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 1–10 of 10 results for author: <span class="mathjax">Zamora, C</span> </h1> </div> <div class="level-right is-hidden-mobile">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> <div class="content"> <form method="GET" action="/search/astro-ph" aria-role="search"> Searching in archive <strong>astro-ph</strong>. <a href="/search/?searchtype=author&query=Zamora%2C+C">Search in all archives.</a> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Zamora, C"> </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=Zamora%2C+C&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="Zamora, C"> <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/2406.16217">arXiv:2406.16217</a> <span> [<a href="https://arxiv.org/pdf/2406.16217">pdf</a>, <a href="https://arxiv.org/format/2406.16217">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/acrefore/9780190871994.013.115">10.1093/acrefore/9780190871994.013.115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monopole Excitation and Nuclear Compressibility: Present and Future Perspectives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+J+C">J. C. Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Giraud%2C+S">S. Giraud</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.16217v1-abstract-short" style="display: inline;"> Isoscalar giant resonances are nuclear collective excitations associated with the oscillation in phase of protons and neutrons according to a certain multipolarity $L$. In particular, the isoscalar giant monopole resonance ($L=0$) is the strongest nuclear compression mode, and its excitation energy is directly related to the compression modulus for finite nuclei. Typically, microscopic calculation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16217v1-abstract-full').style.display = 'inline'; document.getElementById('2406.16217v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.16217v1-abstract-full" style="display: none;"> Isoscalar giant resonances are nuclear collective excitations associated with the oscillation in phase of protons and neutrons according to a certain multipolarity $L$. In particular, the isoscalar giant monopole resonance ($L=0$) is the strongest nuclear compression mode, and its excitation energy is directly related to the compression modulus for finite nuclei. Typically, microscopic calculations are utilized to establish a relationship between the experimental compression modulus and the nuclear incompressibility that is a crucial parameter of the equation of state for nuclear matter. The incompressibility of nuclear matter has been determined with an accuracy of 10 to 20\% using relativistic and non-relativistic microscopic models for describing the monopole distributions in ${}^{208}$Pb and ${}^{90}$Zr isotopes. However, the same theoretical models are not able to describe data for open-shell nuclei, such as those of tin and cadmium isotopes. In fact, only effective interactions with a softer nuclear-matter incompressibility are able to predict the centroid energy of monopole distributions for open-shell nuclei. An unified description of the monopole resonance in ${}^{208}$Pb and other open-shell nuclei remains unsolved from the theory side. Most of this uncertainty is due to our poor knowledge of the symmetry energy, which is another essential component of the equation of state of nuclear matter. Therefore, new experimental data along isotopic chains covering a wide range in $N/Z$ ratios, including neutron-deficient and neutron-rich nuclei, are of paramount importance for determining both the nuclear-matter incompressibility and the symmetry energy more precisely. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16217v1-abstract-full').style.display = 'none'; document.getElementById('2406.16217v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">In Oxford Research Encyclopedia of Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.10385">arXiv:2307.10385</a> <span> [<a href="https://arxiv.org/pdf/2307.10385">pdf</a>, <a href="https://arxiv.org/format/2307.10385">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/10.3847/1538-3881/ace69b">10.3847/1538-3881/ace69b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PCAT-DE: Reconstructing point-like and diffuse signals in astronomical images using spatial and spectral information </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feder%2C+R+M">Richard M. Feder</a>, <a href="/search/astro-ph?searchtype=author&query=Butler%2C+V">Victoria Butler</a>, <a href="/search/astro-ph?searchtype=author&query=Daylan%2C+T">Tansu Daylan</a>, <a href="/search/astro-ph?searchtype=author&query=Portillo%2C+S+K+N">Stephen K. N. Portillo</a>, <a href="/search/astro-ph?searchtype=author&query=Sayers%2C+J">Jack Sayers</a>, <a href="/search/astro-ph?searchtype=author&query=Vaughan%2C+B+J">Benjamin J. Vaughan</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+C+V">Catalina V. Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Zemcov%2C+M">Michael Zemcov</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="2307.10385v1-abstract-short" style="display: inline;"> Observational data from astronomical imaging surveys contain information about a variety of source populations and environments, and its complexity will increase substantially as telescopes become more sensitive. Even for existing observations, measuring the correlations between point-like and diffuse emission can be crucial to correctly inferring the properties of any individual component. For th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10385v1-abstract-full').style.display = 'inline'; document.getElementById('2307.10385v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.10385v1-abstract-full" style="display: none;"> Observational data from astronomical imaging surveys contain information about a variety of source populations and environments, and its complexity will increase substantially as telescopes become more sensitive. Even for existing observations, measuring the correlations between point-like and diffuse emission can be crucial to correctly inferring the properties of any individual component. For this task information is typically lost, either because of conservative data cuts, aggressive filtering or incomplete treatment of contaminated data. We present the code PCAT-DE, an extension of probabilistic cataloging designed to simultaneously model point-like and diffuse signals. This work incorporates both explicit spatial templates and a set of non-parametric Fourier component templates into a forward model of astronomical images, reducing the number of processing steps applied to the observed data. Using synthetic Herschel-SPIRE multiband observations, we demonstrate that point source and diffuse emission can be reliably separated and measured. We present two applications of this model. For the first, we perform point source detection/photometry in the presence of galactic cirrus and demonstrate that cosmic infrared background (CIB) galaxy counts can be recovered in cases of significant contamination. In the second we show that the spatially extended thermal Sunyaev-Zel'dovich (tSZ) effect signal can be reliably measured even when it is subdominant to the point-like emission from individual galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10385v1-abstract-full').style.display = 'none'; document.getElementById('2307.10385v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 13 figures, Accepted for publication in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.00636">arXiv:2109.00636</a> <span> [<a href="https://arxiv.org/pdf/2109.00636">pdf</a>, <a href="https://arxiv.org/format/2109.00636">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2022/04/016">10.1088/1475-7516/2022/04/016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neural networks and standard cosmography with newly calibrated high redshift GRB observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Escamilla-Rivera%2C+C">Celia Escamilla-Rivera</a>, <a href="/search/astro-ph?searchtype=author&query=Carvajal%2C+M">Maryi Carvajal</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+C">Cristian Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Hendry%2C+M">Martin Hendry</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="2109.00636v2-abstract-short" style="display: inline;"> Gamma-ray bursts (GRBs) detected at high redshift can be used to trace the cosmic expansion history. However, the calibration of their luminosity distances is not an easy task in comparison to Type Ia Supernovae (SNeIa). To calibrate these data, correlations between their luminosity and other observed properties of GRBs need to be identified, and we must consider the validity of our assumptions ab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.00636v2-abstract-full').style.display = 'inline'; document.getElementById('2109.00636v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.00636v2-abstract-full" style="display: none;"> Gamma-ray bursts (GRBs) detected at high redshift can be used to trace the cosmic expansion history. However, the calibration of their luminosity distances is not an easy task in comparison to Type Ia Supernovae (SNeIa). To calibrate these data, correlations between their luminosity and other observed properties of GRBs need to be identified, and we must consider the validity of our assumptions about these correlations over their entire observed redshift range. In this work, we propose a new method to calibrate GRBs as cosmological distance indicators using SNeIa observations with a machine learning architecture. As well we include a new data GRB calibrated sample using extended cosmography in a redshift range above $z>3.6$. An overview of this machine learning technique was developed in [1] to study the evolution of dark energy models at high redshift. The aim of the method developed in this work is to combine two networks: a Recurrent Neural Network (RNN) and a Bayesian Neural Network (BNN). Using this computational approach, denoted RNN+BNN, we extend the network's efficacy by adding the computation of covariance matrices to the Bayesian process. Once this is done, the SNeIa distance-redshift relation can be tested on the full GRB sample and therefore used to implement a cosmographic reconstruction of the distance-redshift relation in different regimes. Thus, our newly-trained neural network is used to constrain the parameters describing the kinematical state of the Universe via a cosmographic approach at high redshifts (up to $z\approx 10$), wherein we require a very minimal set of assumptions on the deep learning architecture itself that do not rely on dynamical equations for any specific theory of gravity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.00636v2-abstract-full').style.display = 'none'; document.getElementById('2109.00636v2-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">20 pages, 4 figures. Tables 1, 2 and 3 contains newly calibrated high redshift GRB. Version accepted in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.08575">arXiv:2010.08575</a> <span> [<a href="https://arxiv.org/pdf/2010.08575">pdf</a>, <a href="https://arxiv.org/format/2010.08575">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202037830">10.1051/0004-6361/202037830 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for associations containing young stars (SACY) VIII. An updated census of spectroscopic binary systems showing hints of non-universal multiplicity among these associations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Z%C3%BA%C3%B1iga-Fern%C3%A1ndez%2C+S">S. Z煤帽iga-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Elliott%2C+P">P. Elliott</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+C">C. Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Corval%C3%A1n%2C+G">G. Corval谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Haubois%2C+X">X. Haubois</a>, <a href="/search/astro-ph?searchtype=author&query=Corral-Santana%2C+J+M">J. M. Corral-Santana</a>, <a href="/search/astro-ph?searchtype=author&query=Olofsson%2C+J">J. Olofsson</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%C3%A9lamo%2C+N">N. Hu茅lamo</a>, <a href="/search/astro-ph?searchtype=author&query=Sterzik%2C+M+F">M. F. Sterzik</a>, <a href="/search/astro-ph?searchtype=author&query=Torres%2C+C+A+O">C. A. O. Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Quast%2C+G+R">G. R. Quast</a>, <a href="/search/astro-ph?searchtype=author&query=Melo%2C+C+H+F">C. H. F. Melo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.08575v2-abstract-short" style="display: inline;"> We seek to update the spectroscopy binary fraction of the SACY (Search for Associations Containing Young stars) sample taking in consideration all possible biases in our identification of binary candidates, such as activity and rotation. Using high-resolution spectroscopic observations we have produced $\sim$1300 cross-correlation functions (CCFs) to disentangle the previously mentioned sources of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.08575v2-abstract-full').style.display = 'inline'; document.getElementById('2010.08575v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.08575v2-abstract-full" style="display: none;"> We seek to update the spectroscopy binary fraction of the SACY (Search for Associations Containing Young stars) sample taking in consideration all possible biases in our identification of binary candidates, such as activity and rotation. Using high-resolution spectroscopic observations we have produced $\sim$1300 cross-correlation functions (CCFs) to disentangle the previously mentioned sources of contamination. The radial velocity values obtained were cross-matched with the literature and were used to revise and update the spectroscopic binary (SB) fraction in each of the SACY association. In order to better describe the CCF profile, we calculated a set of high-order cross-correlation features to determine the origin of the variations in radial velocities. We identified 68 SB candidates from our sample of 410 objects. Our results hint that the youngest associations have a higher SB fraction. Specifically, we found sensitivity-corrected SB fractions of $22 \substack{+15 \\ -11} \%$ for $蔚$~Cha , $31 \substack{+16 \\ -14} \%$ for TW Hya and $32 \substack{+9 \\ -8} \%$ for $尾$~Pictoris, in contrast with the five oldest ($\sim 35-125$ Myr) associations we have sampled which are $\sim 10\%$ or lower. This result seems independent of the methodology used to asses membership to the associations. The new CCF analysis, radial velocity estimates and SB candidates are particularly relevant for membership revision of targets in young stellar associations. These targets would be ideal candidates for follow-up campaigns using high-resolution techniques in order to confirm binarity, resolve the orbits, and ideally calculate dynamical masses. Additionally, if the results on SB fraction in the youngest associations are confirmed, it could hint of non-universal multiplicity among SACY associations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.08575v2-abstract-full').style.display = 'none'; document.getElementById('2010.08575v2-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">The paper has been accepted in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 645, A30 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.04747">arXiv:1910.04747</a> <span> [<a href="https://arxiv.org/pdf/1910.04747">pdf</a>, <a href="https://arxiv.org/format/1910.04747">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/10.1093/mnras/stz2888">10.1093/mnras/stz2888 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An unusually large gaseous transit in a debris disc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iglesias%2C+D+P">Daniela P. Iglesias</a>, <a href="/search/astro-ph?searchtype=author&query=Olofsson%2C+J">Johan Olofsson</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">Amelia Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Zieba%2C+S">Sebastian Zieba</a>, <a href="/search/astro-ph?searchtype=author&query=Montesinos%2C+M">Mat铆as Montesinos</a>, <a href="/search/astro-ph?searchtype=author&query=Smoker%2C+J">Jonathan Smoker</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+G+M">Grant M. Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Godoy%2C+N">Nicol谩s Godoy</a>, <a href="/search/astro-ph?searchtype=author&query=Pantoja%2C+B">Blake Pantoja</a>, <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J">Geert Jan Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Wahhaj%2C+Z">Zahed Wahhaj</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+C">Catalina Zamora</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="1910.04747v1-abstract-short" style="display: inline;"> We present the detection of an unusually large transient gas absorption in several ionized species in the debris disc star HD 37306 using high-resolution optical spectra. We have been analysing a large sample of debris discs searching for circumstellar gas absorptions aiming to determine the frequency of gas in debris discs. HD 37306 stood out showing remarkably broad absorptions superimposed onto… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.04747v1-abstract-full').style.display = 'inline'; document.getElementById('1910.04747v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.04747v1-abstract-full" style="display: none;"> We present the detection of an unusually large transient gas absorption in several ionized species in the debris disc star HD 37306 using high-resolution optical spectra. We have been analysing a large sample of debris discs searching for circumstellar gas absorptions aiming to determine the frequency of gas in debris discs. HD 37306 stood out showing remarkably broad absorptions superimposed onto several photospheric Ca ii, Fe ii and Ti ii lines. The observed absorptions, unlike typical exocometary transits, lasted for at least eight days. Here we analyse simultaneous spectroscopic and photometric data of the event and evaluate different scenarios that might explain the observed features. We conclude that the most likely scenario might be an exocometary break-up releasing a significant amount of gas close to the star, producing an occulting "ring"/"torus" shape. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.04747v1-abstract-full').style.display = 'none'; document.getElementById('1910.04747v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 10 figures, accepted in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.10378">arXiv:1908.10378</a> <span> [<a href="https://arxiv.org/pdf/1908.10378">pdf</a>, <a href="https://arxiv.org/format/1908.10378">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201935998">10.1051/0004-6361/201935998 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dust production in the debris disk around HR 4796 A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Olofsson%2C+J">J. Olofsson</a>, <a href="/search/astro-ph?searchtype=author&query=Milli%2C+J">J. Milli</a>, <a href="/search/astro-ph?searchtype=author&query=Th%C3%A9bault%2C+P">P. Th茅bault</a>, <a href="/search/astro-ph?searchtype=author&query=Kral%2C+Q">Q. Kral</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9nard%2C+F">F. M茅nard</a>, <a href="/search/astro-ph?searchtype=author&query=Janson%2C+M">M. Janson</a>, <a href="/search/astro-ph?searchtype=author&query=Augereau%2C+J+-">J. -C. Augereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Beam%C3%ADn%2C+J+C">J. C. Beam铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Th. Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Iglesias%2C+D">D. Iglesias</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+G+M">G. M. Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Montesinos%2C+M">M. Montesinos</a>, <a href="/search/astro-ph?searchtype=author&query=Pawellek%2C+N">N. Pawellek</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+M+R">M. R. Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+C">C. Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Carbillet%2C+M">M. Carbillet</a>, <a href="/search/astro-ph?searchtype=author&query=Feautrier%2C+P">P. Feautrier</a>, <a href="/search/astro-ph?searchtype=author&query=Fusco%2C+T">T. Fusco</a>, <a href="/search/astro-ph?searchtype=author&query=Madec%2C+F">F. Madec</a>, <a href="/search/astro-ph?searchtype=author&query=Rabou%2C+P">P. Rabou</a>, <a href="/search/astro-ph?searchtype=author&query=Sevin%2C+A">A. Sevin</a>, <a href="/search/astro-ph?searchtype=author&query=Szul%C3%A1gyi%2C+J">J. Szul谩gyi</a>, <a href="/search/astro-ph?searchtype=author&query=Zurlo%2C+A">A. Zurlo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1908.10378v1-abstract-short" style="display: inline;"> Debris disks are the natural by-products of the planet formation process. Scattered or polarized light observations are mostly sensitive to small dust grains that are released from the grinding down of bigger planetesimals. High angular resolution observations at optical wavelengths can provide key constraints on the radial and azimuthal distribution of the small dust grains. These constraints can… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.10378v1-abstract-full').style.display = 'inline'; document.getElementById('1908.10378v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.10378v1-abstract-full" style="display: none;"> Debris disks are the natural by-products of the planet formation process. Scattered or polarized light observations are mostly sensitive to small dust grains that are released from the grinding down of bigger planetesimals. High angular resolution observations at optical wavelengths can provide key constraints on the radial and azimuthal distribution of the small dust grains. These constraints can help us better understand where most of the dust grains are released upon collisions. We present SPHERE/ZIMPOL observations of the debris disk around HR 4796 A, and model the radial profiles along several azimuthal angles of the disk with a code that accounts for the effect of stellar radiation pressure. This enables us to derive an appropriate description for the radial and azimuthal distribution of the small dust grains. Even though we only model the radial profiles along (or close to) the semi-major axis of the disk, our best-fit model is not only in good agreement with our observations but also with previously published datasets (from near-IR to sub-mm wavelengths). We find that the reference radius is located at $76.4\pm0.4$ au, and the disk has an eccentricity of $0.076_{-0.010}^{+0.016}$, with the pericenter located on the front side of the disk (north of the star). We find that small dust grains must be preferentially released near the pericenter to explain the observed brightness asymmetry. Even though parent bodies spend more time near the apocenter, the brightness asymmetry implies that collisions happen more frequently near the pericenter of the disk. Our model can successfully reproduce the shape of the outer edge of the disk, without having to invoke an outer planet shepherding the debris disk. With a simple treatment of the effect of the radiation pressure, we conclude that the parent planetesimals are located in a narrow ring of about $3.6$ au in width. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.10378v1-abstract-full').style.display = 'none'; document.getElementById('1908.10378v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 figures, accepted by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 630, A142 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.03985">arXiv:1908.03985</a> <span> [<a href="https://arxiv.org/pdf/1908.03985">pdf</a>, <a href="https://arxiv.org/ps/1908.03985">ps</a>, <a href="https://arxiv.org/format/1908.03985">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.100.045805">10.1103/PhysRevC.100.045805 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints for stellar electron-capture rates on $^{86}$Kr via the $^{86}$Kr($t$,$^{3}$He$+纬$)$^{86}$Br reaction and the implications for core-collapse supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Titus%2C+R">R. Titus</a>, <a href="/search/astro-ph?searchtype=author&query=Ney%2C+E+M">E. M. Ney</a>, <a href="/search/astro-ph?searchtype=author&query=Zegers%2C+R+G+T">R. G. T. Zegers</a>, <a href="/search/astro-ph?searchtype=author&query=Bazin%2C+D">D. Bazin</a>, <a href="/search/astro-ph?searchtype=author&query=Belarge%2C+J">J. Belarge</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+P+C">P. C. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Campbell%2C+C+M">C. M. Campbell</a>, <a href="/search/astro-ph?searchtype=author&query=Elman%2C+B">B. Elman</a>, <a href="/search/astro-ph?searchtype=author&query=Engel%2C+J">J. Engel</a>, <a href="/search/astro-ph?searchtype=author&query=Gade%2C+A">A. Gade</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+B">B. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Kwan%2C+E">E. Kwan</a>, <a href="/search/astro-ph?searchtype=author&query=Lipschutz%2C+S">S. Lipschutz</a>, <a href="/search/astro-ph?searchtype=author&query=Longfellow%2C+B">B. Longfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Lunderberg%2C+E">E. Lunderberg</a>, <a href="/search/astro-ph?searchtype=author&query=Mijatovic%2C+T">T. Mijatovic</a>, <a href="/search/astro-ph?searchtype=author&query=Noji%2C+S">S. Noji</a>, <a href="/search/astro-ph?searchtype=author&query=Pereira%2C+J">J. Pereira</a>, <a href="/search/astro-ph?searchtype=author&query=Schmitt%2C+J">J. Schmitt</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+C">C. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Weisshaar%2C+D">D. Weisshaar</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+J+C">J. C. Zamora</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1908.03985v1-abstract-short" style="display: inline;"> In the late stages of stellar core-collapse, prior to core bounce, electron captures on medium-heavy nuclei drive deleptonization and simulations require the use of accurate reaction rates. Nuclei with neutron number near $N=50$, just above atomic number $Z=28$, play an important role, but rates used in astrophysical simulations rely primarily on a relatively simple single-state approximation. In… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.03985v1-abstract-full').style.display = 'inline'; document.getElementById('1908.03985v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.03985v1-abstract-full" style="display: none;"> In the late stages of stellar core-collapse, prior to core bounce, electron captures on medium-heavy nuclei drive deleptonization and simulations require the use of accurate reaction rates. Nuclei with neutron number near $N=50$, just above atomic number $Z=28$, play an important role, but rates used in astrophysical simulations rely primarily on a relatively simple single-state approximation. In order to improve the accuracy of astrophysical simulations, experimental data are needed to test the electron-capture rates and to guide the development of better theoretical models. This work presents the results of the $^{86}$Kr($t$,$^{3}$He+$纬$) experiment at the NSCL, from which an upper limit for the Gamow-Teller strength up to an excitation energy in $^{86}$Br of 5 MeV is extracted. The derived upper limit for the electron-capture rate on $^{86}$Kr indicates that the rate estimated through the single-state approximation is too high and that rates based on Gamow-Teller strengths estimated in shell-model and QRPA calculations are more accurate. The QRPA calculations tested in this manner were used for estimating the electron capture rates for 78 isotopes near $N=50$ and above $Z=28$. The impact of using these new electron-capture rates in simulations of supernovae instead of the rates based on the single-state approximation is investigated, indicating a significant reduction in the deleptonization that affects multi-messenger signals, such as the emission of neutrinos and gravitational waves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.03985v1-abstract-full').style.display = 'none'; document.getElementById('1908.03985v1-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 100, 045805 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.06091">arXiv:1906.06091</a> <span> [<a href="https://arxiv.org/pdf/1906.06091">pdf</a>, <a href="https://arxiv.org/format/1906.06091">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.122.232701">10.1103/PhysRevLett.122.232701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the Neutron Star Compactness: Extraction of the $^{23}$Al($p,纬$) Reaction Rate for the $rp$-Process </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+C">C. Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Langer%2C+C">C. Langer</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+F">F. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Pereira%2C+J">J. Pereira</a>, <a href="/search/astro-ph?searchtype=author&query=Ong%2C+W+-">W. -J. Ong</a>, <a href="/search/astro-ph?searchtype=author&query=Poxon-Pearson%2C+T">T. Poxon-Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+S">S. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Ayoub%2C+S">S. Ayoub</a>, <a href="/search/astro-ph?searchtype=author&query=Baumann%2C+T">T. Baumann</a>, <a href="/search/astro-ph?searchtype=author&query=Bazin%2C+D">D. Bazin</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+P+C">P. C. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Browne%2C+J">J. Browne</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+H">H. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Cyburt%2C+R+H">R. H. Cyburt</a>, <a href="/search/astro-ph?searchtype=author&query=Deleeuw%2C+E">E. Deleeuw</a>, <a href="/search/astro-ph?searchtype=author&query=Elman%2C+B">B. Elman</a>, <a href="/search/astro-ph?searchtype=author&query=Fiebiger%2C+S">S. Fiebiger</a>, <a href="/search/astro-ph?searchtype=author&query=Gade%2C+A">A. Gade</a>, <a href="/search/astro-ph?searchtype=author&query=Gastis%2C+P">P. Gastis</a>, <a href="/search/astro-ph?searchtype=author&query=Lipschutz%2C+S">S. Lipschutz</a>, <a href="/search/astro-ph?searchtype=author&query=Longfellow%2C+B">B. Longfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Meisel%2C+Z">Z. Meisel</a>, <a href="/search/astro-ph?searchtype=author&query=Nunes%2C+F+M">F. M. Nunes</a>, <a href="/search/astro-ph?searchtype=author&query=Perdikakis%2C+G">G. Perdikakis</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1906.06091v1-abstract-short" style="display: inline;"> The $^{23}$Al($p,纬$)$^{24}$Si reaction is among the most important reactions driving the energy generation in Type-I X-ray bursts. However, the present reaction-rate uncertainty limits constraints on neutron star properties that can be achieved with burst model-observation comparisons. Here, we present a novel technique for constraining this important reaction by combining the GRETINA array with t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.06091v1-abstract-full').style.display = 'inline'; document.getElementById('1906.06091v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.06091v1-abstract-full" style="display: none;"> The $^{23}$Al($p,纬$)$^{24}$Si reaction is among the most important reactions driving the energy generation in Type-I X-ray bursts. However, the present reaction-rate uncertainty limits constraints on neutron star properties that can be achieved with burst model-observation comparisons. Here, we present a novel technique for constraining this important reaction by combining the GRETINA array with the neutron detector LENDA coupled to the S800 spectrograph at the National Superconducting Cyclotron Laboratory. The $^{23}$Al($d,n$) reaction was used to populate the astrophysically important states in $^{24}$Si. This enables a measurement in complete kinematics for extracting all relevant inputs necessary to calculate the reaction rate. For the first time, a predicted close-lying doublet of a 2$_2^+$ and (4$_1^+$,0$_2^+$) state in $^{24}$Si was disentangled, finally resolving conflicting results from two previous measurements. Moreover, it was possible to extract spectroscopic factors using GRETINA and LENDA simultaneously. This new technique may be used to constrain other important reaction rates for various astrophysical scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.06091v1-abstract-full').style.display = 'none'; document.getElementById('1906.06091v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physical Review Letter 122, 232701 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.05934">arXiv:1906.05934</a> <span> [<a href="https://arxiv.org/pdf/1906.05934">pdf</a>, <a href="https://arxiv.org/format/1906.05934">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</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/10.1103/PhysRevC.100.032801">10.1103/PhysRevC.100.032801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental Constraint on Stellar Electron-Capture Rates from the ${}^{88}\text{Sr}(t,{}^{3}\text{He}+纬){}^{88}\text{Rb}$ reaction at 115 MeV/u </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+J+C">J. C. Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Zegers%2C+R+G+T">R. G. T. Zegers</a>, <a href="/search/astro-ph?searchtype=author&query=Austin%2C+S+M">Sam M. Austin</a>, <a href="/search/astro-ph?searchtype=author&query=Bazin%2C+D">D. Bazin</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+P+C">P. C. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+H+L">H. L. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Engel%2C+J">J. Engel</a>, <a href="/search/astro-ph?searchtype=author&query=Falduto%2C+A">A. Falduto</a>, <a href="/search/astro-ph?searchtype=author&query=Gade%2C+A">A. Gade</a>, <a href="/search/astro-ph?searchtype=author&query=Gastis%2C+P">P. Gastis</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+B">B. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Ginter%2C+T">T. Ginter</a>, <a href="/search/astro-ph?searchtype=author&query=Guess%2C+C+J">C. J. Guess</a>, <a href="/search/astro-ph?searchtype=author&query=Lipschutz%2C+S">S. Lipschutz</a>, <a href="/search/astro-ph?searchtype=author&query=Longfellow%2C+B">B. Longfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Macchiavelli%2C+A+O">A. O. Macchiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Miki%2C+K">K. Miki</a>, <a href="/search/astro-ph?searchtype=author&query=Ney%2C+E">E. Ney</a>, <a href="/search/astro-ph?searchtype=author&query=Noji%2C+S">S. Noji</a>, <a href="/search/astro-ph?searchtype=author&query=Pereira%2C+J">J. Pereira</a>, <a href="/search/astro-ph?searchtype=author&query=Schmitt%2C+J">J. Schmitt</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+C">C. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Titus%2C+R">R. Titus</a>, <a href="/search/astro-ph?searchtype=author&query=Weisshaar%2C+D">D. Weisshaar</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="1906.05934v1-abstract-short" style="display: inline;"> The Gamow-Teller strength distribution from ${}^{88}$Sr was extracted from a $(t,{}^{3}\text{He}+纬)$ experiment at 115 MeV/$u$ to constrain estimates for the electron-capture rates on nuclei around $N=50$, between and including $^{78}$Ni and $^{88}$Sr, which are important for the late evolution of core-collapse supernovae. The observed strength below an excitation energy of 8 MeV was consistent wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.05934v1-abstract-full').style.display = 'inline'; document.getElementById('1906.05934v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.05934v1-abstract-full" style="display: none;"> The Gamow-Teller strength distribution from ${}^{88}$Sr was extracted from a $(t,{}^{3}\text{He}+纬)$ experiment at 115 MeV/$u$ to constrain estimates for the electron-capture rates on nuclei around $N=50$, between and including $^{78}$Ni and $^{88}$Sr, which are important for the late evolution of core-collapse supernovae. The observed strength below an excitation energy of 8 MeV was consistent with zero and below 10 MeV amounted to $0.1\pm0.05$. Except for a very-weak transition that could come from the 2.231-MeV $1^{+}$ state, no $纬$ lines that could be associated with the decay of known $1^{+}$ states were identified. The derived electron-capture rate from the measured strength distribution is more than an order of magnitude smaller than rates based on the single-state approximation presently used in astrophysical simulations for most nuclei near $N=50$. Rates based on shell-model and quasiparticle random-phase approximation calculations that account for Pauli blocking and core-polarization effects provide better estimates than the single-state approximation, although a relatively strong transition to the first $1^{+}$ state in $^{88}$Rb is not observed in the data. Pauli unblocking effects due to high stellar temperatures could partially counter the low electron-capture rates. The new data serves as a zero-temperature benchmark for constraining models used to estimate such effects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.05934v1-abstract-full').style.display = 'none'; document.getElementById('1906.05934v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.09252">arXiv:1806.09252</a> <span> [<a href="https://arxiv.org/pdf/1806.09252">pdf</a>, <a href="https://arxiv.org/format/1806.09252">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/10.1093/mnras/stz1133">10.1093/mnras/stz1133 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sub-millimeter non-contaminated detection of the disk around TWA\,7 by ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Olofsson%2C+J">J. Olofsson</a>, <a href="/search/astro-ph?searchtype=author&query=Matra%2C+L">L. Matra</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Gallardo%2C+J">J. Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=de+Gregorio-Monsalvo%2C+I">I. de Gregorio-Monsalvo</a>, <a href="/search/astro-ph?searchtype=author&query=Booth%2C+M">M. Booth</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+C">C. Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Iglesias%2C+D">D. Iglesias</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Th. Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+M+R">M. R. Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">C. Caceres</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1806.09252v3-abstract-short" style="display: inline;"> Debris disks can be seen as the left-overs of giant planet formation and the possible nurseries of rocky planets. While M-type stars out-number more massive stars we know very little about the time evolution of their circumstellar disks at ages older than $\sim 10$\,Myr. Sub-millimeter observations are best to provide first order estimates of the available mass reservoir and thus better constrain… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09252v3-abstract-full').style.display = 'inline'; document.getElementById('1806.09252v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.09252v3-abstract-full" style="display: none;"> Debris disks can be seen as the left-overs of giant planet formation and the possible nurseries of rocky planets. While M-type stars out-number more massive stars we know very little about the time evolution of their circumstellar disks at ages older than $\sim 10$\,Myr. Sub-millimeter observations are best to provide first order estimates of the available mass reservoir and thus better constrain the evolution of such disks. Here, we present ALMA Cycle\,3 Band\,7 observations of the debris disk around the M2 star TWA\,7, which had been postulated to harbor two spatially separated dust belts, based on unresolved far-infrared and sub-millimeter data. We show that most of the emission at wavelengths longer than $\sim 300$\,$渭$m is in fact arising from a contaminant source, most likely a sub-mm galaxy, located at about 6.6" East of TWA\,7 (in 2016). Fortunately, the high resolution of our ALMA data allows us to disentangle the contaminant emission from that of the disc and report a significant detection of the disk in the sub-millimeter for the first time with a flux density of 2.1$\pm$0.4 mJy at 870 $渭$m. With this detection, we show that the SED can be reproduced with a single dust belt. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09252v3-abstract-full').style.display = 'none'; document.getElementById('1806.09252v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, accepted to MNRAS</span> </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