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 1–21 of 21 results for author: <span class="mathjax">Ambrosone, A</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=Ambrosone%2C+A">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="Ambrosone, A"> </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=Ambrosone%2C+A&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="Ambrosone, A"> <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/2411.10092">arXiv:2411.10092</a> <span> [<a href="https://arxiv.org/pdf/2411.10092">pdf</a>, <a href="https://arxiv.org/format/2411.10092">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> First Searches for Dark Matter with the KM3NeT Neutrino Telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=KM3NeT+Collaboration"> KM3NeT Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alhebsi%2C+A+R">A. R. Alhebsi</a>, <a href="/search/astro-ph?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/astro-ph?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/astro-ph?searchtype=author&query=Bennani%2C+M">M. Bennani</a>, <a href="/search/astro-ph?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a>, <a href="/search/astro-ph?searchtype=author&query=Berbee%2C+E">E. Berbee</a> , et al. (240 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="2411.10092v1-abstract-short" style="display: inline;"> Indirect dark matter detection methods are used to observe the products of dark matter annihilations or decays originating from astrophysical objects where large amounts of dark matter are thought to accumulate. With neutrino telescopes, an excess of neutrinos is searched for in nearby dark matter reservoirs, such as the Sun and the Galactic Centre, which could potentially produce a sizeable flux… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10092v1-abstract-full').style.display = 'inline'; document.getElementById('2411.10092v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10092v1-abstract-full" style="display: none;"> Indirect dark matter detection methods are used to observe the products of dark matter annihilations or decays originating from astrophysical objects where large amounts of dark matter are thought to accumulate. With neutrino telescopes, an excess of neutrinos is searched for in nearby dark matter reservoirs, such as the Sun and the Galactic Centre, which could potentially produce a sizeable flux of Standard Model particles. The KM3NeT infrastructure, currently under construction, comprises the ARCA and ORCA undersea 膶erenkov neutrino detectors located at two different sites in the Mediterranean Sea, offshore of Italy and France, respectively. The two detector configurations are optimised for the detection of neutrinos of different energies, enabling the search for dark matter particles with masses ranging from a few GeV/c$^2$ to hundreds of TeV/c$^2$. In this work, searches for dark matter annihilations in the Galactic Centre and the Sun with data samples taken with the first configurations of both detectors are presented. No significant excess over the expected background was found in either of the two analyses. Limits on the velocity-averaged self-annihilation cross section of dark matter particles are computed for five different primary annihilation channels in the Galactic Centre. For the Sun, limits on the spin-dependent and spin-independent scattering cross sections of dark matter with nucleons are given for three annihilation channels. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10092v1-abstract-full').style.display = 'none'; document.getElementById('2411.10092v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.24115">arXiv:2410.24115</a> <span> [<a href="https://arxiv.org/pdf/2410.24115">pdf</a>, <a href="https://arxiv.org/format/2410.24115">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-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="Computational Physics">physics.comp-ph</span> </div> </div> <p class="title is-5 mathjax"> gSeaGen code by KM3NeT: an efficient tool to propagate muons simulated with CORSIKA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alhebsi%2C+A+R">A. R. Alhebsi</a>, <a href="/search/astro-ph?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/astro-ph?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/astro-ph?searchtype=author&query=Bennani%2C+M">M. Bennani</a>, <a href="/search/astro-ph?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a>, <a href="/search/astro-ph?searchtype=author&query=Berbee%2C+E">E. Berbee</a> , et al. (238 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="2410.24115v4-abstract-short" style="display: inline;"> The KM3NeT Collaboration has tackled a common challenge faced by the astroparticle physics community, namely adapting the experiment-specific simulation software to work with the CORSIKA air shower simulation output. The proposed solution is an extension of the open-source code gSeaGen, allowing for the transport of muons generated by CORSIKA to a detector of any size at an arbitrary depth. The gS… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.24115v4-abstract-full').style.display = 'inline'; document.getElementById('2410.24115v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.24115v4-abstract-full" style="display: none;"> The KM3NeT Collaboration has tackled a common challenge faced by the astroparticle physics community, namely adapting the experiment-specific simulation software to work with the CORSIKA air shower simulation output. The proposed solution is an extension of the open-source code gSeaGen, allowing for the transport of muons generated by CORSIKA to a detector of any size at an arbitrary depth. The gSeaGen code was not only extended in terms of functionalities but also underwent a thorough redesign of the muon propagation routine, resulting in a more accurate and efficient simulation. This paper presents the capabilities of the new gSeaGen code as well as prospects for further developments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.24115v4-abstract-full').style.display = 'none'; document.getElementById('2410.24115v4-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">27 pages, 13 figures, submitted to Computer Physics Communications</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.05292">arXiv:2408.05292</a> <span> [<a href="https://arxiv.org/pdf/2408.05292">pdf</a>, <a href="https://arxiv.org/format/2408.05292">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Large-scale cosmic ray anisotropies with 19 years of data from the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Dourado%2C+L+A">L. Andrade Dourado</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a> , et al. (333 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="2408.05292v2-abstract-short" style="display: inline;"> Results are presented for the measurement of large-scale anisotropies in the arrival directions of ultra-high-energy cosmic rays detected at the Pierre Auger Observatory during 19 years of operation, prior to AugerPrime, the upgrade of the Observatory. The 3D dipole amplitude and direction are reconstructed above $4\,$EeV in four energy bins. Besides the established dipolar anisotropy in right asc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.05292v2-abstract-full').style.display = 'inline'; document.getElementById('2408.05292v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.05292v2-abstract-full" style="display: none;"> Results are presented for the measurement of large-scale anisotropies in the arrival directions of ultra-high-energy cosmic rays detected at the Pierre Auger Observatory during 19 years of operation, prior to AugerPrime, the upgrade of the Observatory. The 3D dipole amplitude and direction are reconstructed above $4\,$EeV in four energy bins. Besides the established dipolar anisotropy in right ascension above $8\,$EeV, the Fourier amplitude of the $8$ to $16\,$EeV energy bin is now also above the $5蟽$ discovery level. No time variation of the dipole moment above $8\,$EeV is found, setting an upper limit to the rate of change of such variations of $0.3\%$ per year at the $95\%$ confidence level. Additionally, the results for the angular power spectrum are shown, demonstrating no other statistically significant multipoles. The results for the equatorial dipole component down to $0.03\,$EeV are presented, using for the first time a data set obtained with a trigger that has been optimized for lower energies. Finally, model predictions are discussed and compared with observations, based on two source emission scenarios obtained in the combined fit of spectrum and composition above $0.6\,$EeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.05292v2-abstract-full').style.display = 'none'; document.getElementById('2408.05292v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Minor modifications, accepted for publication in Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.13336">arXiv:2406.13336</a> <span> [<a href="https://arxiv.org/pdf/2406.13336">pdf</a>, <a href="https://arxiv.org/format/2406.13336">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Berezinsky Hidden Sources: An Emergent Tension in the High-Energy Neutrino Sky? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">Antonio Ambrosone</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="2406.13336v1-abstract-short" style="display: inline;"> The IceCube Collaboration has recently reported compelling evidence of high-energy neutrino emission from NGC~1068, and also mild excesses for NGC 4151 and CGCG420-015, local Seyfert galaxies. This has increased the interest along neutrino emission from hot-corona surrounding the super massive black holes of Seyfert Galaxies. In this paper, we revisit phenomenological constraints on the neutrino e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.13336v1-abstract-full').style.display = 'inline'; document.getElementById('2406.13336v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.13336v1-abstract-full" style="display: none;"> The IceCube Collaboration has recently reported compelling evidence of high-energy neutrino emission from NGC~1068, and also mild excesses for NGC 4151 and CGCG420-015, local Seyfert galaxies. This has increased the interest along neutrino emission from hot-corona surrounding the super massive black holes of Seyfert Galaxies. In this paper, we revisit phenomenological constraints on the neutrino emission from hot-coronae of seyfert galaxies, using an assumption of equi-ripartition between cosmic-rays and magnetic energy densities. We show that not only these sources are consistent with such an assumption but also that the data point towards low beta plasma parameters inside Seyfert Galaxies. We exploit this finding to constrain the Seyfert diffuse neutrino flux and we obtain that, in order not to overproduce neutrinos, not all the sources can be in an equi-ripartition state. We conclude (along with previous findings) that seyfert galaxies cannot explain the diffuse neutrino spectrum above $\sim 100\, \rm TeV$, allowing space for other astrophysical sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.13336v1-abstract-full').style.display = 'none'; document.getElementById('2406.13336v1-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 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">17 pages, 1 Table, 6 Figures, 1 appendix</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.05354">arXiv:2404.05354</a> <span> [<a href="https://arxiv.org/pdf/2404.05354">pdf</a>, <a href="https://arxiv.org/format/2404.05354">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Search for Neutrino Emission from GRB 221009A using the KM3NeT ARCA and ORCA detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androutsou%2C+E">E. Androutsou</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/astro-ph?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/astro-ph?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a> , et al. (251 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="2404.05354v2-abstract-short" style="display: inline;"> Gamma-ray bursts are promising candidate sources of high-energy astrophysical neutrinos. The recent GRB 221009A event, identified as the brightest gamma-ray burst ever detected, provides a unique opportunity to investigate hadronic emissions involving neutrinos. The KM3NeT undersea neutrino detectors participated in the worldwide follow-up effort triggered by the event, searching for neutrino even… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05354v2-abstract-full').style.display = 'inline'; document.getElementById('2404.05354v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.05354v2-abstract-full" style="display: none;"> Gamma-ray bursts are promising candidate sources of high-energy astrophysical neutrinos. The recent GRB 221009A event, identified as the brightest gamma-ray burst ever detected, provides a unique opportunity to investigate hadronic emissions involving neutrinos. The KM3NeT undersea neutrino detectors participated in the worldwide follow-up effort triggered by the event, searching for neutrino events. In this letter, we summarize subsequent searches, in a wide energy range from MeV up to a few PeVs. No neutrino events are found in any of the searches performed. Upper limits on the neutrino emission associated with GRB 221009A are computed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05354v2-abstract-full').style.display = 'none'; document.getElementById('2404.05354v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">11 pages, 2 PDF figures. Submitted to 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/2402.18638">arXiv:2402.18638</a> <span> [<a href="https://arxiv.org/pdf/2402.18638">pdf</a>, <a href="https://arxiv.org/format/2402.18638">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/08/040">10.1088/1475-7516/2024/08/040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the hadronic properties of star-forming galaxies above $1\, \rm GeV$ with 15-years Fermi-LAT data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">Antonio Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Chianese%2C+M">Marco Chianese</a>, <a href="/search/astro-ph?searchtype=author&query=Marinelli%2C+A">Antonio Marinelli</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="2402.18638v3-abstract-short" style="display: inline;"> Star-forming and starburst galaxies (SFGs and SBGs) are powerful emitters of non-thermal $纬$-rays and neutrinos, due to their intense phases of star-formation activity, which should confine high-energy Cosmic-Rays (CRs) inside their environments. In this paper, using the publicly-available \texttt{fermitools}, we analyse 15.3 years of $纬$-ray between $1-1000\, \rm GeV$ data for 70 sources, 56 of w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18638v3-abstract-full').style.display = 'inline'; document.getElementById('2402.18638v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18638v3-abstract-full" style="display: none;"> Star-forming and starburst galaxies (SFGs and SBGs) are powerful emitters of non-thermal $纬$-rays and neutrinos, due to their intense phases of star-formation activity, which should confine high-energy Cosmic-Rays (CRs) inside their environments. In this paper, using the publicly-available \texttt{fermitools}, we analyse 15.3 years of $纬$-ray between $1-1000\, \rm GeV$ data for 70 sources, 56 of which were not previously detected. We find at~$4蟽$ level an indication of $纬$-ray emission for other two SBGs, namely M 83 and NGC 1365. By contrast, we find that, even with the new description of background, the significance for the $纬$-ray emission of M 33~(initially reported as discovered) still stands at $\sim \, 4蟽$ (as already reported by previous works). Along with previous findings, the flux of each detected source is consistent with a $\sim E^{-2.3/2.4}$ spectrum, compatible with the injected CR flux inferred for CRs in the Milky-Way. We notice that the correlation between the calorimetric fraction~$F_{\rm cal}$ of high-energy protons in SFGs and SBGs (the fraction of high-energy protons actually producing high-energy $纬$-rays and neutrinos) and the SFR is in accordance with the expected scaling relation for CR escape dominated by advection. We remark that undiscovered sources strongly constrain $F_{\rm cal}$ at 95\% CL, providing fundamental information when we interpret the results as common properties of SFGs and SBGs. Finally, we find that these sources might contribute $(12\pm 3)\%$ to the EGB, while the corresponding diffuse neutrino flux strongly depends on the spectral index distribution along the source class. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18638v3-abstract-full').style.display = 'none'; document.getElementById('2402.18638v3-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">32 pages, 9 figures, 16 Tables. Version 3</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.08363">arXiv:2402.08363</a> <span> [<a href="https://arxiv.org/pdf/2402.08363">pdf</a>, <a href="https://arxiv.org/format/2402.08363">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1140/epjc/s10052-024-13137-2">10.1140/epjc/s10052-024-13137-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Astronomy potential of KM3NeT/ARCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androutsou%2C+E">E. Androutsou</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/astro-ph?searchtype=author&query=Bardacov%C3%A1%2C+Z">Z. Bardacov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Baruzzi%2C+A">A. Baruzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a> , et al. (253 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="2402.08363v3-abstract-short" style="display: inline;"> The KM3NeT/ARCA neutrino detector is currently under construction at 3500 m depth offshore Capo Passero, Sicily, in the Mediterranean Sea. The main science objectives are the detection of high-energy cosmic neutrinos and the discovery of their sources. Simulations were conducted for the full KM3NeT/ARCA detector, instrumenting a volume of 1 km$^3$, to estimate the sensitivity and discovery potenti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08363v3-abstract-full').style.display = 'inline'; document.getElementById('2402.08363v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08363v3-abstract-full" style="display: none;"> The KM3NeT/ARCA neutrino detector is currently under construction at 3500 m depth offshore Capo Passero, Sicily, in the Mediterranean Sea. The main science objectives are the detection of high-energy cosmic neutrinos and the discovery of their sources. Simulations were conducted for the full KM3NeT/ARCA detector, instrumenting a volume of 1 km$^3$, to estimate the sensitivity and discovery potential to point-like neutrino sources and an all-sky diffuse neutrino flux. This paper covers the reconstruction of track- and shower-like signatures, as well as the criteria employed for neutrino event selection. By leveraging both the track and shower observation channels, the KM3NeT/ARCA detector demonstrates the capability to detect the diffuse astrophysical neutrino flux within half a year of operation, achieving a 5$蟽$ statistical significance. With an angular resolution below 0.1$^\circ$ for tracks and under 2$^\circ$ for showers, the sensitivity to point-like neutrino sources surpasses existing observed limits across the entire sky. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08363v3-abstract-full').style.display = 'none'; document.getElementById('2402.08363v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">20 pages, 30 figures, Published by EPJ-C</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 84, 885 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.14872">arXiv:2311.14872</a> <span> [<a href="https://arxiv.org/pdf/2311.14872">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> The Power Board of the KM3NeT Digital Optical Module: design, upgrade, and production </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androutsou%2C+E">E. Androutsou</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/astro-ph?searchtype=author&query=Bardacova%2C+Z">Z. Bardacova</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana%2C+A+B">A. Bariego Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/astro-ph?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a> , et al. (259 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="2311.14872v1-abstract-short" style="display: inline;"> The KM3NeT Collaboration is building an underwater neutrino observatory at the bottom of the Mediterranean Sea consisting of two neutrino telescopes, both composed of a three-dimensional array of light detectors, known as digital optical modules. Each digital optical module contains a set of 31 three inch photomultiplier tubes distributed over the surface of a 0.44 m diameter pressure-resistant gl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.14872v1-abstract-full').style.display = 'inline'; document.getElementById('2311.14872v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.14872v1-abstract-full" style="display: none;"> The KM3NeT Collaboration is building an underwater neutrino observatory at the bottom of the Mediterranean Sea consisting of two neutrino telescopes, both composed of a three-dimensional array of light detectors, known as digital optical modules. Each digital optical module contains a set of 31 three inch photomultiplier tubes distributed over the surface of a 0.44 m diameter pressure-resistant glass sphere. The module includes also calibration instruments and electronics for power, readout and data acquisition. The power board was developed to supply power to all the elements of the digital optical module. The design of the power board began in 2013, and several prototypes were produced and tested. After an exhaustive validation process in various laboratories within the KM3NeT Collaboration, a mass production batch began, resulting in the construction of over 1200 power boards so far. These boards were integrated in the digital optical modules that have already been produced and deployed, 828 until October 2023. In 2017, an upgrade of the power board, to increase reliability and efficiency, was initiated. After the validation of a pre-production series, a production batch of 800 upgraded boards is currently underway. This paper describes the design, architecture, upgrade, validation, and production of the power board, including the reliability studies and tests conducted to ensure the safe operation at the bottom of the Mediterranean Sea throughout the observatory's lifespan <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.14872v1-abstract-full').style.display = 'none'; document.getElementById('2311.14872v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.03804">arXiv:2311.03804</a> <span> [<a href="https://arxiv.org/pdf/2311.03804">pdf</a>, <a href="https://arxiv.org/format/2311.03804">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1088/1475-7516/2024/04/026">10.1088/1475-7516/2024/04/026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searches for neutrino counterparts of gravitational waves from the LIGO/Virgo third observing run with KM3NeT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=KM3NeT+Collaboration"> KM3NeT Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androutsou%2C+E">E. Androutsou</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/astro-ph?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/astro-ph?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a> , et al. (251 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="2311.03804v2-abstract-short" style="display: inline;"> The KM3NeT neutrino telescope is currently being deployed at two different sites in the Mediterranean Sea. First searches for astrophysical neutrinos have been performed using data taken with the partial detector configuration already in operation. The paper presents the results of two independent searches for neutrinos from compact binary mergers detected during the third observing run of the LIG… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03804v2-abstract-full').style.display = 'inline'; document.getElementById('2311.03804v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.03804v2-abstract-full" style="display: none;"> The KM3NeT neutrino telescope is currently being deployed at two different sites in the Mediterranean Sea. First searches for astrophysical neutrinos have been performed using data taken with the partial detector configuration already in operation. The paper presents the results of two independent searches for neutrinos from compact binary mergers detected during the third observing run of the LIGO and Virgo gravitational wave interferometers. The first search looks for a global increase in the detector counting rates that could be associated with inverse beta decay events generated by MeV-scale electron anti-neutrinos. The second one focuses on upgoing track-like events mainly induced by muon (anti-)neutrinos in the GeV--TeV energy range. Both searches yield no significant excess for the sources in the gravitational wave catalogs. For each source, upper limits on the neutrino flux and on the total energy emitted in neutrinos in the respective energy ranges have been set. Stacking analyses of binary black hole mergers and neutron star-black hole mergers have also been performed to constrain the characteristic neutrino emission from these categories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03804v2-abstract-full').style.display = 'none'; document.getElementById('2311.03804v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">19 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 04 (2024) 026 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03007">arXiv:2309.03007</a> <span> [<a href="https://arxiv.org/pdf/2309.03007">pdf</a>, <a href="https://arxiv.org/format/2309.03007">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-023-12279-z">10.1140/epjc/s10052-023-12279-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for combined analyses of hadronic emission from $纬$-ray sources in the Milky Way with CTA and KM3NeT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Unbehaun%2C+T">T. Unbehaun</a>, <a href="/search/astro-ph?searchtype=author&query=Mohrmann%2C+L">L. Mohrmann</a>, <a href="/search/astro-ph?searchtype=author&query=Funk%2C+S">S. Funk</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androutsou%2C+E">E. Androutsou</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/astro-ph?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/astro-ph?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a> , et al. (249 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="2309.03007v2-abstract-short" style="display: inline;"> The Cherenkov Telescope Array and the KM3NeT neutrino telescopes are major upcoming facilities in the fields of $纬$-ray and neutrino astronomy, respectively. Possible simultaneous production of $纬$ rays and neutrinos in astrophysical accelerators of cosmic-ray nuclei motivates a combination of their data. We assess the potential of a combined analysis of CTA and KM3NeT data to determine the contri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03007v2-abstract-full').style.display = 'inline'; document.getElementById('2309.03007v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03007v2-abstract-full" style="display: none;"> The Cherenkov Telescope Array and the KM3NeT neutrino telescopes are major upcoming facilities in the fields of $纬$-ray and neutrino astronomy, respectively. Possible simultaneous production of $纬$ rays and neutrinos in astrophysical accelerators of cosmic-ray nuclei motivates a combination of their data. We assess the potential of a combined analysis of CTA and KM3NeT data to determine the contribution of hadronic emission processes in known Galactic $纬$-ray emitters, comparing this result to the cases of two separate analyses. In doing so, we demonstrate the capability of Gammapy, an open-source software package for the analysis of $纬$-ray data, to also process data from neutrino telescopes. For a selection of prototypical $纬$-ray sources within our Galaxy, we obtain models for primary proton and electron spectra in the hadronic and leptonic emission scenario, respectively, by fitting published $纬$-ray spectra. Using these models and instrument response functions for both detectors, we employ the Gammapy package to generate pseudo data sets, where we assume 200 hours of CTA observations and 10 years of KM3NeT detector operation. We then apply a three-dimensional binned likelihood analysis to these data sets, separately for each instrument and jointly for both. We find that the largest benefit of the combined analysis lies in the possibility of a consistent modelling of the $纬$-ray and neutrino emission. Assuming a purely leptonic scenario as input, we obtain, for the most favourable source, an average expected 68% credible interval that constrains the contribution of hadronic processes to the observed $纬$-ray emission to below 15%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03007v2-abstract-full').style.display = 'none'; document.getElementById('2309.03007v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 16 figures. v2: Matches version published in EPJC</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> European Physical Journal C 84, 112 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.01032">arXiv:2308.01032</a> <span> [<a href="https://arxiv.org/pdf/2308.01032">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> <p class="title is-5 mathjax"> Embedded Software of the KM3NeT Central Logic Board </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androutsou%2C+E">E. Androutsou</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/astro-ph?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/astro-ph?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/astro-ph?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a> , et al. (249 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="2308.01032v2-abstract-short" style="display: inline;"> The KM3NeT Collaboration is building and operating two deep sea neutrino telescopes at the bottom of the Mediterranean Sea. The telescopes consist of latices of photomultiplier tubes housed in pressure-resistant glass spheres, called digital optical modules and arranged in vertical detection units. The two main scientific goals are the determination of the neutrino mass ordering and the discovery… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.01032v2-abstract-full').style.display = 'inline'; document.getElementById('2308.01032v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.01032v2-abstract-full" style="display: none;"> The KM3NeT Collaboration is building and operating two deep sea neutrino telescopes at the bottom of the Mediterranean Sea. The telescopes consist of latices of photomultiplier tubes housed in pressure-resistant glass spheres, called digital optical modules and arranged in vertical detection units. The two main scientific goals are the determination of the neutrino mass ordering and the discovery and observation of high-energy neutrino sources in the Universe. Neutrinos are detected via the Cherenkov light, which is induced by charged particles originated in neutrino interactions. The photomultiplier tubes convert the Cherenkov light into electrical signals that are acquired and timestamped by the acquisition electronics. Each optical module houses the acquisition electronics for collecting and timestamping the photomultiplier signals with one nanosecond accuracy. Once finished, the two telescopes will have installed more than six thousand optical acquisition nodes, completing one of the more complex networks in the world in terms of operation and synchronization. The embedded software running in the acquisition nodes has been designed to provide a framework that will operate with different hardware versions and functionalities. The hardware will not be accessible once in operation, which complicates the embedded software architecture. The embedded software provides a set of tools to facilitate remote manageability of the deployed hardware, including safe reconfiguration of the firmware. This paper presents the architecture and the techniques, methods and implementation of the embedded software running in the acquisition nodes of the KM3NeT neutrino telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.01032v2-abstract-full').style.display = 'none'; document.getElementById('2308.01032v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17285">arXiv:2306.17285</a> <span> [<a href="https://arxiv.org/pdf/2306.17285">pdf</a>, <a href="https://arxiv.org/format/2306.17285">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.043007">10.1103/PhysRevD.109.043007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galactic Diffuse Neutrino Emission from Sources beyond the Discovery Horizon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">Antonio Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Groth%2C+K+M">Kathrine M酶rch Groth</a>, <a href="/search/astro-ph?searchtype=author&query=Peretti%2C+E">Enrico Peretti</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">Markus Ahlers</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.17285v2-abstract-short" style="display: inline;"> The IceCube Neutrino Observatory has recently reported strong evidence for neutrino emission from the Galactic plane. The signal is consistent with model predictions of diffuse emission from cosmic ray propagation in the interstellar medium. However, due to IceCube's limited potential of identifying individual neutrino sources, it is also feasible that unresolved Galactic sources could contribute… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17285v2-abstract-full').style.display = 'inline'; document.getElementById('2306.17285v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17285v2-abstract-full" style="display: none;"> The IceCube Neutrino Observatory has recently reported strong evidence for neutrino emission from the Galactic plane. The signal is consistent with model predictions of diffuse emission from cosmic ray propagation in the interstellar medium. However, due to IceCube's limited potential of identifying individual neutrino sources, it is also feasible that unresolved Galactic sources could contribute to the signal. We investigate the contribution of this quasi-diffuse emission and show that the observed Galactic diffuse flux at 100 TeV could be dominated by hard emission of unresolved sources. Particularly interesting candidate sources are young massive stellar clusters that have been considered as cosmic-ray PeVatrons. We examine whether this hypothesis can be tested by the upcoming KM3NeT detector or the planned future facility IceCube-Gen2 with about five times the sensitivity of IceCube. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17285v2-abstract-full').style.display = 'none'; document.getElementById('2306.17285v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Matches version published in Physical Review D 109, 043007 (2024)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109, 043007 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.05685">arXiv:2210.05685</a> <span> [<a href="https://arxiv.org/pdf/2210.05685">pdf</a>, <a href="https://arxiv.org/format/2210.05685">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-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/10.1103/PhysRevLett.131.111003">10.1103/PhysRevLett.131.111003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Starburst Nuclei as Light Dark Matter Laboratories </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">Antonio Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Chianese%2C+M">Marco Chianese</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorillo%2C+D+F+G">Damiano F. G. Fiorillo</a>, <a href="/search/astro-ph?searchtype=author&query=Marinelli%2C+A">Antonio Marinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Miele%2C+G">Gennaro Miele</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="2210.05685v2-abstract-short" style="display: inline;"> Starburst galaxies are well-motivated astrophysical emitters of high-energy gamma-rays. They are well-known cosmic-ray "reservoirs", thanks to their large magnetic fields which confine high-energy protons for $\sim 10^5$ years. Over such long times, cosmic-ray transport can be significantly affected by scatterings with sub-GeV dark matter. Here we point out that this scattering distorts the cosmic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05685v2-abstract-full').style.display = 'inline'; document.getElementById('2210.05685v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.05685v2-abstract-full" style="display: none;"> Starburst galaxies are well-motivated astrophysical emitters of high-energy gamma-rays. They are well-known cosmic-ray "reservoirs", thanks to their large magnetic fields which confine high-energy protons for $\sim 10^5$ years. Over such long times, cosmic-ray transport can be significantly affected by scatterings with sub-GeV dark matter. Here we point out that this scattering distorts the cosmic-ray spectrum, and the distortion can be indirectly observed by measuring the gamma-rays produced by cosmic-rays via hadronic collisions. Present gamma-ray data show no sign of such a distortion, leading to stringent bounds on the cross section between protons and dark matter. These are highly complementary with current bounds and have large room for improvement with the future gamma-ray measurements in the 0.1-10 TeV range from the Cherenkov Telescope Array, which can strengthen the limits by as much as two orders of magnitude. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05685v2-abstract-full').style.display = 'none'; document.getElementById('2210.05685v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">17 pages, 7 figures. v2: version published in Physical Review Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 131 (2023) 11, 111003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.03642">arXiv:2203.03642</a> <span> [<a href="https://arxiv.org/pdf/2203.03642">pdf</a>, <a href="https://arxiv.org/format/2203.03642">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-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/10.1093/mnras/stac2133">10.1093/mnras/stac2133 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observable Signatures of Cosmic Rays Transport in Starburst Galaxies on Gamma-ray and Neutrino Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Chianese%2C+M">M. Chianese</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorillo%2C+D+F+G">D. F. G. Fiorillo</a>, <a href="/search/astro-ph?searchtype=author&query=Marinelli%2C+A">A. Marinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Miele%2C+G">G. Miele</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="2203.03642v1-abstract-short" style="display: inline;"> The gamma-ray emission from Starburst and Starforming Galaxies (SBGs and SFGs) strongly suggest a correlation between star-forming activity and gamma-ray luminosity. However, the very nature of cosmic-ray (CR) transport and the degree of their confinement within SBG cores are still open questions. We aim at probing the imprints left by CR transport on gamma-ray and neutrino observations of point-l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.03642v1-abstract-full').style.display = 'inline'; document.getElementById('2203.03642v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.03642v1-abstract-full" style="display: none;"> The gamma-ray emission from Starburst and Starforming Galaxies (SBGs and SFGs) strongly suggest a correlation between star-forming activity and gamma-ray luminosity. However, the very nature of cosmic-ray (CR) transport and the degree of their confinement within SBG cores are still open questions. We aim at probing the imprints left by CR transport on gamma-ray and neutrino observations of point-like SFGs and SBGs, looking into quantitative ways to discriminate among different transport models. Moreover, following the reported scenarios, we quantitatively assess the SBGs and SFGs contribution to the Extra-galactic Gamma-Ray Background (EGB data) and the IceCube diffuse observations (HESE data). We analyse the 10-year Fermi-LAT spectral energy distributions of 13 nearby galaxies with two different CR transport models, taking into account the corresponding IR and UV observations. We generate mock gamma-ray data to simulate the CTA performance in detecting these sources. In the way, we propose a test to discriminate between the two CR models, quantifying the statistical confidence at which one model can be preferred over the other. We point out that current data already give a slight preference to CR models which are dominated by advection in their nucleus. Moreover, we show that CTA will allow us to firmly disfavour models dominated by diffusion over self-induced turbulence, compared to advection-dominated models, with Bayes factors which can be as large as $10^7$ for some of the SBGs. Finally, we estimate the diffuse gamma-ray and neutrino fluxes of SFGs and SBGs, showing that they can explain $25\%$ of the diffuse HESE data, while remaining consistent with gamma-ray limits on non-blazar sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.03642v1-abstract-full').style.display = 'none'; document.getElementById('2203.03642v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">9 pages, 5 figures, 3 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/2111.00223">arXiv:2111.00223</a> <span> [<a href="https://arxiv.org/pdf/2111.00223">pdf</a>, <a href="https://arxiv.org/format/2111.00223">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="Instrumentation and Detectors">physics.ins-det</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/10.1016/j.nima.2022.167132">10.1016/j.nima.2022.167132 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nanobeacon: A time calibration device for the KM3NeT neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+A+M+v+d">A. M. van den Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Bertine%2C+V">V. Bertine</a>, <a href="/search/astro-ph?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Cabo%2C+M+B">M. Bou Cabo</a> , et al. (216 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="2111.00223v1-abstract-short" style="display: inline;"> The KM3NeT Collaboration is currently constructing a multi-site high-energy neutrino telescope in the Mediterranean Sea consisting of matrices of pressure-resistant glass spheres, each holding a set of 31 small-area photomultipliers. The main goals of the telescope are the observation of neutrino sources in the Universe and the measurement of the neutrino oscillation parameters with atmospheric ne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.00223v1-abstract-full').style.display = 'inline'; document.getElementById('2111.00223v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.00223v1-abstract-full" style="display: none;"> The KM3NeT Collaboration is currently constructing a multi-site high-energy neutrino telescope in the Mediterranean Sea consisting of matrices of pressure-resistant glass spheres, each holding a set of 31 small-area photomultipliers. The main goals of the telescope are the observation of neutrino sources in the Universe and the measurement of the neutrino oscillation parameters with atmospheric neutrinos. Both extraterrestrial and atmospheric neutrinos are detected through the Cherenkov light induced in seawater by charged particles produced in neutrino interactions in the surrounding medium. A relative time synchronization between photomultipliers of the order of 1 ns is needed to guarantee the required angular resolution of the detector. Due to the large detector volumes to be instrumented by KM3NeT, a cost reduction of the different systems is a priority. To this end, the inexpensive Nanobeacon has been designed and developed by the KM3NeT Collaboration to be used for detector time-calibration studies. At present, more than 600 Nanobeacons have been already produced. The characterization of the optical pulse and the wavelength emission profile of the devices are critical for the time calibration. In this paper, the main features of the Nanobeacon design, production and operation, together with the main properties of the light pulse generated are described. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.00223v1-abstract-full').style.display = 'none'; document.getElementById('2111.00223v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.05890">arXiv:2109.05890</a> <span> [<a href="https://arxiv.org/pdf/2109.05890">pdf</a>, <a href="https://arxiv.org/format/2109.05890">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1140/epjc/s10052-022-10137-y">10.1140/epjc/s10052-022-10137-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Implementation and first results of the KM3NeT real-time core-collapse supernova neutrino search </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=KM3NeT+Collaboration"> KM3NeT Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+A+M+v+d">A. M. van den Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a> , et al. (220 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="2109.05890v2-abstract-short" style="display: inline;"> The KM3NeT research infrastructure is under construction in the Mediterranean Sea. KM3NeT will study atmospheric and astrophysical neutrinos with two multi-purpose neutrino detectors, ARCA and ORCA, primarily aimed at GeV-PeV neutrinos. Thanks to the multi-photomultiplier tube design of the digital optical modules, KM3NeT is capable of detecting the neutrino burst from a Galactic or near-Galactic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.05890v2-abstract-full').style.display = 'inline'; document.getElementById('2109.05890v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.05890v2-abstract-full" style="display: none;"> The KM3NeT research infrastructure is under construction in the Mediterranean Sea. KM3NeT will study atmospheric and astrophysical neutrinos with two multi-purpose neutrino detectors, ARCA and ORCA, primarily aimed at GeV-PeV neutrinos. Thanks to the multi-photomultiplier tube design of the digital optical modules, KM3NeT is capable of detecting the neutrino burst from a Galactic or near-Galactic core-collapse supernova. This potential is already exploitable with the first detection units deployed in the sea. This paper describes the real-time implementation of the supernova neutrino search, operating on the two KM3NeT detectors since the first months of 2019. A quasi-online astronomy analysis is introduced to study the time profile of the detected neutrinos for especially significant events. The mechanism of generation and distribution of alerts, as well as the integration into the SNEWS and SNEWS 2.0 global alert systems are described. The approach for the follow-up of external alerts with a search for a neutrino excess in the archival data is defined. Finally, an overview of the current detector capabilities and a report after the first two years of operation are given. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.05890v2-abstract-full').style.display = 'none'; document.getElementById('2109.05890v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">19 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 82, 317 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.00176">arXiv:2108.00176</a> <span> [<a href="https://arxiv.org/pdf/2108.00176">pdf</a>, <a href="https://arxiv.org/format/2108.00176">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-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/10.1088/1748-0221/16/12/C12016">10.1088/1748-0221/16/12/C12016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KM3NeT/ARCA expectations in view of a novel multimessenger study of starburst galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marinelli%2C+A">Antonio Marinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">Antonio Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ibnsalih%2C+W+I">Walid Idrissi Ibnsalih</a>, <a href="/search/astro-ph?searchtype=author&query=Miele%2C+G">Gennaro Miele</a>, <a href="/search/astro-ph?searchtype=author&query=Migliozzi%2C+P">Pasquale Migliozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pisanti%2C+O">Ofelia Pisanti</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+A">Ankur Sharma</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="2108.00176v3-abstract-short" style="display: inline;"> Starburst galaxies (SBGs) and more in general starforming galaxies represent a class of galaxies with a high star formation rate (up to 100 solar masses/year). Despite their low luminosity, they can 19 be considered as guaranteed "factories" of high energy neutrinos, being "reservoirs" of accelerated 20 cosmic rays and hosting a high density target gas in the central region. In this contribution 2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00176v3-abstract-full').style.display = 'inline'; document.getElementById('2108.00176v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.00176v3-abstract-full" style="display: none;"> Starburst galaxies (SBGs) and more in general starforming galaxies represent a class of galaxies with a high star formation rate (up to 100 solar masses/year). Despite their low luminosity, they can 19 be considered as guaranteed "factories" of high energy neutrinos, being "reservoirs" of accelerated 20 cosmic rays and hosting a high density target gas in the central region. In this contribution 21 we present a novel multimessenger study of these sources and the possibility of observing their 22 neutrino signals with the KM3NeT/ARCA telescope. The differential sensitivity for different SBG 23 scenarios is reported considering track-like neutrino events in the 100 GeV-100 PeV energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00176v3-abstract-full').style.display = 'none'; document.getElementById('2108.00176v3-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Presented at the 9th Very Large Volume Neutrino Telescope Workshop (VLVnT 2021), Prepared for submission to JINST</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.13248">arXiv:2106.13248</a> <span> [<a href="https://arxiv.org/pdf/2106.13248">pdf</a>, <a href="https://arxiv.org/format/2106.13248">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac25ff">10.3847/2041-8213/ac25ff <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Could nearby star-forming galaxies light up the point-like neutrino sky? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">Antonio Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Chianese%2C+M">Marco Chianese</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorillo%2C+D+F+G">Damiano F. G. Fiorillo</a>, <a href="/search/astro-ph?searchtype=author&query=Marinelli%2C+A">Antonio Marinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Miele%2C+G">Gennaro Miele</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="2106.13248v2-abstract-short" style="display: inline;"> Star-forming and starburst galaxies, which are well-known cosmic-rays reservoirs, are expected to emit gamma-rays and neutrinos predominantly via hadronic collisions. In this Letter, we analyze the 10-year Fermi-LAT spectral energy distributions of 13 nearby galaxies by means of a physical model which accounts for high-energy proton transport in starburst nuclei and includes the contribution of pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.13248v2-abstract-full').style.display = 'inline'; document.getElementById('2106.13248v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.13248v2-abstract-full" style="display: none;"> Star-forming and starburst galaxies, which are well-known cosmic-rays reservoirs, are expected to emit gamma-rays and neutrinos predominantly via hadronic collisions. In this Letter, we analyze the 10-year Fermi-LAT spectral energy distributions of 13 nearby galaxies by means of a physical model which accounts for high-energy proton transport in starburst nuclei and includes the contribution of primary and secondary electrons. In particular, we test the hypothesis that the observed gamma-ray fluxes are mostly due to star-forming activity, in agreement with the available star formation rates coming from IR and UV observations. Through this observation-based approach, we determine the most-likely neutrino counterpart from star-forming and starburst galaxies and quantitatively assess the ability of current and upcoming neutrino telescopes to detect them as point-like sources. Remarkably, we find that the cores of the Small Magellanic Cloud and the Circinus galaxy are potentially observable by KM3NeT/ARCA with 6 years of observation. Moreover, most of the nearby galaxies are likely to be just a factor of a few below the KM3NeT and IceCube-Gen2 point-like sensitivities. After investigating the prospects for detection of gamma-rays above TeV energies from these sources, we conclude that the joint observations of high-energy neutrinos and gamma-rays with upcoming telescopes will be an objective test for our emission model and may provide compelling evidence of star-forming activity as a tracer of neutrino production. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.13248v2-abstract-full').style.display = 'none'; document.getElementById('2106.13248v2-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">7 pages, 2 figures, version 2, accepted and published in APJ letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL 919 L32 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.11980">arXiv:2106.11980</a> <span> [<a href="https://arxiv.org/pdf/2106.11980">pdf</a>, <a href="https://arxiv.org/format/2106.11980">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-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/PhysRevD.105.045001">10.1103/PhysRevD.105.045001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Towards baryogenesis via absorption from Primordial Black Holes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">Antonio Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+R">Roberta Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorillo%2C+D+F+G">Damiano F. G. Fiorillo</a>, <a href="/search/astro-ph?searchtype=author&query=Miele%2C+G">Gennaro Miele</a>, <a href="/search/astro-ph?searchtype=author&query=Morisi%2C+S">Stefano Morisi</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="2106.11980v2-abstract-short" style="display: inline;"> Recently Dolgov and Pozdnyakov proposed a new baryogenesis mechanism in which baryon asymmetry is produced without violating baryon number at the Lagrangian level. In this scenario, baryon asymmetry is generated by absorption of a new particle X carrying baryon number onto Primordial Black Holes (PBHs). Assuming CP-violation, the particle X is absorbed at a different rate than the antiparticle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.11980v2-abstract-full').style.display = 'inline'; document.getElementById('2106.11980v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.11980v2-abstract-full" style="display: none;"> Recently Dolgov and Pozdnyakov proposed a new baryogenesis mechanism in which baryon asymmetry is produced without violating baryon number at the Lagrangian level. In this scenario, baryon asymmetry is generated by absorption of a new particle X carrying baryon number onto Primordial Black Holes (PBHs). Assuming CP-violation, the particle X is absorbed at a different rate than the antiparticle $\bar{X}$, producing an asymmetry in the baryonic number. We independently test this scenario, finding that it suffers from two fundamental issues.\\ At the phenomenological level, strong absorption by PBHs initially increases the baryon asymmetry. However, at later times such asymmetry is completely absorbed by PBHs. In order to overcome this issue, we account for PBH evaporation, which provides a natural way of halting the absorption while keeping a finite baryon asymmetry. We provide a systematic study of the parameter space, identifying the regions leading to the production of the baryon asymmetry without violating the known constraints on PBHs concentration. At the theoretical level, a model realizing the CP-violation postulated in this scenario is difficult to realize. We show, by implementing a minimal model, that the framework proposed in the original work in order to produce CP-violation, even if qualitatively correct, is quantitatively in disagreement with the observed baryon asymmetry, namely this mechanism produces only a fraction of the total baryon asymmetry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.11980v2-abstract-full').style.display = 'none'; document.getElementById('2106.11980v2-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">8 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.05977">arXiv:2102.05977</a> <span> [<a href="https://arxiv.org/pdf/2102.05977">pdf</a>, <a href="https://arxiv.org/format/2102.05977">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-021-09187-5">10.1140/epjc/s10052-021-09187-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The KM3NeT potential for the next core-collapse supernova observation with neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=KM3NeT+Collaboration"> KM3NeT Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/astro-ph?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+A+M+v+d">A. M. van den Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/astro-ph?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a> , et al. (223 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="2102.05977v2-abstract-short" style="display: inline;"> The KM3NeT research infrastructure is under construction in the Mediterranean Sea. It consists of two water Cherenkov neutrino detectors, ARCA and ORCA, aimed at neutrino astrophysics and oscillation research, respectively. Instrumenting a large volume of sea water with $\sim$ 6,200 optical modules comprising a total of $\sim$ 200,000 photomultiplier tubes, KM3NeT will achieve sensitivity to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.05977v2-abstract-full').style.display = 'inline'; document.getElementById('2102.05977v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.05977v2-abstract-full" style="display: none;"> The KM3NeT research infrastructure is under construction in the Mediterranean Sea. It consists of two water Cherenkov neutrino detectors, ARCA and ORCA, aimed at neutrino astrophysics and oscillation research, respectively. Instrumenting a large volume of sea water with $\sim$ 6,200 optical modules comprising a total of $\sim$ 200,000 photomultiplier tubes, KM3NeT will achieve sensitivity to $\sim$ 10 MeV neutrinos from Galactic and near-Galactic core-collapse supernovae through the observation of coincident hits in photomultipliers above the background. In this paper, the sensitivity of KM3NeT to a supernova explosion is estimated from detailed analyses of background data from the first KM3NeT detection units and simulations of the neutrino signal. The KM3NeT observational horizon (for a $5\,蟽$ discovery) covers essentially the Milky-Way and for the most optimistic model, extends to the Small Magellanic Cloud ($\sim$ 60 kpc). Detailed studies of the time profile of the neutrino signal allow assessment of the KM3NeT capability to determine the arrival time of the neutrino burst with a few milliseconds precision for sources up to 5$-$8 kpc away, and detecting the peculiar signature of the standing accretion shock instability if the core-collapse supernova explosion happens closer than 3$-$5 kpc, depending on the progenitor mass. KM3NeT's capability to measure the neutrino flux spectral parameters is also presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.05977v2-abstract-full').style.display = 'none'; document.getElementById('2102.05977v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to EPJC</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 81, 445 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.02483">arXiv:2011.02483</a> <span> [<a href="https://arxiv.org/pdf/2011.02483">pdf</a>, <a href="https://arxiv.org/format/2011.02483">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-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/10.1093/mnras/stab659">10.1093/mnras/stab659 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Starburst galaxies strike back: a multi-messenger analysis with Fermi-LAT and IceCube data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">Antonio Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Chianese%2C+M">Marco Chianese</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorillo%2C+D+F+G">Damiano F. G. Fiorillo</a>, <a href="/search/astro-ph?searchtype=author&query=Marinelli%2C+A">Antonio Marinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Miele%2C+G">Gennaro Miele</a>, <a href="/search/astro-ph?searchtype=author&query=Pisanti%2C+O">Ofelia Pisanti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.02483v2-abstract-short" style="display: inline;"> Starburst galaxies, which are known as "reservoirs" of high-energy cosmic-rays, can represent an important high-energy neutrino "factory" contributing to the diffuse neutrino flux observed by IceCube. In this paper, we revisit the constraints affecting the neutrino and gamma-ray hadronuclear emissions from this class of astrophysical objects. In particular, we go beyond the standard prototype-base… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.02483v2-abstract-full').style.display = 'inline'; document.getElementById('2011.02483v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.02483v2-abstract-full" style="display: none;"> Starburst galaxies, which are known as "reservoirs" of high-energy cosmic-rays, can represent an important high-energy neutrino "factory" contributing to the diffuse neutrino flux observed by IceCube. In this paper, we revisit the constraints affecting the neutrino and gamma-ray hadronuclear emissions from this class of astrophysical objects. In particular, we go beyond the standard prototype-based approach leading to a simple power-law neutrino flux, and investigate a more realistic model based on a data-driven blending of spectral indexes, thereby capturing the observed changes in the properties of individual emitters. We then perform a multi-messenger analysis considering the extragalactic gamma-ray background (EGB) measured by Fermi-LAT and different IceCube data samples: the 7.5-year High-Energy Starting Events (HESE) and the 6-year high-energy cascade data. Along with starburst galaxies, we take into account the contributions from blazars and radio galaxies as well as the secondary gamma-rays from electromagnetic cascades. Remarkably, we find that, differently from the highly-constrained prototype scenario, the spectral index blending allows starburst galaxies to account for up to $40\%$ of the HESE events at $95.4\%$ CL, while satisfying the limit on the non-blazar EGB component. Moreover, values of $\mathcal{O}(100~\mathrm{PeV})$ for the maximal energy of accelerated cosmic-rays by supernovae remnants inside the starburst are disfavoured in our scenario. In broad terms, our analysis points out that a better modeling of astrophysical sources could alleviate the tension between neutrino and gamma-ray data interpretation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.02483v2-abstract-full').style.display = 'none'; document.getElementById('2011.02483v2-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 15 figures. v2: updated to published version</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