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aria-current="page">4 </a> </li> </ul> </nav> <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/2407.00328">arXiv:2407.00328</a> <span> [<a href="https://arxiv.org/pdf/2407.00328">pdf</a>, <a href="https://arxiv.org/format/2407.00328">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">10.1088/1475-7516/2024/08 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on the energy spectrum of the diffuse cosmic neutrino flux from the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a> , et al. (117 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="2407.00328v2-abstract-short" style="display: inline;"> High-significance evidences of the existence of a high-energy diffuse flux of cosmic neutrinos have emerged in the last decade from several observations by the IceCube Collaboration. The ANTARES neutrino telescope took data for 15 years in the Mediterranean Sea, from 2007 to 2022, and collected a high-purity all-flavour neutrino sample. The search for a diffuse cosmic neutrino signal using this da… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.00328v2-abstract-full').style.display = 'inline'; document.getElementById('2407.00328v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.00328v2-abstract-full" style="display: none;"> High-significance evidences of the existence of a high-energy diffuse flux of cosmic neutrinos have emerged in the last decade from several observations by the IceCube Collaboration. The ANTARES neutrino telescope took data for 15 years in the Mediterranean Sea, from 2007 to 2022, and collected a high-purity all-flavour neutrino sample. The search for a diffuse cosmic neutrino signal using this dataset is presented in this article. This final analysis did not provide a statistically significant observation of the cosmic diffuse flux. However, this is converted into limits on the properties of the cosmic neutrino spectrum. In particular, given the sensitivity of the ANTARES neutrino telescope between 1 and 50 TeV, constraints on single-power-law hypotheses are derived for the cosmic diffuse flux below 20 TeV, especially for power-law fits of the IceCube data with spectral index softer than 2.8. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.00328v2-abstract-full').style.display = 'none'; document.getElementById('2407.00328v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP08(2024)038 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.03060">arXiv:2406.03060</a> <span> [<a href="https://arxiv.org/pdf/2406.03060">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-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/10.1029/2024JA032661">10.1029/2024JA032661 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Whistler waves in the quasi-parallel and quasi-perpendicular magnetosheath </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Svenningsson%2C+I">Ida Svenningsson</a>, <a href="/search/astro-ph?searchtype=author&query=Yordanova%2C+E">Emiliya Yordanova</a>, <a href="/search/astro-ph?searchtype=author&query=Khotyaintsev%2C+Y+V">Yuri V. Khotyaintsev</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">Mats Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cozzani%2C+G">Giulia Cozzani</a>, <a href="/search/astro-ph?searchtype=author&query=Steinvall%2C+K">Konrad Steinvall</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="2406.03060v2-abstract-short" style="display: inline;"> In the Earth's magnetosheath (MSH), several processes contribute to energy dissipation and plasma heating, one of which is wave-particle interactions between whistler waves and electrons. However, the overall impact of whistlers on electron dynamics in the MSH remains to be quantified. We analyze 18 hours of burst-mode measurements from the Magnetospheric Multiscale (MMS) mission, including data f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.03060v2-abstract-full').style.display = 'inline'; document.getElementById('2406.03060v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.03060v2-abstract-full" style="display: none;"> In the Earth's magnetosheath (MSH), several processes contribute to energy dissipation and plasma heating, one of which is wave-particle interactions between whistler waves and electrons. However, the overall impact of whistlers on electron dynamics in the MSH remains to be quantified. We analyze 18 hours of burst-mode measurements from the Magnetospheric Multiscale (MMS) mission, including data from the unbiased magnetosheath campaign during February-March 2023. We present a statistical study of 34,409 whistler waves found using automatic detection. We compare wave occurrence in the different MSH geometries and find three times higher occurrence in the quasi-perpendicular MSH compared to the quasi-parallel case. We also study the wave properties and find that the waves propagate quasi-parallel to the background magnetic field, have a median frequency of 0.2 times the electron cyclotron frequency, median amplitude of 0.03-0.06 nT (30-60 pT), and median duration of a few tens of wave periods. The whistler waves are preferentially observed in local magnetic dips and density peaks and are not associated with an increased temperature anisotropy. Also, almost no whistlers are observed in regions with parallel electron plasma beta lower than 0.1. Importantly, when estimating pitch-angle diffusion times we find that the whistler waves cause significant pitch-angle scattering of electrons in the MSH. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.03060v2-abstract-full').style.display = 'none'; document.getElementById('2406.03060v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">Published 16 June 2024 in JGR Space Physics. 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> Journal of Geophysical Research: Space Physics, 129, e2024JA032661 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.07230">arXiv:2405.07230</a> <span> [<a href="https://arxiv.org/pdf/2405.07230">pdf</a>, <a href="https://arxiv.org/format/2405.07230">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> <p class="title is-5 mathjax"> Acoustic Positioning for Deep Sea Neutrino Telescopes with a System of Piezo Sensors Integrated into Glass Spheres </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a>, <a href="/search/astro-ph?searchtype=author&query=Campion%2C+S">S. Campion</a> , et al. (115 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="2405.07230v1-abstract-short" style="display: inline;"> Position calibration in the deep sea is typically done by means of acoustic multilateration using three or more acoustic emitters installed at known positions. Rather than using hydrophones as receivers that are exposed to the ambient pressure, the sound signals can be coupled to piezo ceramics glued to the inside of existing containers for electronics or measuring instruments of a deep sea infras… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.07230v1-abstract-full').style.display = 'inline'; document.getElementById('2405.07230v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.07230v1-abstract-full" style="display: none;"> Position calibration in the deep sea is typically done by means of acoustic multilateration using three or more acoustic emitters installed at known positions. Rather than using hydrophones as receivers that are exposed to the ambient pressure, the sound signals can be coupled to piezo ceramics glued to the inside of existing containers for electronics or measuring instruments of a deep sea infrastructure. The ANTARES neutrino telescope operated from 2006 until 2022 in the Mediterranean Sea at a depth exceeding 2000m. It comprised nearly 900 glass spheres with 432mm diameter and 15mm thickness, equipped with photomultiplier tubes to detect Cherenkov light from tracks of charged elementary particles. In an experimental setup within ANTARES, piezo sensors have been glued to the inside of such - otherwise empty - glass spheres. These sensors recorded signals from acoustic emitters with frequencies from 46545 to 60235Hz. Two waves propagating through the glass sphere are found as a result of the excitation by the waves in the water. These can be qualitatively associated with symmetric and asymmetric Lamb-like waves of zeroth order: a fast (early) one with $v_e \approx 5$mm/$渭$s and a slow (late) one with $v_\ell \approx 2$mm/$渭$s. Taking these findings into account improves the accuracy of the position calibration. The results can be transferred to the KM3NeT neutrino telescope, currently under construction at multiple sites in the Mediterranean Sea, for which the concept of piezo sensors glued to the inside of glass spheres has been adapted for monitoring the positions of the photomultiplier tubes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.07230v1-abstract-full').style.display = 'none'; document.getElementById('2405.07230v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">submitted to "Experimental Astronomy"</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/2402.16498">arXiv:2402.16498</a> <span> [<a href="https://arxiv.org/pdf/2402.16498">pdf</a>, <a href="https://arxiv.org/format/2402.16498">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"> Results of the follow-up of ANTARES neutrino alerts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nzas%2C+H">H. Br芒nzas</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a> , et al. (166 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="2402.16498v1-abstract-short" style="display: inline;"> High-energy neutrinos could be produced in the interaction of charged cosmic rays with matter or radiation surrounding astrophysical sources. To look for transient sources associated with neutrino emission, a follow-up program of neutrino alerts has been operating within the ANTARES Collaboration since 2009. This program, named TAToO, has triggered robotic optical telescopes (MASTER, TAROT, ROTSE… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.16498v1-abstract-full').style.display = 'inline'; document.getElementById('2402.16498v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.16498v1-abstract-full" style="display: none;"> High-energy neutrinos could be produced in the interaction of charged cosmic rays with matter or radiation surrounding astrophysical sources. To look for transient sources associated with neutrino emission, a follow-up program of neutrino alerts has been operating within the ANTARES Collaboration since 2009. This program, named TAToO, has triggered robotic optical telescopes (MASTER, TAROT, ROTSE and the SVOM ground based telescopes) immediately after the detection of any relevant neutrino candidate and scheduled several observations in the weeks following the detection. A subset of ANTARES events with highest probabilities of being of cosmic origin has also been followed by the Swift and the INTEGRAL satellites, the Murchison Widefield Array radio telescope and the H.E.S.S. high-energy gamma-ray telescope. The results of twelve years of observations are reported. No optical counterpart has been significantly associated with an ANTARES candidate neutrino signal during image analysis. Constraints on transient neutrino emission have been set. In September 2015, ANTARES issued a neutrino alert and during the follow-up, a potential transient counterpart was identified by Swift and MASTER. A multi-wavelength follow-up campaign has allowed to identify the nature of this source and has proven its fortuitous association with the neutrino. The return of experience is particularly important for the design of the alert system of KM3NeT, the next generation neutrino telescope in the Mediterranean Sea. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.16498v1-abstract-full').style.display = 'none'; document.getElementById('2402.16498v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 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">27 pages, 14 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/2402.08363">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/2309.07109">arXiv:2309.07109</a> <span> [<a href="https://arxiv.org/pdf/2309.07109">pdf</a>, <a href="https://arxiv.org/ps/2309.07109">ps</a>, <a href="https://arxiv.org/format/2309.07109">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="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> <p class="title is-5 mathjax"> Real-time Monitoring for the Next Core-Collapse Supernova in JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/astro-ph?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/astro-ph?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/astro-ph?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/astro-ph?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/astro-ph?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/astro-ph?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/astro-ph?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/astro-ph?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/astro-ph?searchtype=author&query=Beretta%2C+M">Marco Beretta</a>, <a href="/search/astro-ph?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a> , et al. (606 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="2309.07109v2-abstract-short" style="display: inline;"> The core-collapse supernova (CCSN) is considered one of the most energetic astrophysical events in the universe. The early and prompt detection of neutrinos before (pre-SN) and during the supernova (SN) burst presents a unique opportunity for multi-messenger observations of CCSN events. In this study, we describe the monitoring concept and present the sensitivity of the system to pre-SN and SN neu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07109v2-abstract-full').style.display = 'inline'; document.getElementById('2309.07109v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.07109v2-abstract-full" style="display: none;"> The core-collapse supernova (CCSN) is considered one of the most energetic astrophysical events in the universe. The early and prompt detection of neutrinos before (pre-SN) and during the supernova (SN) burst presents a unique opportunity for multi-messenger observations of CCSN events. In this study, we describe the monitoring concept and present the sensitivity of the system to pre-SN and SN neutrinos at the Jiangmen Underground Neutrino Observatory (JUNO), a 20 kton liquid scintillator detector currently under construction in South China. The real-time monitoring system is designed to ensure both prompt alert speed and comprehensive coverage of progenitor stars. It incorporates prompt monitors on the electronic board as well as online monitors at the data acquisition stage. Assuming a false alert rate of 1 per year, this monitoring system exhibits sensitivity to pre-SN neutrinos up to a distance of approximately 1.6 (0.9) kiloparsecs and SN neutrinos up to about 370 (360) kiloparsecs for a progenitor mass of 30 solar masses, considering both normal and inverted mass ordering scenarios. The pointing ability of the CCSN is evaluated by analyzing the accumulated event anisotropy of inverse beta decay interactions from pre-SN or SN neutrinos. This, along with the early alert, can play a crucial role in facilitating follow-up multi-messenger observations of the next galactic or nearby extragalactic CCSN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07109v2-abstract-full').style.display = 'none'; document.getElementById('2309.07109v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 9 figures, accepted for the publication at 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/2309.06874">arXiv:2309.06874</a> <span> [<a href="https://arxiv.org/pdf/2309.06874">pdf</a>, <a href="https://arxiv.org/format/2309.06874">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad1f5b">10.3847/1538-4357/ad1f5b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searches for neutrinos in the direction of radio-bright blazars with the ANTARES telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+J">J. J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a> , et al. (140 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="2309.06874v1-abstract-short" style="display: inline;"> Active galaxies, especially blazars, are among the most promising neutrino source candidates. To date, ANTARES searches for these objects considered GeV-TeV $纬$-ray bright blazars. Here, a statistically complete radio-bright blazar sample is used as the target for searches of origins of neutrinos collected by the ANTARES neutrino telescope over 13 years of operation. The hypothesis of a neutrino-b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.06874v1-abstract-full').style.display = 'inline'; document.getElementById('2309.06874v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.06874v1-abstract-full" style="display: none;"> Active galaxies, especially blazars, are among the most promising neutrino source candidates. To date, ANTARES searches for these objects considered GeV-TeV $纬$-ray bright blazars. Here, a statistically complete radio-bright blazar sample is used as the target for searches of origins of neutrinos collected by the ANTARES neutrino telescope over 13 years of operation. The hypothesis of a neutrino-blazar directional correlation is tested by pair counting and by a complementary likelihood-based approach. The resulting post-trial $p$-value is $3.0\%$ ($2.2蟽$ in the two-sided convention), possibly indicating a correlation. Additionally, a time-dependent analysis is performed to search for temporal clustering of neutrino candidates as a mean of detecting neutrino flares in blazars. None of the investigated sources alone reaches a significant flare detection level. However, the presence of 18 sources with a pre-trial significance above $3蟽$ indicates a $p=1.4\%$ ($2.5蟽$ in the two-sided convention) detection of a time-variable neutrino flux. An \textit{a posteriori} investigation reveals an intriguing temporal coincidence of neutrino, radio, and $纬$-ray flares of the J0242+1101 blazar at a $p=0.5\%$ ($2.9蟽$ in the two-sided convention) level. Altogether, the results presented here suggest a possible connection of neutrino candidates detected by the ANTARES telescope with radio-bright blazars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.06874v1-abstract-full').style.display = 'none'; document.getElementById('2309.06874v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 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">Journal ref:</span> ApJ 964 (2024) 3 </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/2306.09567">arXiv:2306.09567</a> <span> [<a href="https://arxiv.org/pdf/2306.09567">pdf</a>, <a href="https://arxiv.org/format/2306.09567">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="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/10.1088/1475-7516/2023/09/001">10.1088/1475-7516/2023/09/001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/astro-ph?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/astro-ph?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/astro-ph?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/astro-ph?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/astro-ph?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/astro-ph?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/astro-ph?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/astro-ph?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/astro-ph?searchtype=author&query=Bellato%2C+M">Marco Bellato</a> , et al. (581 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="2306.09567v3-abstract-short" style="display: inline;"> We discuss JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo via detecting inverse beta decay reactions of electron anti-neutrinos resulting from the annihilation. We study possible backgrounds to the signature, including the reactor neutrinos, diffuse supernova neutrino background, charged- and neutral-current interactions of atmospheric neutrinos, backgrounds from muon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09567v3-abstract-full').style.display = 'inline'; document.getElementById('2306.09567v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.09567v3-abstract-full" style="display: none;"> We discuss JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo via detecting inverse beta decay reactions of electron anti-neutrinos resulting from the annihilation. We study possible backgrounds to the signature, including the reactor neutrinos, diffuse supernova neutrino background, charged- and neutral-current interactions of atmospheric neutrinos, backgrounds from muon-induced fast neutrons and cosmogenic isotopes. A fiducial volume cut, as well as the pulse shape discrimination and the muon veto are applied to suppress the above backgrounds. It is shown that JUNO sensitivity to the thermally averaged dark matter annihilation rate in 10 years of exposure would be significantly better than the present-day best limit set by Super-Kamiokande and would be comparable to that expected by Hyper-Kamiokande. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09567v3-abstract-full').style.display = 'none'; document.getElementById('2306.09567v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">25 pages, 9 figures, matches the publised version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 09 (2023) 001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.07723">arXiv:2302.07723</a> <span> [<a href="https://arxiv.org/pdf/2302.07723">pdf</a>, <a href="https://arxiv.org/format/2302.07723">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/10.1088/1475-7516/2023/04/004">10.1088/1475-7516/2023/04/004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for neutrino counterparts to the gravitational wave sources from LIGO/Virgo O3 run with the ANTARES detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a> , et al. (128 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="2302.07723v2-abstract-short" style="display: inline;"> Since 2015 the LIGO and Virgo interferometers have detected gravitational waves from almost one hundred coalescences of compact objects (black holes and neutron stars). This article presents the results of a search performed with data from the ANTARES telescope to identify neutrino counterparts to the gravitational wave sources detected during the third LIGO/Virgo observing run and reported in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07723v2-abstract-full').style.display = 'inline'; document.getElementById('2302.07723v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.07723v2-abstract-full" style="display: none;"> Since 2015 the LIGO and Virgo interferometers have detected gravitational waves from almost one hundred coalescences of compact objects (black holes and neutron stars). This article presents the results of a search performed with data from the ANTARES telescope to identify neutrino counterparts to the gravitational wave sources detected during the third LIGO/Virgo observing run and reported in the catalogues GWTC-2, GWTC-2.1, and GWTC-3. This search is sensitive to all-sky neutrinos of all flavours and of energies $>100$ GeV, thanks to the inclusion of both track-like events (mainly induced by $谓_渭$ charged-current interactions) and shower-like events (induced by other interaction types). Neutrinos are selected if they are detected within $\pm 500$ s from the GW merger and with a reconstructed direction compatible with its sky localisation. No significant excess is found for any of the 80 analysed GW events, and upper limits on the neutrino emission are derived. Using the information from the GW catalogues and assuming isotropic emission, upper limits on the total energy $E_{\rm tot, 谓}$ emitted as neutrinos of all flavours and on the ratio $f_谓= E_{\rm tot, 谓}/E_{\rm GW}$ between neutrino and GW emissions are also computed. Finally, a stacked analysis of all the 72 binary black hole mergers (respectively the 7 neutron star - black hole merger candidates) has been performed to constrain the typical neutrino emission within this population, leading to the limits: $E_{\rm tot, 谓} < 4.0 \times 10^{53}$ erg and $f_谓< 0.15$ (respectively, $E_{\rm tot, 谓} < 3.2 \times 10^{53}$ erg and $f_谓< 0.88$) for $E^{-2}$ spectrum and isotropic emission. Other assumptions including softer spectra and non-isotropic scenarios have also been tested. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07723v2-abstract-full').style.display = 'none'; document.getElementById('2302.07723v2-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">13 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 04 (2023) 004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.11876">arXiv:2212.11876</a> <span> [<a href="https://arxiv.org/pdf/2212.11876">pdf</a>, <a href="https://arxiv.org/format/2212.11876">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/10.1016/j.physletb.2023.137951">10.1016/j.physletb.2023.137951 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hint for a TeV neutrino emission from the Galactic Ridge with ANTARES </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a> , et al. (129 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="2212.11876v2-abstract-short" style="display: inline;"> Interactions of cosmic ray protons, atomic nuclei, and electrons in the interstellar medium in the inner part of the Milky Way produce a $纬$-ray flux from the Galactic Ridge. If the $纬$-ray emission is dominated by proton and nuclei interactions, a neutrino flux comparable to the $纬$-ray flux is expected from the same sky region. Data collected by the ANTARES neutrino telescope are used to constra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11876v2-abstract-full').style.display = 'inline'; document.getElementById('2212.11876v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.11876v2-abstract-full" style="display: none;"> Interactions of cosmic ray protons, atomic nuclei, and electrons in the interstellar medium in the inner part of the Milky Way produce a $纬$-ray flux from the Galactic Ridge. If the $纬$-ray emission is dominated by proton and nuclei interactions, a neutrino flux comparable to the $纬$-ray flux is expected from the same sky region. Data collected by the ANTARES neutrino telescope are used to constrain the neutrino flux from the Galactic Ridge in the 1-100 TeV energy range. Neutrino events reconstructed both as tracks and showers are considered in the analysis and the selection is optimized for the search of an excess in the region $|l| < 30掳$, $|b| < 2掳$. The expected background in the search region is estimated using an off-zone region with similar sky coverage. Neutrino signal originating from a power-law spectrum with spectral index ranging from $螕_谓=1$ to $4$ is simulated in both channels. The observed energy distributions are fitted to constrain the neutrino emission from the Ridge. The energy distributions in the signal region are inconsistent with the background expectation at $\sim 96\%$ confidence level. The mild excess over the background is consistent with a neutrino flux with a power law with a spectral index $2.45^{+0.22}_{-0.34}$ and a flux normalization $dN_谓/dE_谓= 4.0^{+2.7}_{-2.0} \times 10^{-16} \text{GeV}^{-1} \text{cm}^{-2} \text{s}^{-1} \text{sr}^{-1}$ at 40 TeV reference energy. Such flux is consistent with the expected neutrino signal if the bulk of the observed $纬$-ray flux from the Galactic Ridge originates from interactions of cosmic ray protons and nuclei with a power-law spectrum extending well into the PeV energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11876v2-abstract-full').style.display = 'none'; document.getElementById('2212.11876v2-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">8 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physics Letters B, Volume 841, 2023, 137951 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.07551">arXiv:2211.07551</a> <span> [<a href="https://arxiv.org/pdf/2211.07551">pdf</a>, <a href="https://arxiv.org/format/2211.07551">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"> Review of the online analyses of multi-messenger alerts and electromagnetic transient events with the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a>, <a href="/search/astro-ph?searchtype=author&query=Campion%2C+S">S. Campion</a> , et al. (124 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="2211.07551v2-abstract-short" style="display: inline;"> By constantly monitoring at least one complete hemisphere of the sky, neutrino telescopes are well designed to detect neutrinos emitted by transient astrophysical events. Real-time searches with the ANTARES telescope have been performed to look for neutrino candidates coincident with gamma-ray bursts detected by the Swift and Fermi satellites, highenergy neutrino events registered by IceCube, tran… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.07551v2-abstract-full').style.display = 'inline'; document.getElementById('2211.07551v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.07551v2-abstract-full" style="display: none;"> By constantly monitoring at least one complete hemisphere of the sky, neutrino telescopes are well designed to detect neutrinos emitted by transient astrophysical events. Real-time searches with the ANTARES telescope have been performed to look for neutrino candidates coincident with gamma-ray bursts detected by the Swift and Fermi satellites, highenergy neutrino events registered by IceCube, transient events from blazars monitored by HAWC, photon-neutrino coincidences by AMON notices and gravitational wave candidates observed by LIGO/Virgo. By requiring temporal coincidence, this approach increases the sensitivity and the significance of a potential discovery. Thanks to the good angular accuracy of neutrino candidates reconstructed with the ANTARES telescope, a coincident detection can also improve the positioning area of non-well localised triggers such as those detected by gravitational wave interferometers. This paper summarises the results of the follow-up performed by the ANTARES telescope between 01/2014 and 02/2022, which corresponds to the end of the data taking period. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.07551v2-abstract-full').style.display = 'none'; document.getElementById('2211.07551v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">21 pages, 10 figures, JCAP08 (2023) 072 (19 pp</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.08437">arXiv:2210.08437</a> <span> [<a href="https://arxiv.org/pdf/2210.08437">pdf</a>, <a href="https://arxiv.org/format/2210.08437">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="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey 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="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad2bfd">10.3847/1538-4357/ad2bfd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Model Independent Approach of the JUNO $^8$B Solar Neutrino Program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+J">Jie Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Yue%2C+B">Baobiao Yue</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+H">Haoqi Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yufeng Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ling%2C+J">Jiajie Ling</a>, <a href="/search/astro-ph?searchtype=author&query=Yu%2C+Z">Zeyuan Yu</a>, <a href="/search/astro-ph?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/astro-ph?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/astro-ph?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/astro-ph?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/astro-ph?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/astro-ph?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/astro-ph?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+W">Weidong Bai</a> , et al. (579 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="2210.08437v2-abstract-short" style="display: inline;"> The physics potential of detecting $^8$B solar neutrinos will be exploited at the Jiangmen Underground Neutrino Observatory (JUNO), in a model independent manner by using three distinct channels of the charged-current (CC), neutral-current (NC) and elastic scattering (ES) interactions. Due to the largest-ever mass of $^{13}$C nuclei in the liquid-scintillator detectors and the {expected} low backg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08437v2-abstract-full').style.display = 'inline'; document.getElementById('2210.08437v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.08437v2-abstract-full" style="display: none;"> The physics potential of detecting $^8$B solar neutrinos will be exploited at the Jiangmen Underground Neutrino Observatory (JUNO), in a model independent manner by using three distinct channels of the charged-current (CC), neutral-current (NC) and elastic scattering (ES) interactions. Due to the largest-ever mass of $^{13}$C nuclei in the liquid-scintillator detectors and the {expected} low background level, $^8$B solar neutrinos would be observable in the CC and NC interactions on $^{13}$C for the first time. By virtue of optimized event selections and muon veto strategies, backgrounds from the accidental coincidence, muon-induced isotopes, and external backgrounds can be greatly suppressed. Excellent signal-to-background ratios can be achieved in the CC, NC and ES channels to guarantee the $^8$B solar neutrino observation. From the sensitivity studies performed in this work, we show that JUNO, with ten years of data, can reach the {1$蟽$} precision levels of 5%, 8% and 20% for the $^8$B neutrino flux, $\sin^2胃_{12}$, and $螖m^2_{21}$, respectively. It would be unique and helpful to probe the details of both solar physics and neutrino physics. In addition, when combined with SNO, the world-best precision of 3% is expected for the $^8$B neutrino flux measurement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08437v2-abstract-full').style.display = 'none'; document.getElementById('2210.08437v2-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">19 pages, 7 figures, accepted version to appear in The Astrophysical Journal. Yufeng Li and Jiajie Ling are corresponding authors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophysical Journal 965 (2024) 122 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.13462">arXiv:2209.13462</a> <span> [<a href="https://arxiv.org/pdf/2209.13462">pdf</a>, <a href="https://arxiv.org/format/2209.13462">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acafdd">10.3847/1538-4357/acafdd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Gamma-Ray and Neutrino Coincidences Using HAWC and ANTARES Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Solares%2C+H+A+A">H. A. Ayala Solares</a>, <a href="/search/astro-ph?searchtype=author&query=Coutu%2C+S">S. Coutu</a>, <a href="/search/astro-ph?searchtype=author&query=Cowen%2C+D">D. Cowen</a>, <a href="/search/astro-ph?searchtype=author&query=Fox%2C+D+B">D. B. Fox</a>, <a href="/search/astro-ph?searchtype=author&query=Gr%C3%A9goire%2C+T">T. Gr茅goire</a>, <a href="/search/astro-ph?searchtype=author&query=McBride%2C+F">F. McBride</a>, <a href="/search/astro-ph?searchtype=author&query=Mostaf%C3%A1%2C+M">M. Mostaf谩</a>, <a href="/search/astro-ph?searchtype=author&query=Murase%2C+K">K. Murase</a>, <a href="/search/astro-ph?searchtype=author&query=Wissel%2C+S">S. Wissel</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a> , et al. (207 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="2209.13462v2-abstract-short" style="display: inline;"> In the quest for high-energy neutrino sources, the Astrophysical Multimessenger Observatory Network (AMON) has implemented a new search by combining data from the High Altitude Water Cherenkov (HAWC) observatory and the Astronomy with a Neutrino Telescope and Abyss environmental RESearch (ANTARES) neutrino telescope. Using the same analysis strategy as in a previous detector combination of HAWC an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13462v2-abstract-full').style.display = 'inline'; document.getElementById('2209.13462v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.13462v2-abstract-full" style="display: none;"> In the quest for high-energy neutrino sources, the Astrophysical Multimessenger Observatory Network (AMON) has implemented a new search by combining data from the High Altitude Water Cherenkov (HAWC) observatory and the Astronomy with a Neutrino Telescope and Abyss environmental RESearch (ANTARES) neutrino telescope. Using the same analysis strategy as in a previous detector combination of HAWC and IceCube data, we perform a search for coincidences in HAWC and ANTARES events that are below the threshold for sending public alerts in each individual detector. Data were collected between July 2015 and February 2020 with a livetime of 4.39 years. Over this time period, 3 coincident events with an estimated false-alarm rate of $< 1$ coincidence per year were found. This number is consistent with background expectations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13462v2-abstract-full').style.display = 'none'; document.getElementById('2209.13462v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">12 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/2208.12671">arXiv:2208.12671</a> <span> [<a href="https://arxiv.org/pdf/2208.12671">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-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/10.1029/2021JA029518">10.1029/2021JA029518 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Thin current sheet behind the dipolarization front </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nakamura"> Nakamura</a>, <a href="/search/astro-ph?searchtype=author&query=R."> R.</a>, <a href="/search/astro-ph?searchtype=author&query=Baumjohann"> Baumjohann</a>, <a href="/search/astro-ph?searchtype=author&query=W."> W.</a>, <a href="/search/astro-ph?searchtype=author&query=Nakamura"> Nakamura</a>, <a href="/search/astro-ph?searchtype=author&query=M.%2C+T+K">T. K. M.</a>, <a href="/search/astro-ph?searchtype=author&query=Panov"> Panov</a>, <a href="/search/astro-ph?searchtype=author&query=E."> E.</a>, <a href="/search/astro-ph?searchtype=author&query=V."> V.</a>, <a href="/search/astro-ph?searchtype=author&query=Schmid"> Schmid</a>, <a href="/search/astro-ph?searchtype=author&query=D."> D.</a>, <a href="/search/astro-ph?searchtype=author&query=Varsani"> Varsani</a>, <a href="/search/astro-ph?searchtype=author&query=A."> A.</a>, <a href="/search/astro-ph?searchtype=author&query=Apatenkov%2C+S">S. Apatenkov</a>, <a href="/search/astro-ph?searchtype=author&query=Sergeev%2C+V+A">V. A. Sergeev</a>, <a href="/search/astro-ph?searchtype=author&query=Birn%2C+J">J. Birn</a>, <a href="/search/astro-ph?searchtype=author&query=Nagai%2C+T">T. Nagai</a>, <a href="/search/astro-ph?searchtype=author&query=Gabrielse%2C+C">C. Gabrielse</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Burch%2C+J+L">J. L. Burch</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+C">C. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Dandouras%2C+I+S">I. S Dandouras</a>, <a href="/search/astro-ph?searchtype=author&query=Escoubet%2C+C+P">C. P. Escoubet</a>, <a href="/search/astro-ph?searchtype=author&query=A"> A</a>, <a href="/search/astro-ph?searchtype=author&query=Fazakerley%2C+N">N. Fazakerley</a> , et al. (4 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="2208.12671v1-abstract-short" style="display: inline;"> We report a unique conjugate observation of fast flows and associated current sheet disturbances in the near-Earth magnetotail by MMS (Magnetospheric Multiscale) and Cluster preceding a positive bay onset of a small substorm at ~14:10 UT, Sep. 8, 2018. MMS and Cluster were located both at X ~-14 RE. A dipolarization front (DF) of a localized fast flow was detected by Cluster and MMS, separated in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.12671v1-abstract-full').style.display = 'inline'; document.getElementById('2208.12671v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.12671v1-abstract-full" style="display: none;"> We report a unique conjugate observation of fast flows and associated current sheet disturbances in the near-Earth magnetotail by MMS (Magnetospheric Multiscale) and Cluster preceding a positive bay onset of a small substorm at ~14:10 UT, Sep. 8, 2018. MMS and Cluster were located both at X ~-14 RE. A dipolarization front (DF) of a localized fast flow was detected by Cluster and MMS, separated in the dawn-dusk direction by ~4 RE, almost simultaneously. Adiabatic electron acceleration signatures revealed from comparison of the energy spectra confirm that both spacecraft encounter the same DF. We analyzed the change in the current sheet structure based on multi-scale multi-point data analysis. The current sheet thickened during the passage of DF, yet, temporally thinned subsequently associated with another flow enhancement centered more on the dawnward side of the initial flow. MMS and Cluster observed intense perpendicular and parallel current in the off-equatorial region mainly during this interval of the current sheet thinning. Maximum field-aligned currents both at MMS and Cluster are directed tailward. Detailed analysis of MMS data showed that the intense field-aligned currents consisted of multiple small-scale intense current layers accompanied by enhanced Hall-currents in the dawn-dusk flow-shear region. We suggest that the current sheet thinning is related to the flow bouncing process and/or to the expansion/activation of reconnection. Based on these mesoscale and small-scale multipoint observations, 3D evolution of the flow and current-sheet disturbances was inferred preceding the development of a substorm current wedge. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.12671v1-abstract-full').style.display = 'none'; document.getElementById('2208.12671v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Geophysical Research: Space Physics, 126, e2021JA029518, 2021 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.11689">arXiv:2208.11689</a> <span> [<a href="https://arxiv.org/pdf/2208.11689">pdf</a>, <a href="https://arxiv.org/format/2208.11689">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/10.1088/1475-7516/2023/01/012">10.1088/1475-7516/2023/01/012 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on the nuclearite flux using the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a> , et al. (121 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="2208.11689v5-abstract-short" style="display: inline;"> In this work, a search for nuclearites of strange quark matter by using nine years of ANTARES data taken in the period 2009-2017 is presented. The passage through matter of these particles is simulated %according to the model of de R煤jula and Glashow taking into account a detailed description of the detector response to nuclearites and of the data acquisition conditions. A down-going flux of cosmi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.11689v5-abstract-full').style.display = 'inline'; document.getElementById('2208.11689v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.11689v5-abstract-full" style="display: none;"> In this work, a search for nuclearites of strange quark matter by using nine years of ANTARES data taken in the period 2009-2017 is presented. The passage through matter of these particles is simulated %according to the model of de R煤jula and Glashow taking into account a detailed description of the detector response to nuclearites and of the data acquisition conditions. A down-going flux of cosmic nuclearites with Galactic velocities ($尾= 10^{-3}$) was considered for this study. The mass threshold for detecting these particles at the detector level is \mbox{ $4 \times 10^{13}$ GeV/c$^{2}$}. Upper limits on the nuclearite flux for masses up to $10^{17}$ GeV/c$^{2}$ at the level of $\sim 5 \times 10^{-17}$ cm$^{-2}$ s$^{-1}$ sr$^{-1}$ are obtained. These are the first upper limits on nuclearites established with a neutrino telescope and the most stringent ever set for Galactic velocities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.11689v5-abstract-full').style.display = 'none'; document.getElementById('2208.11689v5-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 7 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/2205.08830">arXiv:2205.08830</a> <span> [<a href="https://arxiv.org/pdf/2205.08830">pdf</a>, <a href="https://arxiv.org/format/2205.08830">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="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> <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/10.1088/1475-7516/2022/10/033">10.1088/1475-7516/2022/10/033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for Detecting the Diffuse Supernova Neutrino Background with JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/astro-ph?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/astro-ph?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/astro-ph?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/astro-ph?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/astro-ph?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/astro-ph?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/astro-ph?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/astro-ph?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/astro-ph?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a>, <a href="/search/astro-ph?searchtype=author&query=Blin%2C+S">Sylvie Blin</a> , et al. (577 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="2205.08830v2-abstract-short" style="display: inline;"> We present the detection potential for the diffuse supernova neutrino background (DSNB) at the Jiangmen Underground Neutrino Observatory (JUNO), using the inverse-beta-decay (IBD) detection channel on free protons. We employ the latest information on the DSNB flux predictions, and investigate in detail the background and its reduction for the DSNB search at JUNO. The atmospheric neutrino induced n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08830v2-abstract-full').style.display = 'inline'; document.getElementById('2205.08830v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.08830v2-abstract-full" style="display: none;"> We present the detection potential for the diffuse supernova neutrino background (DSNB) at the Jiangmen Underground Neutrino Observatory (JUNO), using the inverse-beta-decay (IBD) detection channel on free protons. We employ the latest information on the DSNB flux predictions, and investigate in detail the background and its reduction for the DSNB search at JUNO. The atmospheric neutrino induced neutral current (NC) background turns out to be the most critical background, whose uncertainty is carefully evaluated from both the spread of model predictions and an envisaged \textit{in situ} measurement. We also make a careful study on the background suppression with the pulse shape discrimination (PSD) and triple coincidence (TC) cuts. With latest DSNB signal predictions, more realistic background evaluation and PSD efficiency optimization, and additional TC cut, JUNO can reach the significance of 3$蟽$ for 3 years of data taking, and achieve better than 5$蟽$ after 10 years for a reference DSNB model. In the pessimistic scenario of non-observation, JUNO would strongly improve the limits and exclude a significant region of the model parameter space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08830v2-abstract-full').style.display = 'none'; document.getElementById('2205.08830v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">29 pages, 11 figures, final published version in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 10 (2022) 033 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.06029">arXiv:2203.06029</a> <span> [<a href="https://arxiv.org/pdf/2203.06029">pdf</a>, <a href="https://arxiv.org/format/2203.06029">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/10.1088/1475-7516/2022/06/028">10.1088/1475-7516/2022/06/028 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for secluded dark matter towards the Galactic Centre with the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Branzas%2C+H">H. Branzas</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a> , et al. (124 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="2203.06029v1-abstract-short" style="display: inline;"> Searches for dark matter (DM) have not provided any solid evidence for the existence of weakly interacting massive particles in the GeV-TeV mass range. Coincidentally, the scale of new physics is being pushed by collider searches well beyond the TeV domain. This situation strongly motivates the exploration of DM masses much larger than a TeV. Secluded scenarios contain a natural way around the uni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06029v1-abstract-full').style.display = 'inline'; document.getElementById('2203.06029v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.06029v1-abstract-full" style="display: none;"> Searches for dark matter (DM) have not provided any solid evidence for the existence of weakly interacting massive particles in the GeV-TeV mass range. Coincidentally, the scale of new physics is being pushed by collider searches well beyond the TeV domain. This situation strongly motivates the exploration of DM masses much larger than a TeV. Secluded scenarios contain a natural way around the unitarity bound on the DM mass, via the early matter domination induced by the mediator of its interactions with the Standard Model. High-energy neutrinos constitute one of the very few direct accesses to energy scales above a few TeV. An indirect search for secluded DM signals has been performed with the ANTARES neutrino telescope using data from 2007 to 2015. Upper limits on the DM annihilation cross section for DM masses up to 6 PeV are presented and discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06029v1-abstract-full').style.display = 'none'; document.getElementById('2203.06029v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.13786">arXiv:2202.13786</a> <span> [<a href="https://arxiv.org/pdf/2202.13786">pdf</a>, <a href="https://arxiv.org/format/2202.13786">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/10.1016/j.jheap.2022.03.001">10.1016/j.jheap.2022.03.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Magnetic Monopoles with ten years of the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a> , et al. (123 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="2202.13786v3-abstract-short" style="display: inline;"> This work presents a new search for magnetic monopoles using data taken with the ANTARES neutrino telescope over a period of 10 years (January 2008 to December 2017). Compared to previous ANTARES searches, this analysis uses a run-by-run simulation strategy, with a larger exposure as well as a new simulation of magnetic monopoles taking into account the Kasama, Yang and Goldhaber model for their i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13786v3-abstract-full').style.display = 'inline'; document.getElementById('2202.13786v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.13786v3-abstract-full" style="display: none;"> This work presents a new search for magnetic monopoles using data taken with the ANTARES neutrino telescope over a period of 10 years (January 2008 to December 2017). Compared to previous ANTARES searches, this analysis uses a run-by-run simulation strategy, with a larger exposure as well as a new simulation of magnetic monopoles taking into account the Kasama, Yang and Goldhaber model for their interaction cross-section with matter. No signal compatible with the passage of relativistic magnetic monopoles is observed, and upper limits on the flux of magnetic monopoles with $尾$ = v/c $\geq$ 0.55, are presented. For ultra-relativistic magnetic monopoles the flux limit is $\sim$ 7$\times$$10^{-18}$ $\rm cm^{-2} s^{-1} sr^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13786v3-abstract-full').style.display = 'none'; document.getElementById('2202.13786v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">20 pages, 7 figures, accepted for publication in the Journal of High Energy Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.11642">arXiv:2201.11642</a> <span> [<a href="https://arxiv.org/pdf/2201.11642">pdf</a>, <a href="https://arxiv.org/format/2201.11642">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/10.1088/1475-7516/2022/06/018">10.1088/1475-7516/2022/06/018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for solar atmospheric neutrinos with the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a> , et al. (123 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="2201.11642v2-abstract-short" style="display: inline;"> Solar Atmospheric Neutrinos (SA$谓$s) are produced by the interaction of cosmic rays with the solar medium. The detection of SA$谓$s would provide useful information on the composition of primary cosmic rays as well as the solar density. These neutrinos represent an irreducible source of background for indirect searches for dark matter towards the Sun and the measurement of their flux would allow fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11642v2-abstract-full').style.display = 'inline'; document.getElementById('2201.11642v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.11642v2-abstract-full" style="display: none;"> Solar Atmospheric Neutrinos (SA$谓$s) are produced by the interaction of cosmic rays with the solar medium. The detection of SA$谓$s would provide useful information on the composition of primary cosmic rays as well as the solar density. These neutrinos represent an irreducible source of background for indirect searches for dark matter towards the Sun and the measurement of their flux would allow for a better assessment of the uncertainties related to these searches. In this paper we report on the analysis performed, based on an unbinned likelihood maximisation, to search for SA$谓$s with the ANTARES neutrino telescope. After analysing the data collected over 11 years, no evidence for a solar atmospheric neutrino signal has been found. An upper limit at 90\% confidence level on the flux of solar atmospheric neutrinos has been obtained, equal to 7$\times$$10^{-11}$ [TeV$^{-1}$cm$^{-2}$s$^{-1}$] at E$_谓=$ 1 TeV for the reference cosmic ray model assumed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11642v2-abstract-full').style.display = 'none'; document.getElementById('2201.11642v2-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Sections renamed and reorganized as asked by the Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP06(2022)018 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.07313">arXiv:2201.07313</a> <span> [<a href="https://arxiv.org/pdf/2201.07313">pdf</a>, <a href="https://arxiv.org/format/2201.07313">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac6def">10.3847/1538-4357/ac6def <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Spatial Correlations of Neutrinos with Ultra-High-Energy Cosmic Rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+ANTARES+collaboration"> The ANTARES collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a> , et al. (1025 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="2201.07313v3-abstract-short" style="display: inline;"> For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of high-energy astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos, since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields. In this paper, we present three different approaches for corre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07313v3-abstract-full').style.display = 'inline'; document.getElementById('2201.07313v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.07313v3-abstract-full" style="display: none;"> For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of high-energy astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos, since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields. In this paper, we present three different approaches for correlating the arrival directions of neutrinos with the arrival directions of UHECRs. The neutrino data is provided by the IceCube Neutrino Observatory and ANTARES, while the UHECR data with energies above $\sim$50 EeV is provided by the Pierre Auger Observatory and the Telescope Array. All experiments provide increased statistics and improved reconstructions with respect to our previous results reported in 2015. The first analysis uses a high-statistics neutrino sample optimized for point-source searches to search for excesses of neutrinos clustering in the vicinity of UHECR directions. The second analysis searches for an excess of UHECRs in the direction of the highest-energy neutrinos. The third analysis searches for an excess of pairs of UHECRs and highest-energy neutrinos on different angular scales. None of the analyses has found a significant excess, and previously reported over-fluctuations are reduced in significance. Based on these results, we further constrain the neutrino flux spatially correlated with UHECRs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07313v3-abstract-full').style.display = 'none'; document.getElementById('2201.07313v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">39 pages, 7 figures, 4 tables; updated source files including xml authorlist</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-22-033-AD-PPD-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 934 164 (2022) </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/2107.08063">arXiv:2107.08063</a> <span> [<a href="https://arxiv.org/pdf/2107.08063">pdf</a>, <a href="https://arxiv.org/format/2107.08063">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atmospheric and Oceanic Physics">physics.ao-ph</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="Populations and Evolution">q-bio.PE</span> </div> </div> <p class="title is-5 mathjax"> Studying Bioluminescence Flashes with the ANTARES Deep Sea Neutrino Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Reeb%2C+N">N. Reeb</a>, <a href="/search/astro-ph?searchtype=author&query=Hutschenreuter%2C+S">S. Hutschenreuter</a>, <a href="/search/astro-ph?searchtype=author&query=Zehetner%2C+P">P. Zehetner</a>, <a href="/search/astro-ph?searchtype=author&query=Ensslin%2C+T">T. Ensslin</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a> , et al. (119 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="2107.08063v1-abstract-short" style="display: inline;"> We develop a novel technique to exploit the extensive data sets provided by underwater neutrino telescopes to gain information on bioluminescence in the deep sea. The passive nature of the telescopes gives us the unique opportunity to infer information on bioluminescent organisms without actively interfering with them. We propose a statistical method that allows us to reconstruct the light emissio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08063v1-abstract-full').style.display = 'inline'; document.getElementById('2107.08063v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08063v1-abstract-full" style="display: none;"> We develop a novel technique to exploit the extensive data sets provided by underwater neutrino telescopes to gain information on bioluminescence in the deep sea. The passive nature of the telescopes gives us the unique opportunity to infer information on bioluminescent organisms without actively interfering with them. We propose a statistical method that allows us to reconstruct the light emission of individual organisms, as well as their location and movement. A mathematical model is built to describe the measurement process of underwater neutrino telescopes and the signal generation of the biological organisms. The Metric Gaussian Variational Inference algorithm is used to reconstruct the model parameters using photon counts recorded by the neutrino detectors. We apply this method to synthetic data sets and data collected by the ANTARES neutrino telescope. The telescope is located 40 km off the French coast and fixed to the sea floor at a depth of 2475 m. The runs with synthetic data reveal that we can reliably model the emitted bioluminescent flashes of the organisms. Furthermore, we find that the spatial resolution of the localization of light sources highly depends on the configuration of the telescope. Precise measurements of the efficiencies of the detectors and the attenuation length of the water are crucial to reconstruct the light emission. Finally, the application to ANTARES data reveals the first precise localizations of bioluminescent organisms using neutrino telescope data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08063v1-abstract-full').style.display = 'none'; document.getElementById('2107.08063v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.15526">arXiv:2103.15526</a> <span> [<a href="https://arxiv.org/pdf/2103.15526">pdf</a>, <a href="https://arxiv.org/format/2103.15526">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac16d6">10.3847/1538-4357/ac16d6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for neutrinos from the tidal disruption events AT2019dsg and AT2019fdr with the ANTARES telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a> , et al. (119 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="2103.15526v1-abstract-short" style="display: inline;"> On October 1, 2019, the IceCube Collaboration detected a muon track neutrino with high probability of being of astrophysical origin, IC191001A. After a few hours, the tidal disruption event (TDE) AT2019dsg, observed by the Zwicky Transient Facility (ZTF), was indicated as the most likely counterpart of the IceCube track. More recently, the follow-up campaign of the IceCube alerts by ZTF suggested… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.15526v1-abstract-full').style.display = 'inline'; document.getElementById('2103.15526v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.15526v1-abstract-full" style="display: none;"> On October 1, 2019, the IceCube Collaboration detected a muon track neutrino with high probability of being of astrophysical origin, IC191001A. After a few hours, the tidal disruption event (TDE) AT2019dsg, observed by the Zwicky Transient Facility (ZTF), was indicated as the most likely counterpart of the IceCube track. More recently, the follow-up campaign of the IceCube alerts by ZTF suggested a second TDE, AT2019fdr, as a promising counterpart of another IceCube muon track candidate, IC200530A, detected on May 30, 2020. These are the second and third associations between astrophysical sources and high-energy neutrinos after the compelling identification of the blazar TXS 0506+056. Here, the search for ANTARES neutrinos from the directions of AT2019dsg and AT2019fdr using a time-integrated approach is presented. As no significant evidence for space clustering is found in the ANTARES data, upper limits on the one-flavour neutrino flux and fluence are set. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.15526v1-abstract-full').style.display = 'none'; document.getElementById('2103.15526v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 1 figure</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/2101.12170">arXiv:2101.12170</a> <span> [<a href="https://arxiv.org/pdf/2101.12170">pdf</a>, <a href="https://arxiv.org/format/2101.12170">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="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/10.1016/j.physletb.2021.136228">10.1016/j.physletb.2021.136228 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the atmospheric $谓_e$ and $谓_渭$ energy spectra with the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a> , et al. (117 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="2101.12170v2-abstract-short" style="display: inline;"> This letter presents a combined measurement of the energy spectra of atmospheric $谓_e$ and $谓_渭$ in the energy range between $\sim$100 GeV and $\sim$50 TeV with the ANTARES neutrino telescope. The analysis uses 3012 days of detector livetime in the period 2007--2017, and selects 1016 neutrinos interacting in (or close to) the instrumented volume of the detector, yielding shower-like events (mainly… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12170v2-abstract-full').style.display = 'inline'; document.getElementById('2101.12170v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.12170v2-abstract-full" style="display: none;"> This letter presents a combined measurement of the energy spectra of atmospheric $谓_e$ and $谓_渭$ in the energy range between $\sim$100 GeV and $\sim$50 TeV with the ANTARES neutrino telescope. The analysis uses 3012 days of detector livetime in the period 2007--2017, and selects 1016 neutrinos interacting in (or close to) the instrumented volume of the detector, yielding shower-like events (mainly from $谓_e+\overline 谓_e$ charged current plus all neutrino neutral current interactions) and starting track events (mainly from $谓_渭+ \overline 谓_渭$ charged current interactions). The contamination by atmospheric muons in the final sample is suppressed at the level of a few per mill by different steps in the selection analysis, including a Boosted Decision Tree classifier. The distribution of reconstructed events is unfolded in terms of electron and muon neutrino fluxes. The derived energy spectra are compared with previous measurements that, above 100 GeV, are limited to experiments in polar ice and, for $谓_渭$, to Super-Kamiokande. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12170v2-abstract-full').style.display = 'none'; document.getElementById('2101.12170v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Accepted to PLB</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.15082">arXiv:2012.15082</a> <span> [<a href="https://arxiv.org/pdf/2012.15082">pdf</a>, <a href="https://arxiv.org/format/2012.15082">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abe53c">10.3847/1538-4357/abe53c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ANTARES search for point-sources of neutrinos using astrophysical catalogs: a likelihood stacking analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Branzas%2C+H">H. Branzas</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+V">V. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">S. Celli</a> , et al. (114 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="2012.15082v1-abstract-short" style="display: inline;"> A search for astrophysical point-like neutrino sources using the data collected by the ANTARES detector between January 29, 2007 and December 31, 2017 is presented. A likelihood stacking method is used to assess the significance of an excess of muon neutrinos inducing track-like events in correlation with the location of a list of possible sources. Different sets of objects are tested in the analy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.15082v1-abstract-full').style.display = 'inline'; document.getElementById('2012.15082v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.15082v1-abstract-full" style="display: none;"> A search for astrophysical point-like neutrino sources using the data collected by the ANTARES detector between January 29, 2007 and December 31, 2017 is presented. A likelihood stacking method is used to assess the significance of an excess of muon neutrinos inducing track-like events in correlation with the location of a list of possible sources. Different sets of objects are tested in the analysis: a) a sub-sample of the \textit{Fermi} 3LAC catalog of blazars, b) a jet-obscured AGN population, c) a sample of soft gamma-ray selected radio galaxies, d) a star-forming galaxy catalog , and e) a public sample of 56 very-high-energy track events from the IceCube experiment. None of the tested sources shows a significant association with the sample of neutrinos detected by ANTARES. The smallest p-value is obtained for the radio galaxies catalog with an equal weights hypothesis, with a pre-trial p-value equivalent to a $2.8 \, 蟽$ excess, equivalent to $1.6 \, 蟽$ post-trial. In addition, the results of a dedicated analysis for the blazar MG3 J225517+2409 are also reported: this source is found to be the most significant within the \textit{Fermi} 3LAC sample, with 5 ANTARES events located at less than one degree from the source. This blazar showed evidence of flaring activity in \textit{Fermi} data, in space-time coincidence with a high-energy track detected by IceCube. An \emph{a posteriori} significance of $2.0\, 蟽$ for the combination of ANTARES and IceCube data is reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.15082v1-abstract-full').style.display = 'none'; document.getElementById('2012.15082v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.11411">arXiv:2011.11411</a> <span> [<a href="https://arxiv.org/pdf/2011.11411">pdf</a>, <a href="https://arxiv.org/format/2011.11411">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/10.1088/1475-7516/2021/03/092">10.1088/1475-7516/2021/03/092 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ANTARES upper limits on the multi-TeV neutrino emission from the GRBs detected by IACTs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+V">V. Carretero</a> , et al. (113 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="2011.11411v2-abstract-short" style="display: inline;"> The first gamma-ray burst detections by Imaging Atmospheric Cherenkov Telescopes have been recently announced: GRB 190114C, detected by MAGIC, GRB 180720B and GRB 190829A, observed by H.E.S.S. A dedicated search for neutrinos in space and time coincidence with the gamma-ray emission observed by IACTs has been performed using ANTARES data. The search covers both the prompt and afterglow phases, yie… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.11411v2-abstract-full').style.display = 'inline'; document.getElementById('2011.11411v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.11411v2-abstract-full" style="display: none;"> The first gamma-ray burst detections by Imaging Atmospheric Cherenkov Telescopes have been recently announced: GRB 190114C, detected by MAGIC, GRB 180720B and GRB 190829A, observed by H.E.S.S. A dedicated search for neutrinos in space and time coincidence with the gamma-ray emission observed by IACTs has been performed using ANTARES data. The search covers both the prompt and afterglow phases, yielding no neutrinos in coincidence with the three GRBs studied. Upper limits on the energetics of the neutrino emission are inferred. The resulting upper limits are several orders of magnitude above the observed gamma-ray emission, and they do not allow to constrain the available models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.11411v2-abstract-full').style.display = 'none'; document.getElementById('2011.11411v2-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">accepted for publication in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 03 (2021) 092 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.06621">arXiv:2010.06621</a> <span> [<a href="https://arxiv.org/pdf/2010.06621">pdf</a>, <a href="https://arxiv.org/format/2010.06621">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/10.1088/1475-7516/2021/01/064">10.1088/1475-7516/2021/01/064 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monte Carlo simulations for the ANTARES underwater neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+ANTARES+Collaboration"> The ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Branzas%2C+H">H. Branzas</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Cecchini%2C+S">S. Cecchini</a> , et al. (111 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="2010.06621v1-abstract-short" style="display: inline;"> Monte Carlo simulations are a unique tool to check the response of a detector and to monitor its performance. For a deep-sea neutrino telescope, the variability of the environmental conditions that can affect the behaviour of the data acquisition system must be considered, in addition to a reliable description of the active parts of the detector and of the features of physics events, in order to p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.06621v1-abstract-full').style.display = 'inline'; document.getElementById('2010.06621v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.06621v1-abstract-full" style="display: none;"> Monte Carlo simulations are a unique tool to check the response of a detector and to monitor its performance. For a deep-sea neutrino telescope, the variability of the environmental conditions that can affect the behaviour of the data acquisition system must be considered, in addition to a reliable description of the active parts of the detector and of the features of physics events, in order to produce a realistic set of simulated events. In this paper, the software tools used to produce neutrino and cosmic ray signatures in the telescope and the strategy developed to represent the time evolution of the natural environment and of the detector efficiency are described. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.06621v1-abstract-full').style.display = 'none'; document.getElementById('2010.06621v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP01(2021)064 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.02127">arXiv:2008.02127</a> <span> [<a href="https://arxiv.org/pdf/2008.02127">pdf</a>, <a href="https://arxiv.org/format/2008.02127">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> <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/10.1093/mnras/staa3503">10.1093/mnras/staa3503 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the contribution of Gamma-Ray Bursts to the high-energy diffuse neutrino flux with 10 years of ANTARES data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">S. Celli</a> , et al. (111 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="2008.02127v2-abstract-short" style="display: inline;"> Addressing the origin of the astrophysical neutrino flux observed by IceCube is of paramount importance. Gamma-Ray Bursts (GRBs) are among the few astrophysical sources capable of achieving the required energy to contribute to such neutrino flux through p$纬$ interactions. In this work, ANTARES data have been used to search for upward going muon neutrinos in spatial and temporal coincidence with 78… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.02127v2-abstract-full').style.display = 'inline'; document.getElementById('2008.02127v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.02127v2-abstract-full" style="display: none;"> Addressing the origin of the astrophysical neutrino flux observed by IceCube is of paramount importance. Gamma-Ray Bursts (GRBs) are among the few astrophysical sources capable of achieving the required energy to contribute to such neutrino flux through p$纬$ interactions. In this work, ANTARES data have been used to search for upward going muon neutrinos in spatial and temporal coincidence with 784 GRBs occurred from 2007 to 2017. For each GRB, the expected neutrino flux has been calculated in the framework of the internal shock model and the impact of the lack of knowledge on the majority of source redshifts and on other intrinsic parameters of the emission mechanism has been quantified. It is found that the model parameters that set the radial distance where shock collisions occur have the largest impact on neutrino flux expectations. In particular, the bulk Lorentz factor of the source ejecta and the minimum variability timescale are found to contribute significantly to the GRB-neutrino flux uncertainty. For the selected sources, ANTARES data have been analysed, by maximising the discovery probability of the stacking sample through an extended maximum-likelihood strategy. Since no neutrino event passed the quality cuts set by the optimisation procedure, 90\% confidence level upper limits (with their uncertainty) on the total expected diffuse neutrino flux have been derived, according to the model. The GRB contribution to the observed diffuse astrophysical neutrino flux around 100 TeV is constrained to be less than 10\%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.02127v2-abstract-full').style.display = 'none'; document.getElementById('2008.02127v2-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS 500 (2021) 5614 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.16090">arXiv:2007.16090</a> <span> [<a href="https://arxiv.org/pdf/2007.16090">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"> Deep-sea deployment of the KM3NeT neutrino telescope detection units by self-unrolling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+KM3NeT+Collaboration"> The 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=Ameli%2C+F">F. Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Anassontzis%2C+E+G">E. G. Anassontzis</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=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=Bakker%2C+R">R. Bakker</a>, <a href="/search/astro-ph?searchtype=author&query=Barbarino%2C+G">G. Barbarino</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=Berbeen%2C+E">E. Berbeen</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=Billault%2C+M">M. Billault</a> , et al. (230 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="2007.16090v1-abstract-short" style="display: inline;"> KM3NeT is a research infrastructure being installed in the deep Mediterranean Sea. It will house a neutrino telescope comprising hundreds of networked moorings - detection units or strings equipped with optical instrumentation to detect the Cherenkov radiation generated by charged particles from neutrino-induced collisions in its vicinity. In comparison to moorings typically used for oceanography,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.16090v1-abstract-full').style.display = 'inline'; document.getElementById('2007.16090v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.16090v1-abstract-full" style="display: none;"> KM3NeT is a research infrastructure being installed in the deep Mediterranean Sea. It will house a neutrino telescope comprising hundreds of networked moorings - detection units or strings equipped with optical instrumentation to detect the Cherenkov radiation generated by charged particles from neutrino-induced collisions in its vicinity. In comparison to moorings typically used for oceanography, several key features of the KM3NeT string are different: the instrumentation is contained in transparent and thus unprotected glass spheres; two thin Dyneema ropes are used as strength members; and a thin delicate backbone tube with fibre-optics and copper wires for data and power transmission, respectively, runs along the full length of the mooring. Also, compared to other neutrino telescopes such as ANTARES in the Mediterranean Sea and GVD in Lake Baikal, the KM3NeT strings are more slender to minimise the amount of material used for support of the optical sensors. Moreover, the rate of deploying a large number of strings in a period of a few years is unprecedented. For all these reasons, for the installation of the KM3NeT strings, a custom-made, fast deployment method was designed. Despite the length of several hundreds of metres, the slim design of the string allows it to be compacted into a small, re-usable spherical launching vehicle instead of deploying the mooring weight down from a surface vessel. After being lowered to the seafloor, the string unfurls to its full length with the buoyant launching vehicle rolling along the two ropes.The design of the vehicle, the loading with a string, and its underwater self-unrolling are detailed in this paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.16090v1-abstract-full').style.display = 'none'; document.getElementById('2007.16090v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.00931">arXiv:2007.00931</a> <span> [<a href="https://arxiv.org/pdf/2007.00931">pdf</a>, <a href="https://arxiv.org/ps/2007.00931">ps</a>, <a href="https://arxiv.org/format/2007.00931">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> <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/10.1103/PhysRevD.102.122007">10.1103/PhysRevD.102.122007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of the cosmic ray shadow of the Sun with the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma1%2C+B">B. Belhorma1</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">S. Celli</a> , et al. (112 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="2007.00931v2-abstract-short" style="display: inline;"> The ANTARES detector is an undersea neutrino telescope in the Mediterranean Sea. The search for point-like neutrino sources is one of the main goals of the ANTARES telescope, requiring a reliable method to evaluate the detector angular resolution and pointing accuracy. This work describes the study of the Sun "shadow" effect with the ANTARES detector. The shadow is the deficit in the atmospheric m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.00931v2-abstract-full').style.display = 'inline'; document.getElementById('2007.00931v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.00931v2-abstract-full" style="display: none;"> The ANTARES detector is an undersea neutrino telescope in the Mediterranean Sea. The search for point-like neutrino sources is one of the main goals of the ANTARES telescope, requiring a reliable method to evaluate the detector angular resolution and pointing accuracy. This work describes the study of the Sun "shadow" effect with the ANTARES detector. The shadow is the deficit in the atmospheric muon flux in the direction of the Sun caused by the absorption of the primary cosmic rays. This analysis is based on the data collected between 2008 and 2017 by the ANTARES telescope. The observed statistical significance of the Sun shadow detection is $3.7蟽$, with an estimated angular resolution of $0.59^\circ\pm0.10^\circ$ for downward-going muons. The pointing accuracy is found to be consistent with the expectations and no evidence of systematic pointing shifts is observed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.00931v2-abstract-full').style.display = 'none'; document.getElementById('2007.00931v2-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">7 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 102, 122007 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.08254">arXiv:2004.08254</a> <span> [<a href="https://arxiv.org/pdf/2004.08254">pdf</a>, <a href="https://arxiv.org/format/2004.08254">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="High Energy Physics - Experiment">hep-ex</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/10.1088/1748-0221/15/10/P10005">10.1088/1748-0221/15/10/P10005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Event reconstruction for KM3NeT/ORCA using convolutional neural networks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">Arnauld Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">Sergio Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Zineb Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">Fabrizio Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">Michel Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androulakis%2C+G">Giorgos Androulakis</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">Marco Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">Mancia Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">Gisela Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">Miquel Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Bagatelas%2C+C">Christos Bagatelas</a>, <a href="/search/astro-ph?searchtype=author&query=Barbarino%2C+G">Giancarlo Barbarino</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">Bruny Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">Suzan Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">Meriem Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Berbee%2C+E">Edward Berbee</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+V">Vincent Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Biagi%2C+S">Simone Biagi</a>, <a href="/search/astro-ph?searchtype=author&query=Biagioni%2C+A">Andrea Biagioni</a>, <a href="/search/astro-ph?searchtype=author&query=Bissinger%2C+M">Matthias Bissinger</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">Markus Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">Jihad Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">Mohammed Bouta</a> , et al. (207 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="2004.08254v1-abstract-short" style="display: inline;"> The KM3NeT research infrastructure is currently under construction at two locations in the Mediterranean Sea. The KM3NeT/ORCA water-Cherenkov neutrino detector off the French coast will instrument several megatons of seawater with photosensors. Its main objective is the determination of the neutrino mass ordering. This work aims at demonstrating the general applicability of deep convolutional neur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.08254v1-abstract-full').style.display = 'inline'; document.getElementById('2004.08254v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.08254v1-abstract-full" style="display: none;"> The KM3NeT research infrastructure is currently under construction at two locations in the Mediterranean Sea. The KM3NeT/ORCA water-Cherenkov neutrino detector off the French coast will instrument several megatons of seawater with photosensors. Its main objective is the determination of the neutrino mass ordering. This work aims at demonstrating the general applicability of deep convolutional neural networks to neutrino telescopes, using simulated datasets for the KM3NeT/ORCA detector as an example. To this end, the networks are employed to achieve reconstruction and classification tasks that constitute an alternative to the analysis pipeline presented for KM3NeT/ORCA in the KM3NeT Letter of Intent. They are used to infer event reconstruction estimates for the energy, the direction, and the interaction point of incident neutrinos. The spatial distribution of Cherenkov light generated by charged particles induced in neutrino interactions is classified as shower- or track-like, and the main background processes associated with the detection of atmospheric neutrinos are recognized. Performance comparisons to machine-learning classification and maximum-likelihood reconstruction algorithms previously developed for KM3NeT/ORCA are provided. It is shown that this application of deep convolutional neural networks to simulated datasets for a large-volume neutrino telescope yields competitive reconstruction results and performance improvements with respect to classical approaches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.08254v1-abstract-full').style.display = 'none'; document.getElementById('2004.08254v1-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 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 15 P10005 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.14040">arXiv:2003.14040</a> <span> [<a href="https://arxiv.org/pdf/2003.14040">pdf</a>, <a href="https://arxiv.org/format/2003.14040">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.cpc.2020.107477">10.1016/j.cpc.2020.107477 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> gSeaGen: the KM3NeT GENIE-based code for neutrino telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">Arnauld Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Garre%2C+S+A">Sergio Alves Garre</a>, <a href="/search/astro-ph?searchtype=author&query=Aly%2C+Z">Zineb Aly</a>, <a href="/search/astro-ph?searchtype=author&query=Ameli%2C+F">Fabrizio Ameli</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">Michel Andre</a>, <a href="/search/astro-ph?searchtype=author&query=Androulakis%2C+G">Giorgos Androulakis</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">Marco Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+M">Mancia Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">Gisela Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">Miquel Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Bagatelas%2C+C">Christos Bagatelas</a>, <a href="/search/astro-ph?searchtype=author&query=Barbarino%2C+G">Giancarlo Barbarino</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">Bruny Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Pree%2C+S+B+d">Suzan Basegmez du Pree</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">Meriem Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Berbee%2C+E">Edward Berbee</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+V">Vincent Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Biagi%2C+S">Simone Biagi</a>, <a href="/search/astro-ph?searchtype=author&query=Biagioni%2C+A">Andrea Biagioni</a>, <a href="/search/astro-ph?searchtype=author&query=Bissinger%2C+M">Matthias Bissinger</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">Markus Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">Jihad Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bourret%2C+S">Simon Bourret</a> , et al. (211 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="2003.14040v1-abstract-short" style="display: inline;"> The gSeaGen code is a GENIE-based application developed to efficiently generate high statistics samples of events, induced by neutrino interactions, detectable in a neutrino telescope. The gSeaGen code is able to generate events induced by all neutrino flavours, considering topological differences between track-type and shower-like events. Neutrino interactions are simulated taking into account th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.14040v1-abstract-full').style.display = 'inline'; document.getElementById('2003.14040v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.14040v1-abstract-full" style="display: none;"> The gSeaGen code is a GENIE-based application developed to efficiently generate high statistics samples of events, induced by neutrino interactions, detectable in a neutrino telescope. The gSeaGen code is able to generate events induced by all neutrino flavours, considering topological differences between track-type and shower-like events. Neutrino interactions are simulated taking into account the density and the composition of the media surrounding the detector. The main features of gSeaGen are presented together with some examples of its application within the KM3NeT project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.14040v1-abstract-full').style.display = 'none'; document.getElementById('2003.14040v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">45 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Volume 256, November 2020, 107477 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.06614">arXiv:2003.06614</a> <span> [<a href="https://arxiv.org/pdf/2003.06614">pdf</a>, <a href="https://arxiv.org/format/2003.06614">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.102.082002">10.1103/PhysRevD.102.082002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combined search for neutrinos from dark matter self-annihilation in the Galactic Centre with ANTARES and IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">S. Celli</a>, <a href="/search/astro-ph?searchtype=author&query=Chabab%2C+M">M. Chabab</a> , et al. (474 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="2003.06614v2-abstract-short" style="display: inline;"> We present the results of the first combined dark matter search targeting the Galactic Centre using the ANTARES and IceCube neutrino telescopes. For dark matter particles with masses from 50 to 1000 GeV, the sensitivities on the self-annihilation cross section set by ANTARES and IceCube are comparable, making this mass range particularly interesting for a joint analysis. Dark matter self-annihilat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.06614v2-abstract-full').style.display = 'inline'; document.getElementById('2003.06614v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.06614v2-abstract-full" style="display: none;"> We present the results of the first combined dark matter search targeting the Galactic Centre using the ANTARES and IceCube neutrino telescopes. For dark matter particles with masses from 50 to 1000 GeV, the sensitivities on the self-annihilation cross section set by ANTARES and IceCube are comparable, making this mass range particularly interesting for a joint analysis. Dark matter self-annihilation through the $蟿^+蟿^-$, $渭^+渭^-$, $b\bar{b}$ and $W^+W^-$ channels is considered for both the Navarro-Frenk-White and Burkert halo profiles. In the combination of 2,101.6 days of ANTARES data and 1,007 days of IceCube data, no excess over the expected background is observed. Limits on the thermally-averaged dark matter annihilation cross section $\langle蟽_A\upsilon\rangle$ are set. These limits present an improvement of up to a factor of two in the studied dark matter mass range with respect to the individual limits published by both collaborations. When considering dark matter particles with a mass of 200 GeV annihilating through the $蟿^+蟿^-$ channel, the value obtained for the limit is $7.44 \times 10^{-24} \text{cm}^{3}\text{s}^{-1}$ for the Navarro-Frenk-White halo profile. For the purpose of this joint analysis, the model parameters and the likelihood are unified, providing a benchmark for forthcoming dark matter searches performed by neutrino telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.06614v2-abstract-full').style.display = 'none'; document.getElementById('2003.06614v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 102, 082002 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.04022">arXiv:2003.04022</a> <span> [<a href="https://arxiv.org/pdf/2003.04022">pdf</a>, <a href="https://arxiv.org/format/2003.04022">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 - 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/10.1140/epjc/s10052-020-8015-6">10.1140/epjc/s10052-020-8015-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for neutrino counterparts of gravitational-wave events detected by LIGO and Virgo during run O2 with the ANTARES telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+J">J. J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">S. Celli</a> , et al. (113 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="2003.04022v4-abstract-short" style="display: inline;"> An offline search for a neutrino counterpart to gravitational-wave (GW) events detected during the second observation run (O2) of Advanced-LIGO and Advanced-Virgo performed with ANTARES data is presented. In addition to the search for long tracks induced by $谓_渭$ ($\bar谓_渭$) charged current interactions, a search for showering events induced by interactions of neutrinos of any flavour is conducted… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.04022v4-abstract-full').style.display = 'inline'; document.getElementById('2003.04022v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.04022v4-abstract-full" style="display: none;"> An offline search for a neutrino counterpart to gravitational-wave (GW) events detected during the second observation run (O2) of Advanced-LIGO and Advanced-Virgo performed with ANTARES data is presented. In addition to the search for long tracks induced by $谓_渭$ ($\bar谓_渭$) charged current interactions, a search for showering events induced by interactions of neutrinos of any flavour is conducted. The severe spatial and time coincidence provided by the gravitational-wave alert allows regions above the detector horizon to be probed, extending the ANTARES sensitivity over the entire sky. The results of this all-neutrino-flavour and all-sky time dependent analysis are presented. The search for prompt neutrino emission within $\pm$500~s around the time of six GW events yields no neutrino counterparts. Upper limits on the neutrino spectral fluence and constraints on the isotropic radiated energy are set for each GW event analysed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.04022v4-abstract-full').style.display = 'none'; document.getElementById('2003.04022v4-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C volume 80 (2020) 487 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.04412">arXiv:2001.04412</a> <span> [<a href="https://arxiv.org/pdf/2001.04412">pdf</a>, <a href="https://arxiv.org/format/2001.04412">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab7afb">10.3847/1538-4357/ab7afb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ANTARES and IceCube Combined Search for Neutrino Point-like and Extended Sources in the Southern Sky </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a> , et al. (481 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="2001.04412v1-abstract-short" style="display: inline;"> A search for point-like and extended sources of cosmic neutrinos using data collected by the ANTARES and IceCube neutrino telescopes is presented. The data set consists of all the track-like and shower-like events pointing in the direction of the Southern Sky included in the nine-year ANTARES point-source analysis, combined with the through-going track-like events used in the seven-year IceCube po… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.04412v1-abstract-full').style.display = 'inline'; document.getElementById('2001.04412v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.04412v1-abstract-full" style="display: none;"> A search for point-like and extended sources of cosmic neutrinos using data collected by the ANTARES and IceCube neutrino telescopes is presented. The data set consists of all the track-like and shower-like events pointing in the direction of the Southern Sky included in the nine-year ANTARES point-source analysis, combined with the through-going track-like events used in the seven-year IceCube point-source search. The advantageous field of view of ANTARES and the large size of IceCube are exploited to improve the sensitivity in the Southern Sky by a factor $\sim$2 compared to both individual analyses. In this work, the Southern Sky is scanned for possible excesses of spatial clustering, and the positions of preselected candidate sources are investigated. In addition, special focus is given to the region around the Galactic Centre, whereby a dedicated search at the location of SgrA* is performed, and to the location of the supernova remnant RXJ 1713.7-3946. No significant evidence for cosmic neutrino sources is found and upper limits on the flux from the various searches are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.04412v1-abstract-full').style.display = 'none'; document.getElementById('2001.04412v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys. J. 892 (2020) 92 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.02561">arXiv:1911.02561</a> <span> [<a href="https://arxiv.org/pdf/1911.02561">pdf</a>, <a href="https://arxiv.org/format/1911.02561">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"> Neutrino astronomy with the next generation IceCube Neutrino Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aartsen%2C+M+G">M. G. Aartsen</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahrens%2C+M">M. Ahrens</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T">T. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Ansseau%2C+I">I. Ansseau</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Arlen%2C+T+C">T. C. Arlen</a>, <a href="/search/astro-ph?searchtype=author&query=Auffenberg%2C+J">J. Auffenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S">S. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+P">P. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Bagherpour%2C+H">H. Bagherpour</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Barbano%2C+A">A. Barbano</a>, <a href="/search/astro-ph?searchtype=author&query=Bartos%2C+I">I. Bartos</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+B">B. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+V">V. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a> , et al. (378 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="1911.02561v1-abstract-short" style="display: inline;"> The past decade has welcomed the emergence of cosmic neutrinos as a new messenger to explore the most extreme environments of the universe. The discovery measurement of cosmic neutrinos, announced by IceCube in 2013, has opened a new window of observation that has already resulted in new fundamental information that holds the potential to answer key questions associated with the high-energy univer… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.02561v1-abstract-full').style.display = 'inline'; document.getElementById('1911.02561v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.02561v1-abstract-full" style="display: none;"> The past decade has welcomed the emergence of cosmic neutrinos as a new messenger to explore the most extreme environments of the universe. The discovery measurement of cosmic neutrinos, announced by IceCube in 2013, has opened a new window of observation that has already resulted in new fundamental information that holds the potential to answer key questions associated with the high-energy universe, including: what are the sources in the PeV sky and how do they drive particle acceleration; where are cosmic rays of extreme energies produced, and on which paths do they propagate through the universe; and are there signatures of new physics at TeV-PeV energies and above? The planned advancements in neutrino telescope arrays in the next decade, in conjunction with continued progress in broad multimessenger astrophysics, promise to elevate the cosmic neutrino field from the discovery to the precision era and to a survey of the sources in the neutrino sky. The planned detector upgrades to the IceCube Neutrino Observatory, culminating in IceCube-Gen2 (an envisaged $400M facility with anticipated operation in the next decade, described in this white paper) are the cornerstone that will drive the evolution of neutrino astrophysics measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.02561v1-abstract-full').style.display = 'none'; document.getElementById('1911.02561v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">related submission to Astro2020 decadal survey</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.00112">arXiv:1910.00112</a> <span> [<a href="https://arxiv.org/pdf/1910.00112">pdf</a>, <a href="https://arxiv.org/format/1910.00112">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="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/10.1016/j.cpc.2020.107433">10.1016/j.cpc.2020.107433 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Control Unit of the KM3NeT Data Acquisition System </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=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=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=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=Barbarino%2C+G">G. Barbarino</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=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=Biagioni%2C+A">A. Biagioni</a>, <a href="/search/astro-ph?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouvet%2C+G">G. Bouvet</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M">M. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+C">C. Bozza</a> , et al. (195 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="1910.00112v1-abstract-short" style="display: inline;"> The KM3NeT Collaboration runs a multi-site neutrino observatory in the Mediterranean Sea. Water Cherenkov particle detectors, deep in the sea and far off the coasts of France and Italy, are already taking data while incremental construction progresses. Data Acquisition Control software is operating off-shore detectors as well as testing and qualification stations for their components. The software… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.00112v1-abstract-full').style.display = 'inline'; document.getElementById('1910.00112v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.00112v1-abstract-full" style="display: none;"> The KM3NeT Collaboration runs a multi-site neutrino observatory in the Mediterranean Sea. Water Cherenkov particle detectors, deep in the sea and far off the coasts of France and Italy, are already taking data while incremental construction progresses. Data Acquisition Control software is operating off-shore detectors as well as testing and qualification stations for their components. The software, named Control Unit, is highly modular. It can undergo upgrades and reconfiguration with the acquisition running. Interplay with the central database of the Collaboration is obtained in a way that allows for data taking even if Internet links fail. In order to simplify the management of computing resources in the long term, and to cope with possible hardware failures of one or more computers, the KM3NeT Control Unit software features a custom dynamic resource provisioning and failover technology, which is especially important for ensuring continuity in case of rare transient events in multi-messenger astronomy. The software architecture relies on ubiquitous tools and broadly adopted technologies and has been successfully tested on several operating systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.00112v1-abstract-full').style.display = 'none'; document.getElementById('1910.00112v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.11699">arXiv:1907.11699</a> <span>  </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> <p class="title is-5 mathjax"> The IceCube Neutrino Observatory -- Contributions to the 36th International Cosmic Ray Conference (ICRC2019) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=IceCube+Collaboration"> IceCube Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aartsen%2C+M+G">M. G. Aartsen</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahrens%2C+M">M. Ahrens</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T">T. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Ansseau%2C+I">I. Ansseau</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Auffenberg%2C+J">J. Auffenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S">S. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+P">P. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Bagherpour%2C+H">H. Bagherpour</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Barbano%2C+A">A. Barbano</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+B">B. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+V">V. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a> , et al. (334 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="1907.11699v1-abstract-short" style="display: inline;"> Contributions from the IceCube Collaboration presented at the 36th International Cosmic Ray Conference, 24 July - 1 August 2019, Madison, Wisconsin, USA. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.11699v1-abstract-full" style="display: none;"> Contributions from the IceCube Collaboration presented at the 36th International Cosmic Ray Conference, 24 July - 1 August 2019, Madison, Wisconsin, USA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.11699v1-abstract-full').style.display = 'none'; document.getElementById('1907.11699v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To access this list of contributions from IceCube, please follow the "HTML" link</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.06714">arXiv:1907.06714</a> <span> [<a href="https://arxiv.org/pdf/1907.06714">pdf</a>, <a href="https://arxiv.org/format/1907.06714">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab4ae2">10.3847/1538-4357/ab4ae2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Sources of Astrophysical Neutrinos Using Seven Years of IceCube Cascade Events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aartsen%2C+M+G">M. G. Aartsen</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahrens%2C+M">M. Ahrens</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T">T. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Ansseau%2C+I">I. Ansseau</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Auffenberg%2C+J">J. Auffenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S">S. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+P">P. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Bagherpour%2C+H">H. Bagherpour</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Barbano%2C+A">A. Barbano</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+B">B. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+V">V. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a> , et al. (330 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="1907.06714v1-abstract-short" style="display: inline;"> Low background searches for astrophysical neutrino sources anywhere in the sky can be performed using cascade events induced by neutrinos of all flavors interacting in IceCube with energies as low as ~1 TeV. Previously, we showed that even with just two years of data, the resulting sensitivity to sources in the southern sky is competitive with IceCube and ANTARES analyses using muon tracks induced… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.06714v1-abstract-full').style.display = 'inline'; document.getElementById('1907.06714v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.06714v1-abstract-full" style="display: none;"> Low background searches for astrophysical neutrino sources anywhere in the sky can be performed using cascade events induced by neutrinos of all flavors interacting in IceCube with energies as low as ~1 TeV. Previously, we showed that even with just two years of data, the resulting sensitivity to sources in the southern sky is competitive with IceCube and ANTARES analyses using muon tracks induced by charge current muon neutrino interactions - especially if the neutrino emission follows a soft energy spectrum or originates from an extended angular region. Here, we extend that work by adding five more years of data, significantly improving the cascade angular resolution, and including tests for point-like or diffuse Galactic emission to which this dataset is particularly well-suited. For many of the signal candidates considered, this analysis is the most sensitive of any experiment. No significant clustering was observed, and thus many of the resulting constraints are the most stringent to date. In this paper we will describe the improvements introduced in this analysis and discuss our results in the context of other recent work in neutrino astronomy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.06714v1-abstract-full').style.display = 'none'; document.getElementById('1907.06714v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 8 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys. J. 886 (2019) 12 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.06453">arXiv:1907.06453</a> <span> [<a href="https://arxiv.org/pdf/1907.06453">pdf</a>, <a href="https://arxiv.org/format/1907.06453">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> KM3NeT front-end and readout electronics system: hardware, firmware and software </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+KM3NeT+Collaboration"> The 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=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=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=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=Barbarino%2C+G">G. Barbarino</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=Belias%2C+A">A. Belias</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=van+Beveren%2C+V">V. van Beveren</a>, <a href="/search/astro-ph?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/astro-ph?searchtype=author&query=Biagioni%2C+A">A. Biagioni</a>, <a href="/search/astro-ph?searchtype=author&query=Bianucci%2C+S">S. Bianucci</a>, <a href="/search/astro-ph?searchtype=author&query=Billault%2C+M">M. Billault</a>, <a href="/search/astro-ph?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/astro-ph?searchtype=author&query=Bos%2C+P">P. Bos</a>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a> , et al. (215 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="1907.06453v2-abstract-short" style="display: inline;"> The KM3NeT research infrastructure being built at the bottom of the Mediterranean Sea will host water-Cherenkov telescopes for the detection of cosmic neutrinos. The neutrino telescopes will consist of large volume three-dimensional grids of optical modules to detect the Cherenkov light from charged particles produced by neutrino-induced interactions. Each optical module houses 31 3-inch photomult… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.06453v2-abstract-full').style.display = 'inline'; document.getElementById('1907.06453v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.06453v2-abstract-full" style="display: none;"> The KM3NeT research infrastructure being built at the bottom of the Mediterranean Sea will host water-Cherenkov telescopes for the detection of cosmic neutrinos. The neutrino telescopes will consist of large volume three-dimensional grids of optical modules to detect the Cherenkov light from charged particles produced by neutrino-induced interactions. Each optical module houses 31 3-inch photomultiplier tubes, instrumentation for calibration of the photomultiplier signal and positioning of the optical module and all associated electronics boards. By design, the total electrical power consumption of an optical module has been capped at seven watts. This paper presents an overview of the front-end and readout electronics system inside the optical module, which has been designed for a 1~ns synchronization between the clocks of all optical modules in the grid during a life time of at least 20 years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.06453v2-abstract-full').style.display = 'none'; document.getElementById('1907.06453v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Prepared submission to Journal of Astronomical Telescopes, Instruments, and Systems (JATIS)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.06420">arXiv:1904.06420</a> <span> [<a href="https://arxiv.org/pdf/1904.06420">pdf</a>, <a href="https://arxiv.org/format/1904.06420">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab4a74">10.3847/1538-4357/ab4a74 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Search for Cosmic Neutrino and Gamma-Ray Emitting Transients in 7.3 Years of ANTARES and Fermi LAT Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Solares%2C+H+A+A">H. A. Ayala Solares</a>, <a href="/search/astro-ph?searchtype=author&query=Cowen%2C+D+F">D. F. Cowen</a>, <a href="/search/astro-ph?searchtype=author&query=DeLaunay%2C+J+J">J. J. DeLaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Fox%2C+D+B">D. B. Fox</a>, <a href="/search/astro-ph?searchtype=author&query=Keivani%2C+A">A. Keivani</a>, <a href="/search/astro-ph?searchtype=author&query=Mostaf%C3%A1%2C+M">M. Mostaf谩</a>, <a href="/search/astro-ph?searchtype=author&query=Murase%2C+K">K. Murase</a>, <a href="/search/astro-ph?searchtype=author&query=Turley%2C+C+F">C. F. Turley</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</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=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Barrios-Mart%C4%B1%2C+J">J. Barrios-Mart谋</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</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=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a> , et al. (118 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.06420v2-abstract-short" style="display: inline;"> We analyze 7.3 years of ANTARES high-energy neutrino and Fermi LAT 纬-ray data in search of cosmic neutrino + 纬-ray (谓+纬) transient sources or source populations. Our analysis has the potential to detect either individual 谓+纬 transient sources (durations 未t < 1000~s), if they exhibit sufficient 纬-ray or neutrino multiplicity, or a statistical excess of 谓+纬 transients of lower multiplicities. Treati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.06420v2-abstract-full').style.display = 'inline'; document.getElementById('1904.06420v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.06420v2-abstract-full" style="display: none;"> We analyze 7.3 years of ANTARES high-energy neutrino and Fermi LAT 纬-ray data in search of cosmic neutrino + 纬-ray (谓+纬) transient sources or source populations. Our analysis has the potential to detect either individual 谓+纬 transient sources (durations 未t < 1000~s), if they exhibit sufficient 纬-ray or neutrino multiplicity, or a statistical excess of 谓+纬 transients of lower multiplicities. Treating ANTARES track and cascade event types separately, we establish detection thresholds by Monte Carlo scrambling of the neutrino data, and determine our analysis sensitivity by signal injection against scrambled datasets. We find our analysis is sensitive to 谓+纬 transient populations responsible for $>$5\% of the observed gamma-coincident neutrinos in the track data at 90\% confidence. Applying our analysis to the unscrambled data reveals no individual 谓+纬 events of high significance; two ANTARES track + Fermi 纬-ray events are identified that exceed a once per decade false alarm rate threshold ($p=17\%$). No evidence for subthreshold 谓+纬 source populations is found among the track ($p=39\%$) or cascade ($p=60\%$) events. While TXS 0506+056, a blazar and variable (non-transient) Fermi 纬-ray source, has recently been identified as the first source of high-energy neutrinos, the challenges in reconciling observations of the Fermi 纬-ray sky, the IceCube high-energy cosmic neutrinos, and ultra-high energy cosmic rays using only blazars suggest a significant contribution by other source populations. Searches for transient sources of high-energy neutrinos remain interesting, with the potential for neutrino clustering or multimessenger coincidence searches to lead to discovery of the first 谓+纬 transients. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.06420v2-abstract-full').style.display = 'none'; document.getElementById('1904.06420v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 5 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 886 (2019) 98 </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Andr%C3%A9%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Andr%C3%A9%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Andr%C3%A9%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Andr%C3%A9%2C+M&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Andr%C3%A9%2C+M&start=150" class="pagination-link " aria-label="Page 4" 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