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 1–35 of 35 results for author: <span class="mathjax">Williams, R E</span> </h1> </div> <div class="level-right is-hidden-mobile">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> <div class="content"> <form method="GET" action="/search/astro-ph" aria-role="search"> Searching in archive <strong>astro-ph</strong>. <a href="/search/?searchtype=author&query=Williams%2C+R+E">Search in all archives.</a> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Williams, R E"> </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=Williams%2C+R+E&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="Williams, R E"> <ul id="abstracts"><li><input checked id="abstracts-0" name="abstracts" type="radio" value="show"> <label for="abstracts-0">Show abstracts</label></li><li><input id="abstracts-1" name="abstracts" type="radio" value="hide"> <label for="abstracts-1">Hide abstracts</label></li></ul> </div> <div class="box field is-grouped is-grouped-multiline level-item"> <div class="control"> <span class="select is-small"> <select id="size" name="size"><option value="25">25</option><option selected value="50">50</option><option value="100">100</option><option value="200">200</option></select> </span> <label for="size">results per page</label>. </div> <div class="control"> <label for="order">Sort results by</label> <span class="select is-small"> <select id="order" name="order"><option selected value="-announced_date_first">Announcement date (newest first)</option><option value="announced_date_first">Announcement date (oldest first)</option><option value="-submitted_date">Submission date (newest first)</option><option value="submitted_date">Submission date (oldest first)</option><option value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.02090">arXiv:2409.02090</a> <span> [<a href="https://arxiv.org/pdf/2409.02090">pdf</a>, <a href="https://arxiv.org/format/2409.02090">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> <p class="title is-5 mathjax"> The Accelerating Decline of the Mass Transfer Rate in the Recurrent Nova T Pyxidis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Godon%2C+P">P. Godon</a>, <a href="/search/astro-ph?searchtype=author&query=Sion%2C+E+M">E. M. Sion</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Darnley%2C+M+J">M. J. Darnley</a>, <a href="/search/astro-ph?searchtype=author&query=Sokoloski%2C+J+L">J. L. Sokoloski</a>, <a href="/search/astro-ph?searchtype=author&query=lawrence%2C+S+S">S. S. lawrence</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.02090v1-abstract-short" style="display: inline;"> The recurrent nova T Pyxidis has erupted six times since 1890, with its last outburst in 2011, and the relatively short recurrence time between classical nova explosions indicates that T Pyx must have a massive white dwarf accreting at a high rate. It is believed that, since its outburst in 1890, the mass transfer rate in T Pyx was very large due to a feedback loop where the secondary is heated by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02090v1-abstract-full').style.display = 'inline'; document.getElementById('2409.02090v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02090v1-abstract-full" style="display: none;"> The recurrent nova T Pyxidis has erupted six times since 1890, with its last outburst in 2011, and the relatively short recurrence time between classical nova explosions indicates that T Pyx must have a massive white dwarf accreting at a high rate. It is believed that, since its outburst in 1890, the mass transfer rate in T Pyx was very large due to a feedback loop where the secondary is heated by the hot white dwarf. The feedback loop has been slowly shutting off, reducing the mass transfer rate, and thereby explaining the magnitude decline of T Pyx from $\sim13.8$ (before 1890) to 15.7 just before the 2011 eruption. We present an analysis of the latest $Hubble~Space~Telescope$ (HST) far ultraviolet and optical spectra, obtained 12 years after the 2011 outburst, showing that the mass transfer rate has been steadily declining and is now below its pre-outburst level by about 40%: $\dot{M} \sim 1-3\times 10^{-7}M_\odot$/yr for a WD mass of $\sim 1.0-1.4 M_\odot$, an inclination of $50^\circ - 60^\circ$, reddening $E(B-V)=0.30 \pm 0.05$ and a Gaia DR3 distance of $2860^{+816}_{-471}$~pc. This steady decrease in the mass transfer rate in the $\sim$decade after the 2011 ourbutst is in sharp contrast with the more constant pre-outburst UV continuum flux level from archival international ultraviolet explorer (IUE) spectra. The flux (i.e. $\dot{M}$) decline rate is 29 times faster now in the last $\sim$decade than observed since 1890 to $\sim$2010. The feedback loop shut off seems to be accelerating, at least in the decade following its 2011 outburst. In all eventualities, our analysis confirms that T Pyx is going through an unusually peculiar short-lived phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02090v1-abstract-full').style.display = 'none'; document.getElementById('2409.02090v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ - accepted for publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.07097">arXiv:2309.07097</a> <span> [<a href="https://arxiv.org/pdf/2309.07097">pdf</a>, <a href="https://arxiv.org/format/2309.07097">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> <p class="title is-5 mathjax"> Revisiting the classics: On the evolutionary origin of the "Fe II" and "He/N" spectral classes of novae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aydi%2C+E">E. Aydi</a>, <a href="/search/astro-ph?searchtype=author&query=Chomiuk%2C+L">L. Chomiuk</a>, <a href="/search/astro-ph?searchtype=author&query=Strader%2C+J">J. Strader</a>, <a href="/search/astro-ph?searchtype=author&query=Sokolovsky%2C+K+V">K. V. Sokolovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Izzo%2C+L">L. Izzo</a>, <a href="/search/astro-ph?searchtype=author&query=Kyer%2C+R">R. Kyer</a>, <a href="/search/astro-ph?searchtype=author&query=Linford%2C+J+D">J. D. Linford</a>, <a href="/search/astro-ph?searchtype=author&query=Kniazev%2C+A">A. Kniazev</a>, <a href="/search/astro-ph?searchtype=author&query=Metzger%2C+B+D">B. D. Metzger</a>, <a href="/search/astro-ph?searchtype=author&query=Mikolajewska%2C+J">J. Mikolajewska</a>, <a href="/search/astro-ph?searchtype=author&query=Molaro%2C+P">P. Molaro</a>, <a href="/search/astro-ph?searchtype=author&query=Mollina%2C+I">I. Mollina</a>, <a href="/search/astro-ph?searchtype=author&query=Mukai%2C+K">K. Mukai</a>, <a href="/search/astro-ph?searchtype=author&query=Munari%2C+U">U. Munari</a>, <a href="/search/astro-ph?searchtype=author&query=Orio%2C+M">M. Orio</a>, <a href="/search/astro-ph?searchtype=author&query=Panurach%2C+T">T. Panurach</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">B. J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+K+J">K. J. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Sokoloski%2C+J+L">J. L. Sokoloski</a>, <a href="/search/astro-ph?searchtype=author&query=Urquhart%2C+R">R. Urquhart</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F+M">F. M. Walter</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.07097v2-abstract-short" style="display: inline;"> The optical spectra of novae are characterized by emission lines from the hydrogen Balmer series and either Fe II or He/N, leading to their traditional classification into two spectral classes: "Fe II" and "He/N". For decades, the origins of these spectral features were discussed in the literature in the contexts of different bodies of gas or changes in the opacity of the ejecta, particularly asso… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07097v2-abstract-full').style.display = 'inline'; document.getElementById('2309.07097v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.07097v2-abstract-full" style="display: none;"> The optical spectra of novae are characterized by emission lines from the hydrogen Balmer series and either Fe II or He/N, leading to their traditional classification into two spectral classes: "Fe II" and "He/N". For decades, the origins of these spectral features were discussed in the literature in the contexts of different bodies of gas or changes in the opacity of the ejecta, particularly associated with studies by R. E. Williams and S. N. Shore. Here, we revisit these major studies with dedicated, modern data sets, covering the evolution of several novae from early rise to peak all the way to the nebular phase. Our data confirm previous suggestions in the literature that the "Fe II" and "He/N" spectral classes are phases in the spectroscopic evolution of novae driven primarily by changes in the opacity, ionization, and density of the ejecta, and most if not all novae go through at least three spectroscopic phases as their eruptions evolve: an early He/N (phase 1; observed during the early rise to visible peak and characterized by P Cygni lines of He I, N II, and N III), then an Fe II (phase 2; observed near visible peak and characterized by P Cygni lines of Fe II and O I), and then a later He/N (phase 3; observed during the decline and characterized by emission lines of He I. He II, N II, and N III), before entering the nebular phase. This spectral evolution seems to be ubiquitous across novae, regardless of their speed class; however the duration of each of these phase differs based on the speed class of the nova. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07097v2-abstract-full').style.display = 'none'; document.getElementById('2309.07097v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 14 figures, 11 tables, Accepted in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.04306">arXiv:2304.04306</a> <span> [<a href="https://arxiv.org/pdf/2304.04306">pdf</a>, <a href="https://arxiv.org/format/2304.04306">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1914">10.1093/mnras/stad1914 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Catching a nova X-ray/UV flash in the visible? Early spectroscopy of the extremely slow Nova Velorum 2022 (Gaia22alz) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aydi%2C+E">E. Aydi</a>, <a href="/search/astro-ph?searchtype=author&query=Chomiuk%2C+L">L. Chomiuk</a>, <a href="/search/astro-ph?searchtype=author&query=Miko%C5%82ajewska%2C+J">J. Miko艂ajewska</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+J">J. Brink</a>, <a href="/search/astro-ph?searchtype=author&query=Metzger%2C+B+D">B. D. Metzger</a>, <a href="/search/astro-ph?searchtype=author&query=Strader%2C+J">J. Strader</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+E+J">E. J. Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Holoien%2C+T+W+-">T. W. -S. Holoien</a>, <a href="/search/astro-ph?searchtype=author&query=Izzo%2C+L">L. Izzo</a>, <a href="/search/astro-ph?searchtype=author&query=Kawash%2C+A">A. Kawash</a>, <a href="/search/astro-ph?searchtype=author&query=Linford%2C+J+D">J. D. Linford</a>, <a href="/search/astro-ph?searchtype=author&query=Molaro%2C+P">P. Molaro</a>, <a href="/search/astro-ph?searchtype=author&query=Mollina%2C+B">B. Mollina</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Mukai%2C+K">K. Mukai</a>, <a href="/search/astro-ph?searchtype=author&query=Orio%2C+M">M. Orio</a>, <a href="/search/astro-ph?searchtype=author&query=Panurach%2C+T">T. Panurach</a>, <a href="/search/astro-ph?searchtype=author&query=Senchyna%2C+P">P. Senchyna</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">B. J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+K+J">K. J. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Sokoloski%2C+J+L">J. L. Sokoloski</a>, <a href="/search/astro-ph?searchtype=author&query=Sokolovsky%2C+K+V">K. V. Sokolovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Urquhart%2C+R">R. Urquhart</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.04306v1-abstract-short" style="display: inline;"> We present early spectral observations of the very slow Galactic nova Gaia22alz, over its gradual rise to peak brightness that lasted 180 days. During the first 50 days, when the nova was only 3--4 magnitudes above its normal brightness, the spectra showed narrow (FWHM $\approx$ 400 km s$^{-1}$) emission lines of H Balmer, He I, He II, and C IV, but no P Cygni absorption. A few weeks later, the hi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04306v1-abstract-full').style.display = 'inline'; document.getElementById('2304.04306v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.04306v1-abstract-full" style="display: none;"> We present early spectral observations of the very slow Galactic nova Gaia22alz, over its gradual rise to peak brightness that lasted 180 days. During the first 50 days, when the nova was only 3--4 magnitudes above its normal brightness, the spectra showed narrow (FWHM $\approx$ 400 km s$^{-1}$) emission lines of H Balmer, He I, He II, and C IV, but no P Cygni absorption. A few weeks later, the high-excitation He II and C IV lines disappeared, and P Cygni profiles of Balmer, He I, and eventually Fe II lines emerged, yielding a spectrum typical of classical novae before peak. We propose that the early spectra of Gaia22alz are produced in the white dwarf's envelope or accretion disk, reprocessing X-ray and ultraviolet emission from the white dwarf after a dramatic increase in the rate of thermonuclear reactions, during a phase known as the ``early X-ray/UV flash''. If true, this would be one of the rare times that the optical signature of the early X-ray/UV flash has been detected. While this phase might last only a few hours in other novae and thus be easily missed, it was possible to detect in Gaia22alz due to its very slow and gradual rise and thanks to the efficiency of new all-sky surveys in detecting transients on their rise. We also consider alternative scenarios that could explain the early spectral features of Gaia22alz and its unusually slow rise. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04306v1-abstract-full').style.display = 'none'; document.getElementById('2304.04306v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">20 pages, 12 figures, 2 tables. 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/2208.09630">arXiv:2208.09630</a> <span> [<a href="https://arxiv.org/pdf/2208.09630">pdf</a>, <a href="https://arxiv.org/format/2208.09630">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244498">10.1051/0004-6361/202244498 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Persistent nuclear burning in Nova Sgr 2016 N.4 (= V5856 Sgr = ASASSN-16ma) six years past its outburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Munari%2C+U">U. Munari</a>, <a href="/search/astro-ph?searchtype=author&query=Masetti%2C+N">N. Masetti</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F+M">F. M. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Hambsch%2C+F+-">F. -J. Hambsch</a>, <a href="/search/astro-ph?searchtype=author&query=Frigo%2C+A">A. Frigo</a>, <a href="/search/astro-ph?searchtype=author&query=Valisa%2C+P">P. Valisa</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="2208.09630v1-abstract-short" style="display: inline;"> We report on the fast Nova Sgr 2016 N.4 being surprisingly trapped in a long-lasting and bright plateau (Delta I >= 10 mag above quiescence) six years past the nova eruption. Very few other novae experience a similar occurrence. We carried out an intensive observing campaign collecting daily BVRI photometry and monthly high-resolution optical spectroscopy, and observed the nova in ultraviolet and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.09630v1-abstract-full').style.display = 'inline'; document.getElementById('2208.09630v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.09630v1-abstract-full" style="display: none;"> We report on the fast Nova Sgr 2016 N.4 being surprisingly trapped in a long-lasting and bright plateau (Delta I >= 10 mag above quiescence) six years past the nova eruption. Very few other novae experience a similar occurrence. We carried out an intensive observing campaign collecting daily BVRI photometry and monthly high-resolution optical spectroscopy, and observed the nova in ultraviolet and X-rays with Swift satellite at five distinct epochs. The bolometric luminosity radiated during the plateau is ~4200 Lsun (scaled to the distance of the Galactic Bulge), corresponding to stable nuclear burning on a 0.6 Msun white dwarf. A stable wind is blown off at FWZI~1600 km/s, with episodic reinforcement of a faster FWZI~3400 km/s mass loss, probably oriented along the polar directions. The collision of these winds could power the emission detected in X-rays. The burning shell has an outer radius of ~25 Rsun at which the effective temperature is ~7600 K, values similar to those of a F0 II/Ib bright giant. The Delta m < 1 mag variability displayed during the plateau is best described as chaotic, with the irregular appearance of quasi-periodic oscillations with a periodicity of 15-17 days. A limited amount of dust (~3x10^(-11) Msun) continuously condenses at T(dust)~1200 K in the outflowing wind, radiating L(dust)~52 Lsun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.09630v1-abstract-full').style.display = 'none'; document.getElementById('2208.09630v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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 667, A7 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.07857">arXiv:1904.07857</a> <span> [<a href="https://arxiv.org/pdf/1904.07857">pdf</a>, <a href="https://arxiv.org/format/1904.07857">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/ab2c05">10.3847/2041-8213/ab2c05 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of an intermediate-luminosity red transient in M51 and its likely dust-obscured, infrared-variable progenitor </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jencson%2C+J+E">Jacob E. Jencson</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+S+M">Scott M. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+H+E">Howard E. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dyk%2C+S+D">Schuyler D. van Dyk</a>, <a href="/search/astro-ph?searchtype=author&query=Kasliwal%2C+M+M">Mansi M. Kasliwal</a>, <a href="/search/astro-ph?searchtype=author&query=Bally%2C+J">John Bally</a>, <a href="/search/astro-ph?searchtype=author&query=Blagorodnova%2C+N">Nadejda Blagorodnova</a>, <a href="/search/astro-ph?searchtype=author&query=De%2C+K">Kishalay De</a>, <a href="/search/astro-ph?searchtype=author&query=Fremling%2C+C">Christoffer Fremling</a>, <a href="/search/astro-ph?searchtype=author&query=Yao%2C+Y">Yuhan Yao</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A">Andrew Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Barbarino%2C+C">Cristina Barbarino</a>, <a href="/search/astro-ph?searchtype=author&query=Sollerman%2C+J">Jesper Sollerman</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+A+A">Adam A. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Hicks%2C+E+K+S">Erin K. S. Hicks</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Andreoni%2C+I">Igor Andreoni</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E+C">Eric C. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Buchheim%2C+R">Robert Buchheim</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+R">Richard Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Feeney%2C+M">Michael Feeney</a>, <a href="/search/astro-ph?searchtype=author&query=Frederick%2C+S">Sara Frederick</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">Avishay Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrz%2C+R+D">Robert D. Gehrz</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.07857v2-abstract-short" style="display: inline;"> We present the discovery of an optical transient (OT) in Messier 51, designated M51 OT2019-1 (also ZTF19aadyppr, AT 2019abn, ATLAS19bzl), by the Zwicky Transient Facility (ZTF). The OT rose over 15 days to an observed luminosity of $M_r=-13$ ($谓L_谓=9\times10^6~L_{\odot}$), in the luminosity gap between novae and typical supernovae (SNe). Spectra during the outburst show a red continuum, Balmer emi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.07857v2-abstract-full').style.display = 'inline'; document.getElementById('1904.07857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.07857v2-abstract-full" style="display: none;"> We present the discovery of an optical transient (OT) in Messier 51, designated M51 OT2019-1 (also ZTF19aadyppr, AT 2019abn, ATLAS19bzl), by the Zwicky Transient Facility (ZTF). The OT rose over 15 days to an observed luminosity of $M_r=-13$ ($谓L_谓=9\times10^6~L_{\odot}$), in the luminosity gap between novae and typical supernovae (SNe). Spectra during the outburst show a red continuum, Balmer emission with a velocity width of $\approx400$ km s$^{-1}$, Ca II and [Ca II] emission, and absorption features characteristic of an F-type supergiant. The spectra and multiband light curves are similar to the so-called "SN impostors" and intermediate-luminosity red transients (ILRTs). We directly identify the likely progenitor in archival Spitzer Space Telescope imaging with a $4.5~渭$m luminosity of $M_{[4.5]}\approx-12.2$ and a $[3.6]-[4.5]$ color redder than 0.74 mag, similar to those of the prototype ILRTs SN 2008S and NGC 300 OT2008-1. Intensive monitoring of M51 with Spitzer further reveals evidence for variability of the progenitor candidate at [4.5] in the years before the OT. The progenitor is not detected in pre-outburst Hubble Space Telescope optical and near-IR images. The optical colors during outburst combined with spectroscopic temperature constraints imply a higher reddening of $E(B-V)\approx0.7$ mag and higher intrinsic luminosity of $M_r\approx-14.9$ ($谓L_谓=5.3\times10^7~L_{\odot}$) near peak than seen in previous ILRT candidates. Moreover, the extinction estimate is higher on the rise than on the plateau, suggestive of an extended phase of circumstellar dust destruction. These results, enabled by the early discovery of M51 OT2019-1 and extensive pre-outburst archival coverage, offer new clues about the debated origins of ILRTs and may challenge the hypothesis that they arise from the electron-capture induced collapse of extreme asymptotic giant branch stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.07857v2-abstract-full').style.display = 'none'; document.getElementById('1904.07857v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">21 pages, 5 figures, published in ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, 880 (2019) L20 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.00871">arXiv:1901.00871</a> <span> [<a href="https://arxiv.org/pdf/1901.00871">pdf</a>, <a href="https://arxiv.org/format/1901.00871">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab4a01">10.3847/1538-4357/ab4a01 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SPIRITS sample of Luminous Infrared Transients: Uncovering Hidden Supernovae and Dusty Stellar Outbursts in Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jencson%2C+J+E">Jacob E. Jencson</a>, <a href="/search/astro-ph?searchtype=author&query=Kasliwal%2C+M+M">Mansi M. Kasliwal</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+S+M">Scott M. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+H+E">Howard E. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=De%2C+K">Kishalay De</a>, <a href="/search/astro-ph?searchtype=author&query=Johansson%2C+J">Joel Johansson</a>, <a href="/search/astro-ph?searchtype=author&query=Karambelkar%2C+V">Viraj Karambelkar</a>, <a href="/search/astro-ph?searchtype=author&query=Lau%2C+R+M">Ryan M. Lau</a>, <a href="/search/astro-ph?searchtype=author&query=Tinyanont%2C+S">Samaporn Tinyanont</a>, <a href="/search/astro-ph?searchtype=author&query=Ryder%2C+S+D">Stuart D. Ryder</a>, <a href="/search/astro-ph?searchtype=author&query=Cody%2C+A+M">Ann Marie Cody</a>, <a href="/search/astro-ph?searchtype=author&query=Masci%2C+F+J">Frank J. Masci</a>, <a href="/search/astro-ph?searchtype=author&query=Bally%2C+J">John Bally</a>, <a href="/search/astro-ph?searchtype=author&query=Blagorodnova%2C+N">Nadia Blagorodnova</a>, <a href="/search/astro-ph?searchtype=author&query=Castell%C3%B3n%2C+S">Sergio Castell贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Fremling%2C+C">Christoffer Fremling</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrz%2C+R+D">Robert D. Gehrz</a>, <a href="/search/astro-ph?searchtype=author&query=Helou%2C+G">George Helou</a>, <a href="/search/astro-ph?searchtype=author&query=Kilpatrick%2C+C+D">Charles D. Kilpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Milne%2C+P+A">Peter A. Milne</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N">Nidia Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Perley%2C+D+A">Daniel A. Perley</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+M">M. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+N">Nathan Smith</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dyk%2C+S+D">Schuyler D. van Dyk</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="1901.00871v2-abstract-short" style="display: inline;"> We present a systematic study of the most luminous ($M_{\mathrm{IR}}$ [Vega magnitudes] brighter than $-14$) infrared (IR) transients discovered by the SPitzer InfraRed Intensive Transients Survey (SPIRITS) between 2014 and 2018 in nearby galaxies ($D < 35$ Mpc). The sample consists of nine events that span peak IR luminosities of $M_{[4.5],\mathrm{peak}}$ between $-14$ and $-18.2$, show IR colors… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.00871v2-abstract-full').style.display = 'inline'; document.getElementById('1901.00871v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.00871v2-abstract-full" style="display: none;"> We present a systematic study of the most luminous ($M_{\mathrm{IR}}$ [Vega magnitudes] brighter than $-14$) infrared (IR) transients discovered by the SPitzer InfraRed Intensive Transients Survey (SPIRITS) between 2014 and 2018 in nearby galaxies ($D < 35$ Mpc). The sample consists of nine events that span peak IR luminosities of $M_{[4.5],\mathrm{peak}}$ between $-14$ and $-18.2$, show IR colors between $0.2 < ([3.6]{-}[4.5]) < 3.0$, and fade on timescales between $55$ days $< t_{\mathrm{fade}} < 480$ days. The two reddest events ($A_V > 12$) show multiple, luminous IR outbursts over several years and have directly detected, massive progenitors in archival imaging. With analyses of extensive, multiwavelength follow-up, we suggest the following possible classifications: five obscured core-collapse supernovae (CCSNe), two erupting massive stars, one luminous red nova, and one intermediate-luminosity red transient. We define a control sample of all optically discovered transients recovered in SPIRITS galaxies and satisfying the same selection criteria. The control sample consists of eight CCSNe and one Type Iax SN. We find that 7 of the 13 CCSNe in the SPIRITS sample have lower bounds on their extinction of $2 < A_V < 8$. We estimate a nominal fraction of CCSNe in nearby galaxies that are missed by optical surveys as high as $38.5^{+26.0}_{-21.9}$% (90% confidence). This study suggests that a significant fraction of CCSNe may be heavily obscured by dust and therefore undercounted in the census of nearby CCSNe from optical searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.00871v2-abstract-full').style.display = 'none'; document.getElementById('1901.00871v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">47 pages, 16 figures, published in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal 886 (2019) 40 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.09993">arXiv:1812.09993</a> <span> [<a href="https://arxiv.org/pdf/1812.09993">pdf</a>, <a href="https://arxiv.org/ps/1812.09993">ps</a>, <a href="https://arxiv.org/format/1812.09993">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/aafb0b">10.3847/1538-4357/aafb0b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST FUV spectroscopy of the short orbital period recurrent nova CI Aql: Implications for white dwarf mass evolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sion%2C+E+M">Edward M. Sion</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson%2C+R+E">R. E. Wilson</a>, <a href="/search/astro-ph?searchtype=author&query=Godon%2C+P">Patrick Godon</a>, <a href="/search/astro-ph?searchtype=author&query=Starrfield%2C+S">Sumner Starrfield</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Darnley%2C+M+J">Matt J. Darnley</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="1812.09993v1-abstract-short" style="display: inline;"> An HST COS Far UV spectrum (1170 A to 1800 A) was obtained for the short orbital period recurrent novae (T Pyxidis subclass), CI Aquilae. CI Aql is the only classical CV known to have two eclipses of sensible depth per orbit cycle and also have pre- and post-outburst light curves that are steady enough to allow estimates of mass and orbital period changes. Our FUV spectral analysis with model accr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.09993v1-abstract-full').style.display = 'inline'; document.getElementById('1812.09993v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.09993v1-abstract-full" style="display: none;"> An HST COS Far UV spectrum (1170 A to 1800 A) was obtained for the short orbital period recurrent novae (T Pyxidis subclass), CI Aquilae. CI Aql is the only classical CV known to have two eclipses of sensible depth per orbit cycle and also have pre- and post-outburst light curves that are steady enough to allow estimates of mass and orbital period changes. Our FUV spectral analysis with model accretion disks and NLTE high gravity photospheres, together with the Gaia parallax, reveal CI Aql's FUV light is dominated by an optically thick accretion disk with an accretion rate of the order of $4\times 10^{-8}$ $M_{\odot}/yr$. Its database of light curves, radial velocity curves, and eclipse timings is among the best for any CV. Its orbit period ($P$), $dP/dt$, and reference time are re-derived via simultaneous analysis of the three data types, giving a dimensionless post-outburst $dP/dt$ of $-2.49\pm 0.95\times 10^{-10}$. Lack of information on loss of orbital to rotational angular momentum leads to some uncertainty in the translation of $dP/dt$ to white dwarf mass change rate, $dM_1/dt$, but within the modest range of $+4.8\times 10^{-8}$ to $+7.8\times 10^{-8}$ $M_{\odot} /yr$. The estimated white dwarf mass change through outburst for CI Aql, based on simple differencing of its pre- and post outburst orbit period, is unchanged from the previously published $+5.3 \times 10^{-6} M_{\odot}$. At the WD's estimated mass increase rate, it will terminate as a Type Ia supernova within 10 million years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.09993v1-abstract-full').style.display = 'none'; document.getElementById('1812.09993v1-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 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">ApJ, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.08249">arXiv:1806.08249</a> <span> [<a href="https://arxiv.org/pdf/1806.08249">pdf</a>, <a href="https://arxiv.org/format/1806.08249">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aacf06">10.3847/1538-4357/aacf06 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> What we learn from the X-ray grating spectra of Nova SMC 2016 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Orio%2C+M">M. Orio</a>, <a href="/search/astro-ph?searchtype=author&query=Ness%2C+J+-">J. -U. Ness</a>, <a href="/search/astro-ph?searchtype=author&query=Dobrotka%2C+A">A. Dobrotka</a>, <a href="/search/astro-ph?searchtype=author&query=Gatuzz%2C+E">E. Gatuzz</a>, <a href="/search/astro-ph?searchtype=author&query=Ospina%2C+N">N. Ospina</a>, <a href="/search/astro-ph?searchtype=author&query=Aydi%2C+E">E. Aydi</a>, <a href="/search/astro-ph?searchtype=author&query=Behar%2C+E">E. Behar</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Valle%2C+M">M. Della Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">M. Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=Henze%2C+M">M. Henze</a>, <a href="/search/astro-ph?searchtype=author&query=Osborne%2C+J+P">J. P. Osborne</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+K+L">K. L. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Rauch%2C+T">T. Rauch</a>, <a href="/search/astro-ph?searchtype=author&query=Sala%2C+G">G. Sala</a>, <a href="/search/astro-ph?searchtype=author&query=Starrfield%2C+S">S. Starrfield</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Woodward%2C+C+E">C. E. Woodward</a>, <a href="/search/astro-ph?searchtype=author&query=Zemko%2C+P">P. Zemko</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1806.08249v1-abstract-short" style="display: inline;"> Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between day 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera and the Low Energy Transmission Grating (LETG) on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 Decembe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.08249v1-abstract-full').style.display = 'inline'; document.getElementById('1806.08249v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.08249v1-abstract-full" style="display: none;"> Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between day 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera and the Low Energy Transmission Grating (LETG) on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon and sulfur on day 39, and oxygen, nitrogen and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blue-shifted, by about 1800 km/s on day 39 and up to 2100 km/s in the following observations. Spectral lines attributed to low ionization potential transitions in the interstellar medium are also observed. Assuming the distance of the Small Magellanic Cloud, the bolometric luminosity exceeded Eddington level for at least three months. A preliminary analysis with atmospheric models indicates effective temperature around 700,000 K on day 39, peaking at the later dates in the 850,000-900,000 K range, as expected for a 1.25 m(sol) WD. We suggest a possible classification as an oxygen-neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show large, aperiodic ux variability, not associated with spectral variability. We detected red noise, but did not find periodic or quasi-periodic modulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.08249v1-abstract-full').style.display = 'none'; document.getElementById('1806.08249v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal, pending final editorial review after "minor changes"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.03716">arXiv:1710.03716</a> <span> [<a href="https://arxiv.org/pdf/1710.03716">pdf</a>, <a href="https://arxiv.org/format/1710.03716">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/stx2678">10.1093/mnras/stx2678 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength observations of nova SMCN 2016-10a --- one of the brightest novae ever observed </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aydi%2C+E">E. Aydi</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+K+L">K. L. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Kuin%2C+N+P+M">N. P. M. Kuin</a>, <a href="/search/astro-ph?searchtype=author&query=Darnley%2C+M+J">M. J. Darnley</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F+M">F. M. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D">D. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Mohamed%2C+S">S. Mohamed</a>, <a href="/search/astro-ph?searchtype=author&query=Whitelock%2C+P">P. Whitelock</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P">P. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+S+C">S. C. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Orio%2C+M">M. Orio</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Beardmore%2C+A+P">A. P. Beardmore</a>, <a href="/search/astro-ph?searchtype=author&query=Osborne%2C+J+P">J. P. Osborne</a>, <a href="/search/astro-ph?searchtype=author&query=Kniazev%2C+A">A. Kniazev</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+V+A+R+M">V. A. R. M. Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Strader%2C+J">J. Strader</a>, <a href="/search/astro-ph?searchtype=author&query=Chomiuk%2C+L">L. Chomiuk</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1710.03716v1-abstract-short" style="display: inline;"> We report on multiwavelength observations of nova SMCN 2016-10a. The present observational set is one of the most comprehensive for any nova in the Small Magellanic Cloud, including: low, medium, and high resolution optical spectroscopy and spectropolarimetry from SALT, FLOYDS, and SOAR; long-term OGLE $V$- and $I$- bands photometry dating back to six years before eruption; SMARTS optical and near… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.03716v1-abstract-full').style.display = 'inline'; document.getElementById('1710.03716v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.03716v1-abstract-full" style="display: none;"> We report on multiwavelength observations of nova SMCN 2016-10a. The present observational set is one of the most comprehensive for any nova in the Small Magellanic Cloud, including: low, medium, and high resolution optical spectroscopy and spectropolarimetry from SALT, FLOYDS, and SOAR; long-term OGLE $V$- and $I$- bands photometry dating back to six years before eruption; SMARTS optical and near-IR photometry from $\sim$ 11 days until over 280 days post-eruption; $Swift$ satellite X-ray and ultraviolet observations from $\sim$ 6 days until 319 days post-eruption. The progenitor system contains a bright disk and a main sequence or a sub-giant secondary. The nova is very fast with $t_2 \simeq$ 4.0 $\pm$ 1.0 d and $t_3 \simeq$ 7.8 $\pm$ 2.0 d in the $V$-band. If the nova is in the SMC, at a distance of $\sim$ 61 $\pm$ 10 kpc, we derive $M_{V,\mathrm{max}} \simeq - 10.5$ $\pm$ 0.5, making it the brightest nova ever discovered in the SMC and one of the brightest on record. At day 5 post-eruption the spectral lines show a He/N spectroscopic class and a FWHM of $\sim$ 3500 kms$^{-1}$ indicating moderately high ejection velocities. The nova entered the nebular phase $\sim$ 20 days post-eruption, predicting the imminent super-soft source turn-on in the X-rays, which started $\sim$ 28 days post-eruption. The super-soft source properties indicate a white dwarf mass between 1.2 M$_{\odot}$ and 1.3 M$_{\odot}$ in good agreement with the optical conclusions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.03716v1-abstract-full').style.display = 'none'; document.getElementById('1710.03716v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS on 2017 October 10 (31 pages, 26 figures, 11 tables)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.02755">arXiv:1606.02755</a> <span> [<a href="https://arxiv.org/pdf/1606.02755">pdf</a>, <a href="https://arxiv.org/format/1606.02755">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/stw1396">10.1093/mnras/stw1396 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> V5852 Sgr: An Unusual Nova Possibly Associated with the Sagittarius Stream </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aydi%2C+E">E. Aydi</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Whitelock%2C+P+A">P. A. Whitelock</a>, <a href="/search/astro-ph?searchtype=author&query=Mohamed%2C+S">S. Mohamed</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+%C5%81">艁. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Vaisanen%2C+P">P. Vaisanen</a>, <a href="/search/astro-ph?searchtype=author&query=Nagayama%2C+T">T. Nagayama</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+A">A. Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Onozato%2C+H">H. Onozato</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Nishiyama%2C+S">S. Nishiyama</a>, <a href="/search/astro-ph?searchtype=author&query=Yamagishi%2C+M">M. Yamagishi</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+T">T. Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Iwamatsu%2C+A">A. Iwamatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamata%2C+I">I. Kawamata</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="1606.02755v1-abstract-short" style="display: inline;"> We report spectroscopic and photometric follow-up of the peculiar nova V5852~Sgr (discovered as OGLE-2015-NOVA-01), which exhibits a combination of features from different nova classes. The photometry shows a flat-topped light curve with quasi-periodic oscillations, then a smooth decline followed by two fainter recoveries in brightness. Spectroscopy with the Southern African Large Telescope shows… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.02755v1-abstract-full').style.display = 'inline'; document.getElementById('1606.02755v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.02755v1-abstract-full" style="display: none;"> We report spectroscopic and photometric follow-up of the peculiar nova V5852~Sgr (discovered as OGLE-2015-NOVA-01), which exhibits a combination of features from different nova classes. The photometry shows a flat-topped light curve with quasi-periodic oscillations, then a smooth decline followed by two fainter recoveries in brightness. Spectroscopy with the Southern African Large Telescope shows first a classical nova with an Fe II or Fe IIb spectral type. In the later spectrum, broad emissions from helium, nitrogen and oxygen are prominent and the iron has faded which could be an indication to the start of the nebular phase. The line widths suggest ejection velocities around $1000\,{\rm km\,s^{-1}}$. The nova is in the direction of the Galactic bulge and is heavily reddened by an uncertain amount. The $V$ magnitude 16 days after maximum enables a distance to be estimated and this suggests that the nova may be in the extreme trailing stream of the Sagittarius dwarf spheroidal galaxy. If so it is the first nova to be detected from that, or from any dwarf spheroidal galaxy. Given the uncertainty of the method and the unusual light curve we cannot rule out the possibility that it is in the bulge or even the Galactic disk behind the bulge. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.02755v1-abstract-full').style.display = 'none'; document.getElementById('1606.02755v1-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS on June 8th, 2016 (11 pages, 8 figures, 5 tables)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.01777">arXiv:1606.01777</a> <span> [<a href="https://arxiv.org/pdf/1606.01777">pdf</a>, <a href="https://arxiv.org/format/1606.01777">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/10.1051/0004-6361/201527856">10.1051/0004-6361/201527856 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The panchromatic spectroscopic evolution of the classical CO nova V339 Del (Nova Del 2013) until X-ray turnoff </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shore%2C+S+N">S. N. Shore</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+E">E. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Schwarz%2C+G+J">G. J. Schwarz</a>, <a href="/search/astro-ph?searchtype=author&query=Teyssier%2C+F+M">F. M. Teyssier</a>, <a href="/search/astro-ph?searchtype=author&query=Buil%2C+C">C. Buil</a>, <a href="/search/astro-ph?searchtype=author&query=Aquino%2C+I+D+G">I. De Gennaro Aquino</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+K+L">K. L. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Osborne%2C+J+P">J. P. Osborne</a>, <a href="/search/astro-ph?searchtype=author&query=Scaringi%2C+S">S. Scaringi</a>, <a href="/search/astro-ph?searchtype=author&query=Starrfield%2C+S">S. Starrfield</a>, <a href="/search/astro-ph?searchtype=author&query=van+Winckel%2C+H">H. van Winckel</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Woodward%2C+C+E">C. E. Woodward</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="1606.01777v1-abstract-short" style="display: inline;"> Classical novae are the product of thermonuclear runaway-initiated explosions occurring on accreting white dwarfs. V339 Del (Nova Delphinus 2013) was one of the brightest classical novae of the last hundred years. Spectroscopy and photometry are available from $纬$-rays through infrared at stages that have frequently not been well observed. The complete data set is intended to provide a benchmark f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.01777v1-abstract-full').style.display = 'inline'; document.getElementById('1606.01777v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.01777v1-abstract-full" style="display: none;"> Classical novae are the product of thermonuclear runaway-initiated explosions occurring on accreting white dwarfs. V339 Del (Nova Delphinus 2013) was one of the brightest classical novae of the last hundred years. Spectroscopy and photometry are available from $纬$-rays through infrared at stages that have frequently not been well observed. The complete data set is intended to provide a benchmark for comparison with modeling and for understanding more sparsely monitored historical classical and recurrent novae. This paper is the first in the series of reports on the development of the nova. We report here on the early stages of the outburst, through the X-ray active stage. A time sequence of optical, flux calibrated high resolution spectra was obtained with the Nordic Optical Telescope (NOT) using FIES simultaneously, or contemporaneously, with the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope during the early stages of the outburst. These were supplemented with MERCATOR/HERMES optical spectra. High resolution IUE ultraviolet spectra of OS And 1986, taken during the Fe curtain phase, served as a template for the distance determination. We used standard plasma diagnostics (e.g., [O III] and [N II] line ratios, and the H$尾$ line flux) to constrain electron densities and temperatures of the ejecta. Using Monte Carlo modeling of the ejecta, we derived the structure, filling factor, and mass from comparisons of the optical and ultraviolet line profiles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.01777v1-abstract-full').style.display = 'none'; document.getElementById('1606.01777v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 18 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2016 A&A, 590, 123 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.08840">arXiv:1503.08840</a> <span> [<a href="https://arxiv.org/pdf/1503.08840">pdf</a>, <a href="https://arxiv.org/format/1503.08840">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/10.1088/0004-637X/805/2/148">10.1088/0004-637X/805/2/148 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST Images Flash Ionization of Old Ejecta by the 2011 Eruption of Recurrent Nova T Pyxidis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shara%2C+M+M">Michael M. Shara</a>, <a href="/search/astro-ph?searchtype=author&query=Zurek%2C+D">David Zurek</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">Bradley E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+H+E">Howard E. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Godon%2C+P">Patrick Godon</a>, <a href="/search/astro-ph?searchtype=author&query=Mac+Low%2C+M">Mordecai-Mark Mac Low</a>, <a href="/search/astro-ph?searchtype=author&query=Pagnotta%2C+A">Ashley Pagnotta</a>, <a href="/search/astro-ph?searchtype=author&query=Prialnik%2C+D">Dina Prialnik</a>, <a href="/search/astro-ph?searchtype=author&query=Sion%2C+E+M">Edward M. Sion</a>, <a href="/search/astro-ph?searchtype=author&query=Toraskar%2C+J">Jayashree Toraskar</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1503.08840v1-abstract-short" style="display: inline;"> T Pyxidis is the only recurrent nova surrounded by knots of material ejected in previous outbursts. Following the eruption that began on 2011 April 14.29, we obtained seven epochs (from 4 to 383 days after eruption) of Hubble Space Telescope narrowband Ha images of T Pyx . The flash of radiation from the nova event had no effect on the ejecta until at least 55 days after the eruption began. Photoi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.08840v1-abstract-full').style.display = 'inline'; document.getElementById('1503.08840v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.08840v1-abstract-full" style="display: none;"> T Pyxidis is the only recurrent nova surrounded by knots of material ejected in previous outbursts. Following the eruption that began on 2011 April 14.29, we obtained seven epochs (from 4 to 383 days after eruption) of Hubble Space Telescope narrowband Ha images of T Pyx . The flash of radiation from the nova event had no effect on the ejecta until at least 55 days after the eruption began. Photoionization of hydrogen located north and south of the central star was seen 132 days after the beginning of the eruption. That hydrogen recombined in the following 51 days, allowing us to determine a hydrogen atom density of at least 7e5 cm^-3 - at least an order of magnitude denser than the previously detected, unresolved [NII] knots surrounding T Pyx. Material to the northwest and southeast was photoionized between 132 and 183 days after the eruption began. 99 days later that hydrogen had recombined. Both then (282 days after outburst) and 101 days later, we detected almost no trace of hydrogen emission around T Pyx. There is a large reservoir of previously unseen, cold diffuse hydrogen overlapping the previously detected, [NII] - emitting knots of T Pyx ejecta. The mass of this newly detected hydrogen is probably an order of magnitude larger than that of the [NII] knots. We also determine that there is no significant reservoir of undetected ejecta from the outer boundaries of the previously detected ejecta out to about twice that distance, near the plane of the sky. The lack of distant ejecta is consistent with the Schaefer et al (2010) scenario for T Pyx, in which the star underwent its first eruption within five years of 1866 after many millennia of quiescence, followed by the six observed recurrent nova eruptions since 1890. This lack of distant ejecta is not consistent with scenarios in which T Pyx has been erupting continuously as a recurrent nova for many centuries or millennia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.08840v1-abstract-full').style.display = 'none'; document.getElementById('1503.08840v1-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 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 10 figures, submitted to the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1410.0148">arXiv:1410.0148</a> <span> [<a href="https://arxiv.org/pdf/1410.0148">pdf</a>, <a href="https://arxiv.org/ps/1410.0148">ps</a>, <a href="https://arxiv.org/format/1410.0148">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"> On the Evolution of the Late-time {\it Hubble Space Telescope} Imaging of the Outburst of the Recurrent Nova RS Ophiuchi (2006) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+V+A+R+M">Val茅rio A. R. M. Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Bode%2C+M+F">Michael F. Bode</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1410.0148v1-abstract-short" style="display: inline;"> We modelled the late-time {\it Hubble Space Telescope} imaging of RS Ophiuchi with models from Ribeiro et al. (2009), which at the time due to the unknown availability of simultaneous ground-based spectroscopy left some open questions as to the evolution of the expanding nebular from the early to the late time observations. Initial emission line identifications suggest that no forbidden lines are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.0148v1-abstract-full').style.display = 'inline'; document.getElementById('1410.0148v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.0148v1-abstract-full" style="display: none;"> We modelled the late-time {\it Hubble Space Telescope} imaging of RS Ophiuchi with models from Ribeiro et al. (2009), which at the time due to the unknown availability of simultaneous ground-based spectroscopy left some open questions as to the evolution of the expanding nebular from the early to the late time observations. Initial emission line identifications suggest that no forbidden lines are present in the spectra and that the emission lines arising in the region of the WFPC2 F502N images are due to N{\sc ii} and He{\sc i} + Fe{\sc ii}. The best model fit to the spectrum is one where the outer faster moving material expands linearly with time while the inner over-density material either suffered some deceleration or did not change in physical size. The origin of this inner over-density requires further exploration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.0148v1-abstract-full').style.display = 'none'; document.getElementById('1410.0148v1-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 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2014. </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, to appear in Stella Novae: Past and Future Decades, P. A. Woudt & V. A. R. M. Ribeiro (eds), ASPCS 490</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1402.0128">arXiv:1402.0128</a> <span> [<a href="https://arxiv.org/pdf/1402.0128">pdf</a>, <a href="https://arxiv.org/ps/1402.0128">ps</a>, <a href="https://arxiv.org/format/1402.0128">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/10.1088/2041-8205/784/2/L33">10.1088/2041-8205/784/2/L33 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hubble Space Telescope Far Ultraviolet Spectroscopy of the Recurrent Nova T Pyxidis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Godon%2C+P">P. Godon</a>, <a href="/search/astro-ph?searchtype=author&query=Sion%2C+E+M">E. M. Sion</a>, <a href="/search/astro-ph?searchtype=author&query=Starrfield%2C+S">S. Starrfield</a>, <a href="/search/astro-ph?searchtype=author&query=Livio%2C+M">M. Livio</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Woodward%2C+C+E">C. E. Woodward</a>, <a href="/search/astro-ph?searchtype=author&query=Kuin%2C+P">P. Kuin</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+K+L">K. L. Page</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="1402.0128v1-abstract-short" style="display: inline;"> With six recorded nova outbursts, the prototypical recurrent nova T Pyxidis is the ideal cataclysmic variable system to assess the net change of the white dwarf mass within a nova cycle. Recent estimates of the mass ejected in the 2011 outburst ranged from a few 1.E-5 sollar mass to 3.3E-4 sollar mass, and assuming a mass accretion rate of 1.E-8 to 1.E-7 Sollar mass/yr for 44yrs, it has been concl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.0128v1-abstract-full').style.display = 'inline'; document.getElementById('1402.0128v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1402.0128v1-abstract-full" style="display: none;"> With six recorded nova outbursts, the prototypical recurrent nova T Pyxidis is the ideal cataclysmic variable system to assess the net change of the white dwarf mass within a nova cycle. Recent estimates of the mass ejected in the 2011 outburst ranged from a few 1.E-5 sollar mass to 3.3E-4 sollar mass, and assuming a mass accretion rate of 1.E-8 to 1.E-7 Sollar mass/yr for 44yrs, it has been concluded that the white dwaf in T Pyx is actually losing mass. Using NLTE disk modeling spectra to fit our recently obtained Hubble Space Telescope (HST) COS and STIS spectra, we find a mass accretion rate of up to two orders of magnitude larger than previously estimated. Our larger mass accretion rate is due mainly to the newly derived distance of T Pyx (4.8kpc; Sokoloski et al. 2013, larger than the previous 3.5kpc estimate), our derived reddening of E(B-V)=0.35 (based on combined IUE and GALEX spectra) and NLTE disk modeling (compared to black body and raw flux estimates in earlier works). We find that for most values of the reddening (0.25 < E(B-V) < 0.50) and white dwaf mass (0.70 to 1.35 Sollar mass) the accreted mass is larger than the ejected mass. Only for a low reddening (0.25 and smaller) combined with a large white dwaf mass (0.9 sollar mass and larger) is the ejected mass larger than the accreted one. However, the best spectral fitting results are obtained for a larger value of the reddening. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.0128v1-abstract-full').style.display = 'none'; document.getElementById('1402.0128v1-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 February, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">The Astrophysical Journal Letter, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1311.0147">arXiv:1311.0147</a> <span> [<a href="https://arxiv.org/pdf/1311.0147">pdf</a>, <a href="https://arxiv.org/ps/1311.0147">ps</a>, <a href="https://arxiv.org/format/1311.0147">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1088/0004-637X/779/1/38">10.1088/0004-637X/779/1/38 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the Source of the Dust Extinction in Type Ia Supernovae and the Discovery of Anomalously Strong Na I Absorption </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+M">M. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Simon%2C+J+D">Joshua D. Simon</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N">Nidia Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">Christopher R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Cox%2C+N+L+J">Nick L. J. Cox</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R+J">Ryan J. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Karakas%2C+A+I">Amanda I. Karakas</a>, <a href="/search/astro-ph?searchtype=author&query=Patat%2C+F">F. Patat</a>, <a href="/search/astro-ph?searchtype=author&query=Sternberg%2C+A">A. Sternberg</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">A. Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+E+Y">E. Y. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Leonard%2C+D+C">D. C. Leonard</a>, <a href="/search/astro-ph?searchtype=author&query=Persson%2C+S+E">Sven E. Persson</a>, <a href="/search/astro-ph?searchtype=author&query=Stritzinger%2C+M">Maximilian Stritzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+I+B">I. B. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Campillay%2C+A">Abdo Campillay</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+C">Carlos Contreras</a>, <a href="/search/astro-ph?searchtype=author&query=Folatelli%2C+G">Gast贸n Folatelli</a>, <a href="/search/astro-ph?searchtype=author&query=Freedman%2C+W+L">Wendy L. Freedman</a>, <a href="/search/astro-ph?searchtype=author&query=Hamuy%2C+M">Mario Hamuy</a>, <a href="/search/astro-ph?searchtype=author&query=Roth%2C+M">Miguel Roth</a>, <a href="/search/astro-ph?searchtype=author&query=Shields%2C+G+A">Gregory A. Shields</a>, <a href="/search/astro-ph?searchtype=author&query=Suntzeff%2C+N+B">Nicholas B. Suntzeff</a>, <a href="/search/astro-ph?searchtype=author&query=Chomiuk%2C+L">Laura Chomiuk</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1311.0147v1-abstract-short" style="display: inline;"> High-dispersion observations of the Na I D 5890, 5896 and K I 7665, 7699 interstellar lines, and the diffuse interstellar band at 5780 Angstroms in the spectra of 32 Type Ia supernovae are used as an independent means of probing dust extinction. We show that the dust extinction of the objects where the diffuse interstellar band at 5780 Angstroms is detected is consistent with the visual extinction… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.0147v1-abstract-full').style.display = 'inline'; document.getElementById('1311.0147v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1311.0147v1-abstract-full" style="display: none;"> High-dispersion observations of the Na I D 5890, 5896 and K I 7665, 7699 interstellar lines, and the diffuse interstellar band at 5780 Angstroms in the spectra of 32 Type Ia supernovae are used as an independent means of probing dust extinction. We show that the dust extinction of the objects where the diffuse interstellar band at 5780 Angstroms is detected is consistent with the visual extinction derived from the supernova colors. This strongly suggests that the dust producing the extinction is predominantly located in the interstellar medium of the host galaxies and not in circumstellar material associated with the progenitor system. One quarter of the supernovae display anomalously large Na I column densities in comparison to the amount of dust extinction derived from their colors. Remarkably, all of the cases of unusually strong Na I D absorption correspond to "Blueshifted" profiles in the classification scheme of Sternberg et al. (2011). This coincidence suggests that outflowing circumstellar gas is responsible for at least some of the cases of anomalously large Na I column densities. Two supernovae with unusually strong Na I D absorption showed essentially normal K I column densities for the dust extinction implied by their colors, but this does not appear to be a universal characteristic. Overall, we find the most accurate predictor of individual supernova extinction to be the equivalent width of the diffuse interstellar band at 5780 Angstroms, and provide an empirical relation for its use. Finally, we identify ways of producing significant enhancements of the Na abundance of circumstellar material in both the single-degenerate and double-degenerate scenarios for the progenitor system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.0147v1-abstract-full').style.display = 'none'; document.getElementById('1311.0147v1-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 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">55 pages, 13 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1308.5175">arXiv:1308.5175</a> <span> [<a href="https://arxiv.org/pdf/1308.5175">pdf</a>, <a href="https://arxiv.org/ps/1308.5175">ps</a>, <a href="https://arxiv.org/format/1308.5175">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/stt1565">10.1093/mnras/stt1565 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the nature of CP Pup </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mason%2C+E">Elena Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Orio%2C+M">Marina Orio</a>, <a href="/search/astro-ph?searchtype=author&query=Mukai%2C+K">Koji Mukai</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchini%2C+A">Antonio Bianchini</a>, <a href="/search/astro-ph?searchtype=author&query=de+Martino%2C+D">Domitilla de Martino</a>, <a href="/search/astro-ph?searchtype=author&query=di+Mille%2C+F">Francesco di Mille</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Abbot%2C+T">Timothy Abbot</a>, <a href="/search/astro-ph?searchtype=author&query=de+Propris%2C+R">Roberto de Propris</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="1308.5175v1-abstract-short" style="display: inline;"> We present new X-ray and optical spectra of the old nova CP Pup (nova Pup 1942) obtained with Chandra and the CTIO 4m telescope. The X-ray spectrum reveals a multi-temperature optically thin plasma reaching a maximum temperature of 36$^{+19}_{-16}$ keV absorbed by local complex neutral material. The time resolved optical spectroscopy confirms the presence of the $\sim$1.47 hr period, with cycle-to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.5175v1-abstract-full').style.display = 'inline'; document.getElementById('1308.5175v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1308.5175v1-abstract-full" style="display: none;"> We present new X-ray and optical spectra of the old nova CP Pup (nova Pup 1942) obtained with Chandra and the CTIO 4m telescope. The X-ray spectrum reveals a multi-temperature optically thin plasma reaching a maximum temperature of 36$^{+19}_{-16}$ keV absorbed by local complex neutral material. The time resolved optical spectroscopy confirms the presence of the $\sim$1.47 hr period, with cycle-to-cycle amplitude changes, as well as of an additional long term modulation which is suggestive either of a longer period or of non-Keplerian velocities in the emission line regions. These new observational facts add further support to CP Pup as a magnetic cataclysmic variable (mCV). We compare the mCV and the non-mCV scenarios and while we cannot conclude whether CP Pup is a long period system, all observational evidences point at an intermediate polar (IP) type CV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.5175v1-abstract-full').style.display = 'none'; document.getElementById('1308.5175v1-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 August, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on MNRAS. 10 pages and 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/1303.2777">arXiv:1303.2777</a> <span> [<a href="https://arxiv.org/pdf/1303.2777">pdf</a>, <a href="https://arxiv.org/ps/1303.2777">ps</a>, <a href="https://arxiv.org/format/1303.2777">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 multiple periods and the magnetic nature of CP Pup </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mason%2C+E">Elena Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchini%2C+A">Antonio Bianchini</a>, <a href="/search/astro-ph?searchtype=author&query=Orio%2C+M">Marina Orio</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Mukai%2C+K">Koji Mukai</a>, <a href="/search/astro-ph?searchtype=author&query=de+Marino%2C+D">Domitilla de Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Abbot%2C+T+.+M+C">Timothy . M. C. Abbot</a>, <a href="/search/astro-ph?searchtype=author&query=di+Mille%2C+F">Francesco di Mille</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="1303.2777v1-abstract-short" style="display: inline;"> Fast cadence time resolved spectra taken at the CTIO-4m telescope with the RC-spectrograph during 2 consecutive nights revealed a long term modulation of the binary radial velocity. Chandra hard X-ray spectra taken with the HETGS instrument showed features typically observed in magnetic white dwarfs (WD). Here, we present the new data and suggest that CP Pup is possibly a long orbital period inter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1303.2777v1-abstract-full').style.display = 'inline'; document.getElementById('1303.2777v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1303.2777v1-abstract-full" style="display: none;"> Fast cadence time resolved spectra taken at the CTIO-4m telescope with the RC-spectrograph during 2 consecutive nights revealed a long term modulation of the binary radial velocity. Chandra hard X-ray spectra taken with the HETGS instrument showed features typically observed in magnetic white dwarfs (WD). Here, we present the new data and suggest that CP Pup is possibly a long orbital period intermediate polar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1303.2777v1-abstract-full').style.display = 'none'; document.getElementById('1303.2777v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 March, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 3 figures -- Stellae Novae conference proceeding</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.0424">arXiv:1207.0424</a> <span> [<a href="https://arxiv.org/pdf/1207.0424">pdf</a>, <a href="https://arxiv.org/ps/1207.0424">ps</a>, <a href="https://arxiv.org/format/1207.0424">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/10.1051/0004-6361/201219556">10.1051/0004-6361/201219556 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> U Sco 2010 outburst: a new understanding of the binary accretion disk and the secondary star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mason%2C+E">Elena Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">Alessandro Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Valle%2C+M">Massimo Della Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Setiawan%2C+J">Johny Setiawan</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="1207.0424v1-abstract-short" style="display: inline;"> We present optical and NIR spectroscopic observations of U Sco 2010 outburst. From the analysis of lines profiles we identify a broad and a narrow component and show that the latter originates from the reforming accretion disk. We show that the accretion resumes shortly after the outburst, on day +8, roughly when the super-soft (SSS) X-ray phase starts. Consequently U Sco SSS phase is fueled (in p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.0424v1-abstract-full').style.display = 'inline'; document.getElementById('1207.0424v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.0424v1-abstract-full" style="display: none;"> We present optical and NIR spectroscopic observations of U Sco 2010 outburst. From the analysis of lines profiles we identify a broad and a narrow component and show that the latter originates from the reforming accretion disk. We show that the accretion resumes shortly after the outburst, on day +8, roughly when the super-soft (SSS) X-ray phase starts. Consequently U Sco SSS phase is fueled (in part or fully) by accretion and should not be used to estimate $m_{\mathrm{rem}}$, the mass of accreted material which has not been ejected during the outburst. In addition, most of the He emission lines, and the HeII lies in particular, form in the accretion flow/disk within the binary and are optically thick, thus preventing an accurate abundance determination. A late spectrum taken in quiescence and during eclipse shows CaII H&K, the G-band and MgI b absorption from the secondary star. However, no other significant secondary star features have been observed at longer wavelengths and in the NIR band. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.0424v1-abstract-full').style.display = 'none'; document.getElementById('1207.0424v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on A&A. 12 pages and 12 figures (a few are multiple 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/1009.4740">arXiv:1009.4740</a> <span> [<a href="https://arxiv.org/pdf/1009.4740">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <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/10.1088/0004-6256/140/6/1860">10.1088/0004-6256/140/6/1860 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The spectral evolution and ejecta of recurrent nova U Sco in the 2010 outburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Diaz%2C+M+P">M. P. Diaz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Luna%2C+G+J">G. J. Luna</a>, <a href="/search/astro-ph?searchtype=author&query=Moraes%2C+M">M. Moraes</a>, <a href="/search/astro-ph?searchtype=author&query=Takeda%2C+L">L. Takeda</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="1009.4740v1-abstract-short" style="display: inline;"> Synoptic spectroscopic observations of the U Sco 2010 outburst from maximum light to quiescence as well as a contemporaneous X-ray observation are presented and analyzed. The X-ray spectrum 52 days after outburst indicates a hot source (kTbb ~ 70 eV). . Narrow line components from the irradiated companion atmosphere were observed in hydrogen and helium optical recombination lines. The formation of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.4740v1-abstract-full').style.display = 'inline'; document.getElementById('1009.4740v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1009.4740v1-abstract-full" style="display: none;"> Synoptic spectroscopic observations of the U Sco 2010 outburst from maximum light to quiescence as well as a contemporaneous X-ray observation are presented and analyzed. The X-ray spectrum 52 days after outburst indicates a hot source (kTbb ~ 70 eV). . Narrow line components from the irradiated companion atmosphere were observed in hydrogen and helium optical recombination lines. The formation of a nebular spectrum is seen for the first time in this class of recurrent novae, allowing a detailed study of the ejecta using photoionization models. Unusual [OIII] auroral-to-nebular line ratios were found and possible scenarios of their origin are discussed. The modeling of the emission line spectrum suggests a highly heterogeneous ejecta with mass around or above 3 x 10-6 Msun <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.4740v1-abstract-full').style.display = 'none'; document.getElementById('1009.4740v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2010. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1004.3600">arXiv:1004.3600</a> <span> [<a href="https://arxiv.org/pdf/1004.3600">pdf</a>, <a href="https://arxiv.org/ps/1004.3600">ps</a>, <a href="https://arxiv.org/format/1004.3600">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/10.1051/0004-6361/200913610">10.1051/0004-6361/200913610 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The peculiar nova V1309 Sco/Nova Sco 2008: A candidate twin of V838 Mon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mason%2C+E">Elena Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz%2C+M">Marcos Diaz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Preston%2C+G">George Preston</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">Thomas Bensby</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="1004.3600v1-abstract-short" style="display: inline;"> Nova Scorpii 2008 was the target of our Directory Discretionary Time proposal at VLT+UVES in order to study the evolution, origin and abundances of the heavy-element absorption system recently discovered in 80% of classical novae in outburst. The early decline of Nova Scorpii 2008 was monitored with high resolution echelle spectroscopy at 5 different epochs. The analysis of the absorption and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.3600v1-abstract-full').style.display = 'inline'; document.getElementById('1004.3600v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1004.3600v1-abstract-full" style="display: none;"> Nova Scorpii 2008 was the target of our Directory Discretionary Time proposal at VLT+UVES in order to study the evolution, origin and abundances of the heavy-element absorption system recently discovered in 80% of classical novae in outburst. The early decline of Nova Scorpii 2008 was monitored with high resolution echelle spectroscopy at 5 different epochs. The analysis of the absorption and the emission lines show many unusual characteristics. Nova Scorpii 2008 is confirmed to differ from a common Classical Nova as well as a Symbiotic Recurrent Nova, and it shows characteristics which are common to the so called, yet debated, red-novae. The origin of this new nova remains uncertain. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.3600v1-abstract-full').style.display = 'none'; document.getElementById('1004.3600v1-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, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 8 figures. Accepted by A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0705.0701">arXiv:0705.0701</a> <span> [<a href="https://arxiv.org/pdf/0705.0701">pdf</a>, <a href="https://arxiv.org/ps/0705.0701">ps</a>, <a href="https://arxiv.org/format/0705.0701">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/519240">10.1086/519240 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Early Spectrophotometric Evolution of V1186 Scorpii (Nova Scorpii 2004 #1) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schwarz%2C+G+J">G. J. Schwarz</a>, <a href="/search/astro-ph?searchtype=author&query=Woodward%2C+C+E">C. E. Woodward</a>, <a href="/search/astro-ph?searchtype=author&query=Bode%2C+M+F">M. F. Bode</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A">A. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyres%2C+S+P">S. P. Eyres</a>, <a href="/search/astro-ph?searchtype=author&query=Geballe%2C+T+R">T. R. Geballe</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrz%2C+R+D">R. D. Gehrz</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhouse%2C+M+A">M. A. Greenhouse</a>, <a href="/search/astro-ph?searchtype=author&query=Hauschildt%2C+P+H">P. H. Hauschildt</a>, <a href="/search/astro-ph?searchtype=author&query=Helton%2C+L+A">L. A. Helton</a>, <a href="/search/astro-ph?searchtype=author&query=Lynch%2C+D+K">D. K. Lynch</a>, <a href="/search/astro-ph?searchtype=author&query=Lyke%2C+J+E">J. E. Lyke</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+T+J">T. J. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Russell%2C+R+W">R. W. Russell</a>, <a href="/search/astro-ph?searchtype=author&query=Rudy%2C+R+J">R. J. Rudy</a>, <a href="/search/astro-ph?searchtype=author&query=Shore%2C+S+N">S. N. Shore</a>, <a href="/search/astro-ph?searchtype=author&query=Starrfield%2C+S+G">S. G. Starrfield</a>, <a href="/search/astro-ph?searchtype=author&query=Temim%2C+T">T. Temim</a>, <a href="/search/astro-ph?searchtype=author&query=Truran%2C+J+W">J. W. Truran</a>, <a href="/search/astro-ph?searchtype=author&query=Venturini%2C+C+C">C. C. Venturini</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Zamanov%2C+R">R. Zamanov</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="0705.0701v1-abstract-short" style="display: inline;"> We report optical photometry and optical through mid-infrared spectroscopy of the classical nova V1186 Sco. This slowly developing nova had an complex light curve with multiple secondary peaks similar to those seen in PW Vul. The time to decline 2 magnitudes, t$_2$, was 20 days but the erratic nature of the light curve makes determination of intrinsic properties based on the decline time (e.g.,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0705.0701v1-abstract-full').style.display = 'inline'; document.getElementById('0705.0701v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0705.0701v1-abstract-full" style="display: none;"> We report optical photometry and optical through mid-infrared spectroscopy of the classical nova V1186 Sco. This slowly developing nova had an complex light curve with multiple secondary peaks similar to those seen in PW Vul. The time to decline 2 magnitudes, t$_2$, was 20 days but the erratic nature of the light curve makes determination of intrinsic properties based on the decline time (e.g., luminosity) problematic, and the often cited MMRD relationship of Della Valle and Livio (1995) fails to yield a plausible distance. Spectra covering 0.35 to 35 $渭$m were obtained in two separate epochs during the first year of outburst. The first set of spectra, taken about 2 months after visible maximum, are typical of a CO-type nova with narrow line emission from \ion{H}{1}, \ion{Fe}{2}, \ion{O}{1} and \ion{He}{1}. Later data, obtained between 260 and 380 days after maximum, reveal an emerging nebular spectrum. \textit{Spitzer} spectra show weakening hydrogen recombination emission with the emergence of [\ion{Ne}{2}] (12.81 $渭$m) as the strongest line. Strong emission from [\ion{Ne}{3}] (15.56 $渭$m) is also detected. Photoionization models with low effective temperature sources and only marginal neon enhancement (Ne $\sim$ 1.3 Ne$_{\odot}$) are consistent with these IR fine-structure neon lines indicating that V1186 Sco did not occur on a ONeMg white dwarf. In contrast, the slow and erratic light curve evolution, spectral development, and photoionization analysis of the ejecta imply the outburst occurred on a low mass CO white dwarf. We note that this is the first time strong [\ion{Ne}{2}] lines have been detected so early in the outburst of a CO nova and suggests that the presence of mid-infrared neon lines is not directly indicative of a ONeMg nova event. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0705.0701v1-abstract-full').style.display = 'none'; document.getElementById('0705.0701v1-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, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 figures, 37 pages. Astronimocal Journal accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J.134:516-526,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0608598">arXiv:astro-ph/0608598</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0608598">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0608598">ps</a>, <a href="https://arxiv.org/format/astro-ph/0608598">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361:20065741">10.1051/0004-6361:20065741 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early spectral evolution of Nova Sgr 2004 (V5114 Sgr) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+E">E. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Valle%2C+M">M. Della Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmozzi%2C+R">R. Gilmozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Germany%2C+L">L. Germany</a>, <a href="/search/astro-ph?searchtype=author&query=Saviane%2C+I">I. Saviane</a>, <a href="/search/astro-ph?searchtype=author&query=Matteucci%2C+F">F. Matteucci</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Rudy%2C+R+J">R. J. Rudy</a>, <a href="/search/astro-ph?searchtype=author&query=Lynch%2C+D">D. Lynch</a>, <a href="/search/astro-ph?searchtype=author&query=Mazuk%2C+S">S. Mazuk</a>, <a href="/search/astro-ph?searchtype=author&query=Venturini%2C+C+C">C. C. Venturini</a>, <a href="/search/astro-ph?searchtype=author&query=Puetter%2C+R+C">R. C. Puetter</a>, <a href="/search/astro-ph?searchtype=author&query=Perry%2C+R+B">R. B. Perry</a>, <a href="/search/astro-ph?searchtype=author&query=Liller%2C+W">W. Liller</a>, <a href="/search/astro-ph?searchtype=author&query=Rotter%2C+A">A. Rotter</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0608598v1-abstract-short" style="display: inline;"> We present optical and near-infrared spectral evolution of the Galactic nova V5114 Sgr (2004) during few months after the outburst. We use multi-band photometry and line intensities derived from spectroscopy to put constrains on the distance and the physical conditions of the ejecta of V5114 Sgr. The nova showed a fast decline (t_2 \simeq 11 days) and spectral features of FeII spectroscopic clas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0608598v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0608598v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0608598v1-abstract-full" style="display: none;"> We present optical and near-infrared spectral evolution of the Galactic nova V5114 Sgr (2004) during few months after the outburst. We use multi-band photometry and line intensities derived from spectroscopy to put constrains on the distance and the physical conditions of the ejecta of V5114 Sgr. The nova showed a fast decline (t_2 \simeq 11 days) and spectral features of FeII spectroscopic class. It reached M_V = -8.7 \pm 0.2 mag at maximum light, from which we derive a distance of 7700 \pm 700 kpc and a distance from the galactic plane of about 800 pc. Hydrogen and Oxygen mass of the ejecta are measured from emission lines, leading to 10^{-6} and 10^{-7} M_\odot, respectively. We compute the filling factor of the ejecta to be in the range 0.1 -- 10^{-3} . We found the value of the filling factor to decrease with time. The same is also observed in other novae, then giving support to the idea that nova shells are not homogeneously filled in, rather being the material clumped in relatively higher density blobs less affected by the general expanding motion of the ejecta. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0608598v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0608598v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 August, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2006. </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, 16 pages and 8 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/astro-ph/0505217">arXiv:astro-ph/0505217</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0505217">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0505217">ps</a>, <a href="https://arxiv.org/format/astro-ph/0505217">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/432872">10.1086/432872 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio Observations of the Hubble Deep Field South region: I. Survey Description and Initial Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">Ray P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Huynh%2C+M+T">Minh T. Huynh</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+C+A">Carole A. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+B+J">Brian J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Ekers%2C+R+D">Ronald. D. Ekers</a>, <a href="/search/astro-ph?searchtype=author&query=Mitchell%2C+D+A">Daniel A. Mitchell</a>, <a href="/search/astro-ph?searchtype=author&query=Sault%2C+R+J">Robert J. Sault</a>, <a href="/search/astro-ph?searchtype=author&query=Wieringa%2C+M+H">Mark H. Wieringa</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Higdon%2C+J">James Higdon</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0505217v1-abstract-short" style="display: inline;"> This paper is the first of a series describing the results of the Australia Telescope Hubble Deep Field South (ATHDFS) radio survey. The survey was conducted at four wavelengths - 20, 11, 6, and 3 cm, over a 4-year period, and achieves an rms sensitivity of about 10 microJy at each wavelength. We describe the observations and data reduction processes, and present data on radio sources close to t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0505217v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0505217v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0505217v1-abstract-full" style="display: none;"> This paper is the first of a series describing the results of the Australia Telescope Hubble Deep Field South (ATHDFS) radio survey. The survey was conducted at four wavelengths - 20, 11, 6, and 3 cm, over a 4-year period, and achieves an rms sensitivity of about 10 microJy at each wavelength. We describe the observations and data reduction processes, and present data on radio sources close to the centre of the HDF-S. We discuss in detail the properties of a subset of these sources. The sources include both starburst galaxies and galaxies powered by an active galactic nucleus, and range in redshift from 0.1 to 2.2. Some of them are characterised by unusually high radio-to-optical luminosities, presumably caused by dust extinction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0505217v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0505217v1-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 May, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by AJ. 32 pages, 4 tables, 3 figures. PDF with full-resolution figures is on http://www.atnf.csiro.au/people/rnorris/N197.pdf</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J.130:1358-1372,2005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0504153">arXiv:astro-ph/0504153</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0504153">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0504153">ps</a>, <a href="https://arxiv.org/format/astro-ph/0504153">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361:20041351">10.1051/0004-6361:20041351 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early decline spectra of Nova SMC 2001 and Nova LMC 2002 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mason%2C+E">E. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Valle%2C+M">M. Della Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmozzi%2C+R">R. Gilmozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Curto%2C+G+L">G. Lo Curto</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0504153v1-abstract-short" style="display: inline;"> We report results on the spectroscopic follow-up of Nova SMC 2001 and Nova LMC 2002 carried out at La Silla. The analysis of the spectroscopic evolution shows that these objects belong to the {\sl Fe II} class, according to the Cerro Tololo scheme. From the line fluxes and the expansion velocities, we have derived an approximate mass for the ejected shells of 2$\div3\times 10^{-4} M_\odot$. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0504153v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0504153v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0504153v1-abstract-full" style="display: none;"> We report results on the spectroscopic follow-up of Nova SMC 2001 and Nova LMC 2002 carried out at La Silla. The analysis of the spectroscopic evolution shows that these objects belong to the {\sl Fe II} class, according to the Cerro Tololo scheme. From the line fluxes and the expansion velocities, we have derived an approximate mass for the ejected shells of 2$\div3\times 10^{-4} M_\odot$. The filling factor measurements ($蔚\sim 10^{-4}梅10^{-1}$) suggest a clumpy structure for the ejecta. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0504153v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0504153v1-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, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2005. </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+5 figures A&A in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0212416">arXiv:astro-ph/0212416</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0212416">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0212416">ps</a>, <a href="https://arxiv.org/format/astro-ph/0212416">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/345509">10.1086/345509 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Deep Field South Flanking Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">Stefi A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">Thomas M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">Chris Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mello%2C+D">Duilia de Mello</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M+E">Mark E. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A+S">Andrew S. Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+J+P">Jonathan P. Gardner</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+D">Diane Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Lopezlira%2C+R+A">Rosa A. Gonzalez-Lopezlira</a>, <a href="/search/astro-ph?searchtype=author&query=Heyer%2C+I">Inge Heyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hook%2C+R+N">Richard N. Hook</a>, <a href="/search/astro-ph?searchtype=author&query=Kaiser%2C+M+E">Mary Elizabeth Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Mack%2C+J">Jennifer Mack</a>, <a href="/search/astro-ph?searchtype=author&query=Makidon%2C+R">Russell Makidon</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+C+L">Crystal L. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Mutchler%2C+M">Max Mutchler</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+T+E">T. Ed Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">Massimo Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Teplitz%2C+H+I">Harry I. Teplitz</a>, <a href="/search/astro-ph?searchtype=author&query=Wiggs%2C+M+S">Michael S. Wiggs</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Zurek%2C+D+R">David R. Zurek</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0212416v1-abstract-short" style="display: inline;"> As part of the Hubble Deep Field South program, a set of shorter 2-orbit observations were obtained of the area adjacent to the deep fields. The WFPC2 flanking fields cover a contiguous solid angle of 48 square arcminutes. Parallel observations with the STIS and NICMOS instruments produce a patchwork of additional fields with optical and near-infrared (1.6 micron) response. Deeper parallel expos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0212416v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0212416v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0212416v1-abstract-full" style="display: none;"> As part of the Hubble Deep Field South program, a set of shorter 2-orbit observations were obtained of the area adjacent to the deep fields. The WFPC2 flanking fields cover a contiguous solid angle of 48 square arcminutes. Parallel observations with the STIS and NICMOS instruments produce a patchwork of additional fields with optical and near-infrared (1.6 micron) response. Deeper parallel exposures with WFPC2 and NICMOS were obtained when STIS observed the NICMOS deep field. These deeper fields are offset from the rest, and an extended low surface brightness object is visible in the deeper WFPC2 flanking field. In this data paper, which serves as an archival record of the project, we discuss the observations and data reduction, and present SExtractor source catalogs and number counts derived from the data. Number counts are broadly consistent with previous surveys from both ground and space. Among other things, these flanking field observations are useful for defining slit masks for spectroscopic follow-up over a wider area around the deep fields, for studying large-scale structure that extends beyond the deep fields, for future supernova searches, and for number counts and morphological studies, but their ultimate utility will be defined by the astronomical community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0212416v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0212416v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 December, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2002. </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">46 pages, 15 figures. Images and full catalogs available via the HDF-S at http://www.stsci.edu/ftp/science/hdfsouth/hdfs.html at present. The paper is accepted for the February 2003 Astronomical Journal. Full versions of the catalogs will also be available on-line from AJ after publication</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J. 125 (2003) 398 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0210404">arXiv:astro-ph/0210404</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0210404">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0210404">ps</a>, <a href="https://arxiv.org/format/astro-ph/0210404">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.461516">10.1117/12.461516 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Topic maps for custom viewing of data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mahabal%2C+A+A">A A Mahabal</a>, <a href="/search/astro-ph?searchtype=author&query=Djorgovski%2C+S+G">S G Djorgovski</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R E Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+R">R Brunner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0210404v1-abstract-short" style="display: inline;"> A Topic Map is a structured network of hyperlinks that points into an information pool. Topic Maps have an existence independent of the information pool and hence different Topic Maps can form different layers above the same information pool and provide us with different views of it. We explore the use of Topic Maps with the Unified Column Descriptor (UCD) scheme developed in the frame of the ES… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0210404v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0210404v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0210404v1-abstract-full" style="display: none;"> A Topic Map is a structured network of hyperlinks that points into an information pool. Topic Maps have an existence independent of the information pool and hence different Topic Maps can form different layers above the same information pool and provide us with different views of it. We explore the use of Topic Maps with the Unified Column Descriptor (UCD) scheme developed in the frame of the ESO-CDS data mining project. UCD, with its multi-tier hierarchical structure, categorizes parameters reported in tables and catalogs. By using Topic Maps we show how columns from different catalogs with similar but not identical descriptions could be combined. A direct application for the Virtual Observatory community is that of merging catalogs in order to generate customized views of data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0210404v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0210404v1-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 October, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 11 figures. LaTeX, uses spie.sty (included). To appear in Proc. SPIE v. 4846 (2002). More details at http://www.astro.caltech.edu/~aam/science/topicmaps</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0208094">arXiv:astro-ph/0208094</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0208094">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0208094">ps</a>, <a href="https://arxiv.org/format/astro-ph/0208094">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1071/AS02010">10.1071/AS02010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Internal Extinction Curve of NGC 6302 and its Extraordinary Spectrum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B+A">Brent A. Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Dopita%2C+M+A">Michael A. Dopita</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Hua%2C+C">Chon-Trung Hua</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0208094v1-abstract-short" style="display: inline;"> In this paper we present a new method for obtaining the optical wavelength-dependent reddening function of planetary nebulae, using the nebular and stellar continuum. The data used was a spectrum of NGC 6302 obtained with a mean signal to noise of >10^2 A^-1 in the nebular continuum. With such a high S/N the continuum can be accurately compared with a theoretical model nebular plus stellar conti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0208094v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0208094v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0208094v1-abstract-full" style="display: none;"> In this paper we present a new method for obtaining the optical wavelength-dependent reddening function of planetary nebulae, using the nebular and stellar continuum. The data used was a spectrum of NGC 6302 obtained with a mean signal to noise of >10^2 A^-1 in the nebular continuum. With such a high S/N the continuum can be accurately compared with a theoretical model nebular plus stellar continuum. The nebular electron temperature and density used in the model are determined using ratios of prominent emission lines. The reddening function can then be obtained from the ratio of the theoretical and the observed continuum. We find that for NGC 6302, the visible to IR extinction law is indistinguishable from `standard' interstellar reddening, but that the UV extinction curve is much steeper than normal, suggesting that more small dust grains had been ejected into the nebula by the PN central star. Finally, using the extinction law that we have determined, we present a complete de--reddened line list of nearly 600 emission lines, and report on the detection of the He(2-10) and He(2-8) Raman Features at 4331 A and 4852 A, and the detection of Raman-Scattered OVI features at 6830 and 7087 AA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0208094v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0208094v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 August, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2002. </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">32 pages, 7 figures, to appear in PASA 2002, 19</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0205135">arXiv:astro-ph/0205135</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0205135">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0205135">ps</a>, <a href="https://arxiv.org/format/astro-ph/0205135">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361:20020611">10.1051/0004-6361:20020611 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Evolution of Nova V382 Vel 1999 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Della+Valle%2C+M">M. Della Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquini%2C+L">L. Pasquini</a>, <a href="/search/astro-ph?searchtype=author&query=Daou%2C+D">D. Daou</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0205135v1-abstract-short" style="display: inline;"> We report results of spectroscopic observations of V382 Vel (Nova Vel 1999) carried out at La Silla between 5 and 498 days after maximum light (23 May 1999, V(max) $\sim 2.3\pm 0.1$). The analysis of the photometric and spectroscopic evolution shows this object to be a {\sl fast nova} belonging to the Fe II {\sl broad} spectroscopic class. A distance of 1.7 kpc ($\pm 20%$) is derived from the ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0205135v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0205135v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0205135v1-abstract-full" style="display: none;"> We report results of spectroscopic observations of V382 Vel (Nova Vel 1999) carried out at La Silla between 5 and 498 days after maximum light (23 May 1999, V(max) $\sim 2.3\pm 0.1$). The analysis of the photometric and spectroscopic evolution shows this object to be a {\sl fast nova} belonging to the Fe II {\sl broad} spectroscopic class. A distance of 1.7 kpc ($\pm 20%$) is derived from the maximum magnitude vs. rate of decline relationship after correcting for the small reddening toward the nova, E(B--V)$\lsim 0.10$. From the measured H$伪$ flux and the associated rate of expansion we derive an approximate mass for the ejected shell, M$_{env}\lsim 10^{-5}$ M$_\odot$. We have also observed during the early decline a broad, short-lived ($\lsim$ 10 days) feature at 6705-6715 脜for which several identifications are possible, one of which is the lithium doublet at 6708 脜and which could place an empirical limit on the lithium production that might occur during the outburst of a {\sl fast nova}. The high luminosity at maximum, M$_v=-8.9$, and the relatively small height above the galactic plane ($z\lsim 160$pc) suggest that V382 Vel originated from a massive white dwarf, likely in the mass range 1.1--1.2 M$_\odot$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0205135v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0205135v1-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 May, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2002. </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 + 9 plots(gif). Accepted by A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0010245">arXiv:astro-ph/0010245</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0010245">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0010245">ps</a>, <a href="https://arxiv.org/format/astro-ph/0010245">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/316851">10.1086/316851 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WFPC2 Observations of the Hubble Deep Field-South </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mello%2C+D">Duilia de Mello</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A+S">Andrew S. Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Lopezlira%2C+R+A">Rosa A. Gonzalez-Lopezlira</a>, <a href="/search/astro-ph?searchtype=author&query=Heyer%2C+I">Inge Heyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hook%2C+R+N">Richard N. Hook</a>, <a href="/search/astro-ph?searchtype=author&query=Levay%2C+Z">Zolt Levay</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Mack%2C+J">Jennifer Mack</a>, <a href="/search/astro-ph?searchtype=author&query=Makidon%2C+R+B">Russell B. Makidon</a>, <a href="/search/astro-ph?searchtype=author&query=Mutchler%2C+M">Max Mutchler</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+T+E">T. Ed Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">Massimo Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Wiggs%2C+M+S">Michael S. Wiggs</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0010245v1-abstract-short" style="display: inline;"> The Hubble Deep Field-South observations targeted a high-galactic-latitude field near QSO J2233-606. We present WFPC2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distribut… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0010245v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0010245v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0010245v1-abstract-full" style="display: none;"> The Hubble Deep Field-South observations targeted a high-galactic-latitude field near QSO J2233-606. We present WFPC2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared to a new catalog of the HDF-N that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman-break galaxies at z > 2 than the HDF-N. The star-formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z ~ 2.7, and a factor of 1.3 higher at z ~ 4. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0010245v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0010245v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2000. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">93 pages, 25 figures; contains very long tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J.120:2747-2824,2000 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9912167">arXiv:astro-ph/9912167</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9912167">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9912167">ps</a>, <a href="https://arxiv.org/format/astro-ph/9912167">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/301215">10.1086/301215 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Deep Field South - STIS Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+J+P">J. P. Gardner</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">S. A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+C+M">C. M. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen%2C+J">J. Christensen</a>, <a href="/search/astro-ph?searchtype=author&query=Dashevsky%2C+I">I. Dashevsky</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M+E">M. E. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Espey%2C+B+R">B. R. Espey</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">H. C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A+S">A. S. Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Gonnella%2C+A+M">A. M. Gonnella</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Lopezlira%2C+R+A">R. A. Gonzalez-Lopezlira</a>, <a href="/search/astro-ph?searchtype=author&query=Hook%2C+R+N">R. N. Hook</a>, <a href="/search/astro-ph?searchtype=author&query=Kaiser%2C+M+E">M. E. Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+C+L">C. L. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+K+C">K. C. Sahu</a>, <a href="/search/astro-ph?searchtype=author&query=Savaglio%2C+S">S. Savaglio</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+T+E">T. E. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Teplitz%2C+H+I">H. I. Teplitz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson%2C+J">J. Wilson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9912167v1-abstract-short" style="display: inline;"> We present the imaging observations made with the Space Telescope Imaging Spectrograph of the Hubble Deep Field - South. The field was imaged in 4 bandpasses: a clear CCD bandpass for 156 ksec, a long-pass filter for 22-25 ksec per pixel typical exposure, a near-UV bandpass for 23 ksec, and a far-UV bandpass for 52 ksec. The clear visible image is the deepest observation ever made in the UV-opti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9912167v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9912167v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9912167v1-abstract-full" style="display: none;"> We present the imaging observations made with the Space Telescope Imaging Spectrograph of the Hubble Deep Field - South. The field was imaged in 4 bandpasses: a clear CCD bandpass for 156 ksec, a long-pass filter for 22-25 ksec per pixel typical exposure, a near-UV bandpass for 23 ksec, and a far-UV bandpass for 52 ksec. The clear visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10 sigma AB magnitude of 29.4 for an object of area 0.2 square arcseconds. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9912167v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9912167v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 December, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 1999. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages, 10 figures, accepted for publication in the Astronomical Journal, February 2000. The resolution of the images has been reduced; preprints with full resolution images are available at http://hires.gsfc.nasa.gov/~gardner/hdfs/stispaper/index.html</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9910437">arXiv:astro-ph/9910437</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9910437">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9910437">ps</a>, <a href="https://arxiv.org/format/astro-ph/9910437">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> Radio Observations of the Hubble Deep Field South - a New Class of Radio-Luminous Galaxies? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A">A. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Sault%2C+R+J">R. J. Sault</a>, <a href="/search/astro-ph?searchtype=author&query=Ekers%2C+R+D">R. D. Ekers</a>, <a href="/search/astro-ph?searchtype=author&query=Ekers%2C+J">J. Ekers</a>, <a href="/search/astro-ph?searchtype=author&query=Badia%2C+F">F. Badia</a>, <a href="/search/astro-ph?searchtype=author&query=Higdon%2C+J">J. Higdon</a>, <a href="/search/astro-ph?searchtype=author&query=Wieringa%2C+M+H">M. H. Wieringa</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+B+J">B. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9910437v2-abstract-short" style="display: inline;"> We present the first results from a series of radio observations of the Hubble Deep Field South and its flanking fields. Here we consider only those sources greater than 100 microJy at 20 cm, in an 8-arcmin square field that covers the WFPC field, the STIS and NICMOS field, and most of the HST flanking fields and complementary ground-based observations. We have detected 13 such radio sources, tw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9910437v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9910437v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9910437v2-abstract-full" style="display: none;"> We present the first results from a series of radio observations of the Hubble Deep Field South and its flanking fields. Here we consider only those sources greater than 100 microJy at 20 cm, in an 8-arcmin square field that covers the WFPC field, the STIS and NICMOS field, and most of the HST flanking fields and complementary ground-based observations. We have detected 13 such radio sources, two of which are in the WFPC2 field itself. One of the sources in the WFPC field (source c) corresponds to a very faint galaxy, and several others outside the WFPC field can not be identified with sources in the other optical/IR wavebands. The radio and optical luminosities of these galaxies are inconsistent with either conventional starburst galaxies or with radio-loud galaxies. Instead, it appears that it belongs to a population of galaxies which are rare in the local Universe, possibly consisting of a radio-luminous active nucleus embedded in a very dusty starburst galaxy, and which are characterised by a very high radio/optical luminosity ratio. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9910437v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9910437v2-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 October, 1999; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 October, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 1999. </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 "Perspectives in Radio Astronomy: Imperatives at cm and m Wavelengths" (Dwingeloo: NFRA), Edited by: M.P. van Haarlem & J.M. van der Hulst Replacement: last two authors were accidentally omitted from astro-ph listing</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9901022">arXiv:astro-ph/9901022</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9901022">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9901022">ps</a>, <a href="https://arxiv.org/format/astro-ph/9901022">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/311963">10.1086/311963 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Lyman-alpha forest of the QSO in the Hubble Deep Field South </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Savaglio%2C+S">S. Savaglio</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">H. C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Espey%2C+B+R">B. R. Espey</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+K+C">K. C. Sahu</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">S. A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+C+M">C. M. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Kaiser%2C+M+E">M. E. Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">M. Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson%2C+J">J. Wilson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9901022v3-abstract-short" style="display: inline;"> The quasar in the Hubble Deep Field South (HDFS), J2233-606 (z=2.23) has been exhaustively observed by ground based telescopes and by the STIS spectrograph on board the Hubble Space Telescope at low, medium and high resolution in the spectral interval from 1120 A to 10000 A. This very large base-line represents a unique opportunity to study in detail the distribution of clouds associated with em… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9901022v3-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9901022v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9901022v3-abstract-full" style="display: none;"> The quasar in the Hubble Deep Field South (HDFS), J2233-606 (z=2.23) has been exhaustively observed by ground based telescopes and by the STIS spectrograph on board the Hubble Space Telescope at low, medium and high resolution in the spectral interval from 1120 A to 10000 A. This very large base-line represents a unique opportunity to study in detail the distribution of clouds associated with emitting structures in the field of the quasar and in nearby fields already observed as part of the HDFS campaign. Here we report the main properties of the Lyman-alpha clouds in the intermediate redshift range 1.20-2.20, where our present knowledge has been complicated by the difficulty in producing good data. The number density is shown to be higher than what is expected by extrapolating the results from both lower and higher redshifts: 63\pm8 lines with log N_{HI}\geq14.0 are found (including metal systems) at <z>=1.7, to be compared with ~40 lines predicted by extrapolating from previous studies. The redshift distribution of the Lyman-alpha clouds shows a region spanning z=1.383-1.460 (comoving size of 94 h^{-1}_{65} Mpc, Omega_o=1) with a low density of absorption lines; we detect 5 lines in this region, compared with the 16 expected from an average density along the line of sight. The two point correlation function shows a positive signal up to scales of about 3 h^{-1}_{65} Mpc and an amplitude that is larger for larger HI column densities. The average Doppler parameter is about 27 km/s, comparable to the mean value found at z > 3, thus casting doubts on the temperature evolution of the Lyman-alpha clouds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9901022v3-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9901022v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 February, 1999; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 January, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 1999. </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 ApJ Letters. The revised version includes the analysis of the number density evolution of the sample with metal systems</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9809404">arXiv:astro-ph/9809404</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9809404">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9809404">ps</a>, <a href="https://arxiv.org/format/astro-ph/9809404">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> The absorption line spectrum of the QSO J2233-606 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Outram%2C+P+J">P J Outram</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+B+J">B J Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Carswell%2C+R+F">R F Carswell</a>, <a href="/search/astro-ph?searchtype=author&query=Hewett%2C+P+C">P C Hewett</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R E Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R P Norris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9809404v1-abstract-short" style="display: inline;"> We report on high resolution observations (R=35000) of the Hubble Deep Field South QSO J2233-606 obtained with the University College London Echelle Spectrograph at the AAT. We present spectral data and an associated absorption line list for the wavelength region 3530 < lambda < 4390A. The data has a mean signal-to-noise ratio in the continuum of approximately 15 per 0.05A resolution element at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9809404v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9809404v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9809404v1-abstract-full" style="display: none;"> We report on high resolution observations (R=35000) of the Hubble Deep Field South QSO J2233-606 obtained with the University College London Echelle Spectrograph at the AAT. We present spectral data and an associated absorption line list for the wavelength region 3530 < lambda < 4390A. The data has a mean signal-to-noise ratio in the continuum of approximately 15 per 0.05A resolution element at lambda > 3700A. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9809404v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9809404v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 1998; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 1998. </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 LaTeX, including 1 figure, 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/astro-ph/9808282">arXiv:astro-ph/9808282</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9808282">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9808282">ps</a>, <a href="https://arxiv.org/format/astro-ph/9808282">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> An Extremely Red r^{1/4} Galaxy in the Test Image of the Hubble Deep Field South </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">M. Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">A. R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">R. E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">S. A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+G">G. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Blacker%2C+B+S">B. S. Blacker</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+C+M">C. M. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">S. Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M+E">M. E. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Demello%2C+D+F">D. F. Demello</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">H. C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A+S">A. S. Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">R. A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Mackenty%2C+J">J. Mackenty</a>, <a href="/search/astro-ph?searchtype=author&query=Madau%2C+P">P. Madau</a>, <a href="/search/astro-ph?searchtype=author&query=Postman%2C+M">M. Postman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9808282v1-abstract-short" style="display: inline;"> We report the serendipitous discovery of an extremely red object in the Hubble Deep Field South (HDFS) Test NICMOS (Near Infrared Camera and Multi Object Spectrograph) field of view. The object is resolved in the NICMOS image and has a light profile very well described by an r^{1/4} law with effective radius r_e=0."20+-0."05 and H_{AB}=21.7+-0.1 magnitudes. In contrast, the galaxy is undetected… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9808282v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9808282v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9808282v1-abstract-full" style="display: none;"> We report the serendipitous discovery of an extremely red object in the Hubble Deep Field South (HDFS) Test NICMOS (Near Infrared Camera and Multi Object Spectrograph) field of view. The object is resolved in the NICMOS image and has a light profile very well described by an r^{1/4} law with effective radius r_e=0."20+-0."05 and H_{AB}=21.7+-0.1 magnitudes. In contrast, the galaxy is undetected in the R and I band ground based images taken at the CTIO 4 m Blanco Telescope, giving a lower limit to the color of (R-H)_{AB}>3.9 and (I-H)_{AB}>3.5 at the 95% confidence level. The colors of a range of synthetic galactic spectra are computed, showing that the object is likely to be an ``old'' elliptical galaxy at redshift z>~1.7. Alternatively the colors can be reproduced by an ``old'' elliptical galaxy at somewhat lower redshift (z>~1) with significant amount of dust, or by a younger galaxy at higher redshift. This object represents a very interesting target for future VLT observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9808282v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9808282v1-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 August, 1998; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 1998. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A Letters; 5 pages including 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9607174">arXiv:astro-ph/9607174</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9607174">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9607174">ps</a>, <a href="https://arxiv.org/format/astro-ph/9607174">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/118105">10.1086/118105 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Deep Field: Observations, Data Reduction, and Galaxy Photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Williams%2C+R+E">Robert E. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=team%2C+t+H">the HDF team</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9607174v1-abstract-short" style="display: inline;"> The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9607174v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9607174v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9607174v1-abstract-full" style="display: none;"> The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground-based telescopes. The observations were made from 18 to 30 December 1995, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9607174v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9607174v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 July, 1996; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 1996. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, XX PostScript figures, uses aaspp4.sty astrobib.sty. (Astrobib is available from http://www.stsci.edu/software/TeX.html .) To appear the Astronomical Journal. More info on the Hubble deep field can be found at http://www.stsci.edu/../ftp/observer/hdf/hdf.html . More figures (images) can be found at http://www.stsci.edu/../ftp/observer/hdf/references/williams/ and the full source catalog is available at http://www.stsci.edu/../ftp/observer/hdf/archive/v2catalog/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J. 112 (1996) 1335 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

CINXE.COM

Search | arXiv e-print repository