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">Lupu, 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/" aria-role="search"> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Lupu, 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=Lupu%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="Lupu, 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/2204.13727">arXiv:2204.13727</a> <span> [<a href="https://arxiv.org/pdf/2204.13727">pdf</a>, <a href="https://arxiv.org/format/2204.13727">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/stac1331">10.1093/mnras/stac1331 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The impact of ultraviolet heating and cooling on the dynamics and observability of lava planet atmospheres </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nguyen%2C+T+G">T. Giang Nguyen</a>, <a href="/search/?searchtype=author&query=Cowan%2C+N+B">Nicolas B. Cowan</a>, <a href="/search/?searchtype=author&query=Pierrehumbert%2C+R+T">Raymond T. Pierrehumbert</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Moores%2C+J+E">John E. Moores</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.13727v2-abstract-short" style="display: inline;"> Lava planets have non-global, condensible atmospheres similar to icy bodies within the solar system. Because they depend on interior dynamics, studying the atmospheres of lava planets can lead to understanding unique geological processes driven by their extreme environment. Models of lava planet atmospheres have thus far focused on either radiative transfer or hydrodynamics. In this study, we coup… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13727v2-abstract-full').style.display = 'inline'; document.getElementById('2204.13727v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.13727v2-abstract-full" style="display: none;"> Lava planets have non-global, condensible atmospheres similar to icy bodies within the solar system. Because they depend on interior dynamics, studying the atmospheres of lava planets can lead to understanding unique geological processes driven by their extreme environment. Models of lava planet atmospheres have thus far focused on either radiative transfer or hydrodynamics. In this study, we couple the two processes by introducing ultraviolet and infrared radiation to a turbulent boundary layer model. We also test the effect of different vertical temperature profiles on atmospheric dynamics. Results from the model show that UV radiation affects the atmosphere much more than IR. UV heating and cooling work together to produce a horizontally isothermal atmosphere away from the sub-stellar point regardless of the vertical temperature profile. We also find that stronger temperature inversions induce stronger winds and hence cool the atmosphere. Our simulated transmission spectra of the bound atmosphere show a strong SiO feature in the UV that would be challenging to observe in the planet's transit spectrum due to the precision required. Our simulated emission spectra are more promising, with significant SiO spectral features at 4.5 and 9 $渭$m that can be observed with the James Webb Space Telescope. Different vertical temperature profiles produce discernible dayside emission spectra, but not in the way one would expect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13727v2-abstract-full').style.display = 'none'; document.getElementById('2204.13727v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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/2106.00781">arXiv:2106.00781</a> <span> [<a href="https://arxiv.org/pdf/2106.00781">pdf</a>, <a href="https://arxiv.org/format/2106.00781">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac0a7d">10.3847/1538-4357/ac0a7d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Following the Lithium: Tracing Li-bearing Molecules Across Age, Mass, and Gravity in Brown Dwarfs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gharib-Nezhad%2C+E">Ehsan Gharib-Nezhad</a>, <a href="/search/?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/?searchtype=author&query=Batalha%2C+N+E">Natasha E. Batalha</a>, <a href="/search/?searchtype=author&query=Visscher%2C+C">Channon Visscher</a>, <a href="/search/?searchtype=author&query=Freedman%2C+R+S">Richard S. Freedman</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.00781v1-abstract-short" style="display: inline;"> Lithium is an important element for the understanding of ultracool dwarfs because it is lost to fusion at masses above $\sim 68\, M_{\rm J}$. Hence, the presence or absence of atomic Li has served as an indicator of the nearby H-burning boundary at about $75\,M_{\rm J}$ between brown-dwarfs and very low-mass stars. Historically the "Lithium test", a search for the presence and strength of the Li l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00781v1-abstract-full').style.display = 'inline'; document.getElementById('2106.00781v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.00781v1-abstract-full" style="display: none;"> Lithium is an important element for the understanding of ultracool dwarfs because it is lost to fusion at masses above $\sim 68\, M_{\rm J}$. Hence, the presence or absence of atomic Li has served as an indicator of the nearby H-burning boundary at about $75\,M_{\rm J}$ between brown-dwarfs and very low-mass stars. Historically the "Lithium test", a search for the presence and strength of the Li line at 670.8 nm, has been a marker if an object has a substellar mass with stellar-like spectral energy distribution (e.g., a late-type M dwarf). While the Li test could in principle also be used to distinguish masses of later-type L-T dwarfs, Li is predominantly no longer found as an atomic gas, but rather a molecular species such as LiH, LiF, LiOH, and LiCl in their cooler atmospheres. L- and T-type brown dwarfs are also quite faint at 670 nm and thus challenging targets for high resolution spectroscopy. But only recently have experimental molecular line lists become available for the molecular Li species, allowing molecular Li mass discrimination. In this study, we generated the latest opacity of each of these Li-bearing molecules and performed thermochemical equilibrium atmospheric composition calculation of the abundance of these molecules. Finally, we computed thermal emission spectra for a series of radiative-convective equilibrium models of cloudy and cloudless brown dwarf atmospheres (with $T_{\rm eff}=$ 500--2400~K, and $\log g$=4.0, 4.5, 5.0) to understand where the presence or absence of atmospheric lithium-bearing species is most easily detected as a function of brown dwarf mass and age. After atomic Li, the best spectral signatures were found to be LiF at $10.5-12.5$~\micron and LiCl at $14.5-18.5$ $\micron$. LiH also shows a narrow feature at $\sim 9.38$ $\micron$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00781v1-abstract-full').style.display = 'none'; document.getElementById('2106.00781v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 figures, 1 table, In final revision at ApJ. Comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.01980">arXiv:2103.01980</a> <span> [<a href="https://arxiv.org/pdf/2103.01980">pdf</a>, <a href="https://arxiv.org/format/2103.01980">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2562997">10.1117/12.2562997 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Nancy Grace Roman Space Telescope Coronagraph Instrument (CGI) Technology Demonstration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kasdin%2C+N+J">N. Jeremy Kasdin</a>, <a href="/search/?searchtype=author&query=Bailey%2C+V+P">Vanessa P. Bailey</a>, <a href="/search/?searchtype=author&query=Mennesson%2C+B">Bertrand Mennesson</a>, <a href="/search/?searchtype=author&query=Zellem%2C+R+T">Robert T. Zellem</a>, <a href="/search/?searchtype=author&query=Ygouf%2C+M">Marie Ygouf</a>, <a href="/search/?searchtype=author&query=Rhodes%2C+J">Jason Rhodes</a>, <a href="/search/?searchtype=author&query=Luchik%2C+T">Thomas Luchik</a>, <a href="/search/?searchtype=author&query=Zhao%2C+F">Feng Zhao</a>, <a href="/search/?searchtype=author&query=Riggs%2C+A+J+E">A J Eldorado Riggs</a>, <a href="/search/?searchtype=author&query=Seo%2C+Y">Young-Joon Seo</a>, <a href="/search/?searchtype=author&query=Krist%2C+J">John Krist</a>, <a href="/search/?searchtype=author&query=Kern%2C+B">Brian Kern</a>, <a href="/search/?searchtype=author&query=Tang%2C+H">Hong Tang</a>, <a href="/search/?searchtype=author&query=Nemati%2C+B">Bijan Nemati</a>, <a href="/search/?searchtype=author&query=Groff%2C+T+D">Tyler D. Groff</a>, <a href="/search/?searchtype=author&query=Zimmerman%2C+N">Neil Zimmerman</a>, <a href="/search/?searchtype=author&query=Macintosh%2C+B">Bruce Macintosh</a>, <a href="/search/?searchtype=author&query=Turnbull%2C+M">Margaret Turnbull</a>, <a href="/search/?searchtype=author&query=Debes%2C+J">John Debes</a>, <a href="/search/?searchtype=author&query=Douglas%2C+E+S">Ewan S. Douglas</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.01980v1-abstract-short" style="display: inline;"> The Coronagraph Instrument (CGI) on the Nancy Grace Roman Space Telescope will demonstrate the high-contrast technology necessary for visible-light exoplanet imaging and spectroscopy from space via direct imaging of Jupiter-size planets and debris disks. This in-space experience is a critical step toward future, larger missions targeted at direct imaging of Earth-like planets in the habitable zone… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.01980v1-abstract-full').style.display = 'inline'; document.getElementById('2103.01980v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.01980v1-abstract-full" style="display: none;"> The Coronagraph Instrument (CGI) on the Nancy Grace Roman Space Telescope will demonstrate the high-contrast technology necessary for visible-light exoplanet imaging and spectroscopy from space via direct imaging of Jupiter-size planets and debris disks. This in-space experience is a critical step toward future, larger missions targeted at direct imaging of Earth-like planets in the habitable zones of nearby stars. This paper presents an overview of the current instrument design and requirements, highlighting the critical hardware, algorithms, and operations being demonstrated. We also describe several exoplanet and circumstellar disk science cases enabled by these capabilities. A competitively selected Community Participation Program team will be an integral part of the technology demonstration and could perform additional CGI observations beyond the initial tech demo if the instrument performance warrants it. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.01980v1-abstract-full').style.display = 'none'; document.getElementById('2103.01980v1-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">SPIE Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave, 114431U (15 December 2020)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> Proc. SPIE 11443 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.11299">arXiv:2008.11299</a> <span> [<a href="https://arxiv.org/pdf/2008.11299">pdf</a>, <a href="https://arxiv.org/format/2008.11299">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/10.3847/1538-3881/abb46b">10.3847/1538-3881/abb46b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for Characterizing the Haziest Sub-Neptune Exoplanets with High Resolution Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hood%2C+C+E">Callie E. Hood</a>, <a href="/search/?searchtype=author&query=Fortney%2C+J+J">Jonathan J. Fortney</a>, <a href="/search/?searchtype=author&query=Line%2C+M+R">Michael R. Line</a>, <a href="/search/?searchtype=author&query=Martin%2C+E+C">Emily C. Martin</a>, <a href="/search/?searchtype=author&query=Morley%2C+C+V">Caroline V. Morley</a>, <a href="/search/?searchtype=author&query=Birkby%2C+J+L">Jayne L. Birkby</a>, <a href="/search/?searchtype=author&query=Rustamkulov%2C+Z">Zafar Rustamkulov</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Freedman%2C+R+S">Richard S. Freedman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.11299v1-abstract-short" style="display: inline;"> Observations to characterize planets larger than Earth but smaller than Neptune have led to largely inconclusive interpretations at low spectral resolution due to hazes or clouds that obscure molecular features in their spectra. However, here we show that high-resolution spectroscopy (R $\sim$ 25,000 to 100,000) enables one to probe the regions in these atmospheres above the clouds where the cores… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11299v1-abstract-full').style.display = 'inline'; document.getElementById('2008.11299v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.11299v1-abstract-full" style="display: none;"> Observations to characterize planets larger than Earth but smaller than Neptune have led to largely inconclusive interpretations at low spectral resolution due to hazes or clouds that obscure molecular features in their spectra. However, here we show that high-resolution spectroscopy (R $\sim$ 25,000 to 100,000) enables one to probe the regions in these atmospheres above the clouds where the cores of the strongest spectral lines are formed. We present models of transmission spectra for a suite of GJ1214b-like planets with thick photochemical hazes covering 1 - 5 $渭$m at a range of resolutions relevant to current and future ground-based spectrographs. Furthermore, we compare the utility of the cross-correlation function that is typically used with a more formal likelihood-based approach, finding that only the likelihood based method is sensitive to the presence of haze opacity. We calculate the signal-to-noise of these spectra, including telluric contamination, required to robustly detect a host of molecules such as CO, CO$_{2}$, H$_{2}$O, and CH$_{4}$, and photochemical products like HCN, as a function of wavelength range and spectral resolution. Spectra in M band require the lowest S/N$_{res}$ to detect multiple molecules simultaneously. CH$_{4}$ is only observable for the coolest models ($T_{\rm{eff}} =$ 412 K) and only in the L band. We quantitatively assess how these requirements compare to what is achievable with current and future instruments, demonstrating that characterization of small cool worlds with ground-based high resolution spectroscopy is well within reach. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11299v1-abstract-full').style.display = 'none'; document.getElementById('2008.11299v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to AAS Journals, revised to reflect referee comments. Posting of this manuscript on the arXiv was coordinated with S. Ghandi et al</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.09211">arXiv:1911.09211</a> <span> [<a href="https://arxiv.org/pdf/1911.09211">pdf</a>, <a href="https://arxiv.org/format/1911.09211">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/10.3847/1538-3881/ab5a8a">10.3847/1538-3881/ab5a8a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detecting and Characterizing Water Vapor in the Atmospheres of Earth Analogs through Observation of the 0.94 Micron Feature in Reflected Light </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Smith%2C+A+J+R+W">Adam J. R. W. Smith</a>, <a href="/search/?searchtype=author&query=Feng%2C+Y+K">Y. Katherina Feng</a>, <a href="/search/?searchtype=author&query=Fortney%2C+J+J">Jonathan J. Fortney</a>, <a href="/search/?searchtype=author&query=Robinson%2C+T+D">Tyler D. Robinson</a>, <a href="/search/?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Lewis%2C+N+K">Nikole K. Lewis</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1911.09211v1-abstract-short" style="display: inline;"> The characterization of rocky, Earth-like planets is an important goal for future large ground- and space-based telescopes. In support of developing an efficient observational strategy, we have applied Bayesian statistical inference to interpret the albedo spectrum of cloudy true-Earth analogs that include a diverse spread in their atmospheric water vapor mixing ratios. We focus on detecting water… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.09211v1-abstract-full').style.display = 'inline'; document.getElementById('1911.09211v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.09211v1-abstract-full" style="display: none;"> The characterization of rocky, Earth-like planets is an important goal for future large ground- and space-based telescopes. In support of developing an efficient observational strategy, we have applied Bayesian statistical inference to interpret the albedo spectrum of cloudy true-Earth analogs that include a diverse spread in their atmospheric water vapor mixing ratios. We focus on detecting water-bearing worlds by characterizing their atmospheric water vapor content via the strong 0.94$\,渭$m H$_2$O absorption feature, with several observational configurations. Water vapor is an essential signpost when assessing planetary habitability, and determining its presence is important in vetting whether planets are suitable for hosting life. We find that R=140 spectroscopy of the absorption feature combined with a same-phase green optical photometric point at $0.525-0.575\,渭$m is capable of distinguishing worlds with less than $0.1\times$ Earth-like water vapor levels from worlds with $1\times$ Earth-like levels or greater at a signal-to-noise ratio of 5 or better with $2蟽$ confidence. This configuration can differentiate between $0.01\times$ and $0.1\times$ Earth-like levels when the signal-to-noise ratio is 10 or better at the same confidence. However, strong constraints on the water vapor mixing ratio remained elusive with this configuration even at signal-to-noise of 15. We find that adding the same-phase optical photometric point does not significantly help characterize the H$_2$O mixing ratio, but does enable an upper limit on atmospheric ozone levels. Finally, we find that a 0.94$\,渭$m photometric point, instead of spectroscopy, combined with the green-optical point, fails to produce meaningful information about atmospheric water content. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.09211v1-abstract-full').style.display = 'none'; document.getElementById('1911.09211v1-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.00025">arXiv:1904.00025</a> <span> [<a href="https://arxiv.org/pdf/1904.00025">pdf</a>, <a href="https://arxiv.org/format/1904.00025">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/ab2a10">10.3847/2041-8213/ab2a10 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring A Photospheric Radius Correction to Model Secondary Eclipse Spectra for Transiting Exoplanets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fortney%2C+J+J">Jonathan J. Fortney</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Morley%2C+C+V">Caroline V. Morley</a>, <a href="/search/?searchtype=author&query=Freedman%2C+R+S">Richard S. Freedman</a>, <a href="/search/?searchtype=author&query=Hood%2C+C">Callie Hood</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.00025v1-abstract-short" style="display: inline;"> We highlight a physical effect that is often not considered that impacts the calculation of model spectra of planets at secondary eclipse, affecting both emission and reflection spectra. The radius of the emitting surface of the planet is not merely one value measured from a transit light curve, but is itself a function of wavelength, yet it is not directly measurable. At high precision, a similar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.00025v1-abstract-full').style.display = 'inline'; document.getElementById('1904.00025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.00025v1-abstract-full" style="display: none;"> We highlight a physical effect that is often not considered that impacts the calculation of model spectra of planets at secondary eclipse, affecting both emission and reflection spectra. The radius of the emitting surface of the planet is not merely one value measured from a transit light curve, but is itself a function of wavelength, yet it is not directly measurable. At high precision, a similar effect is well-known in transit "transmission spectroscopy" but this related effect also impacts emission and reflection. As is well-appreciated, the photospheric radius can vary across $\sim$4-8 atmospheric scale heights, depending on atmospheric opacity and spectral resolution. This effect leads to a decreased weighting in model calculations at wavelengths where atmospheric opacity is low, and one sees more deeply into the atmosphere, to a smaller radius. The overall effect serves to mute emission spectra features for atmospheres with no thermal inversion but to enhance features for atmospheres with a thermal inversion. While this effect can be ignored for current \emph{Hubble} observations, it can lead to wavelength-dependent 10-20\% changes in planet-to-star flux ratios in the infrared at $R\sim~200-1000$ (readily achievable for JWST) for low-gravity hot Jupiters, although values of 5\% are more typical for the population. The effect is mostly controlled by the ratio of the atmospheric scale height to the planet radius, and can be important at any planetary temperature. Of known planets, the effect is largest for the cool "super-puffs" at very low surface gravity, where it can alter calculated flux ratios by over 100\%. We discuss complexities of including this photospheric radius effect in 1D and 3D atmosphere models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.00025v1-abstract-full').style.display = 'none'; document.getElementById('1904.00025v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 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">Submitted to ApJ Letters, revised to reflect referee comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.02011">arXiv:1808.02011</a> <span> [<a href="https://arxiv.org/pdf/1808.02011">pdf</a>, <a href="https://arxiv.org/format/1808.02011">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/ab2598">10.3847/1538-4357/ab2598 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Effect of 3D Transport-Induced Disequilibrium Carbon Chemistry on the Atmospheric Structure and Phase Curves and Emission Spectra of Hot Jupiter HD 189733b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Steinrueck%2C+M+E">Maria E Steinrueck</a>, <a href="/search/?searchtype=author&query=Parmentier%2C+V">Vivien Parmentier</a>, <a href="/search/?searchtype=author&query=Showman%2C+A+P">Adam P Showman</a>, <a href="/search/?searchtype=author&query=Lothringer%2C+J+D">Joshua D Lothringer</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E Lupu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1808.02011v2-abstract-short" style="display: inline;"> On hot Jupiter exoplanets, strong horizontal and vertical winds should homogenize the abundances of the important absorbers CH$_4$ and CO much faster than chemical reactions restore chemical equilibrium. This effect, typically neglected in general circulation models (GCMs), has been suggested as explanation for discrepancies between observed infrared lightcurves and those predicted by GCMs: On the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02011v2-abstract-full').style.display = 'inline'; document.getElementById('1808.02011v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.02011v2-abstract-full" style="display: none;"> On hot Jupiter exoplanets, strong horizontal and vertical winds should homogenize the abundances of the important absorbers CH$_4$ and CO much faster than chemical reactions restore chemical equilibrium. This effect, typically neglected in general circulation models (GCMs), has been suggested as explanation for discrepancies between observed infrared lightcurves and those predicted by GCMs: On the nightsides of several hot Jupiters, GCMs predict outgoing fluxes that are too large, especially in the Spitzer 4.5 $渭$m band. We modified the SPARC/MITgcm to include disequilibrium abundances of CH$_4$, CO and H$_2$O by assuming that the CH$_4$/CO ratio is constant throughout the simulation domain. We ran simulations of hot Jupiter HD 189733b with 8 CH$_4$/CO ratios. In the more likely CO-dominated regime, we find temperature changes $\geq$50-100 K compared to the equilibrium chemistry case across large regions. This effect is large enough to affect predicted emission spectra and should thus be included in GCMs of hot Jupiters with equilibrium temperatures between 600K and 1300K. We find that spectra in regions with strong methane absorption, including the Spitzer 3.6 and 8 $渭$m bands, are strongly impacted by disequilibrium abundances. We expect chemical quenching to result in much larger nightside fluxes in the 3.6 $渭$m band, in stark contrast to observations. Meanwhile, we find almost no effect on predicted observations in the 4.5 $渭$m band, as the opacity changes due to CO and H$_2$O offset each other. We thus conclude that disequilibrium carbon chemistry cannot explain the observed low nightside fluxes in the 4.5 $渭$m band. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02011v2-abstract-full').style.display = 'none'; document.getElementById('1808.02011v2-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 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 12 figures; accepted for publication in ApJ. Key changes since v1: updated introduction and discussion to include recent literature more thoroughly; added paragraph and figure to clarify change in water abundance; ran simulations for additional 600 days simulation time (leading to small quantitative changes in some figures but no qualitative 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/1803.06403">arXiv:1803.06403</a> <span> [<a href="https://arxiv.org/pdf/1803.06403">pdf</a>, <a href="https://arxiv.org/format/1803.06403">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/10.3847/1538-3881/aab95c">10.3847/1538-3881/aab95c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterizing Earth Analogs in Reflected Light: Atmospheric Retrieval Studies for Future Space Telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Feng%2C+Y+K">Y. Katherina Feng</a>, <a href="/search/?searchtype=author&query=Robinson%2C+T+D">Tyler D. Robinson</a>, <a href="/search/?searchtype=author&query=Fortney%2C+J+J">Jonathan J. Fortney</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/?searchtype=author&query=Lewis%2C+N+K">Nikole K. Lewis</a>, <a href="/search/?searchtype=author&query=Macintosh%2C+B">Bruce Macintosh</a>, <a href="/search/?searchtype=author&query=Line%2C+M+R">Michael R. Line</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="1803.06403v1-abstract-short" style="display: inline;"> Space-based high contrast imaging mission concepts for studying rocky exoplanets in reflected light are currently under community study. We develop an inverse modeling framework to estimate the science return of such missions given different instrument design considerations. By combining an exoplanet albedo model, an instrument noise model, and an ensemble Markov chain Monte Carlo sampler, we expl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.06403v1-abstract-full').style.display = 'inline'; document.getElementById('1803.06403v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.06403v1-abstract-full" style="display: none;"> Space-based high contrast imaging mission concepts for studying rocky exoplanets in reflected light are currently under community study. We develop an inverse modeling framework to estimate the science return of such missions given different instrument design considerations. By combining an exoplanet albedo model, an instrument noise model, and an ensemble Markov chain Monte Carlo sampler, we explore retrievals of atmospheric and planetary properties for Earth twins as a function of signal-to-noise ratio (SNR) and resolution ($R$). Our forward model includes Rayleigh scattering, single-layer water clouds with patchy coverage, and pressure-dependent absorption due to water vapor, oxygen, and ozone. We simulate data at $R = 70$ and $R = 140$ from 0.4-1.0 $渭$m with SNR $ = 5, 10, 15, 20$ at 550 nm (i.e., for HabEx/LUVOIR-type instruments). At these same SNR, we simulate data for WFIRST paired with a starshade, which includes two photometric points between 0.48-0.6 $渭$m and $R = 50$ spectroscopy from 0.6-0.97 $渭$m. Given our noise model for WFIRST-type detectors, we find that weak detections of water vapor, ozone, and oxygen can be achieved with observations with at least $R = 70$ / SNR$\ = 15$, or $R = 140$ / SNR$\ = 10$ for improved detections. Meaningful constraints are only achieved with $R = 140$ / SNR$\ = 20$ data. The WFIRST data offer limited diagnostic information, needing at least SNR = 20 to weakly detect gases. Most scenarios place limits on planetary radius, but cannot constrain surface gravity and, thus, planetary mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.06403v1-abstract-full').style.display = 'none'; document.getElementById('1803.06403v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Resubmitted to AAS Journals after incorporating reviewer feedback. 26 pages, 18 figure, 9 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/1801.01144">arXiv:1801.01144</a> <span> [<a href="https://arxiv.org/pdf/1801.01144">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/aaa549">10.3847/1538-4357/aaa549 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct detection and characterization of M-dwarf planets using light echoes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</a>, <a href="/search/?searchtype=author&query=White%2C+R+L">Richard L. White</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Ford%2C+H+C">Holland C. Ford</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="1801.01144v1-abstract-short" style="display: inline;"> Exoplanets orbiting M dwarf stars are a prime target in the search for life in the Universe. M dwarf stars are active, with powerful flares that could adversely impact prospects for life, though there are counter-arguments. Here, we turn flaring to advantage and describe ways in which it can be used to enhance the detectability of planets, in the absence of transits or a coronagraph, significantly… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.01144v1-abstract-full').style.display = 'inline'; document.getElementById('1801.01144v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.01144v1-abstract-full" style="display: none;"> Exoplanets orbiting M dwarf stars are a prime target in the search for life in the Universe. M dwarf stars are active, with powerful flares that could adversely impact prospects for life, though there are counter-arguments. Here, we turn flaring to advantage and describe ways in which it can be used to enhance the detectability of planets, in the absence of transits or a coronagraph, significantly expanding the accessible discovery and characterization space. Flares produce brief bursts of intense luminosity, after which the star dims. Due to the light travel time between the star and planet, the planet receives the high intensity pulse, which it re-emits through scattering (a light echo) or intrinsic emission when the star is much fainter, thereby increasing the planet's detectability. The planet's light echo emission can potentially be discriminated from that of the host star by means of a time delay, Doppler shift, spatial shift, and polarization, each of which can improve the contrast of the planet to the star. Scattered light can reveal the albedo spectrum of the planet to within a size scale factor, and is likely to be polarized. Intrinsic emission mechanisms include fluorescent pumping of multiple molecular hydrogen and neutral oxygen lines by intense LyAlpha and LyBeta flare emission, recombination radiation of ionized and photodissociated species, and atmospheric processes such as terrestrial upper atmosphere airglow and near infrared hydroxyl emission. We discuss the feasibility of detecting light echoes and find that under favorable circumstances, echo detection is possible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.01144v1-abstract-full').style.display = 'none'; document.getElementById('1801.01144v1-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 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.04734">arXiv:1612.04734</a> <span> [<a href="https://arxiv.org/pdf/1612.04734">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/1.JATIS.3.3.036002">10.1117/1.JATIS.3.3.036002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High Efficiency UV/Optical/NIR Detectors for Large Aperture Telescopes and UV Explorer Missions: Development of and Field Observations with Delta-doped Arrays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nikzad%2C+S">Shouleh Nikzad</a>, <a href="/search/?searchtype=author&query=Jewell%2C+A+D">April D. Jewell</a>, <a href="/search/?searchtype=author&query=Hoenk%2C+M+E">Michael E. Hoenk</a>, <a href="/search/?searchtype=author&query=Jones%2C+T">Todd Jones</a>, <a href="/search/?searchtype=author&query=Hennessy%2C+J">John Hennessy</a>, <a href="/search/?searchtype=author&query=Goodsall%2C+T">Tim Goodsall</a>, <a href="/search/?searchtype=author&query=Carver%2C+A">Alexander Carver</a>, <a href="/search/?searchtype=author&query=Shapiro%2C+C">Charles Shapiro</a>, <a href="/search/?searchtype=author&query=Cheng%2C+S+R">Samuel R. Cheng</a>, <a href="/search/?searchtype=author&query=Hamden%2C+E">Erika Hamden</a>, <a href="/search/?searchtype=author&query=Kyne%2C+G">Gillian Kyne</a>, <a href="/search/?searchtype=author&query=Martin%2C+D+C">D. Christopher Martin</a>, <a href="/search/?searchtype=author&query=Schiminovich%2C+D">David Schiminovich</a>, <a href="/search/?searchtype=author&query=Scowen%2C+P">Paul Scowen</a>, <a href="/search/?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S">Stephan McCandliss</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</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="1612.04734v2-abstract-short" style="display: inline;"> A number of exciting concepts are under development for Flagship, Probe class, Explorer class, and Suborbital class NASA missions in the ultraviolet/optical spectral ranges. These missions will depend on high performance silicon detector arrays being delivered affordably and in high numbers. In a focused effort we have advanced delta-doping technology to high throughput and high yield wafer-scale… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.04734v2-abstract-full').style.display = 'inline'; document.getElementById('1612.04734v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.04734v2-abstract-full" style="display: none;"> A number of exciting concepts are under development for Flagship, Probe class, Explorer class, and Suborbital class NASA missions in the ultraviolet/optical spectral ranges. These missions will depend on high performance silicon detector arrays being delivered affordably and in high numbers. In a focused effort we have advanced delta-doping technology to high throughput and high yield wafer-scale processing, encompassing a multitude of state-of-the-art silicon-based detector formats and designs. As part of this technology advancement and in preparation for upcoming missions, we have embarked on a number of field observations, instrument integrations, and independent evaluations of delta-doped arrays. In this paper, we present recent data and innovations from the Advanced Detectors and Systems program at JPL, including two-dimensional doping technology; our end-to-end post-fabrication processing of high performance UV/Optical/NIR arrays; and advanced coatings for detectors and optical elements. Additionally, we present examples of past, in-progress, and planned observations and deployments of delta-doped arrays. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.04734v2-abstract-full').style.display = 'none'; document.getElementById('1612.04734v2-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 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">submitted to JATIS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.03871">arXiv:1611.03871</a> <span> [<a href="https://arxiv.org/pdf/1611.03871">pdf</a>, <a href="https://arxiv.org/ps/1611.03871">ps</a>, <a href="https://arxiv.org/format/1611.03871">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1538-3873/aa61ef">10.1088/1538-3873/aa61ef <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exo-Transmit: An Open-Source Code for Calculating Transmission Spectra for Exoplanet Atmospheres of Varied Composition </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kempton%2C+E+M+-">Eliza M. -R. Kempton</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Owusu-Asare%2C+A">Albert Owusu-Asare</a>, <a href="/search/?searchtype=author&query=Slough%2C+P">Patrick Slough</a>, <a href="/search/?searchtype=author&query=Cale%2C+B">Bryson Cale</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1611.03871v1-abstract-short" style="display: inline;"> We present Exo-Transmit, a software package to calculate exoplanet transmission spectra for planets of varied composition. The code is designed to generate spectra of planets with a wide range of atmospheric composition, temperature, surface gravity, and size, and is therefore applicable to exoplanets ranging in mass and size from hot Jupiters down to rocky super-Earths. Spectra can be generated w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.03871v1-abstract-full').style.display = 'inline'; document.getElementById('1611.03871v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.03871v1-abstract-full" style="display: none;"> We present Exo-Transmit, a software package to calculate exoplanet transmission spectra for planets of varied composition. The code is designed to generate spectra of planets with a wide range of atmospheric composition, temperature, surface gravity, and size, and is therefore applicable to exoplanets ranging in mass and size from hot Jupiters down to rocky super-Earths. Spectra can be generated with or without clouds or hazes with options to (1) include an optically thick cloud deck at a user-specified atmospheric pressure or (2) to augment the nominal Rayleigh scattering by a user-specified factor. The Exo-Transmit code is written in C and is extremely easy to use. Typically the user will only need to edit parameters in a single user input file in order to run the code for a planet of their choosing. Exo-Transmit is available publicly on Github with open-source licensing at https://github.com/elizakempton/Exo_Transmit . <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.03871v1-abstract-full').style.display = 'none'; document.getElementById('1611.03871v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 7 figures, 1 table, submitted to PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.07424">arXiv:1604.07424</a> <span> [<a href="https://arxiv.org/pdf/1604.07424">pdf</a>, <a href="https://arxiv.org/ps/1604.07424">ps</a>, <a href="https://arxiv.org/format/1604.07424">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/10.3847/2041-8205/824/2/L25">10.3847/2041-8205/824/2/L25 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hunt for Planet Nine: Atmosphere, Spectra, Evolution, and Detectability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fortney%2C+J+J">Jonathan J. Fortney</a>, <a href="/search/?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/?searchtype=author&query=Laughlin%2C+G">Gregory Laughlin</a>, <a href="/search/?searchtype=author&query=Nettelmann%2C+N">Nadine Nettelmann</a>, <a href="/search/?searchtype=author&query=Morley%2C+C+V">Caroline V. Morley</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Visscher%2C+C">Channon Visscher</a>, <a href="/search/?searchtype=author&query=Jeremic%2C+P">Pavle Jeremic</a>, <a href="/search/?searchtype=author&query=Khadder%2C+W+G">Wade G. Khadder</a>, <a href="/search/?searchtype=author&query=Hargrave%2C+M">Mason Hargrave</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="1604.07424v2-abstract-short" style="display: inline;"> We investigate the physical characteristics of the Solar System's proposed Planet Nine using modeling tools with a heritage in studying Uranus and Neptune. For a range of plausible masses and interior structures, we find upper limits on the intrinsic Teff, from ~35-50 K for masses of 5-20 M_Earth, and we also explore lower Teff values. Possible planetary radii could readily span from 3 to 6 R_Eart… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.07424v2-abstract-full').style.display = 'inline'; document.getElementById('1604.07424v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.07424v2-abstract-full" style="display: none;"> We investigate the physical characteristics of the Solar System's proposed Planet Nine using modeling tools with a heritage in studying Uranus and Neptune. For a range of plausible masses and interior structures, we find upper limits on the intrinsic Teff, from ~35-50 K for masses of 5-20 M_Earth, and we also explore lower Teff values. Possible planetary radii could readily span from 3 to 6 R_Earth depending on the mass fraction of any H/He envelope. Given its cold temperature, the planet encounters significant methane condensation, which dramatically alters the atmosphere away from simple Neptune-like expectations. We find the atmosphere is strongly depleted in molecular absorption at visible wavelengths, suggesting a Rayleigh scattering atmosphere with a high geometric albedo approaching 0.75. We highlight two diagnostics for the atmosphere's temperature structure, the first being the value of the methane mixing ratio above the methane cloud. The second is the wavelength at which cloud scattering can be seen, which yields the cloud-top pressure. Surface reflection may be seen if the atmosphere is thin. Due to collision-induced opacity of H2 in the infrared, the planet would be extremely blue (instead of red) in the shortest wavelength WISE colors if methane is depleted, and would, in some cases, exist on the verge of detectability by WISE. For a range of models, thermal fluxes from ~3-5 microns are ~20 orders of magnitude larger than blackbody expectations. We report a search of the AllWISE Source Catalog for Planet Nine, but find no detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.07424v2-abstract-full').style.display = 'none'; document.getElementById('1604.07424v2-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">v1</span> submitted 25 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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 to ApJ Letters, with minor changes from the submitted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.05370">arXiv:1604.05370</a> <span> [<a href="https://arxiv.org/pdf/1604.05370">pdf</a>, <a href="https://arxiv.org/format/1604.05370">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0004-6256/152/6/217">10.3847/0004-6256/152/6/217 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Developing Atmospheric Retrieval Methods for Direct Imaging Spectroscopy of Gas Giants in Reflected Light I: Methane Abundances and Basic Cloud Properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/?searchtype=author&query=Lewis%2C+N">Nikole Lewis</a>, <a href="/search/?searchtype=author&query=Line%2C+M">Michael Line</a>, <a href="/search/?searchtype=author&query=Traub%2C+W+A">Wesley A. Traub</a>, <a href="/search/?searchtype=author&query=Zahnle%2C+K">Kevin Zahnle</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="1604.05370v2-abstract-short" style="display: inline;"> Upcoming space-based coronagraphic instruments in the next decade will perform reflected light spectroscopy and photometry of cool, directly imaged extrasolar giant planets. We are developing a new atmospheric retrieval methodology to help assess the science return and inform the instrument design for such future missions, and ultimately interpret the resulting observations. Our retrieval techniqu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.05370v2-abstract-full').style.display = 'inline'; document.getElementById('1604.05370v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.05370v2-abstract-full" style="display: none;"> Upcoming space-based coronagraphic instruments in the next decade will perform reflected light spectroscopy and photometry of cool, directly imaged extrasolar giant planets. We are developing a new atmospheric retrieval methodology to help assess the science return and inform the instrument design for such future missions, and ultimately interpret the resulting observations. Our retrieval technique employs a geometric albedo model coupled with both a Markov chain Monte Carlo Ensemble Sampler (emcee) and a multimodal nested sampling algorithm (MultiNest) to map the posterior distribution. This combination makes the global evidence calculation more robust for any given model, and highlights possible discrepancies in the likelihood maps. As a proof-of-concept, our current atmospheric model contains 1 or 2 cloud layers, methane as a major absorber, and a H$_2$-He background gas. This 6-to-9 parameter model is appropriate for Jupiter-like planets and can be easily expanded in the future. In addition to deriving the marginal likelihood distribution and confidence intervals for the model parameters, we perform model selection to determine the significance of methane and cloud detection as a function of expected signal-to-noise in the presence of spectral noise correlations. After internal validation, the method is applied to realistic spectra of Jupiter, Saturn, and HD 99492 c, a model observing target. We find that the presence or absence of clouds and methane can be determined with high confidence, while parameter uncertainties are model-dependent and correlated. Such general methods will also be applicable to the interpretation of direct imaging spectra of cloudy terrestrial planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.05370v2-abstract-full').style.display = 'none'; document.getElementById('1604.05370v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">37 pages, 30 figures, accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.0026">arXiv:1409.0026</a> <span> [<a href="https://arxiv.org/pdf/1409.0026">pdf</a>, <a href="https://arxiv.org/ps/1409.0026">ps</a>, <a href="https://arxiv.org/format/1409.0026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0067-0049/214/2/25">10.1088/0067-0049/214/2/25 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaseous Mean Opacities for Giant Planet and Ultracool Dwarf Atmospheres over a Range of Metallicities and Temperatures </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Freedman%2C+R+S">Richard S. Freedman</a>, <a href="/search/?searchtype=author&query=Lustig-Yaeger%2C+J">Jacob Lustig-Yaeger</a>, <a href="/search/?searchtype=author&query=Fortney%2C+J+J">Jonathan J. Fortney</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/?searchtype=author&query=Lodders%2C+K">Katharina Lodders</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="1409.0026v2-abstract-short" style="display: inline;"> We present new calculations of Rosseland and Planck gaseous mean opacities relevant to the atmospheres of giant planets and ultracool dwarfs. Such calculations are used in modeling the atmospheres, interiors, formation, and evolution of these objects. Our calculations are an expansion of those presented in Freedman et al. (2008) to include lower pressures, finer temperature resolution, and also th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.0026v2-abstract-full').style.display = 'inline'; document.getElementById('1409.0026v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.0026v2-abstract-full" style="display: none;"> We present new calculations of Rosseland and Planck gaseous mean opacities relevant to the atmospheres of giant planets and ultracool dwarfs. Such calculations are used in modeling the atmospheres, interiors, formation, and evolution of these objects. Our calculations are an expansion of those presented in Freedman et al. (2008) to include lower pressures, finer temperature resolution, and also the higher metallicities most relevant for giant planet atmospheres. Calculations span 1 microbar to 300 bar, and 75 K to 4000 K, in a nearly square grid. Opacities at metallicities from solar to 50 times solar abundances are calculated. We also provide an analytic fit to the Rosseland mean opacities over the grid in pressure, temperature, and metallicity. In addition to computing mean opacities at these local temperatures, we also calculate them with weighting functions up to 7000 K, to simulate the mean opacities for incident stellar intensities, rather than locally thermally emitted intensities. The chemical equilibrium calculations account for the settling of condensates in a gravitational field and are applicable to cloud-free giant planet and ultracool dwarf atmospheres, but not circumstellar disks. We provide our extensive opacity tables for public use. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.0026v2-abstract-full').style.display = 'none'; document.getElementById('1409.0026v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">This version fixes a units description error that was only in the arxiv version, but is correct in the ApJS version. In equations 4 and 5 pressure is in dyne/cm2. Online tables available at the ApJS website: https://iopscience.iop.org/article/10.1088/0067-0049/214/2/25</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.4859">arXiv:1406.4859</a> <span> [<a href="https://arxiv.org/pdf/1406.4859">pdf</a>, <a href="https://arxiv.org/ps/1406.4859">ps</a>, <a href="https://arxiv.org/format/1406.4859">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201424410">10.1051/0004-6361/201424410 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Herschel-ATLAS and ALMA: HATLAS J142935.3-002836, a lensed major merger at redshift 1.027 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Messias%2C+H">Hugo Messias</a>, <a href="/search/?searchtype=author&query=Dye%2C+S">Simon Dye</a>, <a href="/search/?searchtype=author&query=Nagar%2C+N">Neil Nagar</a>, <a href="/search/?searchtype=author&query=Orellana%2C+G">Gustavo Orellana</a>, <a href="/search/?searchtype=author&query=Bussmann%2C+R+S">R. Shane Bussmann</a>, <a href="/search/?searchtype=author&query=Calanog%2C+J">Jae Calanog</a>, <a href="/search/?searchtype=author&query=Dannerbauer%2C+H">Helmut Dannerbauer</a>, <a href="/search/?searchtype=author&query=Fu%2C+H">Hai Fu</a>, <a href="/search/?searchtype=author&query=Ibar%2C+E">Edo Ibar</a>, <a href="/search/?searchtype=author&query=Inohara%2C+A">Andrew Inohara</a>, <a href="/search/?searchtype=author&query=Ivison%2C+R+J">R. J. Ivison</a>, <a href="/search/?searchtype=author&query=Negrello%2C+M">Mattia Negrello</a>, <a href="/search/?searchtype=author&query=Riechers%2C+D+A">Dominik A. Riechers</a>, <a href="/search/?searchtype=author&query=Sheen%2C+Y">Yun-Kyeong Sheen</a>, <a href="/search/?searchtype=author&query=Amber%2C+S">Simon Amber</a>, <a href="/search/?searchtype=author&query=Birkinshaw%2C+M">Mark Birkinshaw</a>, <a href="/search/?searchtype=author&query=Bourne%2C+N">Nathan Bourne</a>, <a href="/search/?searchtype=author&query=Clements%2C+D+L">Dave L. Clements</a>, <a href="/search/?searchtype=author&query=Cooray%2C+A">Asantha Cooray</a>, <a href="/search/?searchtype=author&query=De+Zotti%2C+G">Gianfranco De Zotti</a>, <a href="/search/?searchtype=author&query=Demarco%2C+R">Ricardo Demarco</a>, <a href="/search/?searchtype=author&query=Dunne%2C+L">Loretta Dunne</a>, <a href="/search/?searchtype=author&query=Eales%2C+S">Stephen Eales</a>, <a href="/search/?searchtype=author&query=Fleuren%2C+S">Simone Fleuren</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1406.4859v1-abstract-short" style="display: inline;"> [Abridged] Aims: This work focuses on one lensed system, HATLAS J142935.3-002836 (H1429-0028), selected in the Herschel-ATLAS field. Gathering a rich, multi-wavelength dataset, we aim to confirm the lensing hypothesis and model the background source's morphology and dynamics, as well as to provide a full physical characterisation. Methods: Multi-wavelength high-resolution data is utilised to asses… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.4859v1-abstract-full').style.display = 'inline'; document.getElementById('1406.4859v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.4859v1-abstract-full" style="display: none;"> [Abridged] Aims: This work focuses on one lensed system, HATLAS J142935.3-002836 (H1429-0028), selected in the Herschel-ATLAS field. Gathering a rich, multi-wavelength dataset, we aim to confirm the lensing hypothesis and model the background source's morphology and dynamics, as well as to provide a full physical characterisation. Methods: Multi-wavelength high-resolution data is utilised to assess the nature of the system. A lensing-analysis algorithm which simultaneously fits different wavebands is adopted to characterise the lens. The background galaxy dynamical information is studied by reconstructing the 3-D source-plane of the ALMA CO(J:4-3) transition. Near-IR imaging from HST and Keck-AO allows to constrain rest-frame optical photometry independently for the foreground and background systems. Physical parameters (such as stellar and dust masses) are estimated via modelling of the spectral energy distribution taking into account source blending, foreground obscuration, and differential magnification. Results: The system comprises a foreground edge-on disk galaxy (at z_sp=0.218) with an almost complete Einstein ring around it. The background source (at z_sp=1.027) is magnified by a factor of ~8-10 depending on wavelength. It is comprised of two components and a tens of kpc long tidal tail resembling the Antennae merger. As a whole, the system is a massive stellar system (1.32[-0.41,+0.63] x1E11 Mo) forming stars at a rate of 394+-90 Mo/yr, and has a significant gas reservoir M_ISM = 4.6+-1.7 x1E10 Mo. Its depletion time due to star formation alone is thus expected to be tau_SF=M_ISM/SFR=117+-51 Myr. The dynamical mass of one of the components is estimated to be 5.8+-1.7 x1E10 Mo, and, together with the photometric total mass estimate, it implies that H1429-0028 is a major merger system (1:2.8[-1.5,+1.8]). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.4859v1-abstract-full').style.display = 'none'; document.getElementById('1406.4859v1-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 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">submitted to A&A, 20 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 568, A92 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.0210">arXiv:1406.0210</a> <span> [<a href="https://arxiv.org/pdf/1406.0210">pdf</a>, <a href="https://arxiv.org/ps/1406.0210">ps</a>, <a href="https://arxiv.org/format/1406.0210">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Cloud structure of brown dwarfs from spectroscopic variability observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Buenzli%2C+E">Esther Buenzli</a>, <a href="/search/?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/?searchtype=author&query=Apai%2C+D">Daniel Apai</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</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="1406.0210v1-abstract-short" style="display: inline;"> Recent discoveries of variable brown dwarfs have provided us with a new window into their three-dimensional cloud structure. The highest variables are found at the L/T transition, where the cloud cover is thought to break up, but variability has been found to occur also for both cloudy L dwarfs and (mostly) cloud-free mid T dwarfs. We summarize results from recent HST programs measuring the spectr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.0210v1-abstract-full').style.display = 'inline'; document.getElementById('1406.0210v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.0210v1-abstract-full" style="display: none;"> Recent discoveries of variable brown dwarfs have provided us with a new window into their three-dimensional cloud structure. The highest variables are found at the L/T transition, where the cloud cover is thought to break up, but variability has been found to occur also for both cloudy L dwarfs and (mostly) cloud-free mid T dwarfs. We summarize results from recent HST programs measuring the spectral variability of brown dwarfs in the near-infrared and compare to results from ground-based programs. We discuss the patchy cloud structure of L/T transition objects, for which it is becoming increasingly certain that the variability does not arise from cloud holes into the deep hot regions but from varying cloud thickness. We present a new patchy cloud model to explain the spectral variability of 2MASSJ21392676+0220226. We also discuss the curious multi-wavelength variability behavior of the recently discovered very nearby early T dwarf WISE J104915.57-531906.1B (Luhman 16B) and the mid T dwarf 2MASS J22282889-431026. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.0210v1-abstract-full').style.display = 'none'; document.getElementById('1406.0210v1-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 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">4 pages, 1 figure, submitted to the proceedings of "Gaia and the unseen - the brown dwarf question", Torino, 24-26 March 2014, to be published in Memorie della Societa' Astronomica Italiana (SAIt), eds Ricky Smart, David Barrado, Jackie Faherty</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.1499">arXiv:1401.1499</a> <span> [<a href="https://arxiv.org/pdf/1401.1499">pdf</a>, <a href="https://arxiv.org/format/1401.1499">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/784/1/27">10.1088/0004-637X/784/1/27 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Atmospheres of Earth-like Planets after Giant Impact Events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lupu%2C+R+E">R. E. Lupu</a>, <a href="/search/?searchtype=author&query=Zahnle%2C+K">Kevin Zahnle</a>, <a href="/search/?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/?searchtype=author&query=Schaefer%2C+L">Laura Schaefer</a>, <a href="/search/?searchtype=author&query=Fegley%2C+B">Bruce Fegley</a>, <a href="/search/?searchtype=author&query=Morley%2C+C">Caroline Morley</a>, <a href="/search/?searchtype=author&query=Cahoy%2C+K">Kerri Cahoy</a>, <a href="/search/?searchtype=author&query=Freedman%2C+R">Richard Freedman</a>, <a href="/search/?searchtype=author&query=Fortney%2C+J+J">Jonathan J. Fortney</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="1401.1499v1-abstract-short" style="display: inline;"> It is now understood that the accretion of terrestrial planets naturally involves giant collisions, the moon-forming impact being a well known example. In the aftermath of such collisions the surface of the surviving planet is very hot and potentially detectable. Here we explore the atmospheric chemistry, photochemistry, and spectral signatures of post-giant-impact terrestrial planets enveloped by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.1499v1-abstract-full').style.display = 'inline'; document.getElementById('1401.1499v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.1499v1-abstract-full" style="display: none;"> It is now understood that the accretion of terrestrial planets naturally involves giant collisions, the moon-forming impact being a well known example. In the aftermath of such collisions the surface of the surviving planet is very hot and potentially detectable. Here we explore the atmospheric chemistry, photochemistry, and spectral signatures of post-giant-impact terrestrial planets enveloped by thick atmospheres consisting predominantly of CO2, and H2O. The atmospheric chemistry and structure are computed self-consistently for atmospheres in equilibrium with hot surfaces with composition reflecting either the bulk silicate Earth (which includes the crust, mantle, atmosphere and oceans) or Earth's continental crust. We account for all major molecular and atomic opacity sources including collision-induced absorption. We find that these atmospheres are dominated by H2O and CO2, while the formation of CH4, and NH3 is quenched due to short dynamical timescales. Other important constituents are HF, HCl, NaCl, and SO2. These are apparent in the emerging spectra, and can be indicative that an impact has occurred. The use of comprehensive opacities results in spectra that are a factor of 2 lower in surface brightness in the spectral windows than predicted by previous models. The estimated luminosities show that the hottest post-giant-impact planets will be detectable with near-infrared coronagraphs on the planned 30m-class telescopes. The 1-4um region will be most favorable for such detections, offering bright features and better contrast between the planet and a potential debris disk. We derive cooling timescales on the order of 10^5-10^6 Myrs, based on the modeled effective temperatures. This leads to the possibility of discovering tens of such planets in future surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.1499v1-abstract-full').style.display = 'none'; document.getElementById('1401.1499v1-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, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">51 pages, 16 figures, preprint format; ApJ submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.3275">arXiv:1309.3275</a> <span> [<a href="https://arxiv.org/pdf/1309.3275">pdf</a>, <a href="https://arxiv.org/format/1309.3275">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> </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/779/1/67">10.1088/0004-637X/779/1/67 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SPT 0538-50: Physical conditions in the ISM of a strongly lensed dusty star-forming galaxy at z=2.8 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bothwell%2C+M+S">M. S. Bothwell</a>, <a href="/search/?searchtype=author&query=Aguirre%2C+J+E">J. E. Aguirre</a>, <a href="/search/?searchtype=author&query=Chapman%2C+S+C">S. C. Chapman</a>, <a href="/search/?searchtype=author&query=Marrone%2C+D+P">D. P. Marrone</a>, <a href="/search/?searchtype=author&query=Vieira%2C+J+D">J. D. Vieira</a>, <a href="/search/?searchtype=author&query=Ashby%2C+M+L+N">M. L. N. Ashby</a>, <a href="/search/?searchtype=author&query=Aravena%2C+M">M. Aravena</a>, <a href="/search/?searchtype=author&query=Benson%2C+B+A">B. A. Benson</a>, <a href="/search/?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/?searchtype=author&query=Bradford%2C+C+M">C. M. Bradford</a>, <a href="/search/?searchtype=author&query=Brodwin%2C+M">M. Brodwin</a>, <a href="/search/?searchtype=author&query=Carlstrom%2C+J">J. Carlstrom</a>, <a href="/search/?searchtype=author&query=Crawford%2C+T+M">T. M. Crawford</a>, <a href="/search/?searchtype=author&query=de+Breuck%2C+C">C. de Breuck</a>, <a href="/search/?searchtype=author&query=Downes%2C+T+P">T. P. Downes</a>, <a href="/search/?searchtype=author&query=Fassnacht%2C+C+D">C. D. Fassnacht</a>, <a href="/search/?searchtype=author&query=Gonzalez%2C+A+H">A. H. Gonzalez</a>, <a href="/search/?searchtype=author&query=Greve%2C+T+R">T. R. Greve</a>, <a href="/search/?searchtype=author&query=Gullberg%2C+B">B. Gullberg</a>, <a href="/search/?searchtype=author&query=Hezaveh%2C+Y">Y. Hezaveh</a>, <a href="/search/?searchtype=author&query=Holder%2C+G+P">G. P. Holder</a>, <a href="/search/?searchtype=author&query=Holzapfel%2C+W+L">W. L. Holzapfel</a>, <a href="/search/?searchtype=author&query=Ibar%2C+E">E. Ibar</a>, <a href="/search/?searchtype=author&query=Ivison%2C+R">R. Ivison</a>, <a href="/search/?searchtype=author&query=Kamenetzky%2C+J">J. Kamenetzky</a> , et al. (16 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="1309.3275v1-abstract-short" style="display: inline;"> We present observations of SPT-S J053816-5030.8, a gravitationally-lensed dusty star forming galaxy (DSFG) at z = 2.7817, first discovered at millimeter wavelengths by the South Pole Telescope. SPT 0538-50 is typical of the brightest sources found by wide-field millimeter-wavelength surveys, being lensed by an intervening galaxy at moderate redshift (in this instance, at z = 0.441). We present a w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.3275v1-abstract-full').style.display = 'inline'; document.getElementById('1309.3275v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.3275v1-abstract-full" style="display: none;"> We present observations of SPT-S J053816-5030.8, a gravitationally-lensed dusty star forming galaxy (DSFG) at z = 2.7817, first discovered at millimeter wavelengths by the South Pole Telescope. SPT 0538-50 is typical of the brightest sources found by wide-field millimeter-wavelength surveys, being lensed by an intervening galaxy at moderate redshift (in this instance, at z = 0.441). We present a wide array of multi-wavelength spectroscopic and photometric data on SPT 0538-50, including data from ALMA, Herschel PACS and SPIRE, Hubble, Spitzer, VLT, ATCA, APEX, and the SMA. We use high resolution imaging from HST to de-blend SPT 0538-50, separating DSFG emission from that of the foreground lens. Combined with a source model derived from ALMA imaging (which suggests a magnification factor of 21 +/- 4), we derive the intrinsic properties of SPT 0538-50, including the stellar mass, far-IR luminosity, star formation rate, molecular gas mass, and - using molecular line fluxes - the excitation conditions within the ISM. The derived physical properties argue that we are witnessing compact, merger-driven star formation in SPT 0538-50, similar to local starburst galaxies, and unlike that seen in some other DSFGs at this epoch. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.3275v1-abstract-full').style.display = 'none'; document.getElementById('1309.3275v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">16 pages, 11 figures. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1308.5681">arXiv:1308.5681</a> <span> [<a href="https://arxiv.org/pdf/1308.5681">pdf</a>, <a href="https://arxiv.org/ps/1308.5681">ps</a>, <a href="https://arxiv.org/format/1308.5681">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> </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/stt1369">10.1093/mnras/stt1369 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> H-ATLAS: estimating redshifts of Herschel sources from sub-mm fluxes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pearson%2C+E+A">E. A. Pearson</a>, <a href="/search/?searchtype=author&query=Eales%2C+S">S. Eales</a>, <a href="/search/?searchtype=author&query=Dunne%2C+L">L. Dunne</a>, <a href="/search/?searchtype=author&query=Nuevo%2C+J+G">J. Gonzalez Nuevo</a>, <a href="/search/?searchtype=author&query=Maddox%2C+S">S. Maddox</a>, <a href="/search/?searchtype=author&query=Aguirre%2C+J+E">J. E. Aguirre</a>, <a href="/search/?searchtype=author&query=Baes%2C+M">M. Baes</a>, <a href="/search/?searchtype=author&query=Baker%2C+A+J">A. J. Baker</a>, <a href="/search/?searchtype=author&query=Bourne%2C+N">N. Bourne</a>, <a href="/search/?searchtype=author&query=Bradford%2C+C+M">C. M. Bradford</a>, <a href="/search/?searchtype=author&query=Clark%2C+C+J+R">C. J. R. Clark</a>, <a href="/search/?searchtype=author&query=Cooray%2C+A">A. Cooray</a>, <a href="/search/?searchtype=author&query=Dariush%2C+A">A. Dariush</a>, <a href="/search/?searchtype=author&query=De+Zotti%2C+G">G. De Zotti</a>, <a href="/search/?searchtype=author&query=Dye%2C+S">S. Dye</a>, <a href="/search/?searchtype=author&query=Frayer%2C+D">D. Frayer</a>, <a href="/search/?searchtype=author&query=Gomez%2C+H+L">H. L. Gomez</a>, <a href="/search/?searchtype=author&query=Harris%2C+A+I">A. I. Harris</a>, <a href="/search/?searchtype=author&query=Hopwood%2C+R">R. Hopwood</a>, <a href="/search/?searchtype=author&query=Ibar%2C+E">E. Ibar</a>, <a href="/search/?searchtype=author&query=Ivison%2C+R+J">R. J. Ivison</a>, <a href="/search/?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a>, <a href="/search/?searchtype=author&query=Krips%2C+M">M. Krips</a>, <a href="/search/?searchtype=author&query=Lapi%2C+A">A. Lapi</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">R. E. Lupu</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1308.5681v1-abstract-short" style="display: inline;"> Upon its completion the Herschel ATLAS (H-ATLAS) will be the largest submillimetre survey to date, detecting close to half-a-million sources. It will only be possible to measure spectroscopic redshifts for a small fraction of these sources. However, if the rest-frame spectral energy distribution (SED) of a typical H-ATLAS source is known, this SED and the observed Herschel fluxes can be used to es… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.5681v1-abstract-full').style.display = 'inline'; document.getElementById('1308.5681v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1308.5681v1-abstract-full" style="display: none;"> Upon its completion the Herschel ATLAS (H-ATLAS) will be the largest submillimetre survey to date, detecting close to half-a-million sources. It will only be possible to measure spectroscopic redshifts for a small fraction of these sources. However, if the rest-frame spectral energy distribution (SED) of a typical H-ATLAS source is known, this SED and the observed Herschel fluxes can be used to estimate the redshifts of the H-ATLAS sources without spectroscopic redshifts. In this paper, we use a subset of 40 H-ATLAS sources with previously measured redshifts in the range 0.5<z<4.2 to derive a suitable average template for high redshift H-ATLAS sources. We find that a template with two dust components T_c = 23.9 K, T_h = 46.9 K and ratio of mass of cold dust to mass of warm dust of 30.1) provides a good fit to the rest-frame fluxes of the sources in our calibration sample. We use a jackknife technique to estimate the accuracy of the redshifts estimated with this template, finding a root mean square of Delta z/(1+z) = 0.26. For sources for which there is prior information that they lie at z > 1 we estimate that the rms of Delta z/(1+z) = 0.12. We have used this template to estimate the redshift distribution for the sources detected in the H-ATLAS equatorial fields, finding a bimodal distribution with a mean redshift of 1.2, 1.9 and 2.5 for 250, 350 and 500 um selected sources respectively. \end{abstract} <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.5681v1-abstract-full').style.display = 'none'; document.getElementById('1308.5681v1-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 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">13 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1304.4256">arXiv:1304.4256</a> <span> [<a href="https://arxiv.org/pdf/1304.4256">pdf</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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/nature12050">10.1038/nature12050 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Dust-Obscured Massive Maximum-Starburst Galaxy at a Redshift of 6.34 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Riechers%2C+D+A">Dominik A. Riechers</a>, <a href="/search/?searchtype=author&query=Bradford%2C+C+M">C. M. Bradford</a>, <a href="/search/?searchtype=author&query=Clements%2C+D+L">D. L. Clements</a>, <a href="/search/?searchtype=author&query=Dowell%2C+C+D">C. D. Dowell</a>, <a href="/search/?searchtype=author&query=Perez-Fournon%2C+I">I. Perez-Fournon</a>, <a href="/search/?searchtype=author&query=Ivison%2C+R+J">R. J. Ivison</a>, <a href="/search/?searchtype=author&query=Bridge%2C+C">C. Bridge</a>, <a href="/search/?searchtype=author&query=Conley%2C+A">A. Conley</a>, <a href="/search/?searchtype=author&query=Fu%2C+H">Hai Fu</a>, <a href="/search/?searchtype=author&query=Vieira%2C+J+D">J. D. Vieira</a>, <a href="/search/?searchtype=author&query=Wardlow%2C+J">J. Wardlow</a>, <a href="/search/?searchtype=author&query=Calanog%2C+J">J. Calanog</a>, <a href="/search/?searchtype=author&query=Cooray%2C+A">A. Cooray</a>, <a href="/search/?searchtype=author&query=Hurley%2C+P">P. Hurley</a>, <a href="/search/?searchtype=author&query=Neri%2C+R">R. Neri</a>, <a href="/search/?searchtype=author&query=Kamenetzky%2C+J">J. Kamenetzky</a>, <a href="/search/?searchtype=author&query=Aguirre%2C+J+E">J. E. Aguirre</a>, <a href="/search/?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/?searchtype=author&query=Arumugam%2C+V">V. Arumugam</a>, <a href="/search/?searchtype=author&query=Benford%2C+D+J">D. J. Benford</a>, <a href="/search/?searchtype=author&query=Bethermin%2C+M">M. Bethermin</a>, <a href="/search/?searchtype=author&query=Bock%2C+J">J. Bock</a>, <a href="/search/?searchtype=author&query=Burgarella%2C+D">D. Burgarella</a>, <a href="/search/?searchtype=author&query=Cabrera-Lavers%2C+A">A. Cabrera-Lavers</a>, <a href="/search/?searchtype=author&query=Chapman%2C+S+C">S. C. Chapman</a> , et al. (39 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="1304.4256v1-abstract-short" style="display: inline;"> Massive present-day early-type (elliptical and lenticular) galaxies probably gained the bulk of their stellar mass and heavy elements through intense, dust-enshrouded starbursts - that is, increased rates of star formation - in the most massive dark matter halos at early epochs. However, it remains unknown how soon after the Big Bang such massive starburst progenitors exist. The measured redshift… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.4256v1-abstract-full').style.display = 'inline'; document.getElementById('1304.4256v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1304.4256v1-abstract-full" style="display: none;"> Massive present-day early-type (elliptical and lenticular) galaxies probably gained the bulk of their stellar mass and heavy elements through intense, dust-enshrouded starbursts - that is, increased rates of star formation - in the most massive dark matter halos at early epochs. However, it remains unknown how soon after the Big Bang such massive starburst progenitors exist. The measured redshift distribution of dusty, massive starbursts has long been suspected to be biased low in redshift owing to selection effects, as confirmed by recent findings of systems out to redshift z~5. Here we report the identification of a massive starburst galaxy at redshift 6.34 through a submillimeter color-selection technique. We unambiguously determined the redshift from a suite of molecular and atomic fine structure cooling lines. These measurements reveal a hundred billion solar masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at least 40% of the baryonic mass. A "maximum starburst" converts the gas into stars at a rate more than 2,000 times that of the Milky Way, a rate among the highest observed at any epoch. Despite the overall downturn of cosmic star formation towards the highest redshifts, it seems that environments mature enough to form the most massive, intense starbursts existed at least as early as 880 million years after the Big Bang. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.4256v1-abstract-full').style.display = 'none'; document.getElementById('1304.4256v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">35 pages, 19 figures, 5 tables, including Supplementary Information (version formatted by the authors). To appear in Nature. Under press embargo until 18:00 London time/13:00 US Eastern Time on 17 April 2013</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature 496:329-333,2013 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1104.4115">arXiv:1104.4115</a> <span> [<a href="https://arxiv.org/pdf/1104.4115">pdf</a>, <a href="https://arxiv.org/ps/1104.4115">ps</a>, <a href="https://arxiv.org/format/1104.4115">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> </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/733/1/29">10.1088/0004-637X/733/1/29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Redshift Determination and CO Line Excitation Modeling for the Multiply-Lensed Galaxy HLSW-01 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Scott%2C+K+S">K. S. Scott</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">R. E. Lupu</a>, <a href="/search/?searchtype=author&query=Aguirre%2C+J+E">J. E. Aguirre</a>, <a href="/search/?searchtype=author&query=Auld%2C+R">R. Auld</a>, <a href="/search/?searchtype=author&query=Aussel%2C+H">H. Aussel</a>, <a href="/search/?searchtype=author&query=Baker%2C+A+J">A. J. Baker</a>, <a href="/search/?searchtype=author&query=Beelen%2C+A">A. Beelen</a>, <a href="/search/?searchtype=author&query=Bock%2C+J">J. Bock</a>, <a href="/search/?searchtype=author&query=Bradford%2C+C+M">C. M. Bradford</a>, <a href="/search/?searchtype=author&query=Brisbin%2C+D">D. Brisbin</a>, <a href="/search/?searchtype=author&query=Burgarella%2C+D">D. Burgarella</a>, <a href="/search/?searchtype=author&query=Carpenter%2C+J+M">J. M. Carpenter</a>, <a href="/search/?searchtype=author&query=Chanial%2C+P">P. Chanial</a>, <a href="/search/?searchtype=author&query=Chapman%2C+S+C">S. C. Chapman</a>, <a href="/search/?searchtype=author&query=Clements%2C+D+L">D. L. Clements</a>, <a href="/search/?searchtype=author&query=Conley%2C+A">A. Conley</a>, <a href="/search/?searchtype=author&query=Cooray%2C+A">A. Cooray</a>, <a href="/search/?searchtype=author&query=Cox%2C+P">P. Cox</a>, <a href="/search/?searchtype=author&query=Dowell%2C+C+D">C. D. Dowell</a>, <a href="/search/?searchtype=author&query=Eales%2C+S">S. Eales</a>, <a href="/search/?searchtype=author&query=Farrah%2C+D">D. Farrah</a>, <a href="/search/?searchtype=author&query=Franceschini%2C+A">A. Franceschini</a>, <a href="/search/?searchtype=author&query=Frayer%2C+D+T">D. T. Frayer</a>, <a href="/search/?searchtype=author&query=Gavazzi%2C+R">R. Gavazzi</a>, <a href="/search/?searchtype=author&query=Glenn%2C+J">J. Glenn</a> , et al. (38 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="1104.4115v1-abstract-short" style="display: inline;"> We report on the redshift measurement and CO line excitation of HERMES J105751.1+573027 (HLSW-01), a strongly lensed submillimeter galaxy discovered in Herschel/SPIRE observations as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). HLSW-01 is an ultra-luminous galaxy with an intrinsic far-infrared luminosity of 1.4x10^(13) solar luminosities, and is lensed by a massive group of gal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1104.4115v1-abstract-full').style.display = 'inline'; document.getElementById('1104.4115v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1104.4115v1-abstract-full" style="display: none;"> We report on the redshift measurement and CO line excitation of HERMES J105751.1+573027 (HLSW-01), a strongly lensed submillimeter galaxy discovered in Herschel/SPIRE observations as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). HLSW-01 is an ultra-luminous galaxy with an intrinsic far-infrared luminosity of 1.4x10^(13) solar luminosities, and is lensed by a massive group of galaxies into at least four images with a total magnification of 10.9+/-0.7. With the 100 GHz instantaneous bandwidth of the Z-Spec instrument on the Caltech Submillimeter Observatory, we robustly identify a redshift of z=2.958+/-0.007 for this source, using the simultaneous detection of four CO emission lines (J = 7-6, J = 8-7, J = 9-8, and J = 10-9). Combining the measured line fluxes for these high-J transitions with the J = 1-0, J = 3-2 and J = 5-4 line fluxes measured with the Green Bank Telescope, the Combined Array for Research in Millimeter Astronomy, and the Plateau de Bure Interferometer, respectively, we model the physical properties of the molecular gas in this galaxy. We find that the full CO spectral line energy distribution is well described by warm, moderate-density gas with Tkin = 86-235 K and n(H2) = (1.1-3.5)x10^3 cm^(-3). However, it is possible that the highest-J transitions are tracing a small fraction of very dense gas in molecular cloud cores, and two-component models that include a warm/dense molecular gas phase with Tkin ~ 200 K, n(H2) ~ 10^5 cm^(-3) are also consistent with these data. Higher signal-to-noise measurements of the J(upper) > 7 transitions with high spectral resolution, combined with high spatial resolution CO maps, are needed to improve our understanding of the gas excitation, morphology, and dynamics of this interesting high-redshift galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1104.4115v1-abstract-full').style.display = 'none'; document.getElementById('1104.4115v1-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, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 5 figures, 2 table. 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/1102.5377">arXiv:1102.5377</a> <span> [<a href="https://arxiv.org/pdf/1102.5377">pdf</a>, <a href="https://arxiv.org/ps/1102.5377">ps</a>, <a href="https://arxiv.org/format/1102.5377">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/732/1/37">10.1088/0004-637X/732/1/37 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observations and modeling of H_2 fluorescence with partial frequency redistribution in giant planet atmospheres </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Feldman%2C+P+D">Paul D. Feldman</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">Stephan R. McCandliss</a>, <a href="/search/?searchtype=author&query=Strobel%2C+D+F">Darrell F. Strobel</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="1102.5377v1-abstract-short" style="display: inline;"> Partial frequency redistribution (PRD), describing the formation of the line profile, has negligible observational effects for optical depths smaller than ~10^3, at the resolving power of most current instruments. However, when the spectral resolution is sufficiently high, PRD modeling becomes essential in interpreting the line shapes and determining the total line fluxes. We demonstrate the effec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1102.5377v1-abstract-full').style.display = 'inline'; document.getElementById('1102.5377v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1102.5377v1-abstract-full" style="display: none;"> Partial frequency redistribution (PRD), describing the formation of the line profile, has negligible observational effects for optical depths smaller than ~10^3, at the resolving power of most current instruments. However, when the spectral resolution is sufficiently high, PRD modeling becomes essential in interpreting the line shapes and determining the total line fluxes. We demonstrate the effects of PRD on the H_2 line profiles observed at high spectral resolution by the Far-Ultraviolet Spectroscopic Explorer (FUSE) in the atmospheres of Jupiter and Saturn. In these spectra, the asymmetric shapes of the lines in the Lyman (v"- 6) progression pumped by the solar Ly-beta are explained by coherent scattering of the photons in the line wings. We introduce a simple computational approximation to mitigate the numerical difficulties of radiative transfer with PRD, and show that it reproduces the exact radiative transfer solution to better than 10%. The lines predicted by our radiative transfer model with PRD, including the H_2 density and temperature distribution as a function of height in the atmosphere, are in agreement with the line profiles observed by FUSE. We discuss the observational consequences of PRD, and show that this computational method also allows us to include PRD in modeling the continuum pumped H_2 fluorescence, treating about 4000 lines simultaneously. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1102.5377v1-abstract-full').style.display = 'none'; document.getElementById('1102.5377v1-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 February, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 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/1011.1255">arXiv:1011.1255</a> <span> [<a href="https://arxiv.org/pdf/1011.1255">pdf</a>, <a href="https://arxiv.org/ps/1011.1255">ps</a>, <a href="https://arxiv.org/format/1011.1255">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1126/science.1193420">10.1126/science.1193420 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Detection of a Population of Submillimeter-Bright, Strongly-Lensed Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Negrello%2C+M">Mattia Negrello</a>, <a href="/search/?searchtype=author&query=Hopwood%2C+R">R. Hopwood</a>, <a href="/search/?searchtype=author&query=De+Zotti%2C+G">G. De Zotti</a>, <a href="/search/?searchtype=author&query=Cooray%2C+A">A. Cooray</a>, <a href="/search/?searchtype=author&query=Verma%2C+A">A. Verma</a>, <a href="/search/?searchtype=author&query=Bock%2C+J">J. Bock</a>, <a href="/search/?searchtype=author&query=Frayer%2C+D+T">D. T. Frayer</a>, <a href="/search/?searchtype=author&query=Gurwell%2C+M+A">M. A. Gurwell</a>, <a href="/search/?searchtype=author&query=Omont%2C+A">A. Omont</a>, <a href="/search/?searchtype=author&query=Neri%2C+R">R. Neri</a>, <a href="/search/?searchtype=author&query=Dannerbauer%2C+H">H. Dannerbauer</a>, <a href="/search/?searchtype=author&query=Leeuw%2C+L+L">L. L. Leeuw</a>, <a href="/search/?searchtype=author&query=Barton%2C+E">E. Barton</a>, <a href="/search/?searchtype=author&query=Cooke%2C+J">J. Cooke</a>, <a href="/search/?searchtype=author&query=Kim%2C+S">S. Kim</a>, <a href="/search/?searchtype=author&query=da+Cunha%2C+E">E. da Cunha</a>, <a href="/search/?searchtype=author&query=Rodighiero%2C+G">G. Rodighiero</a>, <a href="/search/?searchtype=author&query=Cox%2C+P">P. Cox</a>, <a href="/search/?searchtype=author&query=Bonfield%2C+D+G">D. G. Bonfield</a>, <a href="/search/?searchtype=author&query=Jarvis%2C+M+J">M. J. Jarvis</a>, <a href="/search/?searchtype=author&query=Serjeant%2C+S">S. Serjeant</a>, <a href="/search/?searchtype=author&query=Ivison%2C+R+J">R. J. Ivison</a>, <a href="/search/?searchtype=author&query=Dye%2C+S">S. Dye</a>, <a href="/search/?searchtype=author&query=Aretxaga%2C+I">I. Aretxaga</a>, <a href="/search/?searchtype=author&query=Hughes%2C+D+H">D. H. Hughes</a> , et al. (64 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="1011.1255v1-abstract-short" style="display: inline;"> Gravitational lensing is a powerful astrophysical and cosmological probe and is particularly valuable at submillimeter wavelengths for the study of the statistical and individual properties of dusty starforming galaxies. However the identification of gravitational lenses is often time-intensive, involving the sifting of large volumes of imaging or spectroscopic data to find few candidates. We used… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1011.1255v1-abstract-full').style.display = 'inline'; document.getElementById('1011.1255v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1011.1255v1-abstract-full" style="display: none;"> Gravitational lensing is a powerful astrophysical and cosmological probe and is particularly valuable at submillimeter wavelengths for the study of the statistical and individual properties of dusty starforming galaxies. However the identification of gravitational lenses is often time-intensive, involving the sifting of large volumes of imaging or spectroscopic data to find few candidates. We used early data from the Herschel Astrophysical Terahertz Large Area Survey to demonstrate that wide-area submillimeter surveys can simply and easily detect strong gravitational lensing events, with close to 100% efficiency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1011.1255v1-abstract-full').style.display = 'none'; document.getElementById('1011.1255v1-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 November, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">This is the author's version of the work. It is posted here by permission of the AAAS for personal use, not for redistribution. The definitive version was published in Science VOL 330, (Nov 5th, 2010), doi:10.1126/science.1193420</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1010.0007">arXiv:1010.0007</a> <span> [<a href="https://arxiv.org/pdf/1010.0007">pdf</a>, <a href="https://arxiv.org/ps/1010.0007">ps</a>, <a href="https://arxiv.org/format/1010.0007">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/725/1/159">10.1088/0004-637X/725/1/159 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spitzer Mapping of PAHs and H2 in Photodissociation Regions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fleming%2C+B+T">Brian T. Fleming</a>, <a href="/search/?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">Stephan R. McCandliss</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="1010.0007v1-abstract-short" style="display: inline;"> The mid-infrared (MIR) spectra of dense photodissociation regions (PDRs) are typically dominated by emission from polycyclic aromatic hydrocarbons (PAHs) and the lowest pure rotational states of molecular hydrogen (H2); two species which are probes of the physical properties of gas and dust in intense UV radiation fields. We utilize the high angular resolution of the Infrared Spectrograph on the S… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1010.0007v1-abstract-full').style.display = 'inline'; document.getElementById('1010.0007v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1010.0007v1-abstract-full" style="display: none;"> The mid-infrared (MIR) spectra of dense photodissociation regions (PDRs) are typically dominated by emission from polycyclic aromatic hydrocarbons (PAHs) and the lowest pure rotational states of molecular hydrogen (H2); two species which are probes of the physical properties of gas and dust in intense UV radiation fields. We utilize the high angular resolution of the Infrared Spectrograph on the Spitzer Space Telescope to construct spectral maps of the PAH and H2 features for three of the best studied PDRs in the galaxy, NGC 7023, NGC 2023 and IC 63. We present spatially resolved maps of the physical properties, including the H2 ortho-to-para ratio, temperature, and G_o/n_H. We also present evidence for PAH dehydrogenation, which may support theories of H2 formation on PAH surfaces, and a detection of preferential self-shielding of ortho-H2. All PDRs studied exhibit average temperatures of ~500 - 800K, warm H2 column densities of ~10^20 cm^-2, G_o/n_H ~ 0.1 - 0.8, and ortho-to-para ratios of ~ 1.8. We find that while the average of each of these properties is consistent with previous single value measurements of these PDRs, when available, the addition of spatial resolution yields a diversity of values with gas temperatures as high as 1500 K, column densities spanning ~ 2 orders of magnitude, and extreme ortho-to-para ratios of < 1 and > 3. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1010.0007v1-abstract-full').style.display = 'none'; document.getElementById('1010.0007v1-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, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2010ApJ...725..159F </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1009.5983">arXiv:1009.5983</a> <span> [<a href="https://arxiv.org/pdf/1009.5983">pdf</a>, <a href="https://arxiv.org/ps/1009.5983">ps</a>, <a href="https://arxiv.org/format/1009.5983">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> </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/757/2/135">10.1088/0004-637X/757/2/135 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of CO redshifts with Z-Spec for lensed submillimeter galaxies discovered in the H-ATLAS survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lupu%2C+R+E">R. E. Lupu</a>, <a href="/search/?searchtype=author&query=Scott%2C+K+S">K. S. Scott</a>, <a href="/search/?searchtype=author&query=Aguirre%2C+J+E">J. E. Aguirre</a>, <a href="/search/?searchtype=author&query=Aretxaga%2C+I">I. Aretxaga</a>, <a href="/search/?searchtype=author&query=Auld%2C+R">R. Auld</a>, <a href="/search/?searchtype=author&query=Barton%2C+E">E. Barton</a>, <a href="/search/?searchtype=author&query=Beelen%2C+A">A. Beelen</a>, <a href="/search/?searchtype=author&query=Bertoldi%2C+F">F. Bertoldi</a>, <a href="/search/?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/?searchtype=author&query=Bonfield%2C+D">D. Bonfield</a>, <a href="/search/?searchtype=author&query=Bradford%2C+C+M">C. M. Bradford</a>, <a href="/search/?searchtype=author&query=Buttiglione%2C+S">S. Buttiglione</a>, <a href="/search/?searchtype=author&query=Cava%2C+A">A. Cava</a>, <a href="/search/?searchtype=author&query=Clements%2C+D+L">D. L. Clements</a>, <a href="/search/?searchtype=author&query=Cooke%2C+J">J. Cooke</a>, <a href="/search/?searchtype=author&query=Cooray%2C+A">A. Cooray</a>, <a href="/search/?searchtype=author&query=Dannerbauer%2C+H">H. Dannerbauer</a>, <a href="/search/?searchtype=author&query=Dariush%2C+A">A. Dariush</a>, <a href="/search/?searchtype=author&query=De+Zotti%2C+G">G. De Zotti</a>, <a href="/search/?searchtype=author&query=Dunne%2C+L">L. Dunne</a>, <a href="/search/?searchtype=author&query=Dye%2C+S">S. Dye</a>, <a href="/search/?searchtype=author&query=Eales%2C+S">S. Eales</a>, <a href="/search/?searchtype=author&query=Frayer%2C+D">D. Frayer</a>, <a href="/search/?searchtype=author&query=Fritz%2C+J">J. Fritz</a>, <a href="/search/?searchtype=author&query=Glenn%2C+J">J. Glenn</a> , et al. (28 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1009.5983v3-abstract-short" style="display: inline;"> We present new observations from Z-Spec, a broadband 185-305 GHz spectrometer, of five sub-millimeter bright lensed sources selected from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) science demonstration phase (SDP) catalog. We construct a redshift finding algorithm using combinations of the signal-to-noise of all the lines falling in the Z-Spec bandpass to determine redshifts… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.5983v3-abstract-full').style.display = 'inline'; document.getElementById('1009.5983v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1009.5983v3-abstract-full" style="display: none;"> We present new observations from Z-Spec, a broadband 185-305 GHz spectrometer, of five sub-millimeter bright lensed sources selected from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) science demonstration phase (SDP) catalog. We construct a redshift finding algorithm using combinations of the signal-to-noise of all the lines falling in the Z-Spec bandpass to determine redshifts with high confidence, even in cases where the signal-to-noise in individual lines is low. We measure the dust continuum in all sources and secure CO redshifts for four out of five (z~1.5-3). In one source, SDP.17, we tentatively identify two independent redshifts and a water line, confirmed at z=2.308. Our sources have properties characteristic of dusty starburst galaxies, with magnification-corrected star formation rates of 10^(2-3) M_sun/yr. Lower limits for the dust masses (~a few 10^8 M_sun) and spatial extents (~1 kpc equivalent radius) are derived from the continuum spectral energy distributions, corresponding to dust temperatures between 54 and 69K. In the LTE approximation, we derive relatively low CO excitation temperatures (< 100 K) and optical depths (tau<1). Performing a non-LTE excitation analysis using RADEX, we find that the CO lines measured by Z-Spec (from J=4->3 to 10->9, depending on the galaxy) localize the best solutions to either a high-temperature / low-density region, or a low-temperature / high-density region near the LTE solution, with the optical depth varying accordingly. Observations of additional CO lines, CO(1-0) in particular, are needed to constrain the non-LTE models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.5983v3-abstract-full').style.display = 'none'; document.getElementById('1009.5983v3-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 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 September, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">28 pages, 15 figures, accepted for publication in ApJ, October 1, 2012, Issue 757 - 2</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0905.1695">arXiv:0905.1695</a> <span> [<a href="https://arxiv.org/pdf/0905.1695">pdf</a>, <a href="https://arxiv.org/ps/0905.1695">ps</a>, <a href="https://arxiv.org/format/0905.1695">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </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/699/2/1104">10.1088/0004-637X/699/2/1104 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Far Ultraviolet Spectral Signatures of Formaldehyde and Carbon Dioxide in Comets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Feldman%2C+P+D">Paul D. Feldman</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">Stephan R. McCandliss</a>, <a href="/search/?searchtype=author&query=Weaver%2C+H+A">Harold A. Weaver</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="0905.1695v1-abstract-short" style="display: inline;"> Observations of four comets made with the Far Ultraviolet Spectroscopic Explorer show the rotational envelope of the (0,0) band of the CO Hopfield-Birge system (C - X) at 1088 A to consist of both "cold" and "hot" components, the "cold" component accounting for ~75% of the flux and with a rotational temperature in the range 55-75 K. We identify the "hot" component as coming from the dissociation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0905.1695v1-abstract-full').style.display = 'inline'; document.getElementById('0905.1695v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0905.1695v1-abstract-full" style="display: none;"> Observations of four comets made with the Far Ultraviolet Spectroscopic Explorer show the rotational envelope of the (0,0) band of the CO Hopfield-Birge system (C - X) at 1088 A to consist of both "cold" and "hot" components, the "cold" component accounting for ~75% of the flux and with a rotational temperature in the range 55-75 K. We identify the "hot" component as coming from the dissociation of CO2 into rotationally "hot" CO, with electron impact dissociation probably dominant over photodissociation near the nucleus. An additional weak, broad satellite band is seen centered near the position of the P(40) line that we attribute to CO fluorescence from a non-thermal high J rotational population produced by photodissociation of formaldehyde into CO and H2. This process also leaves the H2 preferentially populated in excited vibrational levels which are identified by fluorescent H2 lines in the spectrum excited by solar OVI 1031.9 and solar Lyman-alpha. The amount of H2 produced by H2CO dissociation is comparable to the amount produced by photodissociation of H2O. Electron impact excitation of CO, rather than resonance fluorescence, appears to be the primary source of the observed (B - X) (0,0) band at 1151 A. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0905.1695v1-abstract-full').style.display = 'none'; document.getElementById('0905.1695v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 May, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 7 figures, accepted for publication in the Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.699:1104-1112,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0812.2046">arXiv:0812.2046</a> <span> [<a href="https://arxiv.org/pdf/0812.2046">pdf</a>, <a href="https://arxiv.org/ps/0812.2046">ps</a>, <a href="https://arxiv.org/format/0812.2046">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/10.1063/1.3154056">10.1063/1.3154056 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modeling H2 Fluorescence in Planetary Atmospheres with Partial Frequency Redistribution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lupu%2C+R+E">R. E. Lupu</a>, <a href="/search/?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">S. R. McCandliss</a>, <a href="/search/?searchtype=author&query=France%2C+K">K. France</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="0812.2046v1-abstract-short" style="display: inline;"> We present the modeling of partial frequency redistribution (PRD) effects for the fluorescent emission lines of molecular hydrogen, the general computational approximations, and the applications to planetary atmospheres, as well as interstellar medium. Our model is applied to FUSE observations of Jupiter, Saturn, and reflection nebulae, allowing an independent confirmation of the H2 abundance an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0812.2046v1-abstract-full').style.display = 'inline'; document.getElementById('0812.2046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0812.2046v1-abstract-full" style="display: none;"> We present the modeling of partial frequency redistribution (PRD) effects for the fluorescent emission lines of molecular hydrogen, the general computational approximations, and the applications to planetary atmospheres, as well as interstellar medium. Our model is applied to FUSE observations of Jupiter, Saturn, and reflection nebulae, allowing an independent confirmation of the H2 abundance and the structure of planetary atmospheres. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0812.2046v1-abstract-full').style.display = 'none'; document.getElementById('0812.2046v1-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 December, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in Proc. Future Directions in Ultraviolet Spectroscopy, Annapolis, Oct. 20-22 2008</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0807.2295">arXiv:0807.2295</a> <span> [<a href="https://arxiv.org/pdf/0807.2295">pdf</a>, <a href="https://arxiv.org/ps/0807.2295">ps</a>, <a href="https://arxiv.org/format/0807.2295">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/10.1117/12.789574">10.1117/12.789574 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Project Lyman </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">Stephan R. McCandliss</a>, <a href="/search/?searchtype=author&query=Kruk%2C+J+W">Jeffrey W. Kruk</a>, <a href="/search/?searchtype=author&query=Blair%2C+W+P">William P. Blair</a>, <a href="/search/?searchtype=author&query=Kaiser%2C+M+E">Mary Elizabeth Kaiser</a>, <a href="/search/?searchtype=author&query=Feldman%2C+P+D">Paul D. Feldman</a>, <a href="/search/?searchtype=author&query=Meurer%2C+G+R">Gerhardt R. Meurer</a>, <a href="/search/?searchtype=author&query=Dixon%2C+W+V">William V. Dixon</a>, <a href="/search/?searchtype=author&query=Sahnow%2C+D+J">David J. Sahnow</a>, <a href="/search/?searchtype=author&query=Neufeld%2C+D+A">David A. Neufeld</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Fleming%2C+B">Brian Fleming</a>, <a href="/search/?searchtype=author&query=Smee%2C+S+A">Stephen A. Smee</a>, <a href="/search/?searchtype=author&query=Andersson%2C+B+G">B. G. Andersson</a>, <a href="/search/?searchtype=author&query=Moseley%2C+S+H">Samuel H. Moseley</a>, <a href="/search/?searchtype=author&query=Kutyrev%2C+A+S">Alexander S. Kutyrev</a>, <a href="/search/?searchtype=author&query=Li%2C+M+J">Mary J. Li</a>, <a href="/search/?searchtype=author&query=Sonneborn%2C+G">George Sonneborn</a>, <a href="/search/?searchtype=author&query=Siegmund%2C+O+H+W">Oswald H. W. Siegmund</a>, <a href="/search/?searchtype=author&query=Vallerga%2C+J+V">John V. Vallerga</a>, <a href="/search/?searchtype=author&query=Welsh%2C+B+Y">Barry Y. Welsh</a>, <a href="/search/?searchtype=author&query=Stiavelli%2C+M">Massimo Stiavelli</a>, <a href="/search/?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</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="0807.2295v1-abstract-short" style="display: inline;"> We explore the design of a space mission, Project Lyman, which has the goal of quantifying the ionization history of the universe from the present epoch to a redshift of z ~ 3. Observations from WMAP and SDSS show that before a redshift of z >~ 6 the first collapsed objects, possibly dwarf galaxies, emitted Lyman continuum (LyC) radiation shortward of 912 A, reionizing most of the universe. How… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0807.2295v1-abstract-full').style.display = 'inline'; document.getElementById('0807.2295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0807.2295v1-abstract-full" style="display: none;"> We explore the design of a space mission, Project Lyman, which has the goal of quantifying the ionization history of the universe from the present epoch to a redshift of z ~ 3. Observations from WMAP and SDSS show that before a redshift of z >~ 6 the first collapsed objects, possibly dwarf galaxies, emitted Lyman continuum (LyC) radiation shortward of 912 A, reionizing most of the universe. How LyC escapes from galactic environments, whether it induces positive or negative feedback on the local and global collapse of structures, and the role played by clumping, molecules, metallicity and dust are major unanswered theoretical questions, requiring observational constraint. Numerous intervening Lyman limit systems, which frustrate the detection of LyC from high z objects, thin below z ~ 3 where there are a few objects with apparently very high fesc. At low z there are only controversial detections and a handful of upper limits. A wide-field multi-object spectroscopic survey with moderate spectral and spatial resolution can quantify fesc within diverse spatially resolved galactic environments over redshifts with significant evolution in galaxy assemblage and quasar activity. It can also calibrate LyC escape against Ly-alpha escape, providing an essential tool to JWST for probing the beginnings of reionization. We present calculations showing the evolution of the characteristic apparent magnitude of star-forming galaxy luminosity functions at 900 A, as a function of redshift and assumed escape fraction to determine the required aperture for detecting LyC. We review our efforts to build a pathfinding dual order multi-object spectro/telescope with a (0.5deg)^2 field-of-view, using a GSFC microshutter array, and crossed delay-line micro-channel plate detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0807.2295v1-abstract-full').style.display = 'none'; document.getElementById('0807.2295v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 July, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2008. </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">SPIE oral paper 7011-76 presented at Astronomical Telescopes 2008 - 23 -- 28 June Marseille, France, 12 page, 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/0806.1755">arXiv:0806.1755</a> <span> [<a href="https://arxiv.org/pdf/0806.1755">pdf</a>, <a href="https://arxiv.org/ps/0806.1755">ps</a>, <a href="https://arxiv.org/format/0806.1755">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/10.1117/12.786435">10.1117/12.786435 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration and flight performance of the long-slit imaging dual order spectrograph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">Stephan R. McCandliss</a>, <a href="/search/?searchtype=author&query=Fleming%2C+B">Brian Fleming</a>, <a href="/search/?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/?searchtype=author&query=Feldman%2C+P+D">Paul D. Feldman</a>, <a href="/search/?searchtype=author&query=Nikzad%2C+S">Shouleh Nikzad</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="0806.1755v1-abstract-short" style="display: inline;"> We present a preliminary calibration and flight performance of the Long-Slit Imaging Dual Order Spectrograph (LIDOS), a rocket-borne instrument with a large dynamic range in the 900 - 1700A bandpass. The instrument observes UV-bright objects with a CCD channel and fainter nebulosity with an MCP detector. The image quality and the detector quantum efficiencies were determined using the calibratio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0806.1755v1-abstract-full').style.display = 'inline'; document.getElementById('0806.1755v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0806.1755v1-abstract-full" style="display: none;"> We present a preliminary calibration and flight performance of the Long-Slit Imaging Dual Order Spectrograph (LIDOS), a rocket-borne instrument with a large dynamic range in the 900 - 1700A bandpass. The instrument observes UV-bright objects with a CCD channel and fainter nebulosity with an MCP detector. The image quality and the detector quantum efficiencies were determined using the calibration and test equipment at the Johns Hopkins University, and further monitored using an on-board electron-impact calibration lamp. We review results from each of the three flights of the instrument. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0806.1755v1-abstract-full').style.display = 'none'; document.getElementById('0806.1755v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2008. </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. to appear in Proc. SPIE 7011</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0708.3088">arXiv:0708.3088</a> <span> [<a href="https://arxiv.org/pdf/0708.3088">pdf</a>, <a href="https://arxiv.org/ps/0708.3088">ps</a>, <a href="https://arxiv.org/format/0708.3088">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/10.1086/522328">10.1086/522328 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fourth Positive System of Carbon Monoxide in the Hubble Space Telescope Spectra of Comets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Feldman%2C+P+D">Paul D. Feldman</a>, <a href="/search/?searchtype=author&query=Weaver%2C+H+A">Harold A. Weaver</a>, <a href="/search/?searchtype=author&query=Tozzi%2C+G">Gian-Paolo Tozzi</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="0708.3088v1-abstract-short" style="display: inline;"> The rich structure of the Fourth Positive System (A-X) of carbon monoxide accounts for many of the spectral features seen in long slit HST-STIS observations of comets 153P/Ikeya-Zhang, C/2001 Q4 (NEAT), and C/2000 WM1 (LINEAR), as well as in the HST-GHRS spectrum of comet C/1996 B2 Hyakutake. A detailed CO fluorescence model is developed to derive the CO abundances in these comets by simultaneou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0708.3088v1-abstract-full').style.display = 'inline'; document.getElementById('0708.3088v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0708.3088v1-abstract-full" style="display: none;"> The rich structure of the Fourth Positive System (A-X) of carbon monoxide accounts for many of the spectral features seen in long slit HST-STIS observations of comets 153P/Ikeya-Zhang, C/2001 Q4 (NEAT), and C/2000 WM1 (LINEAR), as well as in the HST-GHRS spectrum of comet C/1996 B2 Hyakutake. A detailed CO fluorescence model is developed to derive the CO abundances in these comets by simultaneously fitting all of the observed A-X bands. The model includes the latest values for the oscillator strengths and state parameters, and accounts for optical depth effects due to line overlap and self-absorption. The model fits yield radial profiles of CO column density that are consistent with a predominantly native source for all the comets observed by STIS. The derived CO abundances relative to water in these comets span a wide range, from 0.44% for C/2000 WM1 (LINEAR), 7.2% for 153P/Ikeya-Zhang, 8.8% for C/2001 Q4 (NEAT) to 20.9% for C/1996 B2 (Hyakutake). The subtraction of the CO spectral features using this model leads to the first identification of a molecular hydrogen line pumped by solar HI Lyman-beta longward of 1200A in the spectrum of comet 153P/Ikeya-Zhang. (Abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0708.3088v1-abstract-full').style.display = 'none'; document.getElementById('0708.3088v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 August, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">12 pages, 11 figures, ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0707.1044">arXiv:0707.1044</a> <span> [<a href="https://arxiv.org/pdf/0707.1044">pdf</a>, <a href="https://arxiv.org/ps/0707.1044">ps</a>, <a href="https://arxiv.org/format/0707.1044">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/10.1086/521348">10.1086/521348 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Low-Mass H2 Component to the AU Microscopii Circumstellar Disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/?searchtype=author&query=Roberge%2C+A">Aki Roberge</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Redfield%2C+S">Seth Redfield</a>, <a href="/search/?searchtype=author&query=Feldman%2C+P+D">Paul D. Feldman</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="0707.1044v1-abstract-short" style="display: inline;"> We present a determination of the molecular gas mass in the AU Microscopii circumstellar disk. Direct detection of a gas component to the AU Mic disk has proven elusive, with upper limits derived from ultraviolet absorption line and submillimeter CO emission studies. Fluorescent emission lines of H2, pumped by the OVI 1032 resonance line through the C-X (1 -- 1) Q(3) 1031.87 脜 transition, are de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0707.1044v1-abstract-full').style.display = 'inline'; document.getElementById('0707.1044v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0707.1044v1-abstract-full" style="display: none;"> We present a determination of the molecular gas mass in the AU Microscopii circumstellar disk. Direct detection of a gas component to the AU Mic disk has proven elusive, with upper limits derived from ultraviolet absorption line and submillimeter CO emission studies. Fluorescent emission lines of H2, pumped by the OVI 1032 resonance line through the C-X (1 -- 1) Q(3) 1031.87 脜 transition, are detected by the Far Ultraviolet Spectroscopic Explorer. These lines are used to derive the H2 column density associated with the AU Mic system. The derived column density is in the range N(H2) = 1.9 x 10^{17} - 2.8 x 10^{15} cm^{-2}, roughly two orders of magnitude lower than the upper limit inferred from absorption line studies. This range of column densities reflects the range of H2 excitation temperature consistent with the observations, T(H2) = 800 -- 2000 K, derived from the presence of emission lines excited by OVI in the absence of those excited by LyA. Within the observational uncertainties, the data are consistent with the H2 gas residing in the disk. The inferred N(H2) range corresponds to H2-to-dust ratios of < 1/30:1 and a total M(H2) = 4.0 x 10^{-4} - 5.8 x 10^{-6} Earth masses. We use these results to predict the intensity of the associated rovibrational emission lines of H2 at infrared wavelengths covered by ground-based instruments, HST-NICMOS, and the Spitzer-IRS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0707.1044v1-abstract-full').style.display = 'none'; document.getElementById('0707.1044v1-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 July, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">ApJ, accepted. 9 pages, 4 figures, emulateapj</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/0701439">arXiv:astro-ph/0701439</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0701439">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0701439">ps</a>, <a href="https://arxiv.org/format/astro-ph/0701439">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/10.1086/512803">10.1086/512803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Molecular and Atomic Excitation Stratification in the Outflow of the Planetary Nebula M27 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">Stephan R. McCandliss</a>, <a href="/search/?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=Burgh%2C+E+B">Eric B. Burgh</a>, <a href="/search/?searchtype=author&query=Sembach%2C+K">Kenneth Sembach</a>, <a href="/search/?searchtype=author&query=Kruk%2C+J">Jeffrey Kruk</a>, <a href="/search/?searchtype=author&query=Andersson%2C+B+-">B. -G. Andersson</a>, <a href="/search/?searchtype=author&query=Feldman%2C+P+D">Paul D. Feldman</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/0701439v1-abstract-short" style="display: inline;"> High resolution spectroscopy with FUSE and STIS of atomic and molecular velocity stratification in the nebular outflow of M27 challenge models for the abundance kinematics in planetary nebulae. The simple picture of a very high speed (~ 1000 km/s), high ionization, radiation driven stellar wind surrounded by a slower (~ 10 km/s) mostly molecular outflow, with low ionization and neutral atomic sp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0701439v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0701439v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0701439v1-abstract-full" style="display: none;"> High resolution spectroscopy with FUSE and STIS of atomic and molecular velocity stratification in the nebular outflow of M27 challenge models for the abundance kinematics in planetary nebulae. The simple picture of a very high speed (~ 1000 km/s), high ionization, radiation driven stellar wind surrounded by a slower (~ 10 km/s) mostly molecular outflow, with low ionization and neutral atomic species residing at the wind interaction interface, is not supported... We find ...there is a fast (33 -- 65 km/s) low ionization zone, surrounding a slower (<~ 33 km/s) high ionization zone and, at the transition velocity (33 km/s), vibrationally excited H_2 is intermixed with a predominately neutral atomic medium... Far-UV continuum fluorescence of H_2 is not detected, but Lyman alpha (Lya) fluorescence is present. The diffuse nebular medium is inhospitable to molecules and dust. Maintaining the modest equilibrium abundance of H_2 (N(H_2)/N(HI) << 1) in the diffuse nebular medium requires a source of H_2, mostly likely the clumpy nebular medium. The stellar SED shows no signs of reddening (E(B-V) < 0.01), but paradoxically measurements of Ha/Hb ... indicate E(B-V) ~ 0.1. ...the apparent enhancement of Ha/Hb in the absence of dust may result from a two step process of H_2 ionization by Lyman continuum (Lyc) photons followed by dissociative recombination (H_2 + gamma -> H_2^+ + e -> H(1s) + H (nl)), which ultimately produces fluorescence of Ha and Lya. In the optically thin limit at the inferred radius of the velocity transition we find dissociation of H_2 by stellar Lyc photons is an order of magnitude more efficient than spontaneous dissociation by far-UV photons. We suggest that the importance of this H_2 destruction process in HII regions has been overlooked. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0701439v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0701439v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 January, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">In emulateapj 2 column, 28 pages total, 18 figures. Accepted for publication in the Astrophysical Journal on 5 January 2007. Abstract abridged</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.659:1291-1316,2007 </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/0610953">arXiv:astro-ph/0610953</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0610953">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0610953">ps</a>, <a href="https://arxiv.org/format/astro-ph/0610953">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/10.1086/510481">10.1086/510481 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Cometary Bow Shock and Mid-Infrared Emission Variations Revealed in Spitzer Observations of HD 34078 and IC 405 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">Stephan R. McCandliss</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</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/0610953v1-abstract-short" style="display: inline;"> We present new infrared observations of the emission/reflection nebula IC 405 obtained with the Spitzer Space Telescope. Infrared images in the four IRAC bands (3.6, 4.5, 5.8, and 8.0 um) and two MIPS bands (24 and 70 um) are complemented by IRS spectroscopy (5-30 um) of two nebular filaments. The IRAC (8.0 um) and MIPS imaging shows evidence of a bow shock associated with the runaway O9.5V star… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0610953v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0610953v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0610953v1-abstract-full" style="display: none;"> We present new infrared observations of the emission/reflection nebula IC 405 obtained with the Spitzer Space Telescope. Infrared images in the four IRAC bands (3.6, 4.5, 5.8, and 8.0 um) and two MIPS bands (24 and 70 um) are complemented by IRS spectroscopy (5-30 um) of two nebular filaments. The IRAC (8.0 um) and MIPS imaging shows evidence of a bow shock associated with the runaway O9.5V star, HD 34078, created by the interaction between the star and nebular material. The ratio of emission at 24 to 70 um is higher in the immediate vicinity of HD 34078 than in the outer filaments, providing evidence for elevated dust temperatures (T_d > 90 K) in the shock region. The nebular imaging reveals that the morphology is band dependent, with varying contributions from aromatic emission features, H2, and dust emission. Nebular spectroscopy is used to quantify these contributions, showing several aromatic emission bands between 6-14 um, the S(5), S(3), S(2), and S(1) pure rotational emission lines of H2, and atomic fine structure lines of Ne, S, and Ar. The low-dispersion spectra provide constraints on the ionization state of the large molecules responsible for the aromatic infrared features. H2 rotational temperatures of the two bright nebular filaments are determined from the observed line strengths. An average T(H2) ~ 400 K is inferred, with evidence for additional non-uniform excitation by UV photons in the intense radiation field of HD 34078. The photoexcitation hypothesis is supported by direct measurement of the far-UV H2 fluorescence spectrum, obtained with FUSE. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0610953v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0610953v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">ApJ accepted, uses emulateapj, images compressed for astro-ph</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.655:920-939,2007 </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/0607185">arXiv:astro-ph/0607185</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0607185">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0607185">ps</a>, <a href="https://arxiv.org/format/astro-ph/0607185">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/10.1086/507464">10.1086/507464 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Carbon Monoxide in Comet 9P/Tempel 1 before and after the Deep Impact Encounter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Feldman%2C+P+D">Paul D. Feldman</a>, <a href="/search/?searchtype=author&query=Lupu%2C+R+E">Roxana E. Lupu</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">Stephan R. McCandliss</a>, <a href="/search/?searchtype=author&query=Weaver%2C+H+A">Harold A. Weaver</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">Michael F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Belton%2C+M+J+S">Michael J. S. Belton</a>, <a href="/search/?searchtype=author&query=Meech%2C+K+J">Karen J. Meech</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/0607185v1-abstract-short" style="display: inline;"> One of the goals of the Hubble Space Telescope program to observe periodic comet 9P/Tempel 1 in conjunction with NASA's Deep Impact mission was to study the generation and evolution of the gaseous coma resulting from the impact. For this purpose, the Solar Blind Channel of the Advanced Camera for Surveys was used with the F140LP filter which is sensitive primarily to the ultraviolet emission (>1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0607185v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0607185v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0607185v1-abstract-full" style="display: none;"> One of the goals of the Hubble Space Telescope program to observe periodic comet 9P/Tempel 1 in conjunction with NASA's Deep Impact mission was to study the generation and evolution of the gaseous coma resulting from the impact. For this purpose, the Solar Blind Channel of the Advanced Camera for Surveys was used with the F140LP filter which is sensitive primarily to the ultraviolet emission (>1400 A) from the CO Fourth Positive system. Following the impact we detected an increase in brightness, which if all due to CO corresponds to 1.5 x 10^31 molecules or a mass of 6.6 x 10^5 kg, an amount that would normally be produced by 7-10 hours of quiescent outgassing from the comet. This number is less than or equal to 10% of the number of water molecules excavated, and suggests that the volatile content of the material excavated by the impact did not differ significantly from the surface or near sub-surface material responsible for the quiescent outgassing of the comet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0607185v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0607185v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">10 pages, 4 postscript figures. Accepted for publication in ApJ (Letters)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.647:L61-L64,2006 </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/0602547">arXiv:astro-ph/0602547</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0602547">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0602547">ps</a>, <a href="https://arxiv.org/format/astro-ph/0602547">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/10.1086/503603">10.1086/503603 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of Lyman-alpha Pumped Molecular Hydrogen Emission in the Planetary Nebulae NGC 6853 and NGC 3132 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lupu%2C+R+E">R. E. Lupu</a>, <a href="/search/?searchtype=author&query=France%2C+K">K. France</a>, <a href="/search/?searchtype=author&query=McCandliss%2C+S+R">S. R. McCandliss</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/0602547v1-abstract-short" style="display: inline;"> We report the first observation of Ly$伪$ pumped molecular hydrogen emission lines in planetary nebulae. The H$_{2}$ emission observed in the ultraviolet spectra of NGC 6853 and NGC 3132 can be explained by excitation of vibrationally hot H$_{2}$ by Ly$伪$ photons. Constraints are placed on the nebular Ly$伪$ emission profile, as well as the molecular hydrogen temperature, column density and turbul… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0602547v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0602547v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0602547v1-abstract-full" style="display: none;"> We report the first observation of Ly$伪$ pumped molecular hydrogen emission lines in planetary nebulae. The H$_{2}$ emission observed in the ultraviolet spectra of NGC 6853 and NGC 3132 can be explained by excitation of vibrationally hot H$_{2}$ by Ly$伪$ photons. Constraints are placed on the nebular Ly$伪$ emission profile, as well as the molecular hydrogen temperature, column density and turbulent motion. These parameters are similar for the two nebulae, pointing to similar physical conditions in these objects. The ro-vibrational cascade following Ly$伪$ pumping is predicted to have low surface brightness signatures in the visible and near infrared. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0602547v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0602547v1-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 February, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">emulate ApJ, 9 pages, 8 figures, 9 tables, ApJ accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 644 (2006) 981-989 </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