratios, and thus to estimate the ages of the observed regions. We take into account the mean uncertainties and the interrelationships between parameters when computing \Ha/FUV. We propose a Bayesian hierarchical model where a joint probability distribution is defined to determine the parameters (age, metallicity, IMF) from the observed data (the observed flux ratios \Ha/FUV). The joint distribution of the parameters is described through independent and identically distributed (i.i.d.) random variables generated through MCMC (Markov Chain Monte Carlo) techniques. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.05273v1-abstract-full').style.display = 'none'; document.getElementById('1811.05273v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages; 25 figures</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Alfaro%2C+J&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

CINXE.COM

Search | arXiv e-print repository