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 154 results for author: <span class="mathjax">Simon-Diaz, S</span> </h1> </div> <div class="level-right is-hidden-mobile">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> <div class="content"> <form method="GET" action="/search/" aria-role="search"> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Simon-Diaz, S"> </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=Simon-Diaz%2C+S&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="Simon-Diaz, S"> <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=Simon-Diaz%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S&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/2407.14593">arXiv:2407.14593</a> <span> [<a href="https://arxiv.org/pdf/2407.14593">pdf</a>, <a href="https://arxiv.org/format/2407.14593">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/10.1051/0004-6361/202451586">10.1051/0004-6361/202451586 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Binarity at LOw Metallicity (BLOeM): a spectroscopic VLT monitoring survey of massive stars in the SMC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Shenar%2C+T">T. Shenar</a>, <a href="/search/?searchtype=author&query=Bodensteiner%2C+J">J. Bodensteiner</a>, <a href="/search/?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/?searchtype=author&query=Crowther%2C+P+A">P. A. Crowther</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Abdul-Masih%2C+M">M. Abdul-Masih</a>, <a href="/search/?searchtype=author&query=Almeida%2C+L+A">L. A. Almeida</a>, <a href="/search/?searchtype=author&query=Backs%2C+F">F. Backs</a>, <a href="/search/?searchtype=author&query=Berlanas%2C+S+R">S. R. Berlanas</a>, <a href="/search/?searchtype=author&query=Bernini-Peron%2C+M">M. Bernini-Peron</a>, <a href="/search/?searchtype=author&query=Bestenlehner%2C+J+M">J. M. Bestenlehner</a>, <a href="/search/?searchtype=author&query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/?searchtype=author&query=Bronner%2C+V+A">V. A. Bronner</a>, <a href="/search/?searchtype=author&query=Britavskiy%2C+N">N. Britavskiy</a>, <a href="/search/?searchtype=author&query=de+Koter%2C+A">A. de Koter</a>, <a href="/search/?searchtype=author&query=de+Mink%2C+S+E">S. E. de Mink</a>, <a href="/search/?searchtype=author&query=Deshmukh%2C+K">K. Deshmukh</a>, <a href="/search/?searchtype=author&query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/?searchtype=author&query=Fabry%2C+M">M. Fabry</a>, <a href="/search/?searchtype=author&query=Gieles%2C+M">M. Gieles</a>, <a href="/search/?searchtype=author&query=Gilkis%2C+A">A. Gilkis</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez-Tor%C3%A0%2C+G">G. Gonz谩lez-Tor脿</a>, <a href="/search/?searchtype=author&query=Gr%C3%A4fener%2C+G">G. Gr盲fener</a>, <a href="/search/?searchtype=author&query=G%C3%B6tberg%2C+Y">Y. G枚tberg</a>, <a href="/search/?searchtype=author&query=Hawcroft%2C+C">C. Hawcroft</a> , et al. (52 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="2407.14593v2-abstract-short" style="display: inline;"> Surveys in the Milky Way and Large Magellanic Cloud revealed that the majority of massive stars will interact with companions during their lives. However, knowledge of the binary properties of massive stars at low metallicity, which approaches the conditions of the Early Universe, remains sparse. We present the Binarity at LOw Metallicity (BLOeM) campaign - an ESO large programme designed to obtai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14593v2-abstract-full').style.display = 'inline'; document.getElementById('2407.14593v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.14593v2-abstract-full" style="display: none;"> Surveys in the Milky Way and Large Magellanic Cloud revealed that the majority of massive stars will interact with companions during their lives. However, knowledge of the binary properties of massive stars at low metallicity, which approaches the conditions of the Early Universe, remains sparse. We present the Binarity at LOw Metallicity (BLOeM) campaign - an ESO large programme designed to obtain 25 epochs of spectroscopy for 929 massive stars in the SMC - the lowest metallicity conditions in which multiplicity is probed to date (Z = 0.2 Zsun). BLOeM will provide (i) the binary fraction, (ii) the orbital configurations of systems with periods P < 3 yr, (iii) dormant OB+BH binaries, and (iv) a legacy database of physical parameters of massive stars at low metallicity. The stars are observed with the LR02 setup of the giraffe instrument of the Very Large Telescope (3960-4570A, resolving power R=6200; typical signal-to-noise ratio S/N=70-100). This paper utilises the first 9 epochs obtained over a three-month time. We describe the survey and data reduction, perform a spectral classification of the stacked spectra, and construct a Hertzsprung-Russell diagram of the sample via spectral-type and photometric calibrations. The sample covers spectral types from O4 to F5, spanning the effective temperature and luminosity ranges 6.5<Teff/kK<45 and 3.7<log L/Lsun<6.1 and initial masses 8<Mini/Msun<80. It comprises 159 O-type stars, 331 early B-type (B0-3) dwarfs and giants (luminosity classes V-III), 303 early B-type supergiants (II-I), and 136 late-type supergiants. At least 82 stars are Oe/Be stars: 20 O-type and 62 B-type (13% and 11% of the respective samples). In addition, it includes 4 high-mass X-ray binaries, 3 stars resembling luminous blue variables, 2 bloated stripped-star candidates, 2 candidate magnetic stars, and 74 eclipsing binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14593v2-abstract-full').style.display = 'none'; document.getElementById('2407.14593v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to A&A on 27 Aug 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A289 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04163">arXiv:2407.04163</a> <span> [<a href="https://arxiv.org/pdf/2407.04163">pdf</a>, <a href="https://arxiv.org/format/2407.04163">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/10.1051/0004-6361/202449298">10.1051/0004-6361/202449298 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project XII. A new grid of northern standards for the spectral classification of B-type stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Negueruela%2C+I">Ignacio Negueruela</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">Sergio Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=de+Burgos%2C+A">Abel de Burgos</a>, <a href="/search/?searchtype=author&query=Casasbuenas%2C+A">Alba Casasbuenas</a>, <a href="/search/?searchtype=author&query=Beck%2C+P+G">Paul G. Beck</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.04163v2-abstract-short" style="display: inline;"> With the advent of large spectroscopic surveys, automated stellar parameter determination has become commonplace. Nevertheless, spectral classification still offers a quick and useful alternative for obtaining parameter estimates for large samples of spectra of varying quality. We present a new atlas of stellar spectra covering the B-type range, with the intention of providing detailed classificat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04163v2-abstract-full').style.display = 'inline'; document.getElementById('2407.04163v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04163v2-abstract-full" style="display: none;"> With the advent of large spectroscopic surveys, automated stellar parameter determination has become commonplace. Nevertheless, spectral classification still offers a quick and useful alternative for obtaining parameter estimates for large samples of spectra of varying quality. We present a new atlas of stellar spectra covering the B-type range, with the intention of providing detailed classification criteria valid for modern spectra and improving the grid of reliable standards. This new grid will be used in future works to provide classification criteria beyond the classical classification range and addressing, in particular, the use of Gaia/RVS spectra. We analysed historical standards by means of multiple high-resolution spectra, marking out problematic cases and complementing the grid with a new set of reliable comparators. We then elaborated on a new set of classification criteria based on high-quality R=4000 spectra. Our new classification grid is much thicker than any previous set of standards, presenting a high degree of self-consistency. Although it is based entirely on morphological criteria, the grid demonstrates a much better correlation with different physical parameters. The new grid can be used to study classification criteria in other spectral ranges, providing a valuable tool for the study of B-type stars that covers a very wide range of temperatures, luminosities, and stellar masses. The very process of classification also offers valuable insights into stellar evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04163v2-abstract-full').style.display = 'none'; document.getElementById('2407.04163v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This is the authors' version, where content and readability take priority over the A&A style book. Table F is online-only in the published version. All the spectra are downloadable from https://astroplus.ua.es/mkbtypestds/. Please report mistakes, errors and typos, which are bound to be numerous in a project of this size</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A176 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.11209">arXiv:2405.11209</a> <span> [<a href="https://arxiv.org/pdf/2405.11209">pdf</a>, <a href="https://arxiv.org/format/2405.11209">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 IACOB project: CVIII. Hunting for spectroscopic binaries in the O and B supergiant domain.The threat of pulsational variability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Britavskiy%2C+N">N. Britavskiy</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=de+Burgos%2C+A">A. de Burgos</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.11209v1-abstract-short" style="display: inline;"> Observations have definitively strengthened the long-standing assertion that binaries are crucial in massive star evolution. While the percentage of spectroscopic binary systems among main-sequence O stars is well-studied, other phases of massive star evolution remain less explored. We aim to estimate the spectroscopic binary fraction in Galactic late O- and B-type supergiants (OB-Sgs) and set emp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.11209v1-abstract-full').style.display = 'inline'; document.getElementById('2405.11209v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.11209v1-abstract-full" style="display: none;"> Observations have definitively strengthened the long-standing assertion that binaries are crucial in massive star evolution. While the percentage of spectroscopic binary systems among main-sequence O stars is well-studied, other phases of massive star evolution remain less explored. We aim to estimate the spectroscopic binary fraction in Galactic late O- and B-type supergiants (OB-Sgs) and set empirical thresholds in radial velocity (RV) to avoid misidentifying pulsating stars as single-line spectroscopic binaries. Using over 4500 high-resolution spectra of 56 Galactic OB-Sgs (plus 13 O dwarfs/subgiants and 5 early-B giants) from the IACOB project (2008-2020), we apply Gaussian fitting and centroid computation techniques to measure RV for each spectrum. Our findings reveal that intrinsic variability in OB-Sgs can result in peak-to-peak RV amplitudes (RVpp) of up to 20-25 km/s, notably in late-O and early-B Sgs, and decreases to typical values of RVpp in the range of 1-5 km/s for O dwarfs and 2-15 km/s for late B-Sgs. Considering these results and evaluating line-profile variability in each star, we find that 10$\pm$4% of OB-Sgs are clearly single-line spectroscopic binaries. In addition, we find that the percentage of double-line spectroscopic binaries in late O- and early B-Sgs is ~6%, much lower than the ~30% in O-type dwarfs and giants. This study, along with prior research on B-Sgs in the 30 Doradus region of the LMC, indicates that the spectroscopic binary percentage decreases by a factor of 4-5 from O stars to B-Sgs. Our study underscores the need for a thorough characterization of spectroscopic variability due to intrinsic sources to reliably determine the spectroscopic binary fraction among OB-Sgs and O-type stars in general, offering valuable insights into the impact of binaries on massive star evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.11209v1-abstract-full').style.display = 'none'; document.getElementById('2405.11209v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This manuscript, submitted to A&A by mid 2020, encountered some discrepancies between the 1st author and the referee, along with some personal challenges during the COVID-19 pandemic, preventing its acceptance in a reasonable timescale. Believing it still valuable, I have decided to upload it to ArXiv as it was in 2021. A follow-up paper with a larger sample will be submitted soon</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.09868">arXiv:2405.09868</a> <span> [<a href="https://arxiv.org/pdf/2405.09868">pdf</a>, <a href="https://arxiv.org/format/2405.09868">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/10.1051/0004-6361/202450301">10.1051/0004-6361/202450301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project XI. No increase of mass-loss rates over the bistability region </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=de+Burgos%2C+A">Abel de Burgos</a>, <a href="/search/?searchtype=author&query=Keszthelyi%2C+Z">Zsolt Keszthelyi</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">Sergio Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Urbaneja%2C+M+A">Miguel A. Urbaneja</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.09868v2-abstract-short" style="display: inline;"> The properties of blue supergiants are key for constraining the end of the main sequence (MS) of massive stars. Whether the observed drop in the relative number of fast-rotating stars below $\sim$21$\,$kK is due to enhanced mass-loss rates at the location of the bistability jump, or the result of the end of the MS is still debated. Here, we combine newly derived estimates of photospheric and wind… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.09868v2-abstract-full').style.display = 'inline'; document.getElementById('2405.09868v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.09868v2-abstract-full" style="display: none;"> The properties of blue supergiants are key for constraining the end of the main sequence (MS) of massive stars. Whether the observed drop in the relative number of fast-rotating stars below $\sim$21$\,$kK is due to enhanced mass-loss rates at the location of the bistability jump, or the result of the end of the MS is still debated. Here, we combine newly derived estimates of photospheric and wind parameters with Gaia distances and wind terminal velocities from the literature to obtain upper limits on the mass-loss rates for a sample of 116 Galactic luminous blue supergiants. The parameter space covered by the sample ranges between 35-15$\,$kK in $T_{\rm eff}$ and 4.8-5.8$\,$dex in log(L/L$_{\odot}$). Our results show no increase in the mass-loss rates over the bistability jump. Therefore, we argue that the drop in rotational velocities cannot be explained by enhanced mass loss. Since a large jump in the mass-loss rates is commonly included in evolutionary models, we suggest an urgent revision of the currently used default prescriptions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.09868v2-abstract-full').style.display = 'none'; document.getElementById('2405.09868v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics, 9 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, L16 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.05195">arXiv:2401.05195</a> <span> [<a href="https://arxiv.org/pdf/2401.05195">pdf</a>, <a href="https://arxiv.org/format/2401.05195">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"> Astro+: Design, construction, and scientific exploitation of a large-scale massive star spectroscopic database </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rubke%2C+K">Klaus Rubke</a>, <a href="/search/?searchtype=author&query=Marco%2C+A">Amparo Marco</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">Ignacio Negueruela</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">Artemio Herrero</a>, <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S">Sergio Simon-Diaz</a>, <a href="/search/?searchtype=author&query=Tabernero%2C+H">Hugo Tabernero</a>, <a href="/search/?searchtype=author&query=Patrick%2C+L">Lee Patrick</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="2401.05195v1-abstract-short" style="display: inline;"> Massive stars condition the evolution of the interstellar medium by the amount of energy released during their lives and especially by their deaths as supernova explosions. The vast amounts of spectroscopic data for massive stars provided by previous and existing instruments on ground-based and space-based telescopes have already saturated our capability to process them by the use of human routine… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.05195v1-abstract-full').style.display = 'inline'; document.getElementById('2401.05195v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.05195v1-abstract-full" style="display: none;"> Massive stars condition the evolution of the interstellar medium by the amount of energy released during their lives and especially by their deaths as supernova explosions. The vast amounts of spectroscopic data for massive stars provided by previous and existing instruments on ground-based and space-based telescopes have already saturated our capability to process them by the use of human routines. As a consequence, there is a pressing need for machine-assisted tools to help handle incoming data. To this end, we present the development of a massive star spectroscopic multiwavelength interactive database designed for scientific research and a fully automatic stellar parameter determination tool. Here we show the preliminary results of the application of these tools to optical spectra of O-type stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.05195v1-abstract-full').style.display = 'none'; document.getElementById('2401.05195v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Highlights of Spanish Astrophysics XI, Proceedings of the XV Scientific Meeting of the Spanish Astronomical Society</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2023hsa..conf..306R </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.00241">arXiv:2312.00241</a> <span> [<a href="https://arxiv.org/pdf/2312.00241">pdf</a>, <a href="https://arxiv.org/format/2312.00241">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/10.1051/0004-6361/202348808">10.1051/0004-6361/202348808 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project X. Large-scale quantitative spectroscopic analysis of Galactic luminous blue stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=de+Burgos%2C+A">Abel de Burgos</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">Sergio Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Urbaneja%2C+M+A">Miguel A. Urbaneja</a>, <a href="/search/?searchtype=author&query=Puls%2C+J">Joachim Puls</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.00241v2-abstract-short" style="display: inline;"> Blue supergiants (BSGs) are key objects for understanding the evolution of massive stars. However, discrepancies between theoretical predictions and empirical observations have opened up important questions yet to be answered. Studying statistically significant and unbiased samples of BSGs can help to improve the situation. We aim to perform a homogeneous and comprehensive quantitative spectroscop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.00241v2-abstract-full').style.display = 'inline'; document.getElementById('2312.00241v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.00241v2-abstract-full" style="display: none;"> Blue supergiants (BSGs) are key objects for understanding the evolution of massive stars. However, discrepancies between theoretical predictions and empirical observations have opened up important questions yet to be answered. Studying statistically significant and unbiased samples of BSGs can help to improve the situation. We aim to perform a homogeneous and comprehensive quantitative spectroscopic analysis of a large sample of Galactic luminous blue stars (being the majority BSGs) from the IACOB spectroscopic database. We derive the projected rotational velocity ($v\sin i$) and macroturbulent broadening ($v_{\rm mac}$) using IACOB-BROAD. We used FASTWIND computations to derive effective temperatures ($T_{\rm eff}$), surface gravities, microturbulences ($尉$), Si and He surface abundances, and the wind-strength parameter. We provide estimates of these quantities for the largest sample of Galactic luminous O9-B5 stars spectroscopically analyzed to date, with 527 targets. We find a drop in the relative number of stars at ~21 kK, coinciding with a scarcity of fast rotating stars below that temperature. We speculate that this feature might be roughly delineating the location of the Terminal-Age-Main-Sequence in the 15-85M$_\odot$ range. By investigating the main characteristics of the $v\sin i$ distribution as a function of $T_{\rm eff}$, we propose that an efficient mechanism transporting angular momentum from the stellar core to the surface might be operating along the main sequence. We find correlations between $尉$, $v_{\rm mac}$ and the spectroscopic luminosity. We also find that no more than 20% of the stars in our sample have atmospheres clearly enriched in He, and suggest that the origin of this specific sub-sample might be in binary evolution. We do not find clear empirical evidence of an increase in the wind-strength over the wind bi-stability region towards lower temperatures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.00241v2-abstract-full').style.display = 'none'; document.getElementById('2312.00241v2-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics, 22 pages, 20 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A228 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.02368">arXiv:2308.02368</a> <span> [<a href="https://arxiv.org/pdf/2308.02368">pdf</a>, <a href="https://arxiv.org/ps/2308.02368">ps</a>, <a href="https://arxiv.org/format/2308.02368">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad2280">10.1093/mnras/stad2280 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extreme mass ratios and fast rotation in three massive binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Naze%2C+Y">Yael Naze</a>, <a href="/search/?searchtype=author&query=Britavskiy%2C+N">Nikolay Britavskiy</a>, <a href="/search/?searchtype=author&query=Rauw%2C+G">Gregor Rauw</a>, <a href="/search/?searchtype=author&query=Labadie-Bartz%2C+J">Jonathan Labadie-Bartz</a>, <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S">S. Simon-Diaz</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.02368v2-abstract-short" style="display: inline;"> The origin of rapid rotation in massive stars remains debated, although binary interactions are now often advocated as a cause. However, the broad and shallow lines in the spectra of fast rotators make direct detection of binarity difficult. In this paper, we report on the discovery and analysis of multiplicity for three fast-rotating massive stars: HD25631 (B3V), HD191495 (B0V), and HD46485 (O7V)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.02368v2-abstract-full').style.display = 'inline'; document.getElementById('2308.02368v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.02368v2-abstract-full" style="display: none;"> The origin of rapid rotation in massive stars remains debated, although binary interactions are now often advocated as a cause. However, the broad and shallow lines in the spectra of fast rotators make direct detection of binarity difficult. In this paper, we report on the discovery and analysis of multiplicity for three fast-rotating massive stars: HD25631 (B3V), HD191495 (B0V), and HD46485 (O7V). They display strikingly similar TESS light curves, with two narrow eclipses superimposed on a sinusoidal variation due to reflection effects. We complement these photometric data by spectroscopy from various instruments (X-Shooter, Espadons, FUSE...), to further constrain the nature of these systems. The detailed analyses of these data demonstrates that the companions of the massive OB stars have low masses (~1Msol) with rather large radii (2-4 Rsol) and low temperatures (<15 kK). These companions display no UV signature, which would exclude a hot subdwarf nature, but disentangling of the large set of X-Shooter spectra of HD25631 revealed the typical signature of chromospheric activity in the companion's spectrum. In addition, despite the short orbital periods (P=3-7d), the fast-rotating OB-stars still display non-synchronized rotation and all systems appear young (<20Myr). This suggests that, as in a few other cases, these massive stars are paired in those systems with non-degenerate, low-mass PMS companions, implying that fast rotation would not be a consequence of a past binary interactions in their case. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.02368v2-abstract-full').style.display = 'none'; document.getElementById('2308.02368v2-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication 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/2307.10812">arXiv:2307.10812</a> <span> [<a href="https://arxiv.org/pdf/2307.10812">pdf</a>, <a href="https://arxiv.org/format/2307.10812">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"> Constraining stellar and orbital co-evolution through ensemble seismology of solar-like oscillators in binary systems -- A census of oscillating red-giants and main-sequence stars in Gaia DR3 binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Beck%2C+P+G">P. G. Beck</a>, <a href="/search/?searchtype=author&query=Grossmann%2C+D+H">D. H. Grossmann</a>, <a href="/search/?searchtype=author&query=Steinwender%2C+L">L. Steinwender</a>, <a href="/search/?searchtype=author&query=Schimak%2C+L+S">L. S. Schimak</a>, <a href="/search/?searchtype=author&query=Muntean%2C+N">N. Muntean</a>, <a href="/search/?searchtype=author&query=Vrard%2C+M">M. Vrard</a>, <a href="/search/?searchtype=author&query=Patton%2C+R+A">R. A. Patton</a>, <a href="/search/?searchtype=author&query=Merc%2C+J">J. Merc</a>, <a href="/search/?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/?searchtype=author&query=Pinsonneault%2C+M+H">M. H. Pinsonneault</a>, <a href="/search/?searchtype=author&query=Rowan%2C+D+M">D. M. Rowan</a>, <a href="/search/?searchtype=author&query=Gaulme%2C+P">P. Gaulme</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Arellano-C%C3%B3rdova%2C+K+Z">K. Z. Arellano-C贸rdova</a>, <a href="/search/?searchtype=author&query=Cao%2C+L">L. Cao</a>, <a href="/search/?searchtype=author&query=Corsaro%2C+E">E. Corsaro</a>, <a href="/search/?searchtype=author&query=Creevey%2C+O">O. Creevey</a>, <a href="/search/?searchtype=author&query=Hambleton%2C+K+M">K. M. Hambleton</a>, <a href="/search/?searchtype=author&query=Hanslmeier%2C+A">A. Hanslmeier</a>, <a href="/search/?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/?searchtype=author&query=Johnson%2C+J">J. Johnson</a>, <a href="/search/?searchtype=author&query=Mathis%2C+S">S. Mathis</a>, <a href="/search/?searchtype=author&query=Godoy-Rivera%2C+D">D. Godoy-Rivera</a>, <a href="/search/?searchtype=author&query=S%C3%ADmon-D%C3%ADaz%2C+S">S. S铆mon-D铆az</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.10812v3-abstract-short" style="display: inline;"> Binary systems constitute a valuable astrophysics tool for testing our understanding of stellar structure and evolution. Systems containing a oscillating component are interesting as asteroseismology offers independent parameters for the oscillating component that aid the analysis. About 150 of such systems are known in the literature. To enlarge the sample of these benchmark objects, we crossmatc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10812v3-abstract-full').style.display = 'inline'; document.getElementById('2307.10812v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.10812v3-abstract-full" style="display: none;"> Binary systems constitute a valuable astrophysics tool for testing our understanding of stellar structure and evolution. Systems containing a oscillating component are interesting as asteroseismology offers independent parameters for the oscillating component that aid the analysis. About 150 of such systems are known in the literature. To enlarge the sample of these benchmark objects, we crossmatch the Two-Body-Orbit Catalogue (TBO) of Gaia DR3, with catalogs of confirmed solar-like oscillators on the main-sequence and red-giant phase from NASA Kepler and TESS. We obtain 954 new binary system candidates hosting solar-like oscillators, of which 45 and 909 stars are on the main sequence and red-giant, resp., including 2 new red giants in eclipsing systems. 918 oscillators in potentially long-periodic systems are reported. We increase the sample size of known solar-like oscillators in binary systems by an order of magnitude. We present the seismic properties of the full sample and conclude that the grand majority of the orbital elements in the TBO is physically reasonable. 82% of all TBO binary candidates with multiple times with APOGEE are confirmed from radial-velocity measurement. However, we suggest that due to instrumental noise of the TESS satellite the seismically inferred masses and radii of stars with $谓_\textrm{max}$$\lesssim$30$渭$Hz could be significantly overestimated. For 146 giants the seismically inferred evolutionary state has been determined and shows clear differences in their distribution in the orbital parameters, which are accounted the accumulative effect of the equilibrium tide acting in these evolved binary systems. For other 146 systems hosting oscillating stars values for the orbital inclination were found in the TBO. From testing the TBO on the SB9 catalogue, we obtain a completeness factor of 1/3. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10812v3-abstract-full').style.display = 'none'; document.getElementById('2307.10812v3-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in Astronomy&Astrophysics (23 pages + 4 pages of appendix, 21 figures, 33 pages of tables in the Appendix)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.11798">arXiv:2306.11798</a> <span> [<a href="https://arxiv.org/pdf/2306.11798">pdf</a>, <a href="https://arxiv.org/format/2306.11798">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"> A calibration point for stellar evolution from massive star asteroseismology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Burssens%2C+S">Siemen Burssens</a>, <a href="/search/?searchtype=author&query=Bowman%2C+D+M">Dominic M. Bowman</a>, <a href="/search/?searchtype=author&query=Michielsen%2C+M">Mathias Michielsen</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">Sergio Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/?searchtype=author&query=Vanlaer%2C+V">Vincent Vanlaer</a>, <a href="/search/?searchtype=author&query=Banyard%2C+G">Gareth Banyard</a>, <a href="/search/?searchtype=author&query=Nardetto%2C+N">Nicolas Nardetto</a>, <a href="/search/?searchtype=author&query=Townsend%2C+R+H+D">Richard H. D. Townsend</a>, <a href="/search/?searchtype=author&query=Handler%2C+G">Gerald Handler</a>, <a href="/search/?searchtype=author&query=Mombarg%2C+J+S+G">Joey S. G. Mombarg</a>, <a href="/search/?searchtype=author&query=Vanderspek%2C+R">Roland Vanderspek</a>, <a href="/search/?searchtype=author&query=Ricker%2C+G">George Ricker</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="2306.11798v2-abstract-short" style="display: inline;"> Massive stars are progenitors of supernovae, neutron stars and black holes. During the hydrogen-core burning phase their convective cores are the prime drivers of their evolution, but inferences of core masses are subject to unconstrained boundary mixing processes. Moreover, uncalibrated transport mechanisms can lead to strong envelope mixing and differential radial rotation. Ascertaining the effi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11798v2-abstract-full').style.display = 'inline'; document.getElementById('2306.11798v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.11798v2-abstract-full" style="display: none;"> Massive stars are progenitors of supernovae, neutron stars and black holes. During the hydrogen-core burning phase their convective cores are the prime drivers of their evolution, but inferences of core masses are subject to unconstrained boundary mixing processes. Moreover, uncalibrated transport mechanisms can lead to strong envelope mixing and differential radial rotation. Ascertaining the efficiency of the transport mechanisms is challenging because of a lack of observational constraints. Here we deduce the convective core mass and robustly demonstrate non-rigid radial rotation in a supernova progenitor, the $12.0^{+1.5}_{-1.5}$ solar-mass hydrogen-burning star HD 192575, using asteroseismology, TESS photometry, high-resolution spectroscopy, and Gaia astrometry. We infer a convective core mass ($M_{\rm cc} = 2.9^{+0.5}_{-0.8}$ solar masses), and find the core to be rotating between 1.4 and 6.3 times faster than the stellar envelope depending on the location of the rotational shear layer. Our results deliver a robust inferred core mass of a massive star using asteroseismology from space-based photometry. HD 192575 is a unique anchor point for studying interior rotation and mixing processes, and thus also angular momentum transport mechanisms inside massive stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11798v2-abstract-full').style.display = 'none'; document.getElementById('2306.11798v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">41 pages, 5 figures, 1 table. Version comment: updated erroneous affiliation</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.09769">arXiv:2306.09769</a> <span> [<a href="https://arxiv.org/pdf/2306.09769">pdf</a>, <a href="https://arxiv.org/format/2306.09769">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346707">10.1051/0004-6361/202346707 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solar-like oscillations in $纬$ Cephei A as seen through SONG and TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Knudstrup%2C+E">E. Knudstrup</a>, <a href="/search/?searchtype=author&query=Lund%2C+M+N">M. N. Lund</a>, <a href="/search/?searchtype=author&query=Andersen%2C+M+F">M. Fredslund Andersen</a>, <a href="/search/?searchtype=author&query=R%C3%B8rsted%2C+J+L">J. L. R酶rsted</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez%2C+F+P">F. P茅rez Hern谩ndez</a>, <a href="/search/?searchtype=author&query=Grundahl%2C+F">F. Grundahl</a>, <a href="/search/?searchtype=author&query=Pall%C3%A9%2C+P+L">P. L. Pall茅</a>, <a href="/search/?searchtype=author&query=Stello%2C+D">D. Stello</a>, <a href="/search/?searchtype=author&query=White%2C+T+R">T. R. White</a>, <a href="/search/?searchtype=author&query=Kjeldsen%2C+H">H. Kjeldsen</a>, <a href="/search/?searchtype=author&query=Vrard%2C+M">M. Vrard</a>, <a href="/search/?searchtype=author&query=Winther%2C+M+L">M. L. Winther</a>, <a href="/search/?searchtype=author&query=Handberg%2C+R">R. Handberg</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</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="2306.09769v1-abstract-short" style="display: inline;"> Fundamental stellar parameters such as mass and radius are some of the most important building blocks in astronomy, both when it comes to understanding the star itself and when deriving the properties of any exoplanet(s) they may host. Asteroseismology of solar-like oscillations allows us to determine these parameters with high precision. We investigate the solar-like oscillations of the red-giant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09769v1-abstract-full').style.display = 'inline'; document.getElementById('2306.09769v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.09769v1-abstract-full" style="display: none;"> Fundamental stellar parameters such as mass and radius are some of the most important building blocks in astronomy, both when it comes to understanding the star itself and when deriving the properties of any exoplanet(s) they may host. Asteroseismology of solar-like oscillations allows us to determine these parameters with high precision. We investigate the solar-like oscillations of the red-giant-branch star $纬$ Cep A, which harbours a giant planet on a wide orbit. We did this by utilising both ground-based radial velocities from the SONG network and space-borne photometry from the NASA TESS mission. From the radial velocities and photometric observations, we created a combined power spectrum, which we used in an asteroseismic analysis to extract individual frequencies. We clearly identify several radial and quadrupole modes as well as multiple mixed, dipole modes. We used these frequencies along with spectroscopic and astrometric constraints to model the star, and we find a mass of $1.27^{+0.05}_{-0.07}$ M$_\odot$, a radius of $4.74^{+0.07}_{-0.08}$ R$_\odot$, and an age of $5.7^{+0.8}_{-0.9}$ Gyr. We then used the mass of $纬$ Cep A and our SONG radial velocities to derive masses for $纬$ Cep B and $纬$ Cep Ab of $0.328^{+0.009}_{-0.012}$ M$_\odot$ and $6.6^{+2.3}_{-2.8}$ M$_{\rm Jup}$, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09769v1-abstract-full').style.display = 'none'; document.getElementById('2306.09769v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 13 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 675, A197 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.00305">arXiv:2305.00305</a> <span> [<a href="https://arxiv.org/pdf/2305.00305">pdf</a>, <a href="https://arxiv.org/format/2305.00305">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/10.1051/0004-6361/202346179">10.1051/0004-6361/202346179 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project IX. Building a modern empirical database of Galactic O9-B9 supergiants: sample selection, description, and completeness </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=de+Burgos%2C+A">Abel de Burgos</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">Sergio Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Urbaneja%2C+M+A">Miguel A. Urbaneja</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">Ignacio Negueruela</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.00305v2-abstract-short" style="display: inline;"> Blue supergiants (BSGs) are important objects to study the intermediate phases of massive star evolution, helping to constrain evolutionary models. However, the lack of a holistic study of a statistically significant and unbiased sample of these objects makes several long-standing questions about their nature to remain unsolved. The present and other upcoming papers of the IACOB series are focused… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.00305v2-abstract-full').style.display = 'inline'; document.getElementById('2305.00305v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.00305v2-abstract-full" style="display: none;"> Blue supergiants (BSGs) are important objects to study the intermediate phases of massive star evolution, helping to constrain evolutionary models. However, the lack of a holistic study of a statistically significant and unbiased sample of these objects makes several long-standing questions about their nature to remain unsolved. The present and other upcoming papers of the IACOB series are focused in studying - from a pure empirical point of view - a sample of 500 Galactic O9 - B9 stars with luminosity classes I and II (plus 250 late O- and early B-type stars with luminosity classes III, IV and V) and covering distances up to 4 kpc from the Sun. We compile an initial set of 11000 high-resolution spectra of 1600 Galactic late O- and B-type stars. We use a new novel spectroscopic strategy based on a simple fitting of the Hbeta line to select stars in a specific region of the spectroscopic HR diagram. We evaluate the completeness of our sample using the Alma Luminous Star catalog (ALS III) and Gaia-DR3 data. We show the benefits of the proposed strategy for identifying BSGs descending from stellar objects born as O-type stars, in the context of single star evolution. The resulting sample reaches a high level of completeness with respect to the ALS III catalog, gathering the 80% for all-sky targets brighter than Bmag < 9 located within 2 kpc. However, we identify the need for new observations in specific regions of the Southern hemisphere. In conclusion, we have explored a very fast and robust method to select BSGs, providing a valuable tool for large spectroscopic surveys like WEAVE-SCIP or 4MIDABLE-LR, and highlighting the risk of using spectral classifications from the literature. Upcoming works will make use of this large and homogeneous spectroscopic sample to study specific properties of these stars in detail. We initially provide first results about their rotational properties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.00305v2-abstract-full').style.display = 'none'; document.getElementById('2305.00305v2-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics. 59 pages, 20 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A212 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.01349">arXiv:2302.01349</a> <span> [<a href="https://arxiv.org/pdf/2302.01349">pdf</a>, <a href="https://arxiv.org/format/2302.01349">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/10.1051/0004-6361/202245145">10.1051/0004-6361/202245145 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project VIII. Searching for empirical signatures of binarity in fast-rotating O-type stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Britavskiy%2C+N">N. Britavskiy</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=Burssens%2C+S">S. Burssens</a>, <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Eldridge%2C+J+J">J. J. Eldridge</a>, <a href="/search/?searchtype=author&query=Naz%C3%A9%2C+Y">Y. Naz茅</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</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="2302.01349v2-abstract-short" style="display: inline;"> The empirical distribution of projected rotational velocities (vsini) in massive O-type stars is characterized by a dominant slow velocity component and a tail of fast rotators. Binary interaction has been proposed to play a dominant role in the formation of this tail. We perform a complete and homogeneous search for empirical signatures of binarity in a sample of 54 fast-rotating stars with the a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01349v2-abstract-full').style.display = 'inline'; document.getElementById('2302.01349v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.01349v2-abstract-full" style="display: none;"> The empirical distribution of projected rotational velocities (vsini) in massive O-type stars is characterized by a dominant slow velocity component and a tail of fast rotators. Binary interaction has been proposed to play a dominant role in the formation of this tail. We perform a complete and homogeneous search for empirical signatures of binarity in a sample of 54 fast-rotating stars with the aim of evaluating this hypothesis. This working sample has been extracted from a larger sample of 415 Galactic O-type stars which covers the full range of vsini values. We use new and archival multi-epoch spectra in order to detect spectroscopic binary systems. We complement this information with Gaia proper motions and TESS photometric data to aid in the identification of runaway stars and eclipsing binaries, respectively. The identified fraction of single-lined spectroscopic binary (SB1) systems and apparently single stars among the fast-rotating sample is $\sim$18% and $\sim$70%, respectively. When comparing these percentages with those corresponding to the slow-rotating sample we find that our sample of fast rotators is characterized by a slightly larger percentage of SB1 systems ($\sim$18% vs. $\sim$13%) and a considerably smaller fraction of clearly detected SB2 systems (8% vs. 33%). Overall, there seems to be a clear deficit of spectroscopic binaries (SB1+SB2) among fast-rotating O-type stars ($\sim$26% vs. $\sim$46%). On the contrary, the fraction of runaway stars is significantly higher in the fast-rotating domain ($\sim$33-50%) than among those stars with vsini < 200 km/s. Lastly, almost 65% of the apparently single fast-rotating stars are runaways. Our empirical results seem to be in good agreement with the idea that the tail of fast-rotating O-type stars (with vsini > 200 km/s) is mostly populated by post-interaction binary products. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01349v2-abstract-full').style.display = 'none'; document.getElementById('2302.01349v2-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> 15 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 16 figures, accepted for publication in "Astronomy and Astrophysics"</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A22 (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/?searchtype=author&query=Jin%2C+S">Shoko Jin</a>, <a href="/search/?searchtype=author&query=Trager%2C+S+C">Scott C. Trager</a>, <a href="/search/?searchtype=author&query=Dalton%2C+G+B">Gavin B. Dalton</a>, <a href="/search/?searchtype=author&query=Aguerri%2C+J+A+L">J. Alfonso L. Aguerri</a>, <a href="/search/?searchtype=author&query=Drew%2C+J+E">J. E. Drew</a>, <a href="/search/?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">Jes煤s Falc贸n-Barroso</a>, <a href="/search/?searchtype=author&query=G%C3%A4nsicke%2C+B+T">Boris T. G盲nsicke</a>, <a href="/search/?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/?searchtype=author&query=Iovino%2C+A">Angela Iovino</a>, <a href="/search/?searchtype=author&query=Pieri%2C+M+M">Matthew M. Pieri</a>, <a href="/search/?searchtype=author&query=Poggianti%2C+B+M">Bianca M. Poggianti</a>, <a href="/search/?searchtype=author&query=Smith%2C+D+J+B">D. J. B. Smith</a>, <a href="/search/?searchtype=author&query=Vallenari%2C+A">Antonella Vallenari</a>, <a href="/search/?searchtype=author&query=Abrams%2C+D+C">Don Carlos Abrams</a>, <a href="/search/?searchtype=author&query=Aguado%2C+D+S">David S. Aguado</a>, <a href="/search/?searchtype=author&query=Antoja%2C+T">Teresa Antoja</a>, <a href="/search/?searchtype=author&query=Arag%C3%B3n-Salamanca%2C+A">Alfonso Arag贸n-Salamanca</a>, <a href="/search/?searchtype=author&query=Ascasibar%2C+Y">Yago Ascasibar</a>, <a href="/search/?searchtype=author&query=Babusiaux%2C+C">Carine Babusiaux</a>, <a href="/search/?searchtype=author&query=Balcells%2C+M">Marc Balcells</a>, <a href="/search/?searchtype=author&query=Barrena%2C+R">R. Barrena</a>, <a href="/search/?searchtype=author&query=Battaglia%2C+G">Giuseppina Battaglia</a>, <a href="/search/?searchtype=author&query=Belokurov%2C+V">Vasily Belokurov</a>, <a href="/search/?searchtype=author&query=Bensby%2C+T">Thomas Bensby</a>, <a href="/search/?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/2207.12776">arXiv:2207.12776</a> <span> [<a href="https://arxiv.org/pdf/2207.12776">pdf</a>, <a href="https://arxiv.org/format/2207.12776">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/10.1051/0004-6361/202243851">10.1051/0004-6361/202243851 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project. VII. The rotational properties of Galactic massive O-type stars revisited </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.12776v1-abstract-short" style="display: inline;"> Stellar rotation is of key importance for the formation process, evolution, and final fate of massive stars. In this paper we review results from the study of the spin rate properties of a sample of more than 400 Galactic O-type stars surveyed by the IACOB and OWN projects. By combining vsini, Teff, and logg estimates (resulting from a detailed quantitative spectroscopic analysis) with information… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12776v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12776v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12776v1-abstract-full" style="display: none;"> Stellar rotation is of key importance for the formation process, evolution, and final fate of massive stars. In this paper we review results from the study of the spin rate properties of a sample of more than 400 Galactic O-type stars surveyed by the IACOB and OWN projects. By combining vsini, Teff, and logg estimates (resulting from a detailed quantitative spectroscopic analysis) with information about the spectroscopic binarity status for an important fraction of the stars in the sample, we provide a renewed overview about how the empirical distribution of projected rotational velocities in the O-star domain depends on mass, evolutionary and binary status. The obtained distributions are then compared with predictions of several state-of-the-art evolutionary models for single stars, as well as from population synthesis simulations including binary interaction, and used to provide hints about the initial velocity distribution of stars with masses in the range ~15-80 Msol. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12776v1-abstract-full').style.display = 'none'; document.getElementById('2207.12776v1-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">24 pages, 19 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, A150 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.11806">arXiv:2202.11806</a> <span> [<a href="https://arxiv.org/pdf/2202.11806">pdf</a>, <a href="https://arxiv.org/format/2202.11806">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab3660">10.1093/mnras/stab3660 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The nature of the Cygnus extreme B-supergiant 2MASS J20395358+4222505 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Berlanas%2C+S+R">S. R. Berlanas</a>, <a href="/search/?searchtype=author&query=de+Paz%2C+A+G">A. Gil de Paz</a>, <a href="/search/?searchtype=author&query=Comer%C3%B3n%2C+F">F. Comer贸n</a>, <a href="/search/?searchtype=author&query=Puls%2C+J">J. Puls</a>, <a href="/search/?searchtype=author&query=Alegr%C3%ADa%2C+S+R">S. Ram铆rez Alegr铆a</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa%2C+M">M. Garc铆a</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Najarro%2C+F">F. Najarro</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Urbaneja%2C+M+A">M. A. Urbaneja</a>, <a href="/search/?searchtype=author&query=Gallego%2C+J">J. Gallego</a>, <a href="/search/?searchtype=author&query=Carrasco%2C+E">E. Carrasco</a>, <a href="/search/?searchtype=author&query=Iglesias%2C+J">J. Iglesias</a>, <a href="/search/?searchtype=author&query=Cedazo%2C+R">R. Cedazo</a>, <a href="/search/?searchtype=author&query=Vargas%2C+M+L+G">M. L. Garc铆a Vargas</a>, <a href="/search/?searchtype=author&query=Castillo-Morales%2C+A">A. Castillo-Morales</a>, <a href="/search/?searchtype=author&query=Pascual%2C+S">S. Pascual</a>, <a href="/search/?searchtype=author&query=Cardiel%2C+N">N. Cardiel</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-Calpena%2C+A">A. P茅rez-Calpena</a>, <a href="/search/?searchtype=author&query=G%C3%B3mez-Alvarez%2C+P">P. G贸mez-Alvarez</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADnez-Delgado%2C+I">I. Mart铆nez-Delgado</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.11806v1-abstract-short" style="display: inline;"> 2MASS J20395358+4222505 is an obscured early B supergiant near the massive OB star association Cyg OB2. Despite its bright infrared magnitude (K$_{s}$=5.82) it has remained largely ignored because of its dim optical magnitude (B=16.63, V=13.68). In a previous paper we classified it as a highly reddened, potentially extremely luminous, early B-type supergiant. We obtained its spectrum in the U, B a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.11806v1-abstract-full').style.display = 'inline'; document.getElementById('2202.11806v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.11806v1-abstract-full" style="display: none;"> 2MASS J20395358+4222505 is an obscured early B supergiant near the massive OB star association Cyg OB2. Despite its bright infrared magnitude (K$_{s}$=5.82) it has remained largely ignored because of its dim optical magnitude (B=16.63, V=13.68). In a previous paper we classified it as a highly reddened, potentially extremely luminous, early B-type supergiant. We obtained its spectrum in the U, B and R spectral bands during commissioning observations with the instrument MEGARA@GTC. It displays a particularly strong H$伪$ emission for its spectral type, B1 Ia. The star seems to be in an intermediate phase between super- and hypergiant, a group that it will probably join in the near (astronomical) future. We observe a radial velocity difference between individual observations and determine the stellar parameters, obtaining T$_{eff}$ = 24000 K, logg$_{c}$= 2.88 $\pm$ 0.15. The rotational velocity found is large for a B-supergiant, vsini= 110 $\pm$ 25 km s$^{-1}$. The abundance pattern is consistent with solar, with a mild C underabundance (based on a single line). Assuming that J20395358+4222505 is at the distance of Cyg OB2 we derive the radius from infrared photometry, finding R= 41.2 $\pm$ 4.0 R$_{\odot}$, log(L/L$_{\odot}$)= 5.71 $\pm$ 0.04 and a spectroscopic mass of 46.5 $\pm$ 15.0 M$_{\odot}$. The clumped mass-loss rate (clumping factor 10) is very high for the spectral type, $\dot{M}$ = 2.4x10$^{-6}$ M$_{\odot}$ a$^{-1}$. The high rotational velocity and mass-loss rate place the star at the hot side of the bi-stability jump. Together with the nearly solar CNO abundance pattern, they may also point to evolution in a binary system, J20395358+4222505 being the initial secondary. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.11806v1-abstract-full').style.display = 'none'; document.getElementById('2202.11806v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 February, 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">Accepted for publication in MNRAS, 13 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/?searchtype=author&query=Daflon%2C+S">S. Daflon</a>, <a href="/search/?searchtype=author&query=Gebran%2C+M">M. Gebran</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/?searchtype=author&query=Martins%2C+F">F. Martins</a>, <a href="/search/?searchtype=author&query=Morel%2C+T">T. Morel</a>, <a href="/search/?searchtype=author&query=Berlanas%2C+S+R">S. R. Berlanas</a>, <a href="/search/?searchtype=author&query=Blazere%2C+A">A. Blazere</a>, <a href="/search/?searchtype=author&query=Fremat%2C+Y">Y. Fremat</a>, <a href="/search/?searchtype=author&query=Gosset%2C+E">E. Gosset</a>, <a href="/search/?searchtype=author&query=Apellaniz%2C+J+M">J. Maiz Apellaniz</a>, <a href="/search/?searchtype=author&query=Santos%2C+W">W. Santos</a>, <a href="/search/?searchtype=author&query=Semaan%2C+T">T. Semaan</a>, <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S">S. Simon-Diaz</a>, <a href="/search/?searchtype=author&query=Volpi%2C+D">D. Volpi</a>, <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=Jimenez-Esteban%2C+F">F. Jimenez-Esteban</a>, <a href="/search/?searchtype=author&query=Nieva%2C+M+F">M. F. Nieva</a>, <a href="/search/?searchtype=author&query=Przybilla%2C+N">N. Przybilla</a>, <a href="/search/?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/?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/2106.08865">arXiv:2106.08865</a> <span> [<a href="https://arxiv.org/pdf/2106.08865">pdf</a>, <a href="https://arxiv.org/format/2106.08865">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/10.1051/0004-6361/202141018">10.1051/0004-6361/202141018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MONOS.II. Orbit review and analysis for 35 single-lined spectroscopic binary systems and candidates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</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="2106.08865v2-abstract-short" style="display: inline;"> [ABRIDGED] AIMS: The MONOS project is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 2nd paper, we tackle the study of the 35 single-line spectroscopic binary (SB1) systems identified in the previous paper of the series (arXiv:1904.11385) by analyzing our data and reviewing the literature orbits of such systems. METHODS: We have measured the radial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.08865v2-abstract-full').style.display = 'inline'; document.getElementById('2106.08865v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.08865v2-abstract-full" style="display: none;"> [ABRIDGED] AIMS: The MONOS project is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 2nd paper, we tackle the study of the 35 single-line spectroscopic binary (SB1) systems identified in the previous paper of the series (arXiv:1904.11385) by analyzing our data and reviewing the literature orbits of such systems. METHODS: We have measured the radial velocities for the ~700 spectra in our database using two different methods: Gaussian fitting for several diagnostic lines per object and cross-correlation using synthetic spectra. We also explored the TESS database and analyzed the light curves for 31 of the systems. RESULTS: We have confirmed 21 SB1 systems, discarded the binary nature of 6 stars (9 Sge, HD 192 281, HDE 229 232 AB, 68 Cyg, HD 108 and 伪Cam), and left 6 stars as inconclusive due to lack of data. The remaining two stars are 15 Mon Aa which has been classified as SB2, and Cyg OB2-22 C, for which we find evidence that it is most likely a triple system where the O star is orbiting an eclipsing SB1. We have also recalculated 20 new orbital solutions, including the first spectroscopic orbital solution for V747 Cep. For Cyg OB2-22 C we have obtained new ephemerides but no new orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.08865v2-abstract-full').style.display = 'none'; document.getElementById('2106.08865v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 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">Table 10 and Appendix C are 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> A&A 655, A4 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.14069">arXiv:2103.14069</a> <span> [<a href="https://arxiv.org/pdf/2103.14069">pdf</a>, <a href="https://arxiv.org/format/2103.14069">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/10.1051/0004-6361/202040253">10.1051/0004-6361/202040253 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hubble spectroscopy of LB-1: comparison with B+black-hole and Be+stripped-star models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Irrgang%2C+A">A. Irrgang</a>, <a href="/search/?searchtype=author&query=Bohlin%2C+R">R. Bohlin</a>, <a href="/search/?searchtype=author&query=Deustua%2C+S">S. Deustua</a>, <a href="/search/?searchtype=author&query=Dufton%2C+P+L">P. L. Dufton</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Casares%2C+J">J. Casares</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Darias%2C+T">T. Mu帽oz-Darias</a>, <a href="/search/?searchtype=author&query=Smartt%2C+S+J">S. J. Smartt</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/?searchtype=author&query=de+Burgos%2C+A">A. de Burgos</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="2103.14069v3-abstract-short" style="display: inline;"> LB-1 has variously been proposed as either an X-ray dim B-type star plus black hole (B+BH) binary, or a Be star plus an inflated stripped star (Be+Bstr) binary. The Space Telescope Imaging Spectrograph (STIS) on board HST was used to obtain a flux-calibrated spectrum that is compared with non-LTE spectral energy distributions (SED) and line profiles for the proposed models. The Hubble data, togeth… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.14069v3-abstract-full').style.display = 'inline'; document.getElementById('2103.14069v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.14069v3-abstract-full" style="display: none;"> LB-1 has variously been proposed as either an X-ray dim B-type star plus black hole (B+BH) binary, or a Be star plus an inflated stripped star (Be+Bstr) binary. The Space Telescope Imaging Spectrograph (STIS) on board HST was used to obtain a flux-calibrated spectrum that is compared with non-LTE spectral energy distributions (SED) and line profiles for the proposed models. The Hubble data, together with the Gaia EDR3 parallax, provide tight constraints on the properties and stellar luminosities of the system. In the case of the Be+Bstr model we adopt the published flux ratio for the Be and Bstr stars, re-determine the T$_{eff}$ of the Bstr using the silicon ionization balance, and infer Teff for the Be star from the fit to the SED. We derive stellar parameters consistent with previous results, but with greater precision enabled by the Hubble SED. While the Be+Bstr model is a better fit to the HeI lines and cores of the Balmer lines in the optical, the B+BH model provides a better fit to the Si iv resonance lines in the UV. The analysis also implies that the Bstr star has roughly twice solar silicon abundance, difficult to reconcile with a stripped star origin. The Be star on the other hand has a rather low luminosity, and a spectroscopic mass inconsistent with its possible dynamical mass. The fit to the UV can be significantly improved by reducing the T$_{eff}$ and radius of the Be star, though at the expense of leading to a different mass ratio. In the B+BH model, the single B-type spectrum is a good match to the UV spectrum. Adopting a mass ratio of 5.1$\pm$0.1 (Liu et al. 2020) implies a BH mass of $\sim$21$^{+9}_{-8}M_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.14069v3-abstract-full').style.display = 'none'; document.getElementById('2103.14069v3-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">8 pages, 7 figures, 1 online table In press with 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 649, A167 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.03672">arXiv:2103.03672</a> <span> [<a href="https://arxiv.org/pdf/2103.03672">pdf</a>, <a href="https://arxiv.org/format/2103.03672">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/10.1051/0004-6361/202039426">10.1051/0004-6361/202039426 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Convective core sizes in rotating massive stars: I. Constraints from solar metallicity OB field stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Martinet%2C+S">S. Martinet</a>, <a href="/search/?searchtype=author&query=Meynet%2C+G">G. Meynet</a>, <a href="/search/?searchtype=author&query=Ekstr%C3%B6m%2C+S">S. Ekstr枚m</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=Georgy%2C+C">C. Georgy</a>, <a href="/search/?searchtype=author&query=Eggenberger%2C+P">P. Eggenberger</a>, <a href="/search/?searchtype=author&query=Buldgen%2C+G">G. Buldgen</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Hirschi%2C+R">R. Hirschi</a>, <a href="/search/?searchtype=author&query=Groh%2C+J">J. Groh</a>, <a href="/search/?searchtype=author&query=Farrell%2C+E">E. Farrell</a>, <a href="/search/?searchtype=author&query=Murphy%2C+L">L. Murphy</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="2103.03672v1-abstract-short" style="display: inline;"> Spectroscopic studies of Galactic O and B stars show that many stars with masses above 8 M$_{\odot}$ are observed in the HR diagram just beyond the Main-Sequence (MS) band predicted by stellar models computed with a moderate overshooting. This may be an indication that the convective core sizes in stars in the upper part of the HR diagram are larger than predicted by these models. Combining stella… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.03672v1-abstract-full').style.display = 'inline'; document.getElementById('2103.03672v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.03672v1-abstract-full" style="display: none;"> Spectroscopic studies of Galactic O and B stars show that many stars with masses above 8 M$_{\odot}$ are observed in the HR diagram just beyond the Main-Sequence (MS) band predicted by stellar models computed with a moderate overshooting. This may be an indication that the convective core sizes in stars in the upper part of the HR diagram are larger than predicted by these models. Combining stellar evolution models and spectroscopic parameters derived for a large sample of Galactic O and B stars, including brand new information about their projected rotational velocities, we reexamine the question of the convective core size in MS massive stars. We confirm that for stars more massive than about 8 M$_{\odot}$, the convective core size at the end of the MS phase increases more rapidly with the mass than in models computed with a constant step overshoot chosen to reproduce the main sequence width in the low mass range (around 2 M$_{\odot}$). This conclusion is valid for both the cases of non-rotating models and rotating models either with a moderate or a strong angular momentum transport. The increase of the convective core mass with the mass obtained from the TAMS position is, however, larger than the one deduced from the surface velocity drop for masses above about 15 M$_{\odot}$. Although observations available at the moment cannot decide what is the best choice between the core sizes given by the TAMS and the velocity drop, we discuss different methods to get out of this dilemma. At the moment, comparisons with eclipsing binaries seem to favor the solution given by the velocity drop. While we confirm the need for larger convective cores at higher masses, we find tensions in-between different methods for stars more massive than 15 M$_{\odot}$. The use of single-aged stellar populations (non-interacting binaries or stellar clusters) would be a great asset to resolve this tension. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.03672v1-abstract-full').style.display = 'none'; document.getElementById('2103.03672v1-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">13 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 648, A126 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.03372">arXiv:2102.03372</a> <span> [<a href="https://arxiv.org/pdf/2102.03372">pdf</a>, <a href="https://arxiv.org/format/2102.03372">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/10.1051/0004-6361/202040008">10.1051/0004-6361/202040008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mapping the core of the Tarantula Nebula with VLT-MUSE II. The spectroscopic Hertzsprung-Russell diagram of OB stars in NGC 2070 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=Crowther%2C+P+A">P. A. Crowther</a>, <a href="/search/?searchtype=author&query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/?searchtype=author&query=Vink%2C+J+S">J. S. Vink</a>, <a href="/search/?searchtype=author&query=Puls%2C+J">J. Puls</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Garcia%2C+M">M. Garcia</a>, <a href="/search/?searchtype=author&query=Selman%2C+F+J">F. J. Selman</a>, <a href="/search/?searchtype=author&query=Roth%2C+M+M">M. M. Roth</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.03372v1-abstract-short" style="display: inline;"> We present the spectroscopic analysis of 333 OB-type stars extracted from VLT-MUSE observations of the central 30 x 30 pc of NGC 2070 in the Tarantula Nebula on the Large Magellanic Cloud, the majority of which are analysed for the the first time. The distribution of stars in the spectroscopic Hertzsprung-Russell diagram (sHRD) shows 281 stars in the main sequence. We find two groups in the main s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.03372v1-abstract-full').style.display = 'inline'; document.getElementById('2102.03372v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.03372v1-abstract-full" style="display: none;"> We present the spectroscopic analysis of 333 OB-type stars extracted from VLT-MUSE observations of the central 30 x 30 pc of NGC 2070 in the Tarantula Nebula on the Large Magellanic Cloud, the majority of which are analysed for the the first time. The distribution of stars in the spectroscopic Hertzsprung-Russell diagram (sHRD) shows 281 stars in the main sequence. We find two groups in the main sequence, with estimated ages of 2.1$\pm$0.8 and 6.2$\pm$2 Myr. A subgroup of 52 stars is apparently beyond the main sequence phase, which we consider to be due to emission-type objects and/or significant nebular contamination affecting the analysis. As in previous studies, stellar masses derived from the sHRD are systematically larger than those obtained from the conventional HRD, with the differences being largest for the most massive stars. Additionally, we do not find any trend between the estimated projected rotational velocity and evolution in the sHRD. The projected rotational velocity distribution presents a tail of fast rotators that resembles findings in the wider population of 30 Doradus. We use published spectral types to calibrate the HeI$位$4921/HeII$位$5411 equivalent-width ratio as a classification diagnostic for early-type main sequence stars when the classical blue-visible region is not observed. Our model-atmosphere analyses demonstrate that the resulting calibration is well correlated with effective temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.03372v1-abstract-full').style.display = 'none'; document.getElementById('2102.03372v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 12 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 648, A65 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.12250">arXiv:2011.12250</a> <span> [<a href="https://arxiv.org/pdf/2011.12250">pdf</a>, <a href="https://arxiv.org/format/2011.12250">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/10.1051/0004-6361/202039479">10.1051/0004-6361/202039479 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lucky spectroscopy, an equivalent technique to Lucky Imaging: II. Spatially-resolved intermediate-resolution blue-violet spectroscopy of 19 close massive binaries using the William Herschel Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Fari%C3%B1a%2C+C">C. Fari帽a</a>, <a href="/search/?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.12250v1-abstract-short" style="display: inline;"> CONTEXT. Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS. We want to continue obtaining spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. METHODS. We have used lucky spectroscopy to obtain many short long-slit spectroscopic exposures of 19 close visual binaries under good seeing conditi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.12250v1-abstract-full').style.display = 'inline'; document.getElementById('2011.12250v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.12250v1-abstract-full" style="display: none;"> CONTEXT. Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS. We want to continue obtaining spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. METHODS. We have used lucky spectroscopy to obtain many short long-slit spectroscopic exposures of 19 close visual binaries under good seeing conditions. We selected those with the best characteristics, extracted the spectra using multiple-profile fitting, and combined the results to derive spatially separated spectra. The results are analyzed in combination with data from lucky imaging, regular intermediate-resolution single-order spectroscopy, and 茅chelle high-resolution spectroscopy. RESULTS. The new application of lucky spectroscopy has allowed us to [a] spatially disentangle for the first time two O stars (FN CMa B and 6 Cas B) with brighter BA supergiant companions; [b] determine that two B stars (alpha Sco B and HD 164492 B) with close and more massive companions are fast rotators; [c] extend the technique to cases with extreme magnitude differences, shorter separations, and fainter primary magnitudes down to B=11; [d] spatially disentangle the spectra of stars with companions as diverse as an A supergiant (6 Cas A), a WR star (WR 157), and an M supergiant (alpha Sco A); [e] discover the unexpected identity of some targets such as two previously unknown bright O stars (HD 51756 B and BD +60 544) and a new member of the rare OC category (HD 8768 A); and [f] identify and classify which of the components of four visual binaries is a double-lined spectroscopic binary and for another seven systems detect signs of spectroscopic binarity using high-spectral-resolution spectroscopy. We also present a determination of the limits of the technique. [ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.12250v1-abstract-full').style.display = 'none'; document.getElementById('2011.12250v1-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 646, A11 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.05136">arXiv:2009.05136</a> <span> [<a href="https://arxiv.org/pdf/2009.05136">pdf</a>, <a href="https://arxiv.org/format/2009.05136">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/staa2801">10.1093/mnras/staa2801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The R136 star cluster dissected with Hubble Space Telescope/STIS. II. Physical properties of the most massive stars in R136 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bestenlehner%2C+J+M">Joachim M. Bestenlehner</a>, <a href="/search/?searchtype=author&query=Crowther%2C+P+A">Paul A. Crowther</a>, <a href="/search/?searchtype=author&query=Caballero-Nieves%2C+S+M">Saida M. Caballero-Nieves</a>, <a href="/search/?searchtype=author&query=Schneider%2C+F+R+N">Fabian R. N. Schneider</a>, <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S">Sergio Simon-Diaz</a>, <a href="/search/?searchtype=author&query=Brands%2C+S+A">Sarah A. Brands</a>, <a href="/search/?searchtype=author&query=de+Koter%2C+A">Alex de Koter</a>, <a href="/search/?searchtype=author&query=Graefener%2C+G">Goetz Graefener</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">Artemio Herrero</a>, <a href="/search/?searchtype=author&query=Langer%2C+N">Norbert Langer</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">Daniel J. Lennon</a>, <a href="/search/?searchtype=author&query=Apellaniz%2C+J+M">Jesus Maiz Apellaniz</a>, <a href="/search/?searchtype=author&query=Puls%2C+J">Joachim Puls</a>, <a href="/search/?searchtype=author&query=Vink%2C+J+S">Jorick 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="2009.05136v1-abstract-short" style="display: inline;"> We present an optical analysis of 55 members of R136, the central cluster in the Tarantula Nebula of the Large Magellanic Cloud. Our sample was observed with STIS aboard the Hubble Space Telescope, is complete down to about 40\,$M_{\odot}$, and includes 7 very massive stars with masses over 100\,$M_{\odot}$. We performed a spectroscopic analysis to derive their physical properties. Using evolution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05136v1-abstract-full').style.display = 'inline'; document.getElementById('2009.05136v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.05136v1-abstract-full" style="display: none;"> We present an optical analysis of 55 members of R136, the central cluster in the Tarantula Nebula of the Large Magellanic Cloud. Our sample was observed with STIS aboard the Hubble Space Telescope, is complete down to about 40\,$M_{\odot}$, and includes 7 very massive stars with masses over 100\,$M_{\odot}$. We performed a spectroscopic analysis to derive their physical properties. Using evolutionary models we find that the initial mass function (IMF) of massive stars in R136 is suggestive of being top-heavy with a power-law exponent $纬\approx 2 \pm 0.3$, but steeper exponents cannot be excluded. The age of R136 lies between 1 and 2\,Myr with a median age of around 1.6\,Myr. Stars more luminous than $\log L/L_{\odot} = 6.3$ are helium enriched and their evolution is dominated by mass loss, but rotational mixing or some other form of mixing could be still required to explain the helium composition at the surface. Stars more massive than 40\,$M_{\odot}$ have larger spectroscopic than evolutionary masses. The slope of the wind-luminosity relation assuming unclumped stellar winds is $2.41\pm0.13$ which is steeper than usually obtained ($\sim 1.8$). The ionising ($\log Q_0\,[{\rm ph/s}] = 51.4$) and mechanical ($\log L_{\rm SW}\,[{\rm erg/s}] = 39.1$) output of R136 is dominated by the most massive stars ($>100\,M_{\odot}$). R136 contributes around a quarter of the ionising flux and around a fifth of the mechanical feedback to the overall budget of the Tarantula Nebula. For a census of massive stars of the Tarantula Nebula region we combined our results with the VLT-FLAMES Tarantula Survey plus other spectroscopic studies. We observe a lack of evolved Wolf-Rayet stars and luminous blue and red supergiants. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05136v1-abstract-full').style.display = 'none'; document.getElementById('2009.05136v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 September, 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">Accepted for publication in MNRAS, 21 pages, 14 figures, 2 tables plus 33 pages of supplementary material</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.13299">arXiv:2008.13299</a> <span> [<a href="https://arxiv.org/pdf/2008.13299">pdf</a>, <a href="https://arxiv.org/format/2008.13299">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/10.1051/0004-6361/202039019">10.1051/0004-6361/202039019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-resolution spectroscopic study of massive blue and red supergiants in Per OB1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=de+Burgos%2C+A">A. de Burgos</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Dorda%2C+R">R. Dorda</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/?searchtype=author&query=Urbaneja%2C+M+A">M. A. Urbaneja</a>, <a href="/search/?searchtype=author&query=Patrick%2C+L+R">L. R. Patrick</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.13299v2-abstract-short" style="display: inline;"> The Perseus OB1 association hosts one of the most populous groupings of blue and red supergiants (Sgs) in the Galaxy. We discuss whether the massive O-type and blue/red Sg stars located in the Per OB1 region are members of the same population and examine their binary and runaway status. We gathered a total of 405 high-resolution spectra for 88 suitable candidates around 4.5 deg from the center of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.13299v2-abstract-full').style.display = 'inline'; document.getElementById('2008.13299v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.13299v2-abstract-full" style="display: none;"> The Perseus OB1 association hosts one of the most populous groupings of blue and red supergiants (Sgs) in the Galaxy. We discuss whether the massive O-type and blue/red Sg stars located in the Per OB1 region are members of the same population and examine their binary and runaway status. We gathered a total of 405 high-resolution spectra for 88 suitable candidates around 4.5 deg from the center of the association, and compiled Gaia DR2 astrometry for all of them. This was used to investigate membership and identify runaway stars. By obtaining high-precision radial velocity (RV) estimates, we investigated the RV distributions of sample and identified spectroscopic binaries (SBs). Most of the investigated stars belong to a physically linked population located at d = 2.5$\pm$0.4 kpc. We identify 79 confirmed or likely members, and 5 member candidates. No important differences are detected in the distribution of parallaxes for stars in h and X Persei or the full sample. On the contrary, most O-type stars seem to be part of a differentiated population in terms of kinematical properties. In particular, the percentage of runaways among them (45%) is considerable higher than for the more evolved targets (that is below 5% in all cases). A similar tendency is also found for the percentage of clearly detected SBs, which already decreases from 15% to 10% when comparing the O star and B Sg samples, respectively, and practically vanishes in the cooler Sgs. All but 4 stars in our working sample can be considered as part of the same (interrelated) population. However, any further attempt to describe the empirical properties of this sample of massive stars in an evolutionary context must take into account that an important fraction of the O stars is - or has likely been - part of a binary/multiple system. In addition, some of the other more evolved targets may have also been affected by binary evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.13299v2-abstract-full').style.display = 'none'; document.getElementById('2008.13299v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 29 pages, 10 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, A116 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.09917">arXiv:2008.09917</a> <span> [<a href="https://arxiv.org/pdf/2008.09917">pdf</a>, <a href="https://arxiv.org/format/2008.09917">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/10.1051/0004-6361/202039015">10.1051/0004-6361/202039015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic characterization of the known O-star population in Cygnus OB2. Evidence of multiple star-forming bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Berlanas%2C+S+R">S. R. Berlanas</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Comer%C3%B3n%2C+F">F. Comer贸n</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Pasquali%2C+A">A. Pasquali</a>, <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/?searchtype=author&query=Peller%C3%ADn%2C+A">A. Peller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="2008.09917v3-abstract-short" style="display: inline;"> Cygnus OB2 provides a unique insight into the high-mass stellar content in one of the largest groups of young massive stars in our Galaxy. Although several studies of its massive population have been carried out over the last decades, an extensive spectroscopic study of the whole known O-star population in the association is still lacking. In this work, we created the most complete spectroscopic c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.09917v3-abstract-full').style.display = 'inline'; document.getElementById('2008.09917v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.09917v3-abstract-full" style="display: none;"> Cygnus OB2 provides a unique insight into the high-mass stellar content in one of the largest groups of young massive stars in our Galaxy. Although several studies of its massive population have been carried out over the last decades, an extensive spectroscopic study of the whole known O-star population in the association is still lacking. In this work, we created the most complete spectroscopic census of O stars carried out so far in Cygnus OB2 using already existing and new spectroscopy. We present the spectra for 78 O-type stars, from which we identify new binary systems, obtain the distribution of rotational velocities, and determine the main stellar parameters for all the stars in the region that have not been detected as double-line spectroscopic binaries. We also derive radii, luminosities, and masses for those stars with reliable Gaia astrometry, in addition to creating the Hertzsprung-Russell Diagram to interpret the evolutionary status of the association. This work has shown the improvement reached when using accurate spectroscopic parameters and astrometry for the interpretation of the evolutionary status of a population, revealing, in the case of Cygnus OB2, at least two star-forming bursts at $\sim$3 and $\sim$5 Myr. We find an apparent deficit of very fast rotators in the distribution of rotational velocities. The inspection of the dynamical distribution of the sample has allowed us to identify nine O stars with peculiar proper motions and discuss a possible dynamical ejection scenario or past supernova explosions in the region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.09917v3-abstract-full').style.display = 'none'; document.getElementById('2008.09917v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 25 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.09239">arXiv:2007.09239</a> <span> [<a href="https://arxiv.org/pdf/2007.09239">pdf</a>, <a href="https://arxiv.org/format/2007.09239">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa2214">10.1093/mnras/staa2214 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An extensive spectroscopic time series of three Wolf-Rayet stars -- II. A search for wind asymmetries in the dust-forming WC7 binary WR137 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=St-Louis%2C+N">N. St-Louis</a>, <a href="/search/?searchtype=author&query=Piaulet%2C+C">C. Piaulet</a>, <a href="/search/?searchtype=author&query=Richardson%2C+N+D">N. D. Richardson</a>, <a href="/search/?searchtype=author&query=Shenar%2C+T">T. Shenar</a>, <a href="/search/?searchtype=author&query=Moffat%2C+A+F+J">A. F. J. Moffat</a>, <a href="/search/?searchtype=author&query=Eversberg%2C+T">T. Eversberg</a>, <a href="/search/?searchtype=author&query=Hill%2C+G+M">G. M. Hill</a>, <a href="/search/?searchtype=author&query=Gauza%2C+B">B. Gauza</a>, <a href="/search/?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</a>, <a href="/search/?searchtype=author&query=Kubat%2C+J">J. Kubat</a>, <a href="/search/?searchtype=author&query=Kubatova%2C+B">B. Kubatova</a>, <a href="/search/?searchtype=author&query=Sablowski%2C+D+P">D. P. Sablowski</a>, <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S">S. Simon-Diaz</a>, <a href="/search/?searchtype=author&query=Bolduan%2C+F">F. Bolduan</a>, <a href="/search/?searchtype=author&query=Dias%2C+F+M">F. M. Dias</a>, <a href="/search/?searchtype=author&query=Dubreuil%2C+P">P. Dubreuil</a>, <a href="/search/?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/?searchtype=author&query=Garrel%2C+T">T. Garrel</a>, <a href="/search/?searchtype=author&query=Grutzeck%2C+G">G. Grutzeck</a>, <a href="/search/?searchtype=author&query=Hunger%2C+T">T. Hunger</a>, <a href="/search/?searchtype=author&query=Kusters%2C+D">D. Kusters</a>, <a href="/search/?searchtype=author&query=Langenbrink%2C+M">M. Langenbrink</a>, <a href="/search/?searchtype=author&query=Leadbeater%2C+R">R. Leadbeater</a>, <a href="/search/?searchtype=author&query=Li%2C+D">D. Li</a>, <a href="/search/?searchtype=author&query=Lopez%2C+A">A. Lopez</a> , et al. (17 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="2007.09239v1-abstract-short" style="display: inline;"> We present the results of a four-month, spectroscopic campaign of the Wolf-Rayet dust-making binary, WR137. We detect only small-amplitude, random variability in the CIII5696 emission line and its integrated quantities (radial velocity, equivalent width, skewness, kurtosis) that can be explained by stochastic clumps in the wind of the WC star. We find no evidence of large-scale, periodic variation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.09239v1-abstract-full').style.display = 'inline'; document.getElementById('2007.09239v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.09239v1-abstract-full" style="display: none;"> We present the results of a four-month, spectroscopic campaign of the Wolf-Rayet dust-making binary, WR137. We detect only small-amplitude, random variability in the CIII5696 emission line and its integrated quantities (radial velocity, equivalent width, skewness, kurtosis) that can be explained by stochastic clumps in the wind of the WC star. We find no evidence of large-scale, periodic variations often associated with Corotating Interaction Regions that could have explained the observed intrinsic continuum polarization of this star. Our moderately high-resolution and high signal-to-noise average Keck spectrum shows narrow double-peak emission profiles in the Halpha, Hbeta, Hgamma, HeII6678 and HeII5876 lines. These peaks have a stable blue-to-red intensity ratio with a mean of 0.997 and a root-mean-square of 0.004, commensurate with the noise level; no variability is found during the entire observing period. We suggest that these profiles arise in a decretion disk around the O9 companion, which is thus an O9e star. The characteristics of the profiles are compatible with those of other Be/Oe stars. The presence of this disk can explain the constant component of the continuum polarization of this system, for which the angle is perpendicular to the plane of the orbit, implying that the rotation axis of the O9e star is aligned with that of the orbit. It remains to be explained why the disk is so stable within the strong ultraviolet radiation field of the O star. We present a binary evolutionary scenario that is compatible with the current stellar and system parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.09239v1-abstract-full').style.display = 'none'; document.getElementById('2007.09239v1-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 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">12 pages, 5 Figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.03012">arXiv:2006.03012</a> <span> [<a href="https://arxiv.org/pdf/2006.03012">pdf</a>, <a href="https://arxiv.org/format/2006.03012">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/10.1051/0004-6361/202038224">10.1051/0004-6361/202038224 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photometric detection of internal gravity waves in upper main-sequence stars. II. Combined TESS photometry and high-resolution spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/?searchtype=author&query=Burssens%2C+S">S. Burssens</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Edelmann%2C+P+V+F">P. V. F. Edelmann</a>, <a href="/search/?searchtype=author&query=Rogers%2C+T+M">T. M. Rogers</a>, <a href="/search/?searchtype=author&query=Horst%2C+L">L. Horst</a>, <a href="/search/?searchtype=author&query=Roepke%2C+F+K">F. K. Roepke</a>, <a href="/search/?searchtype=author&query=Aerts%2C+C">C. Aerts</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.03012v2-abstract-short" style="display: inline;"> Context. Massive stars are predicted to excite internal gravity waves (IGWs) by turbulent core convection and from turbulent pressure fluctuations in their near-surface layers. These IGWs are extremely efficient at transporting angular momentum and chemical species within stellar interiors, but they remain largely unconstrained observationally. Aims. We aim to characterise the photometric detectio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.03012v2-abstract-full').style.display = 'inline'; document.getElementById('2006.03012v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.03012v2-abstract-full" style="display: none;"> Context. Massive stars are predicted to excite internal gravity waves (IGWs) by turbulent core convection and from turbulent pressure fluctuations in their near-surface layers. These IGWs are extremely efficient at transporting angular momentum and chemical species within stellar interiors, but they remain largely unconstrained observationally. Aims. We aim to characterise the photometric detection of IGWs across a large number of O and early-B stars in the Hertzsprung-Russell diagram, and explain the ubiquitous detection of stochastic variability in the photospheres of massive stars. Methods. We combined high-precision time-series photometry from the NASA Transiting Exoplanet Survey Satellite with high-resolution ground-based spectroscopy of 70 stars with spectral types O and B to probe the relationship between the photometric signatures of IGWs and parameters such as spectroscopic mass, luminosity, and macroturbulence. Results. A relationship is found between the location of a star in the spectroscopic Hertzsprung-Russell diagram and the amplitudes and frequencies of stochastic photometric variability in the light curves of massive stars. Furthermore, the properties of the stochastic variability are statistically correlated with macroturbulent velocity broadening in the spectral lines of massive stars. Conclusions. The common ensemble morphology for the stochastic low-frequency variability detected in space photometry and its relationship to macroturbulence is strong evidence for IGWs in massive stars, since these types of waves are unique in providing the dominant tangential velocity field required to explain the observed spectroscopy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.03012v2-abstract-full').style.display = 'none'; document.getElementById('2006.03012v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. 10 pages and 5 figures (and an additional 7 pages of appendix tables and figures). Resolution of appendix figures have been downgraded to meet arXiv's maximum file size of 15Mb. This version (2ver) is post A&A language editing</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 640, A36 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.12595">arXiv:2005.12595</a> <span> [<a href="https://arxiv.org/pdf/2005.12595">pdf</a>, <a href="https://arxiv.org/ps/2005.12595">ps</a>, <a href="https://arxiv.org/format/2005.12595">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/10.3847/1538-4357/aba49e">10.3847/1538-4357/aba49e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Phase-dependent study of near-infrared disk emission lines in LB-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Liu%2C+J">Jifeng Liu</a>, <a href="/search/?searchtype=author&query=Zheng%2C+Z">Zheng Zheng</a>, <a href="/search/?searchtype=author&query=Soria%2C+R">Roberto Soria</a>, <a href="/search/?searchtype=author&query=Aceituno%2C+J">Jesus Aceituno</a>, <a href="/search/?searchtype=author&query=Zhang%2C+H">Haotong Zhang</a>, <a href="/search/?searchtype=author&query=Lu%2C+Y">Youjun Lu</a>, <a href="/search/?searchtype=author&query=Wang%2C+S">Song Wang</a>, <a href="/search/?searchtype=author&query=Hamann%2C+W">Wolf-Rainer Hamann</a>, <a href="/search/?searchtype=author&query=Oskinova%2C+L+M">Lida M. Oskinova</a>, <a href="/search/?searchtype=author&query=Ramachandran%2C+V">Varsha Ramachandran</a>, <a href="/search/?searchtype=author&query=Yuan%2C+H">Hailong Yuan</a>, <a href="/search/?searchtype=author&query=Bai%2C+Z">Zhongrui Bai</a>, <a href="/search/?searchtype=author&query=Wang%2C+S">Shu Wang</a>, <a href="/search/?searchtype=author&query=McKee%2C+B+J">Brendan J. McKee</a>, <a href="/search/?searchtype=author&query=Wu%2C+J">Jianfeng Wu</a>, <a href="/search/?searchtype=author&query=Wang%2C+J">Junfeng Wang</a>, <a href="/search/?searchtype=author&query=Lattanzi%2C+M">Mario Lattanzi</a>, <a href="/search/?searchtype=author&query=Belczynski%2C+K">Krzysztof Belczynski</a>, <a href="/search/?searchtype=author&query=Casares%2C+J">Jorge Casares</a>, <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S">Sergio Simon-Diaz</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">Jonay I. Gonz谩lez Hern谩ndez</a>, <a href="/search/?searchtype=author&query=Rebolo%2C+R">Rafael Rebolo</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="2005.12595v1-abstract-short" style="display: inline;"> The mass, origin and evolutionary stage of the binary system LB-1 has been the subject of intense debate, following the claim that it hosts an $\sim$70$M_{\odot}$ black hole, in stark contrast with the expectations for stellar remnants in the Milky Way. We conducted a high-resolution, phase-resolved spectroscopic study of the near-infrared Paschen lines in this system, using the 3.5-m telescope at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12595v1-abstract-full').style.display = 'inline'; document.getElementById('2005.12595v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.12595v1-abstract-full" style="display: none;"> The mass, origin and evolutionary stage of the binary system LB-1 has been the subject of intense debate, following the claim that it hosts an $\sim$70$M_{\odot}$ black hole, in stark contrast with the expectations for stellar remnants in the Milky Way. We conducted a high-resolution, phase-resolved spectroscopic study of the near-infrared Paschen lines in this system, using the 3.5-m telescope at Calar Alto Observatory. We find that Pa$尾$ and Pa$纬$ (after proper subtraction of the stellar absorption component) are well fitted with a standard double-peaked model, typical of disk emission. We measured the velocity shifts of the red and blue peaks at 28 orbital phases: the line center has an orbital motion in perfect antiphase with the stellar motion, and the radial velocity amplitude ranges from 8 to 13 km/s for different choices of lines and profile modelling. We interpret this curve as proof that the disk is tracing the orbital motion of the primary, ruling out the circumbinary disk and the hierarchical triple scenarios. The phase-averaged peak-to-peak half-separation (proxy for the projected rotational velocity of the outer disk) is $\sim$70 km s$^{-1}$, larger than the stellar orbital velocity and also inconsistent with a circumbinary disk. From those results, we infer a primary mass 4--8 times higher than the secondary mass. Moreover, we show that the ratio of the blue and red peaks (V/R intensity ratio) has a sinusoidal behaviour in phase with the secondary star, which can be interpreted as the effect of external irradiation by the secondary star on the outer disk. Finally, we briefly discuss our findings in the context of alternative scenarios recently proposed for LB-1. Definitive tests between alternative solutions will require further astrometric data from $Gaia$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12595v1-abstract-full').style.display = 'none'; document.getElementById('2005.12595v1-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 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">To be submitted to ApJ. Comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.09658">arXiv:2005.09658</a> <span> [<a href="https://arxiv.org/pdf/2005.09658">pdf</a>, <a href="https://arxiv.org/format/2005.09658">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/10.1051/0004-6361/202037700">10.1051/0004-6361/202037700 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variability of OB stars from TESS southern Sectors 1-13 and high-resolution IACOB and OWN spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Burssens%2C+S">S. Burssens</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=Michielsen%2C+M">M. Michielsen</a>, <a href="/search/?searchtype=author&query=de+Burgos%2C+A">A. de Burgos</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Aerts%2C+C">C. Aerts</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="2005.09658v2-abstract-short" style="display: inline;"> Lack of high-precision long-term continuous photometric data for large samples of stars has prevented the large-scale exploration of pulsational variability in the OB star regime. As a result, the candidates for in-depth asteroseismic modelling remained limited to a few tens of dwarfs. The TESS nominal space mission has surveyed the southern sky, yielding continuous data of at least 27 d for hundr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.09658v2-abstract-full').style.display = 'inline'; document.getElementById('2005.09658v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.09658v2-abstract-full" style="display: none;"> Lack of high-precision long-term continuous photometric data for large samples of stars has prevented the large-scale exploration of pulsational variability in the OB star regime. As a result, the candidates for in-depth asteroseismic modelling remained limited to a few tens of dwarfs. The TESS nominal space mission has surveyed the southern sky, yielding continuous data of at least 27 d for hundreds of OB stars. We aim to couple TESS data in the southern sky with spectroscopy to study the variability over mass and evolution. We focus mainly on the presence of coherent pulsation modes that may or may not be present in the theoretical instability domains and unravel all frequency behaviour in the amplitude spectra of the TESS data. We compose a sample of 98 OB-type stars observed by TESS in Sectors 1-13 and with available high-resolution spectroscopy gathered by the IACOB and OWN surveys. We present the short-cadence 2-min light curves of dozens of OB-type stars, that have one or more spectra in the IACOB or OWN database. Based on these light curves and their Lomb-Scargle periodograms we perform variability classification and frequency analysis, and place the stars in the spectroscopic Hertzsprung-Russell diagram to interpret the variability in an evolutionary context. We deduce diverse origins of the variability found in all of the 98 OB stars in the TESS data. Among these we find several new variable stars, including three hybrid pulsators, three eclipsing binaries, high frequency modes in a Be star, and potential heat-driven pulsations in two Oe stars. We identify stars for which future asteroseismic modelling is possible, provided mode identification is achieved. By comparing the position of the variables to theoretical instability strips we discuss the current shortcomings in non-adiabatic pulsation theory, and the distribution of pulsators in the upper Hertzsprung-Russell diagram. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.09658v2-abstract-full').style.display = 'none'; document.getElementById('2005.09658v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 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">Accepted for publication in A&A. 18(+47) pages, 15(+100) figures, 3(+2) tables. Language edited and typos removed. Fig. 3, 14, 15 corrected for small plotting error (results unchanged)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 639, A81 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.05446">arXiv:2005.05446</a> <span> [<a href="https://arxiv.org/pdf/2005.05446">pdf</a>, <a href="https://arxiv.org/format/2005.05446">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/10.1051/0004-6361/202037699">10.1051/0004-6361/202037699 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project. VI. On the elusive detection of massive O-type stars close to the ZAMS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Haemmerl%C3%A9%2C+L">L. Haemmerl茅</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Cervi%C3%B1o%2C+M">M. Cervi帽o</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Meynet%2C+G">G. Meynet</a>, <a href="/search/?searchtype=author&query=Arias%2C+J+I">J. I. Arias</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="2005.05446v3-abstract-short" style="display: inline;"> The apparent lack of massive O-type stars near the zero-age main sequence (at ages < 2 Myr) is a topic widely discussed. Different explanations for this elusive detection have been proposed, but no firm conclusions have been reached yet. We reassess this empirical result benefiting from the high-quality spectroscopic observations of >400 Galactic O-type stars gathered by the IACOB and OWN surveys.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05446v3-abstract-full').style.display = 'inline'; document.getElementById('2005.05446v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.05446v3-abstract-full" style="display: none;"> The apparent lack of massive O-type stars near the zero-age main sequence (at ages < 2 Myr) is a topic widely discussed. Different explanations for this elusive detection have been proposed, but no firm conclusions have been reached yet. We reassess this empirical result benefiting from the high-quality spectroscopic observations of >400 Galactic O-type stars gathered by the IACOB and OWN surveys. We used temperatures and gravities from a iacob-gbat/fastwind spectroscopic analysis to locate our sample in the Kiel and spectroscopic HR diagrams. We evaluated the completeness of our sample of stars, observational biases using information from the Galactic O star catalog (GOSC), systematics of our methodology, and compare with other recent studies using smaller samples of Galactic O-type stars. We base our discussion on the spectroscopic HR diagram to avoid the use of uncertain distances. We performed a detailed study of the young cluster Trumpler-14 as an example of how Gaia cluster distances can help to construct the associated classical HR diagram. The apparent lack of massive O-type stars near the ZAMS with masses between 30 and 70 Msol persist even when spectroscopic results from a large, non-biased sample of stars are used. We do not find correlation between the dearth of stars and observational biases, limitations of our methodology, or the use of spectroscopic HR diagram instead of the classical one. Investigating the efficiency of mass accretion during the formation process we conclude that an adjustment of the accretion rate towards lower values could reconcile the hotter boundary of detected O-type stars and the theoretical birthline. Last, we discuss that the presence of a small sample of O2-O3.5 stars found closer to the ZAMS might be explained taking into account non-standard star evolution (e.g. binary interaction, mergers, or homogeneous evolution). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05446v3-abstract-full').style.display = 'none'; document.getElementById('2005.05446v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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, 15 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 638, A157 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.09863">arXiv:2003.09863</a> <span> [<a href="https://arxiv.org/pdf/2003.09863">pdf</a>, <a href="https://arxiv.org/format/2003.09863">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa819">10.1093/mnras/staa819 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Analysis of absorption lines in the high resolution spectra of five hot post-AGB candidates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Parthasarathy%2C+M">M. Parthasarathy</a>, <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S">S. Simon-Diaz</a>, <a href="/search/?searchtype=author&query=Hubrig%2C+S">S. Hubrig</a>, <a href="/search/?searchtype=author&query=Sarkar%2C+G">G. Sarkar</a>, <a href="/search/?searchtype=author&query=Muneer%2C+S">S. Muneer</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="2003.09863v1-abstract-short" style="display: inline;"> From an analysis of absorption lines in the high resolution spectra we have derived the radial velocities, stellar parameters (Teff, gravity, wind-strength parameter logQ and projected rotational velocity) and abundances (C, N, O, and Si ) of IRAS 17460-3114, IRAS 18131-3008, IRAS 19336-0400, LSE 45 and LSE 163. Abundances are found to be solar, except for a low Si abundance in IRAS 19336-0400 and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.09863v1-abstract-full').style.display = 'inline'; document.getElementById('2003.09863v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.09863v1-abstract-full" style="display: none;"> From an analysis of absorption lines in the high resolution spectra we have derived the radial velocities, stellar parameters (Teff, gravity, wind-strength parameter logQ and projected rotational velocity) and abundances (C, N, O, and Si ) of IRAS 17460-3114, IRAS 18131-3008, IRAS 19336-0400, LSE 45 and LSE 163. Abundances are found to be solar, except for a low Si abundance in IRAS 19336-0400 and a mild CNO pattern in LSE 163, that rotates at an unusual large rotational velocity for its spectral classification. Combining the stellar parameters information with Gaia DR2 data we are able to derive absolute magnitudes, radii and luminosities and clarify the possible post-AGB nature of the objects. IRAS 17460-3114 and IRAS 18131-3008 are found to be massive OB stars, whereas IRAS 19336-0400 is found to be a post-AGB star, already showing nebular lines in the spectrum. However, we could not confirm the nature of LSE 45 and LSE 163 as post-AGB stars, although their parameters are much more inconsistent with those of massive stars. In both cases, we find a discrepancy between the spectroscopic mass and that derived from the predictions of post-AGB evolutionary tracks. In addition, LSE 45 lacks nebular lines, that are present in IRAS 19336-0400 at a similar temperature. In the case of LSE 163 the rotational velocity (259+/-15 km/s) would be extremely large for a star evolving to CSPN. The combination of this rotational velocity, the high Galactic latitude, slightly large radial velocity and mild CNO enhancement suggests a history of binary interaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.09863v1-abstract-full').style.display = 'none'; document.getElementById('2003.09863v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">15 pages, 10 figures accepted for 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/2001.04853">arXiv:2001.04853</a> <span> [<a href="https://arxiv.org/pdf/2001.04853">pdf</a>, <a href="https://arxiv.org/format/2001.04853">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/10.1007/978-3-030-38509-5_6">10.1007/978-3-030-38509-5_6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A modern guide to quantitative spectroscopy of massive OB stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</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="2001.04853v1-abstract-short" style="display: inline;"> Quantitative spectroscopy is a powerful technique from which we can extract information about the physical properties and surface chemical composition of stars. In this chapter, I guide the reader through the main ideas required to get initiated in the learning process to become an expert in the application of state-of-the-art quantitative spectroscopic techniques to the study of massive OB stars.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.04853v1-abstract-full').style.display = 'inline'; document.getElementById('2001.04853v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.04853v1-abstract-full" style="display: none;"> Quantitative spectroscopy is a powerful technique from which we can extract information about the physical properties and surface chemical composition of stars. In this chapter, I guide the reader through the main ideas required to get initiated in the learning process to become an expert in the application of state-of-the-art quantitative spectroscopic techniques to the study of massive OB stars. NB: This chapter is intended to serve to young students as a first approach to a field which has attracted my attention during the last 20 years. I should note that, despite its importance, at present, the number of real experts in the field around the world is limited to less than 50 people, and about one third of them are close to retirement. Hence, I consider that this is a good moment to write a summary text on the subject to serve as guideline for the next generations of students interested in joining the massive star crew. If you are one of them, please, use this chapter as a first working notebook. Do not stop here. Dig also, for further details, into the literature I quote along the text. And, once there, dig even deeper to find all the original sources explaining in more detail the physical and technical concepts that are presently incorporated into our modern (almost) automatized tools. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.04853v1-abstract-full').style.display = 'none'; document.getElementById('2001.04853v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 January, 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">Accepted for publication in the book "Reviews in Frontiers of Modern Astrophysics: From Space Debris to Cosmology" (eds Kabath, Jones and Skarka; publisher Springer Nature) funded by the European Union Erasmus+ Strategic Partnership grant "Per Aspera Ad Astra Simul" 2017-1-CZ01-KA203-035562</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.04534">arXiv:2001.04534</a> <span> [<a href="https://arxiv.org/pdf/2001.04534">pdf</a>, <a href="https://arxiv.org/format/2001.04534">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"> MOBSTER: Identifying Candidate Magnetic O Stars through Rotational Modulation of TESS Photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Barron%2C+J">James Barron</a>, <a href="/search/?searchtype=author&query=Wade%2C+G+A">Gregg A. Wade</a>, <a href="/search/?searchtype=author&query=Bowman%2C+D+M">Dominic M. Bowman</a>, <a href="/search/?searchtype=author&query=David-Uraz%2C+A">Alexandre David-Uraz</a>, <a href="/search/?searchtype=author&query=Munoz%2C+M+S">Melissa S. Munoz</a>, <a href="/search/?searchtype=author&query=Pablo%2C+H">Herbert Pablo</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">Sergio Sim贸n-D铆az</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="2001.04534v1-abstract-short" style="display: inline;"> Being relatively rare, the properties of magnetic O stars are not fully understood. To date fewer than a dozen of these stars have been confirmed, making any inference of their global properties uncertain due to small number statistics. To better understand these objects it is necessary to increase the known sample. The MOBSTER collaboration aims to do this by identifying candidate magnetic O, B,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.04534v1-abstract-full').style.display = 'inline'; document.getElementById('2001.04534v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.04534v1-abstract-full" style="display: none;"> Being relatively rare, the properties of magnetic O stars are not fully understood. To date fewer than a dozen of these stars have been confirmed, making any inference of their global properties uncertain due to small number statistics. To better understand these objects it is necessary to increase the known sample. The MOBSTER collaboration aims to do this by identifying candidate magnetic O, B, and A stars from the identification of rotational modulation in high-precision photometry from the Transiting Exoplanet Survey Satellite (TESS). Here we discuss the collaboration's efforts to detect rotational modulation in TESS targets to identify candidate magnetic O stars for future spectropolarimetric observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.04534v1-abstract-full').style.display = 'none'; document.getElementById('2001.04534v1-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 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">9 pages, 4 figures, Conference proceedings: "Stellar Magnetic Fields - A workshop in honour of the career and contributions of John Landstreet", London, Canada, July 2019 (to be published in the Proceedings of the Polish Astronomical Society)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.07255">arXiv:1912.07255</a> <span> [<a href="https://arxiv.org/pdf/1912.07255">pdf</a>, <a href="https://arxiv.org/format/1912.07255">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/10.1051/0004-6361/201937318">10.1051/0004-6361/201937318 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A detailed non-LTE analysis of LB-1: Revised parameters and surface abundances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=de+Burgos%2C+A">A. de Burgos</a>, <a href="/search/?searchtype=author&query=Dufton%2C+P+L">P. L. Dufton</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Toledo-Padr%C3%B3n%2C+B">B. Toledo-Padr贸n</a>, <a href="/search/?searchtype=author&query=Smartt%2C+S+J">S. J. Smartt</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="1912.07255v2-abstract-short" style="display: inline;"> LB-1 has recently been proposed to be a binary system at 4 kpc consisting of a B star of 8 Msol and a massive stellar black hole of 70 Msol. This finding challenges our current theories of massive star evolution and formation of BHs at solar metallicity. Our objective is to derive the effective temperature, surface gravity and chemical composition of the B-type component in order to determine it… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.07255v2-abstract-full').style.display = 'inline'; document.getElementById('1912.07255v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.07255v2-abstract-full" style="display: none;"> LB-1 has recently been proposed to be a binary system at 4 kpc consisting of a B star of 8 Msol and a massive stellar black hole of 70 Msol. This finding challenges our current theories of massive star evolution and formation of BHs at solar metallicity. Our objective is to derive the effective temperature, surface gravity and chemical composition of the B-type component in order to determine its nature and evolutionary status and, indirectly, to constrain the mass of the BH. We use the non-LTE stellar atmosphere code FASTWIND to analyse new and archival high resolution data. We determine (Teff, logg) values of (14000$\pm500$ K, 3.50$\pm0.15$ dex) that, combined with the Gaia parallax, implies a spectroscopic mass, from logg, of $3.2^{+2.1}_{-1.9}$ Msol and an evolutionary mass, assuming single star evolution, of $5.2^{+0.3}_{-0.6}$ Msol. We determine an upper limit of 8 km/s for the projected rotational velocity and derive the surface abundances, finding the star to have a silicon abundance below solar, to be significantly enhanced in nitrogen and iron, and depleted in carbon and magnesium. Complementary evidence derived from a photometric extinction analysis and Gaia yields similar results for Teff and logg and a consistent distance around 2~kpc. We propose that the B star is a slightly evolved main sequence star of 3-5 Msol with surface abundances reminiscent of diffusion in late B/A chemically peculiar stars with low rotational velocities. There is also evidence for CN-processed material in its atmosphere. These conclusions rely critically on the distance inferred from the Gaia parallax. The goodness of fit of the Gaia astrometry also favours a high-inclination orbit. If the orbit is edge-on and the B star has a mass of 3-5 Msol, the mass of the dark companion would be 4-5 Msol, which would be easier to explain with our current stellar evolutionary models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.07255v2-abstract-full').style.display = 'none'; document.getElementById('1912.07255v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publiction in A&A on 2020/01/08</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.04687">arXiv:1908.04687</a> <span> [<a href="https://arxiv.org/pdf/1908.04687">pdf</a>, <a href="https://arxiv.org/format/1908.04687">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Massive stars in extremely metal-poor galaxies: A window into the past </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Garcia%2C+M">M. Garcia</a>, <a href="/search/?searchtype=author&query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/?searchtype=author&query=Bestenlehner%2C+J+M">J. M. Bestenlehner</a>, <a href="/search/?searchtype=author&query=Bouret%2C+J+C">J. C. Bouret</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=Cervi%C3%B1o%2C+M">M. Cervi帽o</a>, <a href="/search/?searchtype=author&query=Fullerton%2C+A+W">A. W. Fullerton</a>, <a href="/search/?searchtype=author&query=Gieles%2C+M">M. Gieles</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=de+Koter%2C+A">A. de Koter</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=van+Loon%2C+J+T">J. Th. van Loon</a>, <a href="/search/?searchtype=author&query=Martins%2C+F">F. Martins</a>, <a href="/search/?searchtype=author&query=de+Mink%2C+S+E">S. E. de Mink</a>, <a href="/search/?searchtype=author&query=Najarro%2C+F">F. Najarro</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Sz%C3%A9csi%2C+D">D. Sz茅csi</a>, <a href="/search/?searchtype=author&query=Tramper%2C+F">F. Tramper</a>, <a href="/search/?searchtype=author&query=Vink%2C+J">J. Vink</a>, <a href="/search/?searchtype=author&query=Wofford%2C+A">A. Wofford</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="1908.04687v1-abstract-short" style="display: inline;"> Cosmic History has witnessed the lives and deaths of multiple generations of massive stars, all of them invigorating their host galaxies with ionizing photons, kinetic energy, fresh material and stellar-mass black holes. Ubiquitous engines as they are, Astrophysics needs a good understanding of their formation, evolution, properties and yields throughout the history of the Universe, and with decre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.04687v1-abstract-full').style.display = 'inline'; document.getElementById('1908.04687v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.04687v1-abstract-full" style="display: none;"> Cosmic History has witnessed the lives and deaths of multiple generations of massive stars, all of them invigorating their host galaxies with ionizing photons, kinetic energy, fresh material and stellar-mass black holes. Ubiquitous engines as they are, Astrophysics needs a good understanding of their formation, evolution, properties and yields throughout the history of the Universe, and with decreasing metal content mimicking the environment at the earliest epochs. Ultimately, a physical model that could be extrapolated to zero metallicity would enable tackling long-standing questions such as "What did the First, very massive stars of the Universe look like?" or "What was their role in the re-ionization of the Universe?". Yet, most our knowledge of metal-poor massive stars is drawn from one single point in metallicity. Massive stars in the Small Magellanic Cloud (SMC, $\sim 1/5 Z_{\odot}$) currently serve as templates for low-metallicity objects in the early Universe, even though significant differences with respect to massive stars with poorer metal content have been reported. This White Paper summarizes the current knowledge on extremely (sub-SMC) metal poor massive stars, highlighting the most outstanding open questions and the need to supersede the SMC as standard. A new paradigm can be built from nearby extremely metal-poor galaxies that make a new metallicity ladder, but massive stars in these galaxies are out of reach to current observational facilities. Such task would require an L-size mission, consisting of a 10m-class space telescope operating in the optical and the ultraviolet ranges. Alternatively, we propose that ESA unites efforts with NASA to make the LUVOIR mission concept a reality, thus continuing the successful partnership that made Hubble Space Telescope one of the greatest observatories of all time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.04687v1-abstract-full').style.display = 'none'; document.getElementById('1908.04687v1-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">A white paper submitted for the Voyage 2050 long-term plan in the ESA Science Programme. 21 pages, 1 table, 6 figures. arXiv admin note: substantial text overlap with arXiv:1903.05235</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.02120">arXiv:1905.02120</a> <span> [<a href="https://arxiv.org/pdf/1905.02120">pdf</a>, <a href="https://arxiv.org/format/1905.02120">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/10.1038/s41550-019-0768-1">10.1038/s41550-019-0768-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-frequency gravity waves in blue supergiants revealed by high-precision space photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bowman%2C+D+M">Dominic M. Bowman</a>, <a href="/search/?searchtype=author&query=Burssens%2C+S">Siemen Burssens</a>, <a href="/search/?searchtype=author&query=Pedersen%2C+M+G">May G. Pedersen</a>, <a href="/search/?searchtype=author&query=Johnston%2C+C">Cole Johnston</a>, <a href="/search/?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/?searchtype=author&query=Buysschaert%2C+B">Bram Buysschaert</a>, <a href="/search/?searchtype=author&query=Michielsen%2C+M">Mathias Michielsen</a>, <a href="/search/?searchtype=author&query=Tkachenko%2C+A">Andrew Tkachenko</a>, <a href="/search/?searchtype=author&query=Rogers%2C+T+M">Tamara M. Rogers</a>, <a href="/search/?searchtype=author&query=Edelmann%2C+P+V+F">Philipp V. F. Edelmann</a>, <a href="/search/?searchtype=author&query=Ratnasingam%2C+R+P">Rathish P. Ratnasingam</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">Sergio Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">Norberto Castro</a>, <a href="/search/?searchtype=author&query=Moravveji%2C+E">Ehsan Moravveji</a>, <a href="/search/?searchtype=author&query=Pope%2C+B+J+S">Benjamin J. S. Pope</a>, <a href="/search/?searchtype=author&query=White%2C+T+R">Timothy R. White</a>, <a href="/search/?searchtype=author&query=De+Cat%2C+P">Peter De Cat</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="1905.02120v1-abstract-short" style="display: inline;"> Almost all massive stars explode as supernovae and form a black hole or neutron star. The remnant mass and the impact of the chemical yield on subsequent star formation and galactic evolution strongly depend on the internal physics of the progenitor star, which is currently not well understood. The theoretical uncertainties of stellar interiors accumulate with stellar age, which is particularly pe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.02120v1-abstract-full').style.display = 'inline'; document.getElementById('1905.02120v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.02120v1-abstract-full" style="display: none;"> Almost all massive stars explode as supernovae and form a black hole or neutron star. The remnant mass and the impact of the chemical yield on subsequent star formation and galactic evolution strongly depend on the internal physics of the progenitor star, which is currently not well understood. The theoretical uncertainties of stellar interiors accumulate with stellar age, which is particularly pertinent for the blue supergiant phase. Stellar oscillations represent a unique method of probing stellar interiors, yet inference for blue supergiants is hampered by a dearth of observed pulsation modes. Here we report the detection of diverse variability in blue supergiants using the K2 and TESS space missions. The discovery of pulsation modes or an entire spectrum of low-frequency gravity waves in these stars allow us to map the evolution of hot massive stars towards the ends of their lives. Future asteroseismic modelling will provide constraints on ages, core masses, interior mixing, rotation and angular momentum transport. The discovery of variability in blue supergiants is a step towards a data-driven empirical calibration of theoretical evolution models for the most massive stars in the Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.02120v1-abstract-full').style.display = 'none'; document.getElementById('1905.02120v1-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 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">Publication date: 6 May 2019 at 16:00h (GMT)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Astronomy, 2019 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.11385">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/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Lorenzo%2C+J">J. Lorenzo</a>, <a href="/search/?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/?searchtype=author&query=Gamen%2C+R+C">R. C. Gamen</a>, <a href="/search/?searchtype=author&query=Fari%C3%B1a%2C+C">C. Fari帽a</a>, <a href="/search/?searchtype=author&query=Salas%2C+J">J. Salas</a>, <a href="/search/?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/?searchtype=author&query=Morrell%2C+N+I">N. I. Morrell</a>, <a href="/search/?searchtype=author&query=Pellerin%2C+A">A. Pellerin</a>, <a href="/search/?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Arias%2C+J+I">J. I. Arias</a>, <a href="/search/?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/1902.08312">arXiv:1902.08312</a> <span> [<a href="https://arxiv.org/pdf/1902.08312">pdf</a>, <a href="https://arxiv.org/ps/1902.08312">ps</a>, <a href="https://arxiv.org/format/1902.08312">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/10.3847/2041-8213/ab095f">10.3847/2041-8213/ab095f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroseismology of massive stars with the TESS mission: the runaway Beta Cep pulsator PHL 346 = HN Aqr </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Handler%2C+G">Gerald Handler</a>, <a href="/search/?searchtype=author&query=Pigulski%2C+A">Andrzej Pigulski</a>, <a href="/search/?searchtype=author&query=Daszy%C5%84ska-Daszkiewicz%2C+J">Jadwiga Daszy艅ska-Daszkiewicz</a>, <a href="/search/?searchtype=author&query=Irrgang%2C+A">Andreas Irrgang</a>, <a href="/search/?searchtype=author&query=Kilkenny%2C+D">David Kilkenny</a>, <a href="/search/?searchtype=author&query=Guo%2C+Z">Zhao Guo</a>, <a href="/search/?searchtype=author&query=Przybilla%2C+N">Norbert Przybilla</a>, <a href="/search/?searchtype=author&query=Ali%C3%A7avu%C5%9F%2C+F+K">Filiz Kahraman Ali莽avu艧</a>, <a href="/search/?searchtype=author&query=Kallinger%2C+T">Thomas Kallinger</a>, <a href="/search/?searchtype=author&query=Pascual-Granado%2C+J">Javier Pascual-Granado</a>, <a href="/search/?searchtype=author&query=Niemczura%2C+E">Ewa Niemczura</a>, <a href="/search/?searchtype=author&query=R%C3%B3%C5%BCa%C5%84ski%2C+T">Tomasz R贸偶a艅ski</a>, <a href="/search/?searchtype=author&query=Chowdhury%2C+S">Sowgata Chowdhury</a>, <a href="/search/?searchtype=author&query=Buzasi%2C+D+L">Derek L. Buzasi</a>, <a href="/search/?searchtype=author&query=Mirouh%2C+G+M">Giovanni M. Mirouh</a>, <a href="/search/?searchtype=author&query=Bowman%2C+D+M">Dominic M. Bowman</a>, <a href="/search/?searchtype=author&query=Johnston%2C+C">Cole Johnston</a>, <a href="/search/?searchtype=author&query=Pedersen%2C+M+G">May G. Pedersen</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-Diaz%2C+S">Sergio Sim贸n-Diaz</a>, <a href="/search/?searchtype=author&query=Moravveji%2C+E">Ehsan Moravveji</a>, <a href="/search/?searchtype=author&query=Gazeas%2C+K">Kosmas Gazeas</a>, <a href="/search/?searchtype=author&query=De+Cat%2C+P">Peter De Cat</a>, <a href="/search/?searchtype=author&query=Vanderspek%2C+R+K">Roland K. Vanderspek</a>, <a href="/search/?searchtype=author&query=Ricker%2C+G+R">George R. Ricker</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="1902.08312v1-abstract-short" style="display: inline;"> We report an analysis of the first known Beta Cep pulsator observed by the TESS mission, the runaway star PHL 346 = HN Aqr. The star, previously known as a singly-periodic pulsator, has at least 34 oscillation modes excited, 12 of those in the g-mode domain and 22 p modes. Analysis of archival data implies that the amplitude and frequency of the dominant mode and the stellar radial velocity were v… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.08312v1-abstract-full').style.display = 'inline'; document.getElementById('1902.08312v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.08312v1-abstract-full" style="display: none;"> We report an analysis of the first known Beta Cep pulsator observed by the TESS mission, the runaway star PHL 346 = HN Aqr. The star, previously known as a singly-periodic pulsator, has at least 34 oscillation modes excited, 12 of those in the g-mode domain and 22 p modes. Analysis of archival data implies that the amplitude and frequency of the dominant mode and the stellar radial velocity were variable over time. A binary nature would be inconsistent with the inferred ejection velocity from the Galactic disc of 420 km/s, which is too large to be survivable by a runaway binary system. A kinematic analysis of the star results in an age constraint (23 +- 1 Myr) that can be imposed on asteroseismic modelling and that can be used to remove degeneracies in the modelling process. Our attempts to match the excitation of the observed frequency spectrum resulted in pulsation models that were too young. Hence, asteroseismic studies of runaway pulsators can become vital not only in tracing the evolutionary history of such objects, but to understand the interior structure of massive stars in general. TESS is now opening up these stars for detailed asteroseismic investigation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.08312v1-abstract-full').style.display = 'none'; document.getElementById('1902.08312v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 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">accepted for ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.07576">arXiv:1901.07576</a> <span> [<a href="https://arxiv.org/pdf/1901.07576">pdf</a>, <a href="https://arxiv.org/format/1901.07576">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/10.3847/2041-8213/ab01e1">10.3847/2041-8213/ab01e1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Diverse Variability of O and B Stars Revealed from 2-minute Cadence Light Curves in Sectors 1 and 2 of the TESS Mission: Selection of an Asteroseismic Sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pedersen%2C+M+G">May G. Pedersen</a>, <a href="/search/?searchtype=author&query=Chowdhury%2C+S">Sowgata Chowdhury</a>, <a href="/search/?searchtype=author&query=Johnston%2C+C">Cole Johnston</a>, <a href="/search/?searchtype=author&query=Bowman%2C+D">Dominic Bowman</a>, <a href="/search/?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/?searchtype=author&query=Handler%2C+G">Gerald Handler</a>, <a href="/search/?searchtype=author&query=De+Cat%2C+P">Peter De Cat</a>, <a href="/search/?searchtype=author&query=Neiner%2C+C">Coralie Neiner</a>, <a href="/search/?searchtype=author&query=David-Uraz%2C+A">Alexandre David-Uraz</a>, <a href="/search/?searchtype=author&query=Buzasi%2C+D">Derek Buzasi</a>, <a href="/search/?searchtype=author&query=Tkachenko%2C+A">Andrew Tkachenko</a>, <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S">Sergio Simon-Diaz</a>, <a href="/search/?searchtype=author&query=Moravveji%2C+E">Ehsan Moravveji</a>, <a href="/search/?searchtype=author&query=Sikora%2C+J">James Sikora</a>, <a href="/search/?searchtype=author&query=Mirouh%2C+G+M">Giovanni M. Mirouh</a>, <a href="/search/?searchtype=author&query=Lovekin%2C+C+C">Catherine C. Lovekin</a>, <a href="/search/?searchtype=author&query=Cantiello%2C+M">Matteo Cantiello</a>, <a href="/search/?searchtype=author&query=Daszynska-Daszkiewicz%2C+J">Jadwiga Daszynska-Daszkiewicz</a>, <a href="/search/?searchtype=author&query=Pigulski%2C+A">Andrzej Pigulski</a>, <a href="/search/?searchtype=author&query=Vanderspek%2C+R+K">Roland K. Vanderspek</a>, <a href="/search/?searchtype=author&query=Ricker%2C+G+R">George R. Ricker</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="1901.07576v2-abstract-short" style="display: inline;"> Uncertainties in stellar structure and evolution theory are largest for stars undergoing core convection on the main sequence. A powerful way to calibrate the free parameters used in the theory of stellar interiors is asteroseismology, which provides direct measurements of angular momentum and element transport. We report the detection and classification of new variable O and B stars using high-pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.07576v2-abstract-full').style.display = 'inline'; document.getElementById('1901.07576v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.07576v2-abstract-full" style="display: none;"> Uncertainties in stellar structure and evolution theory are largest for stars undergoing core convection on the main sequence. A powerful way to calibrate the free parameters used in the theory of stellar interiors is asteroseismology, which provides direct measurements of angular momentum and element transport. We report the detection and classification of new variable O and B stars using high-precision short-cadence (2-min) photometric observations assembled by the Transiting Exoplanet Survey Satellite (TESS). In our sample of 154 O and B stars, we detect a high percentage (90%) of variability. Among these we find 23 multiperiodic pulsators, 6 eclipsing binaries, 21 rotational variables, and 25 stars with stochastic low-frequency variability. Several additional variables overlap between these categories. Our study of O and B stars not only demonstrates the high data quality achieved by TESS for optimal studies of the variability of the most massive stars in the Universe, but also represents the first step towards the selection and composition of a large sample of O and B pulsators with high potential for joint asteroseismic and spectroscopic modeling of their interior structure with unprecedented precision. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.07576v2-abstract-full').style.display = 'none'; document.getElementById('1901.07576v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">16 pages, 4 figures, 1 Table, Accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.07560">arXiv:1901.07560</a> <span> [<a href="https://arxiv.org/pdf/1901.07560">pdf</a>, <a href="https://arxiv.org/format/1901.07560">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="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/10.1088/1538-3873/aaff7c">10.1088/1538-3873/aaff7c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Conducting the SONG: The robotic nature and efficiency of a fully automated telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Andersen%2C+M+F">M. Fredslund Andersen</a>, <a href="/search/?searchtype=author&query=Handberg%2C+R">R. Handberg</a>, <a href="/search/?searchtype=author&query=Weiss%2C+E">E. Weiss</a>, <a href="/search/?searchtype=author&query=Frandsen%2C+S">S. Frandsen</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Grundahl%2C+F">F. Grundahl</a>, <a href="/search/?searchtype=author&query=Pall%C3%A9%2C+P">P. Pall茅</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="1901.07560v1-abstract-short" style="display: inline;"> We present a description of "the Conductor", an automated software package which handles all observations at the first Stellar Observations Network Group (SONG) node telescope at the Teide Observatory on the island of Tenerife. The idea was to provide a complete description on the automated procedures for target selection and execution of observations and to demonstrate how the SONG robotic telesc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.07560v1-abstract-full').style.display = 'inline'; document.getElementById('1901.07560v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.07560v1-abstract-full" style="display: none;"> We present a description of "the Conductor", an automated software package which handles all observations at the first Stellar Observations Network Group (SONG) node telescope at the Teide Observatory on the island of Tenerife. The idea was to provide a complete description on the automated procedures for target selection and execution of observations and to demonstrate how the SONG robotic telescope is being operated. The Conductor is a software package developed in Python and running on a server in Aarhus which makes use of a large set of database tables through which it communicates with the SONG nodes. Based on a number of selection criteria the Conductor is able to identify the optimum target to be observed at any given moment taking into account local weather conditions and technical constraints. The Conductor has made it possible for the Hertzsprung SONG telescope to become a highly sophisticated and efficient robotic telescopic facility without human interaction. It can handle everything from Principal Investigators submitting their proposed targets with specific settings to the data being available for download after the observations has been carried out. At present, and thanks to the availability of the Conductor, the first node of the SONG project can be considered a world leading robotic telescope with respect to needed human interactions, efficiency and flexibility in observing strategy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.07560v1-abstract-full').style.display = 'none'; document.getElementById('1901.07560v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 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">11 pages (incl. 4 pages Appendices), 7 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/1812.06837">arXiv:1812.06837</a> <span> [<a href="https://arxiv.org/pdf/1812.06837">pdf</a>, <a href="https://arxiv.org/format/1812.06837">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz850">10.1093/mnras/stz850 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-resolution spectroscopy of Boyajian's star during optical dimming events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+M+J+M">M. J. Mart铆nez Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez-Fern%C3%A1ndez%2C+C">C. Gonz谩lez-Fern谩ndez</a>, <a href="/search/?searchtype=author&query=Ramos%2C+A+A">A. Asensio Ramos</a>, <a href="/search/?searchtype=author&query=Navarro%2C+H+S">H. Socas Navarro</a>, <a href="/search/?searchtype=author&query=Plaza%2C+C+W">C. Westendorp Plaza</a>, <a href="/search/?searchtype=author&query=Boyajian%2C+T+S">T. S. Boyajian</a>, <a href="/search/?searchtype=author&query=Wright%2C+J+T">J. T. Wright</a>, <a href="/search/?searchtype=author&query=Cameron%2C+A+C">A. Collier Cameron</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez%2C+J+G">J. Gonz谩lez Hern谩ndez</a>, <a href="/search/?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/?searchtype=author&query=Kennedy%2C+G+M">G. M. Kennedy</a>, <a href="/search/?searchtype=author&query=Masseron%2C+T">T. Masseron</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Saario%2C+J">J. Saario</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Toledo-Padr%C3%B3n%2C+B">B. Toledo-Padr贸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="1812.06837v1-abstract-short" style="display: inline;"> Boyajian's star is an apparently normal main sequence F-type star with a very unusual light curve. The dipping activity of the star, discovered during the Kepler mission, presents deep, asymmetric, and aperiodic events. Here we present high resolution spectroscopic follow-up during some dimming events recorded post-Kepler observations, from ground-based telescopes. We analise data from the HERMES,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.06837v1-abstract-full').style.display = 'inline'; document.getElementById('1812.06837v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.06837v1-abstract-full" style="display: none;"> Boyajian's star is an apparently normal main sequence F-type star with a very unusual light curve. The dipping activity of the star, discovered during the Kepler mission, presents deep, asymmetric, and aperiodic events. Here we present high resolution spectroscopic follow-up during some dimming events recorded post-Kepler observations, from ground-based telescopes. We analise data from the HERMES, HARPS-N and FIES spectrographs to characterise the stellar atmosphere and to put some constraints on the hypotheses that have appeared in the literature concerning the occulting elements. The star's magnetism, if existing, is not extreme. The spots on the surface, if present, would occupy 0.02% of the area, at most. The chromosphere, irrespective of the epoch of observation, is hotter than the values expected from radiative equilibrium, meaning that the star has some degree of activity. We find no clear evidence of the interstellar medium nor exocoments being responsible for the dimmings of the light curve. However, we detect at 1-2 sigma level, a decrease of the radial velocity of the star during the first dip recorded after the \emph{\emph{Kepler}} observations. We claim the presence of an optically thick object with likely inclined and high impact parameter orbits that produces the observed Rossiter-McLaughlin effect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.06837v1-abstract-full').style.display = 'none'; document.getElementById('1812.06837v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 December, 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">submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.12930">arXiv:1811.12930</a> <span> [<a href="https://arxiv.org/pdf/1811.12930">pdf</a>, <a href="https://arxiv.org/format/1811.12930">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/10.5281/zenodo.1745562">10.5281/zenodo.1745562 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photometric detection of internal gravity waves in early-type stars observed by CoRoT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/?searchtype=author&query=Aerts%2C+C">C. Aerts</a>, <a href="/search/?searchtype=author&query=Johnston%2C+C">C. Johnston</a>, <a href="/search/?searchtype=author&query=Pedersen%2C+M+G">M. G. Pedersen</a>, <a href="/search/?searchtype=author&query=Rogers%2C+T+M">T. M. Rogers</a>, <a href="/search/?searchtype=author&query=Edelmann%2C+P+V+F">P. V. F. Edelmann</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Van+Reeth%2C+T">T. Van Reeth</a>, <a href="/search/?searchtype=author&query=Buysschaert%2C+B">B. Buysschaert</a>, <a href="/search/?searchtype=author&query=Tkachenko%2C+A">A. Tkachenko</a>, <a href="/search/?searchtype=author&query=Triana%2C+S+A">S. A. Triana</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="1811.12930v1-abstract-short" style="display: inline;"> Early-type stars are predicted to excite an entire spectrum of internal gravity waves (IGWs) at the interface of their convective cores and radiative envelopes. Numerical simulations of IGWs predict stochastic low-frequency variability in photometric observations, yet the detection of IGWs in early-type stars has been limited by a dearth of high-quality photometric time series. We present observat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.12930v1-abstract-full').style.display = 'inline'; document.getElementById('1811.12930v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.12930v1-abstract-full" style="display: none;"> Early-type stars are predicted to excite an entire spectrum of internal gravity waves (IGWs) at the interface of their convective cores and radiative envelopes. Numerical simulations of IGWs predict stochastic low-frequency variability in photometric observations, yet the detection of IGWs in early-type stars has been limited by a dearth of high-quality photometric time series. We present observational evidence of stochastic low-frequency variability in the CoRoT photometry of a sample of O, B, A and F stars. The presence of this stochastic low-frequency variability in stars across the upper main-sequence cannot be universally explained as granulation or stellar winds, but its morphology is found to be consistent with predictions from IGW simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.12930v1-abstract-full').style.display = 'none'; document.getElementById('1811.12930v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 November, 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">6 pages, 3 figures, Proceedings of the PHOST "Physics of Oscillating Stars" conference (2-7 Sept. 2018, Banyuls-sur-mer, France), Edited by J. Ballot, S. Vauclair, & G. Vauclair</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.08023">arXiv:1811.08023</a> <span> [<a href="https://arxiv.org/pdf/1811.08023">pdf</a>, <a href="https://arxiv.org/format/1811.08023">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/10.1051/0004-6361/201833662">10.1051/0004-6361/201833662 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the photometric detection of Internal Gravity Waves in upper main-sequence stars I. Methodology and application to CoRoT targets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/?searchtype=author&query=Aerts%2C+C">C. Aerts</a>, <a href="/search/?searchtype=author&query=Johnston%2C+C">C. Johnston</a>, <a href="/search/?searchtype=author&query=Pedersen%2C+M+G">M. G. Pedersen</a>, <a href="/search/?searchtype=author&query=Rogers%2C+T+M">T. M. Rogers</a>, <a href="/search/?searchtype=author&query=Edelmann%2C+P+V+F">P. V. F. Edelmann</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Van+Reeth%2C+T">T. Van Reeth</a>, <a href="/search/?searchtype=author&query=Buysschaert%2C+B">B. Buysschaert</a>, <a href="/search/?searchtype=author&query=Tkachenko%2C+A">A. Tkachenko</a>, <a href="/search/?searchtype=author&query=Triana%2C+S+A">S. A. Triana</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="1811.08023v1-abstract-short" style="display: inline;"> Context. Main sequence stars with a convective core are predicted to stochastically excite Internal Gravity Waves (IGWs), which effectively transport angular momentum throughout the stellar interior and explain the observed near-uniform interior rotation rates of intermediate-mass stars. However, there are few detections of IGWs, and fewer still made using photometry, with more detections needed t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.08023v1-abstract-full').style.display = 'inline'; document.getElementById('1811.08023v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.08023v1-abstract-full" style="display: none;"> Context. Main sequence stars with a convective core are predicted to stochastically excite Internal Gravity Waves (IGWs), which effectively transport angular momentum throughout the stellar interior and explain the observed near-uniform interior rotation rates of intermediate-mass stars. However, there are few detections of IGWs, and fewer still made using photometry, with more detections needed to constrain numerical simulations. Aims. We aim to formalise the detection and characterisation of IGWs in photometric observations of stars born with convective cores (M > 1.5 M$_{\odot}$) and parameterise the low-frequency power excess caused by IGWs. Methods. Using the most recent CoRoT light curves for a sample of O, B, A and F stars, we parameterise the morphology of the flux contribution of IGWs in Fourier space using an MCMC numerical scheme within a Bayesian framework. We compare this to predictions from IGW numerical simulations and investigate how the observed morphology changes as a function of stellar parameters. Results. We demonstrate that a common morphology for the low-frequency power excess is observed in early-type stars observed by CoRoT. Our study shows that a background frequency-dependent source of astrophysical signal is common, which we interpret as IGWs. We provide constraints on the amplitudes of IGWs and the shape of their detected frequency spectrum across a range of mass, which is the first ensemble study of stochastic variability in such a diverse sample of stars. Conclusions. The evidence of a low-frequency power excess across a wide mass range supports the interpretation of IGWs in photometry of O, B, A and F stars. We also discuss the prospects of observing hundreds of massive stars with the Transiting Exoplanet Survey Satellite (TESS) in the near future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.08023v1-abstract-full').style.display = 'none'; document.getElementById('1811.08023v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 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">Accepted for publication in A&A, 41 pages including 11 figures and 32 appendix figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 621, A135 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.10943">arXiv:1810.10943</a> <span> [<a href="https://arxiv.org/pdf/1810.10943">pdf</a>, <a href="https://arxiv.org/format/1810.10943">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"> LiLiMaRlin, a Library of Libraries of Massive-Star High-Resolution Spectra with applications to OWN, MONOS, and CollDIBs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADnez%2C+I+J">I. Jim茅nez Mart铆nez</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Pellerin%2C+A">A. Pellerin</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/?searchtype=author&query=Le%C3%A3o%2C+J+R+S">J. R. Souza Le茫o</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="1810.10943v1-abstract-short" style="display: inline;"> LiLiMaRlin is a library of libraries of massive-star high-resolution optical spectra built by collecting data from [a] our spectroscopic surveys (OWN, IACOB. NoMaDS, and CAF脡-BEANS) and programs and [b] searches in public archives. The current version has 18 077 spectra of 1665 stars obtained with seven different telescopes (HET 9.2 m, NOT 2.56 m, CAHA 2.2 m, MPG/ESO 2.2 m, OHP 1.93 m, Mercator 1.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10943v1-abstract-full').style.display = 'inline'; document.getElementById('1810.10943v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.10943v1-abstract-full" style="display: none;"> LiLiMaRlin is a library of libraries of massive-star high-resolution optical spectra built by collecting data from [a] our spectroscopic surveys (OWN, IACOB. NoMaDS, and CAF脡-BEANS) and programs and [b] searches in public archives. The current version has 18 077 spectra of 1665 stars obtained with seven different telescopes (HET 9.2 m, NOT 2.56 m, CAHA 2.2 m, MPG/ESO 2.2 m, OHP 1.93 m, Mercator 1.2 m, and Stella 1.2 m). All the spectra have been filtered to eliminate misidentifications and bad-quality ones, uniformly reprocessed, and placed on a common format. We present applications of this library of libraries to the analysis of spectroscopic binaries (OWN and MONOS, see poster by E. Trigueros P谩ez at this meeting) and the study of the interstellar medium (CollDIBs). We discuss our plans for the future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10943v1-abstract-full').style.display = 'none'; document.getElementById('1810.10943v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">To appear in Highlights on Spanish Astrophysics X, Proceedings of the XIII Scientific Meeting of the Spanish Astronomical Society held on July 16-20, 2018, in Salamanca, Spain</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.02154">arXiv:1810.02154</a> <span> [<a href="https://arxiv.org/pdf/1810.02154">pdf</a>, <a href="https://arxiv.org/ps/1810.02154">ps</a>, <a href="https://arxiv.org/format/1810.02154">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/10.1051/0004-6361/201833574">10.1051/0004-6361/201833574 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Non-synchronous rotations in massive binary systems. HD93343 revisited </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Putkuri%2C+C">C. Putkuri</a>, <a href="/search/?searchtype=author&query=Gamen%2C+R">R. Gamen</a>, <a href="/search/?searchtype=author&query=Morrell%2C+N+I">N. I. Morrell</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Ferrero%2C+G+A">G. A. Ferrero</a>, <a href="/search/?searchtype=author&query=Arias%2C+J+I">J. I. Arias</a>, <a href="/search/?searchtype=author&query=Solivella%2C+G">G. Solivella</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="1810.02154v1-abstract-short" style="display: inline;"> Context. Most massive stars are in binary or multiple systems. Several massive stars have been detected as doublelined spectroscopic binaries and among these, the OWN Survey has detected a non-negligible number whose components show very different spectral line broadening (i.e., projected rotational velocities). This fact raises a discussion about the contributing processes, such as angular-moment… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.02154v1-abstract-full').style.display = 'inline'; document.getElementById('1810.02154v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.02154v1-abstract-full" style="display: none;"> Context. Most massive stars are in binary or multiple systems. Several massive stars have been detected as doublelined spectroscopic binaries and among these, the OWN Survey has detected a non-negligible number whose components show very different spectral line broadening (i.e., projected rotational velocities). This fact raises a discussion about the contributing processes, such as angular-momentum transfer and tidal forces. Aims. We seek to constrain the physical and evolutionary status of one of such systems, the O+O binary HD 93343. Methods. We analyzed a series of high-resolution multiepoch optical spectra to determine the orbital parameters, projected rotational velocities, and evolutionary status of the system. Results. HD 93343 is a binary system comprised of two O7.5 Vz stars that each have minimum masses of approximately 22 Mo in a wide and eccentric orbit (e = 0.398$\pm$0.004; P=50.432$\pm$0.001 d). Both stars have very similar stellar parameters, and hence ages. As expected from the qualitative appearance of the combined spectrum of the system, however, these stars have very different projected rotational velocities (~65 and ~325 km/s, respectively). Conclusions. The orbits and stellar parameters obtained for both components seem to indicate that their youth and relative separation is enough to discard the effects of mass transfer and tidal friction. Thus, non-synchronization should be intrinsic to their formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.02154v1-abstract-full').style.display = 'none'; document.getElementById('1810.02154v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">9 pages, 7 figures. Accepted to Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 618, A174 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.06644">arXiv:1809.06644</a> <span> [<a href="https://arxiv.org/pdf/1809.06644">pdf</a>, <a href="https://arxiv.org/format/1809.06644">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/10.1051/0004-6361/201833989">10.1051/0004-6361/201833989 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Oxygen and silicon abundances in Cygnus OB2: Chemical homogeneity in a sample of OB slow rotators </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Berlanas%2C+S+R">S. R. Berlanas</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Comer%C3%B3n%2C+F">F. Comer贸n</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Cervi%C3%B1o%2C+M">M. Cervi帽o</a>, <a href="/search/?searchtype=author&query=Pasquali%2C+A">A. Pasquali</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1809.06644v1-abstract-short" style="display: inline;"> Cygnus OB2 is a rich OB association in the Galaxy which has experienced intense star formation in the last 20-25 Myr. Its stellar population shows a correlation between age and Galactic longitude. Exploring the chemical composition of its stellar content we will be able to check the degree of homogeneity of the natal molecular cloud and possible effects of self-enrichment processes. Our aim is to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.06644v1-abstract-full').style.display = 'inline'; document.getElementById('1809.06644v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.06644v1-abstract-full" style="display: none;"> Cygnus OB2 is a rich OB association in the Galaxy which has experienced intense star formation in the last 20-25 Myr. Its stellar population shows a correlation between age and Galactic longitude. Exploring the chemical composition of its stellar content we will be able to check the degree of homogeneity of the natal molecular cloud and possible effects of self-enrichment processes. Our aim is to determine silicon and oxygen abundances for a sample of eight early-type slow rotators in Cygnus OB2 in order to check possible inhomogeneities across the whole association and whether there exists a correlation of chemical composition with Galactic longitude. We have performed a spectroscopic analysis of a sample of late O and early B stars with low rotational velocity, which have been chosen so as to cover the whole association area. We have carried out an analysis based on equivalent widths of metal lines, the wings of the H Balmer lines and FASTWIND stellar atmosphere models to determine their stellar fundamental parameters as well as the silicon and oxygen surface abundances. We derive a rather homogeneous distribution of silicon and oxygen abundances across the region, with average values of 12+log(Si/H)=7.53$\pm$0.08 dex and 12+log(O/H)=8.65$\pm$0.12 dex. We find a homogeneous chemical composition in Cygnus OB2 with no clear evidence for significant chemical self-enrichment, despite indications of strong stellar winds and possible supernovae during the history of the region. Comparison with different scenarios of chemical enrichment by stellar winds and supernovae point to star forming efficiencies not significantly above 10%. The degree of homogeneity that we find is consistent with the observed Milky Way oxygen gradient based on HII regions. We also find that the oxygen scatter within Cygnus OB2 is at least of the same order than among HII regions at similar Galactocentric distance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.06644v1-abstract-full').style.display = 'none'; document.getElementById('1809.06644v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 7 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 620, A56 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.09816">arXiv:1807.09816</a> <span> [<a href="https://arxiv.org/pdf/1807.09816">pdf</a>, <a href="https://arxiv.org/format/1807.09816">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/10.1126/science.aat7032">10.1126/science.aat7032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Response to comment on "An excess of massive stars in the local 30 Doradus starburst" </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schneider%2C+F+R+N">F. R. N. Schneider</a>, <a href="/search/?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/?searchtype=author&query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/?searchtype=author&query=Bestenlehner%2C+J+M">J. M. Bestenlehner</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Gr%C3%A4fener%2C+G">G. Gr盲fener</a>, <a href="/search/?searchtype=author&query=Langer%2C+N">N. Langer</a>, <a href="/search/?searchtype=author&query=Ram%C3%ADrez-Agudelo%2C+O+H">O. H. Ram铆rez-Agudelo</a>, <a href="/search/?searchtype=author&query=Sab%C3%ADn-Sanjuli%C3%A1n%2C+C">C. Sab铆n-Sanjuli谩n</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Tramper%2C+F">F. Tramper</a>, <a href="/search/?searchtype=author&query=Crowther%2C+P+A">P. A. Crowther</a>, <a href="/search/?searchtype=author&query=de+Koter%2C+A">A. de Koter</a>, <a href="/search/?searchtype=author&query=de+Mink%2C+S+E">S. E. de Mink</a>, <a href="/search/?searchtype=author&query=Dufton%2C+P+L">P. L. Dufton</a>, <a href="/search/?searchtype=author&query=Garcia%2C+M">M. Garcia</a>, <a href="/search/?searchtype=author&query=Gieles%2C+M">M. Gieles</a>, <a href="/search/?searchtype=author&query=H%C3%A9nault-Brunet%2C+V">V. H茅nault-Brunet</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Izzard%2C+R+G">R. G. Izzard</a>, <a href="/search/?searchtype=author&query=Kalari%2C+V">V. Kalari</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Markova%2C+N">N. Markova</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="1807.09816v1-abstract-short" style="display: inline;"> Farr and Mandel reanalyse our data, finding initial-mass-function slopes for high mass stars in 30 Doradus that agree with our results. However, their reanalysis appears to underpredict the observed number of massive stars. Their technique results in more precise slopes than in our work, strengthening our conclusion that there is an excess of massive stars above $30\,\mathrm{M}_\odot$ in 30 Doradu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.09816v1-abstract-full').style.display = 'inline'; document.getElementById('1807.09816v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.09816v1-abstract-full" style="display: none;"> Farr and Mandel reanalyse our data, finding initial-mass-function slopes for high mass stars in 30 Doradus that agree with our results. However, their reanalysis appears to underpredict the observed number of massive stars. Their technique results in more precise slopes than in our work, strengthening our conclusion that there is an excess of massive stars above $30\,\mathrm{M}_\odot$ in 30 Doradus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.09816v1-abstract-full').style.display = 'none'; document.getElementById('1807.09816v1-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Authors' version of a response to a technical comment published in Science; 8 pages, 1 figure</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.03821">arXiv:1807.03821</a> <span> [<a href="https://arxiv.org/pdf/1807.03821">pdf</a>, <a href="https://arxiv.org/format/1807.03821">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/10.1051/0004-6361/201833433">10.1051/0004-6361/201833433 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VLT-FLAMES Tarantula Survey. XXIX. Massive star formation in the local 30 Doradus starburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schneider%2C+F+R+N">F. R. N. Schneider</a>, <a href="/search/?searchtype=author&query=Ram%C3%ADrez-Agudelo%2C+O+H">O. H. Ram铆rez-Agudelo</a>, <a href="/search/?searchtype=author&query=Tramper%2C+F">F. Tramper</a>, <a href="/search/?searchtype=author&query=Bestenlehner%2C+J+M">J. M. Bestenlehner</a>, <a href="/search/?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/?searchtype=author&query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/?searchtype=author&query=Sab%C3%ADn-Sanjuli%C3%A1n%2C+C">C. Sab铆n-Sanjuli谩n</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Langer%2C+N">N. Langer</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Gr%C3%A4fener%2C+G">G. Gr盲fener</a>, <a href="/search/?searchtype=author&query=Crowther%2C+P+A">P. A. Crowther</a>, <a href="/search/?searchtype=author&query=de+Mink%2C+S+E">S. E. de Mink</a>, <a href="/search/?searchtype=author&query=de+Koter%2C+A">A. de Koter</a>, <a href="/search/?searchtype=author&query=Gieles%2C+M">M. Gieles</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=Izzard%2C+R+G">R. G. Izzard</a>, <a href="/search/?searchtype=author&query=Kalari%2C+V">V. Kalari</a>, <a href="/search/?searchtype=author&query=Klessen%2C+R+S">R. S. Klessen</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Markova%2C+N">N. Markova</a>, <a href="/search/?searchtype=author&query=van+Loon%2C+J+T">J. Th. van Loon</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="1807.03821v1-abstract-short" style="display: inline;"> The 30 Doradus (30 Dor) nebula in the Large Magellanic Cloud (LMC) is the brightest HII region in the Local Group and a prototype starburst similar to those found in high redshift galaxies. It is thus a stepping stone to understand the complex formation processes of stars in starburst regions across the Universe. Here, we have studied the formation history of massive stars in 30 Dor using masses a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.03821v1-abstract-full').style.display = 'inline'; document.getElementById('1807.03821v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.03821v1-abstract-full" style="display: none;"> The 30 Doradus (30 Dor) nebula in the Large Magellanic Cloud (LMC) is the brightest HII region in the Local Group and a prototype starburst similar to those found in high redshift galaxies. It is thus a stepping stone to understand the complex formation processes of stars in starburst regions across the Universe. Here, we have studied the formation history of massive stars in 30 Dor using masses and ages derived for 452 mainly OB stars from the spectroscopic VLT-FLAMES Tarantula Survey (VFTS). We find that stars of all ages and masses are scattered throughout 30 Dor. This is remarkable because it implies that massive stars either moved large distances or formed independently over the whole field of view in relative isolation. We find that both channels contribute to the 30 Dor massive star population. Massive star formation rapidly accelerated about 8 Myr ago, first forming stars in the field before giving birth to the stellar populations in NGC 2060 and NGC 2070. The R136 star cluster in NGC 2070 formed last and, since then, about 1 Myr ago, star formation seems to be diminished with some continuing in the surroundings of R136. Massive stars within a projected distance of 8 pc of R136 are not coeval but show an age range of up to 6 Myr. Our mass distributions are well populated up to $200\,\mathrm{M}_\odot$. The inferred IMF is shallower than a Salpeter-like IMF and appears to be the same across 30 Dor. By comparing our sample of stars to stellar models in the Hertzsprung-Russell diagram, we find evidence for missing physics in the models above $\log L/\mathrm{L}_\odot=6$ that is likely connected to enhanced wind mass loss for stars approaching the Eddington limit. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.03821v1-abstract-full').style.display = 'none'; document.getElementById('1807.03821v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages (incl. appendix), 15 figures, 2 tables; accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 618, A73 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.08277">arXiv:1805.08277</a> <span> [<a href="https://arxiv.org/pdf/1805.08277">pdf</a>, <a href="https://arxiv.org/format/1805.08277">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/10.1051/0004-6361/201833465">10.1051/0004-6361/201833465 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia DR2 reveals a very massive runaway star ejected from R136 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/?searchtype=author&query=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/?searchtype=author&query=Platais%2C+I">I. Platais</a>, <a href="/search/?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/?searchtype=author&query=de+Mink%2C+S+E">S. E. de Mink</a>, <a href="/search/?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/?searchtype=author&query=Sabbi%2C+E">E. Sabbi</a>, <a href="/search/?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/?searchtype=author&query=Crowther%2C+P+A">P. A. Crowther</a>, <a href="/search/?searchtype=author&query=Langer%2C+N">N. Langer</a>, <a href="/search/?searchtype=author&query=Lerate%2C+M+R">M. Ramos Lerate</a>, <a href="/search/?searchtype=author&query=del+Pino%2C+A">A. del Pino</a>, <a href="/search/?searchtype=author&query=Renzo%2C+M">M. Renzo</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Schneider%2C+F+R+N">F. R. N. Schneider</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="1805.08277v2-abstract-short" style="display: inline;"> A previous spectroscopic study identified the very massive O2 III star VFTS 16 in the Tarantula Nebula as a runaway star based on its peculiar line-of-sight velocity. We use the Gaia DR2 catalog to measure the relative proper motion of VFTS 16 and nearby bright stars to test if this star might have been ejected from the central cluster, R136, via dynamical ejection. We find that the position angle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.08277v2-abstract-full').style.display = 'inline'; document.getElementById('1805.08277v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.08277v2-abstract-full" style="display: none;"> A previous spectroscopic study identified the very massive O2 III star VFTS 16 in the Tarantula Nebula as a runaway star based on its peculiar line-of-sight velocity. We use the Gaia DR2 catalog to measure the relative proper motion of VFTS 16 and nearby bright stars to test if this star might have been ejected from the central cluster, R136, via dynamical ejection. We find that the position angle and magnitude of the relative proper motion (0.338 +/- 0.046 mas/yr, or approximately 80 +\- 11 km/s) of VFTS 16 are consistent with ejection from R136 approximately 1.5 +/- 0.2 Myr ago, very soon after the cluster was formed. There is some tension with the presumed age of VFTS 16 that, from published stellar parameters, cannot be greater than 0.9 +0.3/-0.2 Myr. Older ages for this star would appear to be prohibited due to the absence of He I lines in its optical spectrum, since this sets a firm lower limit on its effective temperature. The dynamical constraints may imply an unusual evolutionary history for this object, perhaps indicating it is a merger product. Gaia DR2 also confirms that another very massive star in the Tarantula Nebula, VFTS 72 (alias BI253; O2 III-V(n)((f*)), is also a runaway on the basis of its proper motion as measured by Gaia. While its tangential proper motion (0.392 +/-0.062 mas/yr or 93 +/-15 km/s) would be consistent with dynamical ejection from R136 approximately 1 Myr ago, its position angle is discrepant with this direction at the 2$蟽$ level. From their Gaia DR2 proper motions we conclude that the two ~100 solar mass O2 stars, VFTS 16 and VFTS72, are fast runaway stars, with space velocities of around 100 km/s relative to R136 and the local massive star population. The dynamics of VFTS16 are consistent with it having been ejected from R136, and this star therefore sets a robust lower limit on the age of the central cluster of ~1.3 Myr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.08277v2-abstract-full').style.display = 'none'; document.getElementById('1805.08277v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">Version 2 is now accepted by A&A with minor updates from V1</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 619, A78 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.06915">arXiv:1804.06915</a> <span> [<a href="https://arxiv.org/pdf/1804.06915">pdf</a>, <a href="https://arxiv.org/format/1804.06915">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/10.1051/0004-6361/201832787">10.1051/0004-6361/201832787 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for Galactic runaway stars using Gaia Data Release 1 and Hipparcos proper motions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</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="1804.06915v2-abstract-short" style="display: inline;"> CONTEXT.The first Gaia Data Release (DR1) significantly improved the previously available proper motions for the majority of the Tycho-2 stars. AIMS. We want to detect runaway stars using Gaia DR1 proper motions and compare our results with previous searches. METHODS. Runaway O stars and BA supergiants are detected using a 2-D proper-motion method. The sample is selected using Simbad, spectra from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.06915v2-abstract-full').style.display = 'inline'; document.getElementById('1804.06915v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.06915v2-abstract-full" style="display: none;"> CONTEXT.The first Gaia Data Release (DR1) significantly improved the previously available proper motions for the majority of the Tycho-2 stars. AIMS. We want to detect runaway stars using Gaia DR1 proper motions and compare our results with previous searches. METHODS. Runaway O stars and BA supergiants are detected using a 2-D proper-motion method. The sample is selected using Simbad, spectra from our GOSSS project, literature spectral types, and photometry processed using CHORIZOS. RESULTS. We detect 76 runaway stars, 17 (possibly 19) of them with no prior identification as such, with an estimated detection rate of approximately one half of the real runaway fraction. An age effect appears to be present, with objects of spectral subtype B1 and later having travelled for longer distances than runaways of earlier subtypes. We also tentatively propose that the fraction of runaways is lower among BA supergiants that among O stars but further studies using future Gaia data releases are needed to confirm this. The frequency of fast rotators is high among runaway O stars, which indicates that a significant fraction of them (and possibly a majority) is produced in supernova explosions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.06915v2-abstract-full').style.display = 'none'; document.getElementById('1804.06915v2-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 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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 616, A149 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.03133">arXiv:1804.03133</a> <span> [<a href="https://arxiv.org/pdf/1804.03133">pdf</a>, <a href="https://arxiv.org/format/1804.03133">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="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/10.1051/0004-6361/201832885">10.1051/0004-6361/201832885 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lucky Spectroscopy, an equivalent technique to Lucky Imaging. Spatially resolved spectroscopy of massive close visual binaries using the William Herschel Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/?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="1804.03133v1-abstract-short" style="display: inline;"> CONTEXT: Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS: We want to obtain spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. METHODS: We obtain a large number of short long-slit spectroscopic exposures of five close binaries under good seeing conditions, select those with the best char… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.03133v1-abstract-full').style.display = 'inline'; document.getElementById('1804.03133v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.03133v1-abstract-full" style="display: none;"> CONTEXT: Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS: We want to obtain spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. METHODS: We obtain a large number of short long-slit spectroscopic exposures of five close binaries under good seeing conditions, select those with the best characteristics, extract the spectra using multiple-profile fitting, and combine the results to derive spatially separated spectra. RESULTS: We demonstrate the usefulness of Lucky Spectroscopy by presenting the spatially resolved spectra of the components of each system, in two cases with separations of only ~0.3". Those are delta Ori Aa+Ab (resolved in the optical for the first time) and sigma Ori AaAb+B (first time ever resolved). We also spatially resolve 15 Mon AaAb+B, zeta Ori AaAb+B (both previously resolved with GOSSS, the Galactic O-Star Spectroscopic Survey), and eta Ori AaAb+B, a system with two spectroscopic B+B binaries and a fifth visual component. The systems have in common that they are composed of an inner pair of slow rotators orbited by one or more fast rotators, a characteristic that could have consequences for the theories of massive star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.03133v1-abstract-full').style.display = 'none'; document.getElementById('1804.03133v1-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 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 7 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 615, A161 (2018) </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=Simon-Diaz%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Simon-Diaz%2C+S&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