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value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.12070">arXiv:2502.12070</a> <span> [<a href="https://arxiv.org/pdf/2502.12070">pdf</a>, <a href="https://arxiv.org/format/2502.12070">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"> KM3NeT Constraint on Lorentz-Violating Superluminal Neutrino Velocity </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=Adriani%2C+O">O. Adriani</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=Arg%C3%BCelles%2C+C">C. Arg眉elles</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=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=Gualandi%2C+F+B">F. Benfenati Gualandi</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> , et al. (268 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="2502.12070v2-abstract-short" style="display: inline;"> Lorentz invariance is a fundamental symmetry of spacetime and foundational to modern physics. One of its most important consequences is the constancy of the speed of light. This invariance, together with the geometry of spacetime, implies that no particle can move faster than the speed of light. In this article, we present the most stringent neutrino-based test of this prediction, using the highes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.12070v2-abstract-full').style.display = 'inline'; document.getElementById('2502.12070v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.12070v2-abstract-full" style="display: none;"> Lorentz invariance is a fundamental symmetry of spacetime and foundational to modern physics. One of its most important consequences is the constancy of the speed of light. This invariance, together with the geometry of spacetime, implies that no particle can move faster than the speed of light. In this article, we present the most stringent neutrino-based test of this prediction, using the highest energy neutrino ever detected to date, KM3-230213A. The arrival of this event, with an energy of $220^{+570}_{-110}\,\text{PeV}$, sets a constraint on $未\equiv c_谓^2-1 < 4\times10^{-22}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.12070v2-abstract-full').style.display = 'none'; document.getElementById('2502.12070v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.08387">arXiv:2502.08387</a> <span> [<a href="https://arxiv.org/pdf/2502.08387">pdf</a>, <a href="https://arxiv.org/format/2502.08387">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"> On the Potential Galactic Origin of the Ultra-High-Energy Event KM3-230213A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adriani%2C+O">O. Adriani</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=Gualandi%2C+F+B">F. Benfenati Gualandi</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. (264 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="2502.08387v2-abstract-short" style="display: inline;"> The KM3NeT observatory detected the most energetic neutrino candidate ever observed, with an energy between 72 PeV and 2.6 EeV at the 90% confidence level. The observed neutrino is likely of cosmic origin. In this article, it is investigated if the neutrino could have been produced within the Milky Way. Considering the low fluxes of the Galactic diffuse emission at these energies, the lack of a ne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.08387v2-abstract-full').style.display = 'inline'; document.getElementById('2502.08387v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.08387v2-abstract-full" style="display: none;"> The KM3NeT observatory detected the most energetic neutrino candidate ever observed, with an energy between 72 PeV and 2.6 EeV at the 90% confidence level. The observed neutrino is likely of cosmic origin. In this article, it is investigated if the neutrino could have been produced within the Milky Way. Considering the low fluxes of the Galactic diffuse emission at these energies, the lack of a nearby potential Galactic particle accelerator in the direction of the event and the difficulty to accelerate particles to such high energies in Galactic systems, we conclude that if the event is indeed cosmic, it is most likely of extragalactic origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.08387v2-abstract-full').style.display = 'none'; document.getElementById('2502.08387v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.08173">arXiv:2502.08173</a> <span> [<a href="https://arxiv.org/pdf/2502.08173">pdf</a>, <a href="https://arxiv.org/format/2502.08173">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"> The ultra-high-energy event KM3-230213A within the global neutrino landscape </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=Adriani%2C+O">O. Adriani</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=Arg%C3%BCelles%2C+C">C. Arg眉elles</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=Gualandi%2C+F+B">F. Benfenati Gualandi</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> , et al. (268 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="2502.08173v1-abstract-short" style="display: inline;"> On February 13th, 2023, the KM3NeT/ARCA telescope detected a neutrino candidate with an estimated energy in the hundreds of PeVs. In this article, the observation of this ultra-high-energy neutrino is discussed in light of null observations above tens of PeV from the IceCube and Pierre Auger observatories. Performing a joint fit of all experiments under the assumption of an isotropic $E^{-2}$ flux… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.08173v1-abstract-full').style.display = 'inline'; document.getElementById('2502.08173v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.08173v1-abstract-full" style="display: none;"> On February 13th, 2023, the KM3NeT/ARCA telescope detected a neutrino candidate with an estimated energy in the hundreds of PeVs. In this article, the observation of this ultra-high-energy neutrino is discussed in light of null observations above tens of PeV from the IceCube and Pierre Auger observatories. Performing a joint fit of all experiments under the assumption of an isotropic $E^{-2}$ flux, the best-fit single-flavour flux normalisation is $E^2 桅^{\rm 1f}_{谓+ \bar 谓} = 7.5 \times 10^{-10}~{\rm GeV cm^{-2} s^{-1} sr^{-1}}$ in the 90% energy range of the KM3NeT event. Furthermore, the ultra-high-energy data are then fit together with the IceCube measurements at lower energies, either with a single power law or with a broken power law, allowing for the presence of a new component in the spectrum. The joint fit including non-observations by other experiments in the ultra-high-energy region shows a slight preference for a break in the PeV regime if the ``High-Energy Starting Events'' sample is included, and no such preference for the other two IceCube samples investigated. A stronger preference for a break appears if only the KM3NeT data is considered in the ultra-high-energy region, though the flux resulting from such a fit would be inconsistent with null observations from IceCube and Pierre Auger. In all cases, the observed tension between KM3NeT and other datasets is of the order of $2.5蟽-3蟽$, and increased statistics are required to resolve this apparent tension and better characterise the neutrino landscape at ultra-high energies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.08173v1-abstract-full').style.display = 'none'; document.getElementById('2502.08173v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </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, 4 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/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="2411.10092v2-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('2411.10092v2-abstract-full').style.display = 'inline'; document.getElementById('2411.10092v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10092v2-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('2411.10092v2-abstract-full').style.display = 'none'; document.getElementById('2411.10092v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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/2405.09678">arXiv:2405.09678</a> <span> [<a href="https://arxiv.org/pdf/2405.09678">pdf</a>, <a href="https://arxiv.org/format/2405.09678">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> How Stellar Stream Torsion may reveal aspherical Dark Matter Haloes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bariego-Quintana%2C+A">Adriana Bariego-Quintana</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="2405.09678v1-abstract-short" style="display: inline;"> Flat rotation curves follow from elongated Dark Matter distributions, as shown by our earlier competitive fits to the SPARC database. Intending to probe that distortion of the DM halo one needs observables not contained by the galactic plane. Stellar streams are caused by tidal stretching of massive substructures such as satellite dwarf galaxies, and would lie on a plane should the DM-halo gravita… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.09678v1-abstract-full').style.display = 'inline'; document.getElementById('2405.09678v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.09678v1-abstract-full" style="display: none;"> Flat rotation curves follow from elongated Dark Matter distributions, as shown by our earlier competitive fits to the SPARC database. Intending to probe that distortion of the DM halo one needs observables not contained by the galactic plane. Stellar streams are caused by tidal stretching of massive substructures such as satellite dwarf galaxies, and would lie on a plane should the DM-halo gravitational field be spherically symmetric. But if the field does not display such spherical symmetry, stellar trajectories, as well as stellar streams, should torsion out of the plane. This is where the torsion of the stream can be of use: it is a local observable that measures the deviation from planarity of a curve; thus, it quantifies how noncentral the gravitational potential is. We have performed small simulations to confirm that indeed a galactic central force produces negligible torsion, and quantified the torsion for prolate haloes instead. Examining observational data, we select several streams at large distance from the galactic center, as most promising for the study, and by means of helicoidal fits extract their differential torsion. We see that their torsion is much larger than expected for a central spherical bulb alone, pointing to an elongated Milky Way halo. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.09678v1-abstract-full').style.display = 'none'; document.getElementById('2405.09678v1-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 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">4 pages, 1 figure, proceedings for ICWIP 2023</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/2402.08363">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/2311.03804">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/2307.07402">arXiv:2307.07402</a> <span> [<a href="https://arxiv.org/pdf/2307.07402">pdf</a>, <a href="https://arxiv.org/format/2307.07402">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202347502">10.1051/0004-6361/202347502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The torsion of stellar streams and the overall shape of galactic gravity's source </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bariego-Quintana%2C+A">Adriana Bariego-Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Llanes-Estrada%2C+F+J">Felipe J. Llanes-Estrada</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.07402v2-abstract-short" style="display: inline;"> Flat rotation curves v(r) are naturally explained by elongated (prolate) Dark Matter (DM) distributions, and we have provided competitive fits to the SPARC database. To further probe the geometry of the halo one needs out-of-plane observables. Stellar streams, poetically analogous to airplane contrails, but caused by tidal dispersion of massive substructures such as satellite dwarf galaxies, would… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.07402v2-abstract-full').style.display = 'inline'; document.getElementById('2307.07402v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.07402v2-abstract-full" style="display: none;"> Flat rotation curves v(r) are naturally explained by elongated (prolate) Dark Matter (DM) distributions, and we have provided competitive fits to the SPARC database. To further probe the geometry of the halo one needs out-of-plane observables. Stellar streams, poetically analogous to airplane contrails, but caused by tidal dispersion of massive substructures such as satellite dwarf galaxies, would lie on a plane should the DM-halo gravitational field be spherically symmetric. We aim at establishing stellar stream torsion, a local observable that measures the deviation from planarity in differential curve geometry. We perform small-scale simulations of tidally distorted star clusters to check that indeed a central force center produces negligible torsion. Turning to observational data, we identify among the known streams those that are at largest distance from the galactic center and likely not affected by the Magellanic clouds, as most promising for the study, and by means of polynomial fits we extract their differential torsion. We find that the torsion of the few known streams that should be sensitive to most of the Milky Way's DM Halo is much larger than expected for a central spherical bulb alone. This is consistent with non-sphericity of the halo. Future studies of stellar stream torsion with larger samples and further out of the galactic plane should be able to extract the ellipticity of the halo to see whether it is just a slight distortion of a spherical shape or rather ressembles a more elongated cigar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.07402v2-abstract-full').style.display = 'none'; document.getElementById('2307.07402v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A46 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.05176">arXiv:2307.05176</a> <span> [<a href="https://arxiv.org/pdf/2307.05176">pdf</a>, <a href="https://arxiv.org/format/2307.05176">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Measuring the Sterile Neutrino Mass in Spallation Source and Direct Detection Experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alonso-Gonz%C3%A1lez%2C+D">David Alonso-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Amaral%2C+D+W+P">Dorian W. P. Amaral</a>, <a href="/search/astro-ph?searchtype=author&query=Bariego-Quintana%2C+A">Adriana Bariego-Quintana</a>, <a href="/search/astro-ph?searchtype=author&query=Cerdeno%2C+D">David Cerdeno</a>, <a href="/search/astro-ph?searchtype=author&query=Rios%2C+M+d+l">Mart铆n de los Rios</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.05176v2-abstract-short" style="display: inline;"> We explore the complementarity of direct detection (DD) and spallation source (SS) experiments for the study of sterile neutrino physics. We focus on the sterile baryonic neutrino model: an extension of the Standard Model that introduces a massive sterile neutrino with couplings to the quark sector via a new gauge boson. In this scenario, the inelastic scattering of an active neutrino with the tar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.05176v2-abstract-full').style.display = 'inline'; document.getElementById('2307.05176v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.05176v2-abstract-full" style="display: none;"> We explore the complementarity of direct detection (DD) and spallation source (SS) experiments for the study of sterile neutrino physics. We focus on the sterile baryonic neutrino model: an extension of the Standard Model that introduces a massive sterile neutrino with couplings to the quark sector via a new gauge boson. In this scenario, the inelastic scattering of an active neutrino with the target material in both DD and SS experiments gives rise to a characteristic nuclear recoil energy spectrum that can allow for the reconstruction of the neutrino mass in the event of a positive detection. We first derive new bounds on this model based on the data from the COHERENT collaboration on CsI and LAr targets, which we find do not yet probe new areas of the parameter space. We then assess how well future SS experiments will be able to measure the sterile neutrino mass and mixings, showing that masses in the range 15-50 MeV can be reconstructed. We show that there is a degeneracy in the measurement of the sterile neutrino mixing that substantially affects the reconstruction of parameters for masses of the order of 40 MeV. Thanks to their lower energy threshold and sensitivity to the solar tau neutrino flux, DD experiments allow us to partially lift the degeneracy in the sterile neutrino mixings and considerably improve its mass reconstruction down to 9 MeV. Our results demonstrate the excellent complementarity between DD and SS experiments in measuring the sterile neutrino mass and highlight the power of DD experiments in searching for new physics in the neutrino sector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.05176v2-abstract-full').style.display = 'none'; document.getElementById('2307.05176v2-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 10 figures. Minor changes</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> IFT-UAM/CSIC-23-89 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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