[2404.11523] Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy

<!DOCTYPE html> <html lang="en"> <head> <title>[2404.11523] Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy</title> <meta name="viewport" content="width=device-width, initial-scale=1"> <link rel="apple-touch-icon" sizes="180x180" href="/static/browse/0.3.4/images/icons/apple-touch-icon.png"> <link rel="icon" type="image/png" sizes="32x32" href="/static/browse/0.3.4/images/icons/favicon-32x32.png"> <link rel="icon" type="image/png" sizes="16x16" href="/static/browse/0.3.4/images/icons/favicon-16x16.png"> <link rel="manifest" href="/static/browse/0.3.4/images/icons/site.webmanifest"> <link rel="mask-icon" href="/static/browse/0.3.4/images/icons/safari-pinned-tab.svg" color="#5bbad5"> <meta name="msapplication-TileColor" content="#da532c"> <meta name="theme-color" content="#ffffff"> <link rel="stylesheet" type="text/css" media="screen" href="/static/browse/0.3.4/css/arXiv.css?v=20241206" /> <link rel="stylesheet" type="text/css" media="print" href="/static/browse/0.3.4/css/arXiv-print.css?v=20200611" /> <link rel="stylesheet" type="text/css" media="screen" href="/static/browse/0.3.4/css/browse_search.css" /> <script language="javascript" src="/static/browse/0.3.4/js/accordion.js" /></script> <link rel="canonical" href="https://arxiv.org/abs/2404.11523"/> <meta name="description" content="Abstract page for arXiv paper 2404.11523: Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy"><meta property="og:type" content="website" /> <meta property="og:site_name" content="arXiv.org" /> <meta property="og:title" content="Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy" /> <meta property="og:url" content="https://arxiv.org/abs/2404.11523v1" /> <meta property="og:image" content="/static/browse/0.3.4/images/arxiv-logo-fb.png" /> <meta property="og:image:secure_url" content="/static/browse/0.3.4/images/arxiv-logo-fb.png" /> <meta property="og:image:width" content="1200" /> <meta property="og:image:height" content="700" /> <meta property="og:image:alt" content="arXiv logo"/> <meta property="og:description" content="Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear insights into the formation channel of individual objects. Aims. Using the Keck Planet Imager and Characterizer (KPIC; R = 35,000), we aim to characterize a young brown dwarf HD 984 B. By measuring its C/O and 12CO/13CO ratios, we expect to gain new knowledge about its origin by confirming the difference in the formation pathways between brown dwarfs and super-Jupiters. Methods. We analysed the KPIC high-resolution spectrum (2.29-2.49 渭m) of HD 984 B using an atmospheric retrieval framework based on nested sampling and petitRADTRANS, using both clear and cloudy models. Results. Using our best-fit model, we find C/O = 0.50+0.01-0.01 (0.01 is the statistical error) for HD 984 B which agrees with that of its host star within 1蟽 (0.40+0.20-0.20). We also retrieve an isotopolog 12CO/13CO ratio of 98+20-25 in its atmosphere, which is similar to that of the Sun. In addition, HD 984 B has a substellar metallicity with [Fe/H] = -0.62+0.02-0.02. Finally, we find that most of the retrieved parameters are independent of our choice of retrieval model. Conclusions. From our measured C/O and 12CO/13CO, the favored formation mechanism of HD 984 B seems to be via gravitational collapse or disk instability and not core accretion, which is a favored formation mechanism for giant exoplanets with m < 13 MJup and semimajor axis between 10 and 100 au. However, with only a few brown dwarfs with a measured 12CO/13CO ratio, similar analyses using high-resolution spectroscopy will become essential in order to determine planet formation processes more precisely."/> <meta name="twitter:site" content="@arxiv"/> <meta name="twitter:card" content="summary"/> <meta name="twitter:title" content="Fresh view of the hot brown dwarf HD 984 B through high-resolution..."/> <meta name="twitter:description" content="Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear..."/> <meta name="twitter:image" content="https://static.arxiv.org/icons/twitter/arxiv-logo-twitter-square.png"/> <meta name="twitter:image:alt" content="arXiv logo"/> <link rel="stylesheet" media="screen" type="text/css" href="/static/browse/0.3.4/css/tooltip.css"/><link rel="stylesheet" media="screen" type="text/css" href="https://static.arxiv.org/js/bibex-dev/bibex.css?20200709"/> <script src="/static/browse/0.3.4/js/mathjaxToggle.min.js" type="text/javascript"></script> <script src="//code.jquery.com/jquery-latest.min.js" type="text/javascript"></script> <script src="//cdn.jsdelivr.net/npm/js-cookie@2/src/js.cookie.min.js" type="text/javascript"></script> <script src="//cdn.jsdelivr.net/npm/dompurify@2.3.5/dist/purify.min.js"></script> <script src="/static/browse/0.3.4/js/toggle-labs.js?20241022" type="text/javascript"></script> <script src="/static/browse/0.3.4/js/cite.js" type="text/javascript"></script><meta name="citation_title" content="Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy" /><meta name="citation_author" content="Costes, J. C." /><meta name="citation_author" content="Xuan, J. W." /><meta name="citation_author" content="Vigan, A." /><meta name="citation_author" content="Wang, J." /><meta name="citation_author" content="D'Orazi, V." /><meta name="citation_author" content="Molli猫re, P." /><meta name="citation_author" content="Baker, A." /><meta name="citation_author" content="Bartos, R." /><meta name="citation_author" content="Blake, G. A." /><meta name="citation_author" content="Calvin, B." /><meta name="citation_author" content="Cetre, S." /><meta name="citation_author" content="Delorme, J." /><meta name="citation_author" content="Doppmann, G." /><meta name="citation_author" content="Echeveri, D." /><meta name="citation_author" content="Finnerty, L." /><meta name="citation_author" content="Fitzgerald, M. P." /><meta name="citation_author" content="Hsu, C." /><meta name="citation_author" content="Jovanovic, N." /><meta name="citation_author" content="Lopez, R." /><meta name="citation_author" content="Mawet, D." /><meta name="citation_author" content="Morris, E." /><meta name="citation_author" content="Pezzato, J." /><meta name="citation_author" content="Phillips, C. L." /><meta name="citation_author" content="Ruffio, J." /><meta name="citation_author" content="Sappey, B." /><meta name="citation_author" content="Schneeberger, A." /><meta name="citation_author" content="Schofield, T." /><meta name="citation_author" content="Skemer, A. J." /><meta name="citation_author" content="Wallace, J. K." /><meta name="citation_author" content="Wang, J." /><meta name="citation_doi" content="10.1051/0004-6361/202348370" /><meta name="citation_date" content="2024/04/17" /><meta name="citation_online_date" content="2024/04/17" /><meta name="citation_pdf_url" content="http://arxiv.org/pdf/2404.11523" /><meta name="citation_arxiv_id" content="2404.11523" /><meta name="citation_abstract" content="Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear insights into the formation channel of individual objects. Aims. Using the Keck Planet Imager and Characterizer (KPIC; R = 35,000), we aim to characterize a young brown dwarf HD 984 B. By measuring its C/O and 12CO/13CO ratios, we expect to gain new knowledge about its origin by confirming the difference in the formation pathways between brown dwarfs and super-Jupiters. Methods. We analysed the KPIC high-resolution spectrum (2.29-2.49 {\mu}m) of HD 984 B using an atmospheric retrieval framework based on nested sampling and petitRADTRANS, using both clear and cloudy models. Results. Using our best-fit model, we find C/O = 0.50+0.01-0.01 (0.01 is the statistical error) for HD 984 B which agrees with that of its host star within 1{\sigma} (0.40+0.20-0.20). We also retrieve an isotopolog 12CO/13CO ratio of 98+20-25 in its atmosphere, which is similar to that of the Sun. In addition, HD 984 B has a substellar metallicity with [Fe/H] = -0.62+0.02-0.02. Finally, we find that most of the retrieved parameters are independent of our choice of retrieval model. Conclusions. From our measured C/O and 12CO/13CO, the favored formation mechanism of HD 984 B seems to be via gravitational collapse or disk instability and not core accretion, which is a favored formation mechanism for giant exoplanets with m < 13 MJup and semimajor axis between 10 and 100 au. However, with only a few brown dwarfs with a measured 12CO/13CO ratio, similar analyses using high-resolution spectroscopy will become essential in order to determine planet formation processes more precisely." /> </head> <body class="with-cu-identity"> <div class="flex-wrap-footer"> <header> <a href="#content" class="is-sr-only">Skip to main content</a>  <div class="columns is-vcentered is-hidden-mobile" id="cu-identity"> <div class="column" id="cu-logo"> <a href="https://www.cornell.edu/"><img src="/static/browse/0.3.4/images/icons/cu/cornell-reduced-white-SMALL.svg" alt="Cornell University" /></a> </div><div class="column" id="support-ack"> <span id="support-ack-url">We gratefully acknowledge support from the Simons Foundation, <a href="https://info.arxiv.org/about/ourmembers.html">member institutions</a>, and all contributors.</span> <a href="https://info.arxiv.org/about/donate.html" class="btn-header-donate">Donate</a> </div> </div> <div id="header" class="is-hidden-mobile"> <a 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class="descriptor">Authors:</span><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Costes,+J+C" rel="nofollow">J. C. Costes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Xuan,+J+W" rel="nofollow">J. W. Xuan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vigan,+A" rel="nofollow">A. Vigan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wang,+J" rel="nofollow">J. Wang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=D'Orazi,+V" rel="nofollow">V. D'Orazi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Molli%C3%A8re,+P" rel="nofollow">P. Molli猫re</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Baker,+A" rel="nofollow">A. Baker</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bartos,+R" rel="nofollow">R. Bartos</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Blake,+G+A" rel="nofollow">G. A. Blake</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Calvin,+B" rel="nofollow">B. Calvin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cetre,+S" rel="nofollow">S. Cetre</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Delorme,+J" rel="nofollow">J. Delorme</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Doppmann,+G" rel="nofollow">G. Doppmann</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Echeveri,+D" rel="nofollow">D. Echeveri</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Finnerty,+L" rel="nofollow">L. Finnerty</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fitzgerald,+M+P" rel="nofollow">M. P. Fitzgerald</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hsu,+C" rel="nofollow">C. Hsu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jovanovic,+N" rel="nofollow">N. Jovanovic</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lopez,+R" rel="nofollow">R. Lopez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mawet,+D" rel="nofollow">D. Mawet</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Morris,+E" rel="nofollow">E. Morris</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pezzato,+J" rel="nofollow">J. Pezzato</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Phillips,+C+L" rel="nofollow">C. L. Phillips</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ruffio,+J" rel="nofollow">J. Ruffio</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sappey,+B" rel="nofollow">B. Sappey</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Schneeberger,+A" rel="nofollow">A. Schneeberger</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Schofield,+T" rel="nofollow">T. Schofield</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Skemer,+A+J" rel="nofollow">A. J. Skemer</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wallace,+J+K" rel="nofollow">J. K. Wallace</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wang,+J" rel="nofollow">J. Wang</a></div> <div id="download-button-info" hidden>View a PDF of the paper titled Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy, by J. C. Costes and 29 other authors</div> <a class="mobile-submission-download" href="/pdf/2404.11523">View PDF</a> <a class="mobile-submission-download" href="https://arxiv.org/html/2404.11523v1">HTML (experimental)</a> <blockquote class="abstract mathjax"> <span class="descriptor">Abstract:</span>Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear insights into the formation channel of individual objects. Aims. Using the Keck Planet Imager and Characterizer (KPIC; R = 35,000), we aim to characterize a young brown dwarf HD 984 B. By measuring its C/O and 12CO/13CO ratios, we expect to gain new knowledge about its origin by confirming the difference in the formation pathways between brown dwarfs and super-Jupiters. Methods. We analysed the KPIC high-resolution spectrum (2.29-2.49 {\mu}m) of HD 984 B using an atmospheric retrieval framework based on nested sampling and petitRADTRANS, using both clear and cloudy models. Results. Using our best-fit model, we find C/O = 0.50+0.01-0.01 (0.01 is the statistical error) for HD 984 B which agrees with that of its host star within 1{\sigma} (0.40+0.20-0.20). We also retrieve an isotopolog 12CO/13CO ratio of 98+20-25 in its atmosphere, which is similar to that of the Sun. In addition, HD 984 B has a substellar metallicity with [Fe/H] = -0.62+0.02-0.02. Finally, we find that most of the retrieved parameters are independent of our choice of retrieval model. Conclusions. From our measured C/O and 12CO/13CO, the favored formation mechanism of HD 984 B seems to be via gravitational collapse or disk instability and not core accretion, which is a favored formation mechanism for giant exoplanets with m < 13 MJup and semimajor axis between 10 and 100 au. However, with only a few brown dwarfs with a measured 12CO/13CO ratio, similar analyses using high-resolution spectroscopy will become essential in order to determine planet formation processes more precisely. </blockquote>  <div class="metatable"> <table summary="Additional metadata"> <tr> <td class="tablecell label">Comments:</td> <td class="tablecell comments mathjax">14 pages, 8 figures</td> </tr> <tr> <td class="tablecell label">Subjects:</td> <td class="tablecell subjects"> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span>; Earth and Planetary Astrophysics (astro-ph.EP)</td> </tr><tr> <td class="tablecell label">Cite as:</td> <td class="tablecell arxivid"><span class="arxivid"><a href="https://arxiv.org/abs/2404.11523">arXiv:2404.11523</a> [astro-ph.SR]</span></td> </tr> <tr> <td class="tablecell label"> </td> <td class="tablecell arxividv">(or <span class="arxivid"> <a href="https://arxiv.org/abs/2404.11523v1">arXiv:2404.11523v1</a> [astro-ph.SR]</span> for this version) </td> </tr> <tr> <td class="tablecell label"> </td> <td class="tablecell arxivdoi"> <a href="https://doi.org/10.48550/arXiv.2404.11523" id="arxiv-doi-link">https://doi.org/10.48550/arXiv.2404.11523</a><div class="button-and-tooltip"> <button class="more-info" aria-describedby="more-info-desc-1"> <svg height="15" role="presentation" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512"><path fill="currentColor" d="M256 8C119.043 8 8 119.083 8 256c0 136.997 111.043 248 248 248s248-111.003 248-248C504 119.083 392.957 8 256 8zm0 110c23.196 0 42 18.804 42 42s-18.804 42-42 42-42-18.804-42-42 18.804-42 42-42zm56 254c0 6.627-5.373 12-12 12h-88c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h12v-64h-12c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h64c6.627 0 12 5.373 12 12v100h12c6.627 0 12 5.373 12 12v24z" class=""></path></svg> <span class="visually-hidden">Focus to learn more</span> </button>  <div role="tooltip" id="more-info-desc-1"> <span class="left-corner"></span> arXiv-issued DOI via DataCite</div> </div> </td> </tr> <tr> <td class="tablecell label">Journal reference:</td> <td class="tablecell jref">A&A 686, A294 (2024)</td> </tr> <tr> <td class="tablecell label"> <abbr title="Digital Object Identifier">Related DOI</abbr>: </td> <td class="tablecell doi"><a href="https://doi.org/10.1051/0004-6361/202348370" data-doi="10.1051/0004-6361/202348370" class="link-https link-external" rel="external noopener nofollow">https://doi.org/10.1051/0004-6361/202348370</a>  <div class="button-and-tooltip"> <button class="more-info" aria-describedby="more-info-desc-1"> <svg height="15" role="presentation" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512"><path fill="currentColor" d="M256 8C119.043 8 8 119.083 8 256c0 136.997 111.043 248 248 248s248-111.003 248-248C504 119.083 392.957 8 256 8zm0 110c23.196 0 42 18.804 42 42s-18.804 42-42 42-42-18.804-42-42 18.804-42 42-42zm56 254c0 6.627-5.373 12-12 12h-88c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h12v-64h-12c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h64c6.627 0 12 5.373 12 12v100h12c6.627 0 12 5.373 12 12v24z" class=""></path></svg> <span class="visually-hidden">Focus to learn more</span> </button>  <div role="tooltip" id="more-info-desc-1"> <span class="left-corner"></span> DOI(s) linking to related resources </div> </div> </td> </tr> </table> </div> </div> </div> <div class="submission-history"> <h2>Submission history</h2> From: Jean Costes [<a href="/show-email/09ee0d32/2404.11523" rel="nofollow">view email</a>] <br/> <strong>[v1]</strong> Wed, 17 Apr 2024 16:15:23 UTC (8,881 KB)<br/> </div> </div>  <div class="extra-services"> <div class="full-text"> <a name="other"></a> <span class="descriptor">Full-text links:</span> <h2>Access Paper:</h2> <ul> <div id="download-button-info" hidden> View a PDF of the paper titled Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy, by J. 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[2404.11523] Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy