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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <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=Albert%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Albert%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Albert%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </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/2411.19078">arXiv:2411.19078</a> <span> [<a href="https://arxiv.org/pdf/2411.19078">pdf</a>, <a href="https://arxiv.org/format/2411.19078">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> </div> </div> <p class="title is-5 mathjax"> Search for non-standard neutrino interactions with the first six detection units of KM3NeT/ORCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alhebsi%2C+A+R">A. R. Alhebsi</a>, <a href="/search/hep-ex?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/hep-ex?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/hep-ex?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/hep-ex?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/hep-ex?searchtype=author&query=Bennani%2C+M">M. Bennani</a>, <a href="/search/hep-ex?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a> , et al. (239 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="2411.19078v1-abstract-short" style="display: inline;"> KM3NeT/ORCA is an underwater neutrino telescope under construction in the Mediterranean Sea. Its primary scientific goal is to measure the atmospheric neutrino oscillation parameters and to determine the neutrino mass ordering. ORCA can constrain the oscillation parameters $螖m^{2}_{31}$ and $胃_{23}$ by reconstructing the arrival direction and energy of multi-GeV neutrinos crossing the Earth. Searc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.19078v1-abstract-full').style.display = 'inline'; document.getElementById('2411.19078v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.19078v1-abstract-full" style="display: none;"> KM3NeT/ORCA is an underwater neutrino telescope under construction in the Mediterranean Sea. Its primary scientific goal is to measure the atmospheric neutrino oscillation parameters and to determine the neutrino mass ordering. ORCA can constrain the oscillation parameters $螖m^{2}_{31}$ and $胃_{23}$ by reconstructing the arrival direction and energy of multi-GeV neutrinos crossing the Earth. Searches for deviations from the Standard Model of particle physics in the forward scattering of neutrinos inside Earth matter, produced by Non-Standard Interactions, can be conducted by investigating distortions of the standard oscillation pattern of neutrinos of all flavours. This work reports on the results of the search for non-standard neutrino interactions using the first six detection units of ORCA and 433 kton-years of exposure. No significant deviation from standard interactions was found in a sample of 5828 events reconstructed in the 1 GeV$-$1 TeV energy range. The flavour structure of the non-standard coupling was constrained at 90\% confidence level to be $|\varepsilon_{渭蟿} | \leq 5.4 \times 10^{-3}$, $|\varepsilon_{e蟿} | \leq 7.4 \times 10^{-2}$, $|\varepsilon_{e渭} | \leq 5.6 \times 10^{-2}$ and $-0.015 \leq \varepsilon_{蟿蟿} - \varepsilon_{渭渭} \leq 0.017$. The results are comparable to the current most stringent limits placed on the parameters by other experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.19078v1-abstract-full').style.display = 'none'; document.getElementById('2411.19078v1-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> 28 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/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alhebsi%2C+A+R">A. R. Alhebsi</a>, <a href="/search/hep-ex?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/hep-ex?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/hep-ex?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/hep-ex?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/hep-ex?searchtype=author&query=Bennani%2C+M">M. Bennani</a>, <a href="/search/hep-ex?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a>, <a href="/search/hep-ex?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/2410.01388">arXiv:2410.01388</a> <span> [<a href="https://arxiv.org/pdf/2410.01388">pdf</a>, <a href="https://arxiv.org/format/2410.01388">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> </div> </div> <p class="title is-5 mathjax"> Search for quantum decoherence in neutrino oscillations with six detection units of KM3NeT/ORCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alhebsi%2C+A+R">A. R. Alhebsi</a>, <a href="/search/hep-ex?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/hep-ex?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/hep-ex?searchtype=author&query=Bardacova%2C+Z">Z. Bardacova</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/hep-ex?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/hep-ex?searchtype=author&query=Bennani%2C+M">M. Bennani</a>, <a href="/search/hep-ex?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a> , et al. (237 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="2410.01388v2-abstract-short" style="display: inline;"> Neutrinos described as an open quantum system may interact with the environment which introduces stochastic perturbations to their quantum phase. This mechanism leads to a loss of coherence along the propagation of the neutrino $-$ a phenomenon commonly referred to as decoherence $-$ and ultimately, to a modification of the oscillation probabilities. Fluctuations in space-time, as envisaged by var… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01388v2-abstract-full').style.display = 'inline'; document.getElementById('2410.01388v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.01388v2-abstract-full" style="display: none;"> Neutrinos described as an open quantum system may interact with the environment which introduces stochastic perturbations to their quantum phase. This mechanism leads to a loss of coherence along the propagation of the neutrino $-$ a phenomenon commonly referred to as decoherence $-$ and ultimately, to a modification of the oscillation probabilities. Fluctuations in space-time, as envisaged by various theories of quantum gravity, are a potential candidate for a decoherence-inducing environment. Consequently, the search for decoherence provides a rare opportunity to investigate quantum gravitational effects which are usually beyond the reach of current experiments. In this work, quantum decoherence effects are searched for in neutrino data collected by the KM3NeT/ORCA detector from January 2020 to November 2021. The analysis focuses on atmospheric neutrinos within the energy range of a few GeV to $100\,\mathrm{GeV}$. Adopting the open quantum system framework, decoherence is described in a phenomenological manner with the strength of the effect given by the parameters $螕_{21}$ and $螕_{31}$. Following previous studies, a dependence of the type $螕_{ij} \propto (E/E_0)^n$ on the neutrino energy is assumed and the cases $n = -2,-1$ are explored. No significant deviation with respect to the standard oscillation hypothesis is observed. Therefore, $90\,\%$ CL upper limits are estimated as $螕_{21} < 4.6\cdot 10^{-21}\,$GeV and $螕_{31} < 8.4\cdot 10^{-21}\,$GeV for $n = -2$, and $螕_{21} < 1.9\cdot 10^{-22}\,$GeV and $螕_{31} < 2.7\cdot 10^{-22}\,$GeV for $n = -1$, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01388v2-abstract-full').style.display = 'none'; document.getElementById('2410.01388v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">17 pages, 5 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/2408.07015">arXiv:2408.07015</a> <span> [<a href="https://arxiv.org/pdf/2408.07015">pdf</a>, <a href="https://arxiv.org/format/2408.07015">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> </div> </div> <p class="title is-5 mathjax"> Measurement of neutrino oscillation parameters with the first six detection units of KM3NeT/ORCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KM3NeT+Collaboration"> KM3NeT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alhebsi%2C+A+R">A. R. Alhebsi</a>, <a href="/search/hep-ex?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Aphecetche%2C+L">L. Aphecetche</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Atmani%2C+H">H. Atmani</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/hep-ex?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/hep-ex?searchtype=author&query=Barda%C4%8Dov%C3%A1%2C+Z">Z. Barda膷ov谩</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Bariego-Quintana%2C+A">A. Bariego-Quintana</a>, <a href="/search/hep-ex?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Benhassi%2C+M">M. Benhassi</a>, <a href="/search/hep-ex?searchtype=author&query=Bennani%2C+M">M. Bennani</a>, <a href="/search/hep-ex?searchtype=author&query=Benoit%2C+D+M">D. M. Benoit</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="2408.07015v2-abstract-short" style="display: inline;"> KM3NeT/ORCA is a water Cherenkov neutrino detector under construction and anchored at the bottom of the Mediterranean Sea. The detector is designed to study oscillations of atmospheric neutrinos and determine the neutrino mass ordering. This paper focuses on an initial configuration of ORCA, referred to as ORCA6, which comprises six out of the foreseen 115 detection units of photo-sensors. A high-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07015v2-abstract-full').style.display = 'inline'; document.getElementById('2408.07015v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.07015v2-abstract-full" style="display: none;"> KM3NeT/ORCA is a water Cherenkov neutrino detector under construction and anchored at the bottom of the Mediterranean Sea. The detector is designed to study oscillations of atmospheric neutrinos and determine the neutrino mass ordering. This paper focuses on an initial configuration of ORCA, referred to as ORCA6, which comprises six out of the foreseen 115 detection units of photo-sensors. A high-purity neutrino sample was extracted, corresponding to an exposure of 433 kton-years. The sample of 5828 neutrino candidates is analysed following a binned log-likelihood method in the reconstructed energy and cosine of the zenith angle. The atmospheric oscillation parameters are measured to be $\sin^2胃_{23}= 0.51^{+0.04}_{-0.05}$, and $ 螖m^2_{31} = 2.18^{+0.25}_{-0.35}\times 10^{-3}~\mathrm{eV^2} \cup \{-2.25,-1.76\}\times 10^{-3}~\mathrm{eV^2}$ at 68\% CL. The inverted neutrino mass ordering hypothesis is disfavoured with a p-value of 0.25. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07015v2-abstract-full').style.display = 'none'; document.getElementById('2408.07015v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 12 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/2407.08849">arXiv:2407.08849</a> <span> [<a href="https://arxiv.org/pdf/2407.08849">pdf</a>, <a href="https://arxiv.org/format/2407.08849">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> <p class="title is-5 mathjax"> TeV Analysis of a Source Rich Region with HAWC Observatory: Is HESS J1809-193 a Potential Hadronic PeVatron? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/hep-ex?searchtype=author&query=Alvarez%2C+C">C. Alvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Arteaga-Vel%C3%A1zquez%2C+J+C">J. C. Arteaga-Vel谩zquez</a>, <a href="/search/hep-ex?searchtype=author&query=Rojas%2C+D+A">D. Avila Rojas</a>, <a href="/search/hep-ex?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/hep-ex?searchtype=author&query=Belmont-Moreno%2C+E">E. Belmont-Moreno</a>, <a href="/search/hep-ex?searchtype=author&query=Bernal%2C+A">A. Bernal</a>, <a href="/search/hep-ex?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/hep-ex?searchtype=author&query=Caballero-Mora%2C+K+S">K. S. Caballero-Mora</a>, <a href="/search/hep-ex?searchtype=author&query=Capistr%C3%A1n%2C+T">T. Capistr谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Carrami%C3%B1ana%2C+A">A. Carrami帽ana</a>, <a href="/search/hep-ex?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/hep-ex?searchtype=author&query=Cotzomi%2C+J">J. Cotzomi</a>, <a href="/search/hep-ex?searchtype=author&query=De+la+Fuente%2C+E">E. De la Fuente</a>, <a href="/search/hep-ex?searchtype=author&query=Depaoli%2C+D">D. Depaoli</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Lalla%2C+N">N. Di Lalla</a>, <a href="/search/hep-ex?searchtype=author&query=Hernandez%2C+R+D">R. Diaz Hernandez</a>, <a href="/search/hep-ex?searchtype=author&query=Dingus%2C+B+L">B. L. Dingus</a>, <a href="/search/hep-ex?searchtype=author&query=DuVernois%2C+M+A">M. A. DuVernois</a>, <a href="/search/hep-ex?searchtype=author&query=Espinoza%2C+C">C. Espinoza</a>, <a href="/search/hep-ex?searchtype=author&query=Fan%2C+K+L">K. L. Fan</a>, <a href="/search/hep-ex?searchtype=author&query=Fang%2C+K">K. Fang</a>, <a href="/search/hep-ex?searchtype=author&query=Fick%2C+B">B. Fick</a>, <a href="/search/hep-ex?searchtype=author&query=Fraija%2C+N">N. Fraija</a> , et al. (57 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="2407.08849v1-abstract-short" style="display: inline;"> HESS J1809-193 is an unidentified TeV source, first detected by the High Energy Stereoscopic System (H.E.S.S.) Collaboration. The emission originates in a source-rich region that includes several Supernova Remnants (SNR) and Pulsars (PSR) including SNR G11.1+0.1, SNR G11.0-0.0, and the young radio pulsar J1809-1917. Originally classified as a pulsar wind nebula (PWN) candidate, recent studies show… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.08849v1-abstract-full').style.display = 'inline'; document.getElementById('2407.08849v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.08849v1-abstract-full" style="display: none;"> HESS J1809-193 is an unidentified TeV source, first detected by the High Energy Stereoscopic System (H.E.S.S.) Collaboration. The emission originates in a source-rich region that includes several Supernova Remnants (SNR) and Pulsars (PSR) including SNR G11.1+0.1, SNR G11.0-0.0, and the young radio pulsar J1809-1917. Originally classified as a pulsar wind nebula (PWN) candidate, recent studies show the peak of the TeV region overlapping with a system of molecular clouds. This resulted in the revision of the original leptonic scenario to look for alternate hadronic scenarios. Marked as a potential PeVatron candidate, this region has been studied extensively by H.E.S.S. due to its emission extending up-to several tens of TeV. In this work, we use 2398 days of data from the High Altitude Water Cherenkov (HAWC) observatory to carry out a systematic source search for the HESS J1809-193 region. We were able to resolve emission detected as an extended component (modelled as a Symmetric Gaussian with a 1 $蟽$ radius of 0.21 $^\circ$) with no clear cutoff at high energies and emitting photons up-to 210 TeV. We model the multi-wavelength observations for the region HESS J1809-193 using a time-dependent leptonic model and a lepto-hadronic model. Our model indicates that both scenarios could explain the observed data within the region of HESS J1809-193. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.08849v1-abstract-full').style.display = 'none'; document.getElementById('2407.08849v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.02717">arXiv:2302.02717</a> <span> [<a href="https://arxiv.org/pdf/2302.02717">pdf</a>, <a href="https://arxiv.org/format/2302.02717">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> </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/10.1007/JHEP04(2023)090">10.1007/JHEP04(2023)090 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing invisible neutrino decay with KM3NeT-ORCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KM3NeT+Collaboration"> KM3NeT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/hep-ex?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/hep-ex?searchtype=author&query=Bailly-Salins%2C+L">L. Bailly-Salins</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/hep-ex?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a>, <a href="/search/hep-ex?searchtype=author&query=Cabo%2C+M+B">M. Bou Cabo</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="2302.02717v3-abstract-short" style="display: inline;"> In the era of precision measurements of the neutrino oscillation parameters, upcoming neutrino experiments will also be sensitive to physics beyond the Standard Model. KM3NeT/ORCA is a neutrino detector optimised for measuring atmospheric neutrinos from a few GeV to around 100 GeV. In this paper, the sensitivity of the KM3NeT/ORCA detector to neutrino decay has been explored. A three-flavour neutr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02717v3-abstract-full').style.display = 'inline'; document.getElementById('2302.02717v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.02717v3-abstract-full" style="display: none;"> In the era of precision measurements of the neutrino oscillation parameters, upcoming neutrino experiments will also be sensitive to physics beyond the Standard Model. KM3NeT/ORCA is a neutrino detector optimised for measuring atmospheric neutrinos from a few GeV to around 100 GeV. In this paper, the sensitivity of the KM3NeT/ORCA detector to neutrino decay has been explored. A three-flavour neutrino oscillation scenario, where the third neutrino mass state $谓_3$ decays into an invisible state, e.g. a sterile neutrino, is considered. We find that KM3NeT/ORCA would be sensitive to invisible neutrino decays with $1/伪_3=蟿_3/m_3 < 180$~$\mathrm{ps/eV}$ at $90\%$ confidence level, assuming true normal ordering. Finally, the impact of neutrino decay on the precision of KM3NeT/ORCA measurements for $胃_{23}$, $螖m^2_{31}$ and mass ordering have been studied. No significant effect of neutrino decay on the sensitivity to these measurements has been found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02717v3-abstract-full').style.display = 'none'; document.getElementById('2302.02717v3-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">27 pages, 14 figures, bibliography updated, typos corrected</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.00815">arXiv:2212.00815</a> <span> [<a href="https://arxiv.org/pdf/2212.00815">pdf</a>, <a href="https://arxiv.org/format/2212.00815">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="Solar and Stellar Astrophysics">astro-ph.SR</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/PhysRevLett.131.051201">10.1103/PhysRevLett.131.051201 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TeV Sun Rises: Discovery of Gamma rays from the Quiescent Sun with HAWC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/hep-ex?searchtype=author&query=Alvarez%2C+C">C. Alvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Arteaga-Velazquez%2C+J+C">J. C. Arteaga-Velazquez</a>, <a href="/search/hep-ex?searchtype=author&query=Rojas%2C+D+A">D. Avila Rojas</a>, <a href="/search/hep-ex?searchtype=author&query=Solares%2C+H+A+A">H. A. Ayala Solares</a>, <a href="/search/hep-ex?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/hep-ex?searchtype=author&query=Belmont-Moreno%2C+E">E. Belmont-Moreno</a>, <a href="/search/hep-ex?searchtype=author&query=Brisbois%2C+C">C. Brisbois</a>, <a href="/search/hep-ex?searchtype=author&query=Caballero-Mora%2C+K+S">K. S. Caballero-Mora</a>, <a href="/search/hep-ex?searchtype=author&query=Capistran%2C+T">T. Capistran</a>, <a href="/search/hep-ex?searchtype=author&query=Carraminana%2C+A">A. Carraminana</a>, <a href="/search/hep-ex?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/hep-ex?searchtype=author&query=Chaparro-Amaro%2C+O">O. Chaparro-Amaro</a>, <a href="/search/hep-ex?searchtype=author&query=Cotti%2C+U">U. Cotti</a>, <a href="/search/hep-ex?searchtype=author&query=Cotzomi%2C+J">J. Cotzomi</a>, <a href="/search/hep-ex?searchtype=author&query=de+Leon%2C+S+C">S. Coutino de Leon</a>, <a href="/search/hep-ex?searchtype=author&query=De+la+Fuente%2C+E">E. De la Fuente</a>, <a href="/search/hep-ex?searchtype=author&query=Hernandez%2C+R+D">R. Diaz Hernandez</a>, <a href="/search/hep-ex?searchtype=author&query=Dingus%2C+B+L">B. L. Dingus</a>, <a href="/search/hep-ex?searchtype=author&query=DuVernois%2C+M+A">M. A. DuVernois</a>, <a href="/search/hep-ex?searchtype=author&query=Durocher%2C+M">M. Durocher</a>, <a href="/search/hep-ex?searchtype=author&query=Diaz-Velez%2C+J+C">J. C. Diaz-Velez</a>, <a href="/search/hep-ex?searchtype=author&query=Ellsworth%2C+R+W">R. W. Ellsworth</a>, <a href="/search/hep-ex?searchtype=author&query=Engel%2C+K">K. Engel</a> , et al. (67 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="2212.00815v2-abstract-short" style="display: inline;"> We report the first detection of a TeV gamma-ray flux from the solar disk (6.3$蟽$), based on 6.1 years of data from the High Altitude Water Cherenkov (HAWC) observatory. The 0.5--2.6 TeV spectrum is well fit by a power law, dN/dE = $A (E/1 \text{ TeV})^{-纬}$, with $A = (1.6 \pm 0.3) \times 10^{-12}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ and $纬= -3.62 \pm 0.14$. The flux shows a strong indication of antico… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00815v2-abstract-full').style.display = 'inline'; document.getElementById('2212.00815v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.00815v2-abstract-full" style="display: none;"> We report the first detection of a TeV gamma-ray flux from the solar disk (6.3$蟽$), based on 6.1 years of data from the High Altitude Water Cherenkov (HAWC) observatory. The 0.5--2.6 TeV spectrum is well fit by a power law, dN/dE = $A (E/1 \text{ TeV})^{-纬}$, with $A = (1.6 \pm 0.3) \times 10^{-12}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ and $纬= -3.62 \pm 0.14$. The flux shows a strong indication of anticorrelation with solar activity. These results extend the bright, hard GeV emission from the disk observed with Fermi-LAT, seemingly due to hadronic Galactic cosmic rays showering on nuclei in the solar atmosphere. However, current theoretical models are unable to explain the details of how solar magnetic fields shape these interactions. HAWC's TeV detection thus deepens the mysteries of the solar-disk emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00815v2-abstract-full').style.display = 'none'; document.getElementById('2212.00815v2-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">15 pages, 8 figures including supplementary material. Accepted for publication in Physical Review Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 131, 051201, 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/2209.13128">arXiv:2209.13128</a> <span> [<a href="https://arxiv.org/pdf/2209.13128">pdf</a>, <a href="https://arxiv.org/format/2209.13128">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Report of the Topical Group on Physics Beyond the Standard Model at Energy Frontier for Snowmass 2021 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Bose%2C+T">Tulika Bose</a>, <a href="/search/hep-ex?searchtype=author&query=Boveia%2C+A">Antonio Boveia</a>, <a href="/search/hep-ex?searchtype=author&query=Doglioni%2C+C">Caterina Doglioni</a>, <a href="/search/hep-ex?searchtype=author&query=Griso%2C+S+P">Simone Pagan Griso</a>, <a href="/search/hep-ex?searchtype=author&query=Hirschauer%2C+J">James Hirschauer</a>, <a href="/search/hep-ex?searchtype=author&query=Lipeles%2C+E">Elliot Lipeles</a>, <a href="/search/hep-ex?searchtype=author&query=Liu%2C+Z">Zhen Liu</a>, <a href="/search/hep-ex?searchtype=author&query=Shah%2C+N+R">Nausheen R. Shah</a>, <a href="/search/hep-ex?searchtype=author&query=Wang%2C+L">Lian-Tao Wang</a>, <a href="/search/hep-ex?searchtype=author&query=Agashe%2C+K">Kaustubh Agashe</a>, <a href="/search/hep-ex?searchtype=author&query=Alimena%2C+J">Juliette Alimena</a>, <a href="/search/hep-ex?searchtype=author&query=Baum%2C+S">Sebastian Baum</a>, <a href="/search/hep-ex?searchtype=author&query=Berkat%2C+M">Mohamed Berkat</a>, <a href="/search/hep-ex?searchtype=author&query=Black%2C+K">Kevin Black</a>, <a href="/search/hep-ex?searchtype=author&query=Gardner%2C+G">Gwen Gardner</a>, <a href="/search/hep-ex?searchtype=author&query=Gherghetta%2C+T">Tony Gherghetta</a>, <a href="/search/hep-ex?searchtype=author&query=Greaves%2C+J">Josh Greaves</a>, <a href="/search/hep-ex?searchtype=author&query=Haehn%2C+M">Maxx Haehn</a>, <a href="/search/hep-ex?searchtype=author&query=Harris%2C+P+C">Phil C. Harris</a>, <a href="/search/hep-ex?searchtype=author&query=Harris%2C+R">Robert Harris</a>, <a href="/search/hep-ex?searchtype=author&query=Hogan%2C+J">Julie Hogan</a>, <a href="/search/hep-ex?searchtype=author&query=Jayawardana%2C+S">Suneth Jayawardana</a>, <a href="/search/hep-ex?searchtype=author&query=Kahn%2C+A">Abraham Kahn</a>, <a href="/search/hep-ex?searchtype=author&query=Kalinowski%2C+J">Jan Kalinowski</a>, <a href="/search/hep-ex?searchtype=author&query=Knapen%2C+S">Simon Knapen</a> , et al. (297 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="2209.13128v2-abstract-short" style="display: inline;"> This is the Snowmass2021 Energy Frontier (EF) Beyond the Standard Model (BSM) report. It combines the EF topical group reports of EF08 (Model-specific explorations), EF09 (More general explorations), and EF10 (Dark Matter at Colliders). The report includes a general introduction to BSM motivations and the comparative prospects for proposed future experiments for a broad range of potential BSM mode… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13128v2-abstract-full').style.display = 'inline'; document.getElementById('2209.13128v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.13128v2-abstract-full" style="display: none;"> This is the Snowmass2021 Energy Frontier (EF) Beyond the Standard Model (BSM) report. It combines the EF topical group reports of EF08 (Model-specific explorations), EF09 (More general explorations), and EF10 (Dark Matter at Colliders). The report includes a general introduction to BSM motivations and the comparative prospects for proposed future experiments for a broad range of potential BSM models and signatures, including compositeness, SUSY, leptoquarks, more general new bosons and fermions, long-lived particles, dark matter, charged-lepton flavor violation, and anomaly detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13128v2-abstract-full').style.display = 'none'; document.getElementById('2209.13128v2-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">108 pages + 38 pages references and appendix, 37 figures, Report of the Topical Group on Beyond the Standard Model Physics at Energy Frontier for Snowmass 2021. The first nine authors are the Conveners, with Contributions from the other authors</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.08215">arXiv:2209.08215</a> <span> [<a href="https://arxiv.org/pdf/2209.08215">pdf</a>, <a href="https://arxiv.org/format/2209.08215">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Report of the Topical Group on Cosmic Probes of Dark Matter for Snowmass 2021 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Drlica-Wagner%2C+A">Alex Drlica-Wagner</a>, <a href="/search/hep-ex?searchtype=author&query=Prescod-Weinstein%2C+C">Chanda Prescod-Weinstein</a>, <a href="/search/hep-ex?searchtype=author&query=Yu%2C+H">Hai-Bo Yu</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">Andrea Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Amin%2C+M">Mustafa Amin</a>, <a href="/search/hep-ex?searchtype=author&query=Banerjee%2C+A">Arka Banerjee</a>, <a href="/search/hep-ex?searchtype=author&query=Baryakhtar%2C+M">Masha Baryakhtar</a>, <a href="/search/hep-ex?searchtype=author&query=Bechtol%2C+K">Keith Bechtol</a>, <a href="/search/hep-ex?searchtype=author&query=Bird%2C+S">Simeon Bird</a>, <a href="/search/hep-ex?searchtype=author&query=Birrer%2C+S">Simon Birrer</a>, <a href="/search/hep-ex?searchtype=author&query=Bringmann%2C+T">Torsten Bringmann</a>, <a href="/search/hep-ex?searchtype=author&query=Caputo%2C+R">Regina Caputo</a>, <a href="/search/hep-ex?searchtype=author&query=Chakrabarti%2C+S">Sukanya Chakrabarti</a>, <a href="/search/hep-ex?searchtype=author&query=Chen%2C+T+Y">Thomas Y. Chen</a>, <a href="/search/hep-ex?searchtype=author&query=Croon%2C+D">Djuna Croon</a>, <a href="/search/hep-ex?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/hep-ex?searchtype=author&query=Dawson%2C+W+A">William A. Dawson</a>, <a href="/search/hep-ex?searchtype=author&query=Dvorkin%2C+C">Cora Dvorkin</a>, <a href="/search/hep-ex?searchtype=author&query=Gluscevic%2C+V">Vera Gluscevic</a>, <a href="/search/hep-ex?searchtype=author&query=Gilman%2C+D">Daniel Gilman</a>, <a href="/search/hep-ex?searchtype=author&query=Grin%2C+D">Daniel Grin</a>, <a href="/search/hep-ex?searchtype=author&query=Hlo%C5%BEek%2C+R">Ren茅e Hlo啪ek</a>, <a href="/search/hep-ex?searchtype=author&query=Leane%2C+R+K">Rebecca K. Leane</a>, <a href="/search/hep-ex?searchtype=author&query=Li%2C+T+S">Ting S. Li</a>, <a href="/search/hep-ex?searchtype=author&query=Mao%2C+Y">Yao-Yuan Mao</a> , et al. (15 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="2209.08215v3-abstract-short" style="display: inline;"> Cosmological and astrophysical observations currently provide the only robust, positive evidence for dark matter. Cosmic probes of dark matter, which seek to determine the fundamental properties of dark matter through observations of the cosmos, have emerged as a promising means to reveal the nature of dark matter. This report summarizes the current status and future potential of cosmic probes to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.08215v3-abstract-full').style.display = 'inline'; document.getElementById('2209.08215v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.08215v3-abstract-full" style="display: none;"> Cosmological and astrophysical observations currently provide the only robust, positive evidence for dark matter. Cosmic probes of dark matter, which seek to determine the fundamental properties of dark matter through observations of the cosmos, have emerged as a promising means to reveal the nature of dark matter. This report summarizes the current status and future potential of cosmic probes to inform our understanding of the fundamental nature of dark matter in the coming decade. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.08215v3-abstract-full').style.display = 'none'; document.getElementById('2209.08215v3-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 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">Report of the CF3 Topical Group for Snowmass 2021; 35 pages, 10 figures, many references. V3 updates Fig 3-2 and the author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.12035">arXiv:2203.12035</a> <span> [<a href="https://arxiv.org/pdf/2203.12035">pdf</a>, <a href="https://arxiv.org/format/2203.12035">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Displaying dark matter constraints from colliders with varying simplified model parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">Andreas Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Boveia%2C+A">Antonio Boveia</a>, <a href="/search/hep-ex?searchtype=author&query=Brandt%2C+O">Oleg Brandt</a>, <a href="/search/hep-ex?searchtype=author&query=Corrigan%2C+E">Eric Corrigan</a>, <a href="/search/hep-ex?searchtype=author&query=Demiragli%2C+Z">Zeynep Demiragli</a>, <a href="/search/hep-ex?searchtype=author&query=Doglioni%2C+C">Caterina Doglioni</a>, <a href="/search/hep-ex?searchtype=author&query=Dreyer%2C+E">Etienne Dreyer</a>, <a href="/search/hep-ex?searchtype=author&query=Gao%2C+B">Boyu Gao</a>, <a href="/search/hep-ex?searchtype=author&query=Greaves%2C+J">Josh Greaves</a>, <a href="/search/hep-ex?searchtype=author&query=Haisch%2C+U">Ulrich Haisch</a>, <a href="/search/hep-ex?searchtype=author&query=Harris%2C+P">Philip Harris</a>, <a href="/search/hep-ex?searchtype=author&query=Landsberg%2C+G">Greg Landsberg</a>, <a href="/search/hep-ex?searchtype=author&query=Moreno%2C+A">Alexander Moreno</a>, <a href="/search/hep-ex?searchtype=author&query=Pachal%2C+K">Katherine Pachal</a>, <a href="/search/hep-ex?searchtype=author&query=Pani%2C+P">Priscilla Pani</a>, <a href="/search/hep-ex?searchtype=author&query=Piazza%2C+F">Federica Piazza</a>, <a href="/search/hep-ex?searchtype=author&query=Tait%2C+T+M+P">Tim M. P. Tait</a>, <a href="/search/hep-ex?searchtype=author&query=Yu%2C+D">David Yu</a>, <a href="/search/hep-ex?searchtype=author&query=Yu%2C+F">Felix Yu</a>, <a href="/search/hep-ex?searchtype=author&query=Wang%2C+L">Lian-Tao Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.12035v1-abstract-short" style="display: inline;"> The search for dark matter is one of the main science drivers of the particle and astroparticle physics communities. Determining the nature of dark matter will require a broad approach, with a range of experiments pursuing different experimental hypotheses. Within this search program, collider experiments provide insights on dark matter which are complementary to direct/indirect detection experime… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12035v1-abstract-full').style.display = 'inline'; document.getElementById('2203.12035v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.12035v1-abstract-full" style="display: none;"> The search for dark matter is one of the main science drivers of the particle and astroparticle physics communities. Determining the nature of dark matter will require a broad approach, with a range of experiments pursuing different experimental hypotheses. Within this search program, collider experiments provide insights on dark matter which are complementary to direct/indirect detection experiments and to astrophysical evidence. To compare results from a wide variety of experiments, a common theoretical framework is required. The ATLAS and CMS experiments have adopted a set of simplified models which introduce two new particles, a dark matter particle and a mediator, and whose interaction strengths are set by the couplings of the mediator. So far, the presentation of LHC and future hadron collider results has focused on four benchmark scenarios with specific coupling values within these simplified models. In this work, we describe ways to extend those four benchmark scenarios to arbitrary couplings, and release the corresponding code for use in further studies. This will allow for more straightforward comparison of collider searches to accelerator experiments that are sensitive to smaller couplings, such as those for the US Community Study on the Future of Particle Physics (Snowmass 2021), and will give a more complete picture of the coupling dependence of dark matter collider searches when compared to direct and indirect detection searches. By using semi-analytical methods to rescale collider limits, we drastically reduce the computing resources needed relative to traditional approaches based on the generation of additional simulated signal samples. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12035v1-abstract-full').style.display = 'none'; document.getElementById('2203.12035v1-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> 22 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/2203.07535">arXiv:2203.07535</a> <span> [<a href="https://arxiv.org/pdf/2203.07535">pdf</a>, <a href="https://arxiv.org/format/2203.07535">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> </div> </div> <p class="title is-5 mathjax"> Strange quark as a probe for new physics in the Higgs sector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">Alexander Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Basso%2C+M+J">Matthew J. Basso</a>, <a href="/search/hep-ex?searchtype=author&query=Bright-Thonney%2C+S+K">Samuel K. Bright-Thonney</a>, <a href="/search/hep-ex?searchtype=author&query=Cairo%2C+V+M+M">Valentina M. M. Cairo</a>, <a href="/search/hep-ex?searchtype=author&query=Damerell%2C+C">Chris Damerell</a>, <a href="/search/hep-ex?searchtype=author&query=Egana-Ugrinovic%2C+D">Daniel Egana-Ugrinovic</a>, <a href="/search/hep-ex?searchtype=author&query=Einhaus%2C+U">Ulrich Einhaus</a>, <a href="/search/hep-ex?searchtype=author&query=Heintz%2C+U">Ulrich Heintz</a>, <a href="/search/hep-ex?searchtype=author&query=Homiller%2C+S">Samuel Homiller</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+S">Shin-ichi Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Luo%2C+J">Jingyu Luo</a>, <a href="/search/hep-ex?searchtype=author&query=Mantel%2C+C">Chester Mantel</a>, <a href="/search/hep-ex?searchtype=author&query=Meade%2C+P">Patrick Meade</a>, <a href="/search/hep-ex?searchtype=author&query=Monroy%2C+J">Jose Monroy</a>, <a href="/search/hep-ex?searchtype=author&query=Narain%2C+M">Meenakshi Narain</a>, <a href="/search/hep-ex?searchtype=author&query=Orr%2C+R+S">Robert S. Orr</a>, <a href="/search/hep-ex?searchtype=author&query=Reichert%2C+J">Joseph Reichert</a>, <a href="/search/hep-ex?searchtype=author&query=Ryd%2C+A">Anders Ryd</a>, <a href="/search/hep-ex?searchtype=author&query=Strube%2C+J">Jan Strube</a>, <a href="/search/hep-ex?searchtype=author&query=Su%2C+D">Dong Su</a>, <a href="/search/hep-ex?searchtype=author&query=Schwartzman%2C+A+G">Ariel G. Schwartzman</a>, <a href="/search/hep-ex?searchtype=author&query=Tanabe%2C+T">Tomohiko Tanabe</a>, <a href="/search/hep-ex?searchtype=author&query=Tian%2C+J">Junping Tian</a>, <a href="/search/hep-ex?searchtype=author&query=Usai%2C+E">Emanuele Usai</a>, <a href="/search/hep-ex?searchtype=author&query=Va%27vra%2C+J">Jerry Va'vra</a> , et al. (3 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="2203.07535v2-abstract-short" style="display: inline;"> This paper describes a novel algorithm for tagging jets originating from the hadronisation of strange quarks (strange-tagging) with the future International Large Detector (ILD) at the International Linear Collider (ILC). It also presents the first application of such a strange-tagger to a Higgs to strange ($h \rightarrow s\bar{s}$) analysis with the $P(e^-,e^+) = (-80\%,+30\%)$ polarisation scena… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07535v2-abstract-full').style.display = 'inline'; document.getElementById('2203.07535v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07535v2-abstract-full" style="display: none;"> This paper describes a novel algorithm for tagging jets originating from the hadronisation of strange quarks (strange-tagging) with the future International Large Detector (ILD) at the International Linear Collider (ILC). It also presents the first application of such a strange-tagger to a Higgs to strange ($h \rightarrow s\bar{s}$) analysis with the $P(e^-,e^+) = (-80\%,+30\%)$ polarisation scenario, corresponding to 900 fb$^{-1}$ of the initial proposed 2000 fb$^{-1}$ of data which will be collected by ILD during its first 10 years of data taking at $\sqrt{s} = 250$ GeV. Upper limits on the Standard Model Higgs-strange coupling strength modifier, $魏_s$, are derived at the 95% confidence level to be 7.14. The paper includes as well a preliminary study of a Ring Imaging Cherenkov (RICH) system capable of discriminating between kaons and pions at high momenta (up to 25 GeV), and thus enhancing strange-tagging performance at future Higgs factory detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07535v2-abstract-full').style.display = 'none'; document.getElementById('2203.07535v2-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">V1: 69 pages; V2: 80 pages, updated figures/numbers, additional appendices</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> Report-no: ILD-PHYS-PROC-2022-001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.14517">arXiv:2112.14517</a> <span> [<a href="https://arxiv.org/pdf/2112.14517">pdf</a>, <a href="https://arxiv.org/format/2112.14517">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> </div> </div> <p class="title is-5 mathjax"> Search for non-standard neutrino interactions with 10 years of ANTARES data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/hep-ex?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nzas%2C+H">H. Br芒nzas</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Caiffi%2C+B">B. Caiffi</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="2112.14517v2-abstract-short" style="display: inline;"> Non-standard interactions of neutrinos arising in many theories beyond the Standard Model can significantly alter matter effects in atmospheric neutrino propagation through the Earth. In this paper, a search for deviations from the prediction of the standard 3-flavour atmospheric neutrino oscillations using the data taken by the ANTARES neutrino telescope is presented. Ten years of atmospheric neu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.14517v2-abstract-full').style.display = 'inline'; document.getElementById('2112.14517v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.14517v2-abstract-full" style="display: none;"> Non-standard interactions of neutrinos arising in many theories beyond the Standard Model can significantly alter matter effects in atmospheric neutrino propagation through the Earth. In this paper, a search for deviations from the prediction of the standard 3-flavour atmospheric neutrino oscillations using the data taken by the ANTARES neutrino telescope is presented. Ten years of atmospheric neutrino data collected from 2007 to 2016, with reconstructed energies in the range from $\sim$16 GeV to $100$ GeV, have been analysed. A log-likelihood ratio test of the dimensionless coefficients $\varepsilon_{渭蟿}$ and $\varepsilon_{蟿蟿} - \varepsilon_{渭渭}$ does not provide clear evidence of deviations from standard interactions. For normal neutrino mass ordering, the combined fit of both coefficients yields a value 1.7$蟽$ away from the null result. However, the 68% and 95% confidence level intervals for $\varepsilon_{渭蟿}$ and $\varepsilon_{蟿蟿} - \varepsilon_{渭渭}$, respectively, contain the null value. Best fit values, one standard deviation errors and bounds at the 90% confidence level for these coefficients are given for both normal and inverted mass orderings. The constraint on $\varepsilon_{渭蟿}$ is among the most stringent to date and it further restrains the strength of possible non-standard interactions in the $渭- 蟿$ sector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.14517v2-abstract-full').style.display = 'none'; document.getElementById('2112.14517v2-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">22 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/2112.01556">arXiv:2112.01556</a> <span> [<a href="https://arxiv.org/pdf/2112.01556">pdf</a>, <a href="https://arxiv.org/format/2112.01556">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 Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/17/04/C04033">10.1088/1748-0221/17/04/C04033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Apollo ATCA Design for the CMS Track Finder and the Pixel Readout at the HL-LHC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Demiragli%2C+Z">Z. Demiragli</a>, <a href="/search/hep-ex?searchtype=author&query=Gastler%2C+D">D. Gastler</a>, <a href="/search/hep-ex?searchtype=author&query=Hahn%2C+K">K. Hahn</a>, <a href="/search/hep-ex?searchtype=author&query=Hazen%2C+E">E. Hazen</a>, <a href="/search/hep-ex?searchtype=author&query=Kotamnives%2C+P">P. Kotamnives</a>, <a href="/search/hep-ex?searchtype=author&query=Noorudhin%2C+S">S. Noorudhin</a>, <a href="/search/hep-ex?searchtype=author&query=Peck%2C+A">A. Peck</a>, <a href="/search/hep-ex?searchtype=author&query=Rohlf%2C+J">J. Rohlf</a>, <a href="/search/hep-ex?searchtype=author&query=Strohman%2C+C">C. Strohman</a>, <a href="/search/hep-ex?searchtype=author&query=Wittich%2C+P">P. Wittich</a>, <a href="/search/hep-ex?searchtype=author&query=Zou%2C+R">R. Zou</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="2112.01556v2-abstract-short" style="display: inline;"> The challenging conditions of the High-Luminosity LHC require tailored hardware designs for the trigger and data acquisition systems. The Apollo platform features a "Service Module" with a powerful system-on-module computer that provides standard ATCA communications and application-specific "Command Module"s with large FPGAs and high-speed optical fiber links. The CMS version of Apollo will be use… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.01556v2-abstract-full').style.display = 'inline'; document.getElementById('2112.01556v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.01556v2-abstract-full" style="display: none;"> The challenging conditions of the High-Luminosity LHC require tailored hardware designs for the trigger and data acquisition systems. The Apollo platform features a "Service Module" with a powerful system-on-module computer that provides standard ATCA communications and application-specific "Command Module"s with large FPGAs and high-speed optical fiber links. The CMS version of Apollo will be used for the track finder and the pixel readout. It features up to two large FPGAs and more than 100 optical links with speeds up to 25\,Gb/s. We study carefully the design and performance of the board by using customized firmware to test power consumption, heat dissipation, and optical link integrity. This paper presents the results of these performance tests, design updates, and future plans. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.01556v2-abstract-full').style.display = 'none'; document.getElementById('2112.01556v2-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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 JINST Proceedings for TWEPP 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.07767">arXiv:2108.07767</a> <span> [<a href="https://arxiv.org/pdf/2108.07767">pdf</a>, <a href="https://arxiv.org/format/2108.07767">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> </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.astropartphys.2021.102670">10.1016/j.astropartphys.2021.102670 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the background for a neutrino search with the HAWC observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=HAWC+Collaboration"> HAWC Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/hep-ex?searchtype=author&query=Alvarez%2C+C">C. Alvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Camacho%2C+J+R+A">J. R. Angeles Camacho</a>, <a href="/search/hep-ex?searchtype=author&query=Arteaga-Vel%C3%A1zquez%2C+J+C">J. C. Arteaga-Vel谩zquez</a>, <a href="/search/hep-ex?searchtype=author&query=Arunbabu%2C+K+P">K. P. Arunbabu</a>, <a href="/search/hep-ex?searchtype=author&query=Belmont-Moreno%2C+E">E. Belmont-Moreno</a>, <a href="/search/hep-ex?searchtype=author&query=Caballero-Mora%2C+K+S">K. S. Caballero-Mora</a>, <a href="/search/hep-ex?searchtype=author&query=Capistr%C3%A1n%2C+T">T. Capistr谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Carrami%C3%B1ana%2C+A">A. Carrami帽ana</a>, <a href="/search/hep-ex?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/hep-ex?searchtype=author&query=Cotti%2C+U">U. Cotti</a>, <a href="/search/hep-ex?searchtype=author&query=Cotzomi%2C+J">J. Cotzomi</a>, <a href="/search/hep-ex?searchtype=author&query=de+Le%C3%B3n%2C+S+C">S. Couti帽o de Le贸n</a>, <a href="/search/hep-ex?searchtype=author&query=De+la+Fuente%2C+E">E. De la Fuente</a>, <a href="/search/hep-ex?searchtype=author&query=Hernandez%2C+R+D">R. Diaz Hernandez</a>, <a href="/search/hep-ex?searchtype=author&query=DuVernois%2C+M+A">M. A. DuVernois</a>, <a href="/search/hep-ex?searchtype=author&query=Durocher%2C+M">M. Durocher</a>, <a href="/search/hep-ex?searchtype=author&query=Espinoza%2C+C">C. Espinoza</a>, <a href="/search/hep-ex?searchtype=author&query=Fan%2C+K+L">K. L. Fan</a>, <a href="/search/hep-ex?searchtype=author&query=Fraija%2C+N">N. Fraija</a>, <a href="/search/hep-ex?searchtype=author&query=Garcia%2C+D">D. Garcia</a>, <a href="/search/hep-ex?searchtype=author&query=Garc%C3%ADa-Gonz%C3%A1lez%2C+J+A">J. A. Garc铆a-Gonz谩lez</a>, <a href="/search/hep-ex?searchtype=author&query=Garfias%2C+F">F. Garfias</a> , et al. (37 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="2108.07767v2-abstract-short" style="display: inline;"> The close location of the HAWC observatory to the largest volcano in Mexico allows to perform a search for neutrino-induced horizontal muon and tau charged leptons. The section of the volcano located at the horizon reaches values of slant depth larger than 8 km of rock, making it an excellent shield for the cosmic ray horizontal background. We report the search method and background suppression te… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.07767v2-abstract-full').style.display = 'inline'; document.getElementById('2108.07767v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.07767v2-abstract-full" style="display: none;"> The close location of the HAWC observatory to the largest volcano in Mexico allows to perform a search for neutrino-induced horizontal muon and tau charged leptons. The section of the volcano located at the horizon reaches values of slant depth larger than 8 km of rock, making it an excellent shield for the cosmic ray horizontal background. We report the search method and background suppression technique developed for the detection of Earth-skimming neutrinos with HAWC, as well as a model that describes the remaining background produced by scattered muons. We show that by increasing the detection energy threshold we could use HAWC to search for neutrino-induced charged leptons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.07767v2-abstract-full').style.display = 'none'; document.getElementById('2108.07767v2-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with the accepted version. Added the journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 137 (2022) 102670 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.06293">arXiv:2108.06293</a> <span> [<a href="https://arxiv.org/pdf/2108.06293">pdf</a>, <a href="https://arxiv.org/format/2108.06293">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 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/10.1007/JHEP03(2022)055">10.1007/JHEP03(2022)055 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combined sensitivity of JUNO and KM3NeT/ORCA to the neutrino mass ordering </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KM3NeT+Collaboration"> KM3NeT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/hep-ex?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Berg%2C+A+M+v+d">A. M. van den Berg</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Boettcher%2C+M">M. Boettcher</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="2108.06293v1-abstract-short" style="display: inline;"> This article presents the potential of a combined analysis of the JUNO and KM3NeT/ORCA experiments to determine the neutrino mass ordering. This combination is particularly interesting as it significantly boosts the potential of either detector, beyond simply adding their neutrino mass ordering sensitivities, by removing a degeneracy in the determination of $螖m_{31}^2$ between the two experiments… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.06293v1-abstract-full').style.display = 'inline'; document.getElementById('2108.06293v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.06293v1-abstract-full" style="display: none;"> This article presents the potential of a combined analysis of the JUNO and KM3NeT/ORCA experiments to determine the neutrino mass ordering. This combination is particularly interesting as it significantly boosts the potential of either detector, beyond simply adding their neutrino mass ordering sensitivities, by removing a degeneracy in the determination of $螖m_{31}^2$ between the two experiments when assuming the wrong ordering. The study is based on the latest projected performances for JUNO, and on simulation tools using a full Monte Carlo approach to the KM3NeT/ORCA response with a careful assessment of its energy systematics. From this analysis, a $5蟽$ determination of the neutrino mass ordering is expected after 6 years of joint data taking for any value of the oscillation parameters. This sensitivity would be achieved after only 2 years of joint data taking assuming the current global best-fit values for those parameters for normal ordering. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.06293v1-abstract-full').style.display = 'none'; document.getElementById('2108.06293v1-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 03 (2022) 055 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.00344">arXiv:2107.00344</a> <span> [<a href="https://arxiv.org/pdf/2107.00344">pdf</a>, <a href="https://arxiv.org/format/2107.00344">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> </div> </div> <p class="title is-5 mathjax"> Sensitivity to light sterile neutrino mixing parameters with KM3NeT/ORCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alshamsi%2C+M">M. Alshamsi</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/hep-ex?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Berg%2C+A+M+v+d">A. M. van den Berg</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?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="2107.00344v2-abstract-short" style="display: inline;"> KM3NeT/ORCA is a next-generation neutrino telescope optimised for atmospheric neutrino oscillations studies. In this paper, the sensitivity of ORCA to the presence of a light sterile neutrino in a 3+1 model is presented. After three years of data taking, ORCA will be able to probe the active-sterile mixing angles $胃_{14}$, $胃_{24}$, $胃_{34}$ and the effective angle $胃_{渭e}$, over a broad range of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.00344v2-abstract-full').style.display = 'inline'; document.getElementById('2107.00344v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.00344v2-abstract-full" style="display: none;"> KM3NeT/ORCA is a next-generation neutrino telescope optimised for atmospheric neutrino oscillations studies. In this paper, the sensitivity of ORCA to the presence of a light sterile neutrino in a 3+1 model is presented. After three years of data taking, ORCA will be able to probe the active-sterile mixing angles $胃_{14}$, $胃_{24}$, $胃_{34}$ and the effective angle $胃_{渭e}$, over a broad range of mass squared difference $螖m^2_{41} \sim [10^{-5}, 10]$ $\rm{eV}^2$, allowing to test the eV-mass sterile neutrino hypothesis as the origin of short baseline anomalies, as well as probing the hypothesis of a very light sterile neutrino, not yet constrained by cosmology. ORCA will be able to explore a relevant fraction of the parameter space not yet reached by present measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.00344v2-abstract-full').style.display = 'none'; document.getElementById('2107.00344v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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/2103.09885">arXiv:2103.09885</a> <span> [<a href="https://arxiv.org/pdf/2103.09885">pdf</a>, <a href="https://arxiv.org/format/2103.09885">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> </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/s10052-021-09893-0">10.1140/epjc/s10052-021-09893-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Determining the Neutrino Mass Ordering and Oscillation Parameters with KM3NeT/ORCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">S. Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Aly%2C+Z">Z. Aly</a>, <a href="/search/hep-ex?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anguita%2C+M">M. Anguita</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Bagatelas%2C+C">C. Bagatelas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Pree%2C+S+B+d">S. Basegmez du Pree</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Benfenati%2C+F">F. Benfenati</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Berg%2C+A+M+v+d">A. M. van den Berg</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a> , et al. (217 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="2103.09885v2-abstract-short" style="display: inline;"> The next generation of water Cherenkov neutrino telescopes in the Mediterranean Sea are under construction offshore France (KM3NeT/ORCA) and Sicily (KM3NeT/ARCA). The KM3NeT/ORCA detector features an energy detection threshold which allows to collect atmospheric neutrinos to study flavour oscillation. This paper reports the KM3NeT/ORCA sensitivity to this phenomenon. The event reconstruction, sele… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.09885v2-abstract-full').style.display = 'inline'; document.getElementById('2103.09885v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.09885v2-abstract-full" style="display: none;"> The next generation of water Cherenkov neutrino telescopes in the Mediterranean Sea are under construction offshore France (KM3NeT/ORCA) and Sicily (KM3NeT/ARCA). The KM3NeT/ORCA detector features an energy detection threshold which allows to collect atmospheric neutrinos to study flavour oscillation. This paper reports the KM3NeT/ORCA sensitivity to this phenomenon. The event reconstruction, selection and classification are described. The sensitivity to determine the neutrino mass ordering was evaluated and found to be 4.4 $蟽$ if the true ordering is normal and 2.3 $蟽$ if inverted, after three years of data taking. The precision to measure $螖m^2_{32}$ and $胃_{23}$ were also estimated and found to be $85\cdot10^{-6}$ eV$^2$ and $(^{+1.9}_{-3.1})^{\circ}$ for normal neutrino mass ordering and, $75\cdot10^{-6}$ eV$^2$ and $(^{+2.0}_{-7.0})^{\circ}$ for inverted ordering. Finally, a unitarity test of the leptonic mixing matrix by measuring the rate of tau neutrinos is described. Three years of data taking were found to be sufficient to exclude $谓_蟿$ and $\bar谓_蟿$ event rate variations larger than 20% at $3蟽$ level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.09885v2-abstract-full').style.display = 'none'; document.getElementById('2103.09885v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">Accepted for publication at 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 82, 26 (2022) </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/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/hep-ex?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/hep-ex?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?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/2007.00931">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/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma1%2C+B">B. Belhorma1</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/hep-ex?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">Arnauld Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Garre%2C+S+A">Sergio Alves Garre</a>, <a href="/search/hep-ex?searchtype=author&query=Aly%2C+Z">Zineb Aly</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">Fabrizio Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">Michel Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Androulakis%2C+G">Giorgos Androulakis</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">Marco Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anguita%2C+M">Mancia Anguita</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">Gisela Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">Miquel Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Bagatelas%2C+C">Christos Bagatelas</a>, <a href="/search/hep-ex?searchtype=author&query=Barbarino%2C+G">Giancarlo Barbarino</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">Bruny Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Pree%2C+S+B+d">Suzan Basegmez du Pree</a>, <a href="/search/hep-ex?searchtype=author&query=Bendahman%2C+M">Meriem Bendahman</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">Edward Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">Vincent Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">Simone Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Biagioni%2C+A">Andrea Biagioni</a>, <a href="/search/hep-ex?searchtype=author&query=Bissinger%2C+M">Matthias Bissinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boettcher%2C+M">Markus Boettcher</a>, <a href="/search/hep-ex?searchtype=author&query=Boumaaza%2C+J">Jihad Boumaaza</a>, <a href="/search/hep-ex?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/2003.04022">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/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+J">J. J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/hep-ex?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?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/1911.06452">arXiv:1911.06452</a> <span> [<a href="https://arxiv.org/pdf/1911.06452">pdf</a>, <a href="https://arxiv.org/format/1911.06452">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 Detectors">physics.ins-det</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/10.22323/1.370.0120">10.22323/1.370.0120 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Apollo ATCA Platform </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Butler%2C+J">J. Butler</a>, <a href="/search/hep-ex?searchtype=author&query=Demiragli%2C+Z">Z. Demiragli</a>, <a href="/search/hep-ex?searchtype=author&query=Finelli%2C+K">K. Finelli</a>, <a href="/search/hep-ex?searchtype=author&query=Gastler%2C+D">D. Gastler</a>, <a href="/search/hep-ex?searchtype=author&query=Hazen%2C+E">E. Hazen</a>, <a href="/search/hep-ex?searchtype=author&query=Rohlf%2C+J">J. Rohlf</a>, <a href="/search/hep-ex?searchtype=author&query=Yuan%2C+S">S. Yuan</a>, <a href="/search/hep-ex?searchtype=author&query=de+Paiva%2C+T+C">T. Costa de Paiva</a>, <a href="/search/hep-ex?searchtype=author&query=Outschoorn%2C+V+M">V. Martinez Outschoorn</a>, <a href="/search/hep-ex?searchtype=author&query=Willocq%2C+S">S. Willocq</a>, <a href="/search/hep-ex?searchtype=author&query=Strohman%2C+C">C. Strohman</a>, <a href="/search/hep-ex?searchtype=author&query=Wittich%2C+P">P. Wittich</a>, <a href="/search/hep-ex?searchtype=author&query=Glein%2C+R">R. Glein</a>, <a href="/search/hep-ex?searchtype=author&query=Ulmer%2C+K">K. Ulmer</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="1911.06452v1-abstract-short" style="display: inline;"> We have developed a novel and generic open-source platform - Apollo - which simplifies the design of custom Advanced Telecommunications Computing Architecture (ATCA) blades by factoring the design into generic infrastructure and application-specific parts. The Apollo "Service Module" provides the required ATCA Intelligent Platform Management Controller, power entry and conditioning, a powerful sys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.06452v1-abstract-full').style.display = 'inline'; document.getElementById('1911.06452v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.06452v1-abstract-full" style="display: none;"> We have developed a novel and generic open-source platform - Apollo - which simplifies the design of custom Advanced Telecommunications Computing Architecture (ATCA) blades by factoring the design into generic infrastructure and application-specific parts. The Apollo "Service Module" provides the required ATCA Intelligent Platform Management Controller, power entry and conditioning, a powerful system-on-module (SoM) computer, and flexible clock and communications infrastructure. The Apollo "Command Module" is customized for each application and typically includes two large field-programmable gate arrays, several hundred optical fiber interfaces operating at speeds up to 28 Gbps, memories, and other supporting infrastructure. The command and service module boards can be operated together or independently on the bench without need for an ATCA shelf. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.06452v1-abstract-full').style.display = 'none'; document.getElementById('1911.06452v1-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 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">Submitted to the Proceedings for TWEPP 2019</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> PoS(TWEPP2019) 120 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.04356">arXiv:1911.04356</a> <span> [<a href="https://arxiv.org/pdf/1911.04356">pdf</a>, <a href="https://arxiv.org/format/1911.04356">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/10.1088/1475-7516/2020/04/026">10.1088/1475-7516/2020/04/026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the Local Burst Rate Density of Primordial Black Holes with HAWC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/hep-ex?searchtype=author&query=Alvarez%2C+C">C. Alvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Arteaga-Vel%C3%A1zquez%2C+J+C">J. C. Arteaga-Vel谩zquez</a>, <a href="/search/hep-ex?searchtype=author&query=Arunbabu%2C+K+P">K. P. Arunbabu</a>, <a href="/search/hep-ex?searchtype=author&query=Rojas%2C+D+A">D. Avila Rojas</a>, <a href="/search/hep-ex?searchtype=author&query=Solares%2C+H+A+A">H. A. Ayala Solares</a>, <a href="/search/hep-ex?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/hep-ex?searchtype=author&query=Belmont-Moreno%2C+E">E. Belmont-Moreno</a>, <a href="/search/hep-ex?searchtype=author&query=BenZvi%2C+S+Y">S. Y. BenZvi</a>, <a href="/search/hep-ex?searchtype=author&query=Brisbois%2C+C">C. Brisbois</a>, <a href="/search/hep-ex?searchtype=author&query=Caballero-Mora%2C+K+S">K. S. Caballero-Mora</a>, <a href="/search/hep-ex?searchtype=author&query=Capistr%C3%A1n%2C+T">T. Capistr谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Carrami%C3%B1ana%2C+A">A. Carrami帽ana</a>, <a href="/search/hep-ex?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/hep-ex?searchtype=author&query=Cotti%2C+U">U. Cotti</a>, <a href="/search/hep-ex?searchtype=author&query=Cotzomi%2C+J">J. Cotzomi</a>, <a href="/search/hep-ex?searchtype=author&query=De+la+Fuente%2C+E">E. De la Fuente</a>, <a href="/search/hep-ex?searchtype=author&query=de+Le%C3%B3n%2C+C">C. de Le贸n</a>, <a href="/search/hep-ex?searchtype=author&query=Dingus%2C+B+L">B. L. Dingus</a>, <a href="/search/hep-ex?searchtype=author&query=DuVernois%2C+M+A">M. A. DuVernois</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%ADaz-V%C3%A9lez%2C+J+C">J. C. D铆az-V茅lez</a>, <a href="/search/hep-ex?searchtype=author&query=Ellsworth%2C+R+W">R. W. Ellsworth</a>, <a href="/search/hep-ex?searchtype=author&query=Engel%2C+K+L">K. L. Engel</a>, <a href="/search/hep-ex?searchtype=author&query=Espinoza%2C+C">C. Espinoza</a> , et al. (62 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="1911.04356v2-abstract-short" style="display: inline;"> Primordial Black Holes (PBHs) may have been created by density fluctuations in the early Universe and could be as massive as $> 10^9$ solar masses or as small as the Planck mass. It has been postulated that a black hole has a temperature inversely-proportional to its mass and will thermally emit all species of fundamental particles via Hawking Radiation. PBHs with initial masses of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.04356v2-abstract-full').style.display = 'inline'; document.getElementById('1911.04356v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.04356v2-abstract-full" style="display: none;"> Primordial Black Holes (PBHs) may have been created by density fluctuations in the early Universe and could be as massive as $> 10^9$ solar masses or as small as the Planck mass. It has been postulated that a black hole has a temperature inversely-proportional to its mass and will thermally emit all species of fundamental particles via Hawking Radiation. PBHs with initial masses of $\sim 5 \times 10^{14}$ g (approximately one gigaton) should be expiring today with bursts of high-energy gamma radiation in the GeV--TeV energy range. The High Altitude Water Cherenkov (HAWC) Observatory is sensitive to gamma rays with energies of $\sim$300 GeV to past 100 TeV, which corresponds to the high end of the PBH burst spectrum. With its large instantaneous field-of-view of $\sim 2$ sr and a duty cycle over 95%, the HAWC Observatory is well suited to perform an all-sky search for PBH bursts. We conducted a search using 959 days of HAWC data and exclude the local PBH burst rate density above $3400~\mathrm{pc^{-3}~yr^{-1}}$ at 99% confidence, the strongest limit on the local PBH burst rate density from any existing electromagnetic measurement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.04356v2-abstract-full').style.display = 'none'; document.getElementById('1911.04356v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">Corresponding authors: K.L. Engel & A. Peisker. 13 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-05 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.01808">arXiv:1909.01808</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="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> HAWC Contributions to the 36th International Cosmic Ray Conference (ICRC2019) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abeysekara%2C+A+U">A. U. Abeysekara</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/hep-ex?searchtype=author&query=Alvarez%2C+C">C. Alvarez</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%81lvarez%2C+J+D">J. D. 脕lvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Camacho%2C+J+R+A">J. R. Angeles Camacho</a>, <a href="/search/hep-ex?searchtype=author&query=Arteaga-Vel%C3%A1zquez%2C+J+C">J. C. Arteaga-Vel谩zquez</a>, <a href="/search/hep-ex?searchtype=author&query=Arunbabu%2C+K+P">K. P. Arunbabu</a>, <a href="/search/hep-ex?searchtype=author&query=Rojas%2C+D+A">D. Avila Rojas</a>, <a href="/search/hep-ex?searchtype=author&query=Solares%2C+H+A+A">H. A. Ayala Solares</a>, <a href="/search/hep-ex?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/hep-ex?searchtype=author&query=Barber%2C+A+S">A. S. Barber</a>, <a href="/search/hep-ex?searchtype=author&query=Gonzalez%2C+J+B">J. Becerra Gonzalez</a>, <a href="/search/hep-ex?searchtype=author&query=Belmont-Moreno%2C+E">E. Belmont-Moreno</a>, <a href="/search/hep-ex?searchtype=author&query=BenZvi%2C+S+Y">S. Y. BenZvi</a>, <a href="/search/hep-ex?searchtype=author&query=Berley%2C+D">D. Berley</a>, <a href="/search/hep-ex?searchtype=author&query=Braun%2C+J">J. Braun</a>, <a href="/search/hep-ex?searchtype=author&query=Brisbois%2C+C">C. Brisbois</a>, <a href="/search/hep-ex?searchtype=author&query=Caballero-Mora%2C+K+S">K. S. Caballero-Mora</a>, <a href="/search/hep-ex?searchtype=author&query=Capistr%C3%A1n%2C+T">T. Capistr谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Carrami%C3%B1ana%2C+A">A. Carrami帽ana</a>, <a href="/search/hep-ex?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/hep-ex?searchtype=author&query=Cotti12%2C+U">U. Cotti12</a>, <a href="/search/hep-ex?searchtype=author&query=Cotzomi%2C+J">J. Cotzomi</a>, <a href="/search/hep-ex?searchtype=author&query=de+Le%C3%B3n%2C+S+C">S. Couti帽o de Le贸n</a> , et al. (105 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="1909.01808v1-abstract-short" style="display: inline;"> List of proceedings from the HAWC 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="1909.01808v1-abstract-full" style="display: none;"> List of proceedings from the HAWC 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('1909.01808v1-abstract-full').style.display = 'none'; document.getElementById('1909.01808v1-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">List of proceedings from the HAWC Collaboration presented at ICRC2019. Corrected typos in the index of the previous version. Follow the "HTML" link to access the list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.03353">arXiv:1906.03353</a> <span> [<a href="https://arxiv.org/pdf/1906.03353">pdf</a>, <a href="https://arxiv.org/format/1906.03353">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> <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/10.1088/1475-7516/2019/12/061">10.1088/1475-7516/2019/12/061 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Dark Matter in the Galactic Halo with a Wide Field of View TeV Gamma-ray Observatory in the Southern Hemisphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Viana%2C+A">Aion Viana</a>, <a href="/search/hep-ex?searchtype=author&query=Schoorlemmer%2C+H">Harm Schoorlemmer</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">Andrea Albert</a>, <a href="/search/hep-ex?searchtype=author&query=de+Souza%2C+V">Vitor de Souza</a>, <a href="/search/hep-ex?searchtype=author&query=Harding%2C+J+P">J. Patrick Harding</a>, <a href="/search/hep-ex?searchtype=author&query=Hinton%2C+J">Jim Hinton</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1906.03353v2-abstract-short" style="display: inline;"> Despite mounting evidence that dark matter (DM) exists in the Universe, its fundamental nature remains unknown. We present sensitivity estimates to detect DM particles with a future very-high-energy ($\gtrsim$ TeV) wide field-of-view gamma-ray observatory in the Southern Hemisphere. This observatory would search for gamma rays from the annihilation or decay of DM particles in the Galactic halo. Wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.03353v2-abstract-full').style.display = 'inline'; document.getElementById('1906.03353v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.03353v2-abstract-full" style="display: none;"> Despite mounting evidence that dark matter (DM) exists in the Universe, its fundamental nature remains unknown. We present sensitivity estimates to detect DM particles with a future very-high-energy ($\gtrsim$ TeV) wide field-of-view gamma-ray observatory in the Southern Hemisphere. This observatory would search for gamma rays from the annihilation or decay of DM particles in the Galactic halo. With a wide field of view, both the Galactic Center and a large fraction of the Galactic halo will be detectable with unprecedented sensitivity to DM in the mass range of $\sim$500 GeV to $\sim$2 PeV. These results, combined with those from other present and future gamma-ray observatories, will likely probe the thermal relic annihilation cross section of Weakly Interacting Massive Particles for all masses from $\sim$80 TeV down to the GeV range in most annihilation channels. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.03353v2-abstract-full').style.display = 'none'; document.getElementById('1906.03353v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in JCAP, 15 pages (+ references), 14 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/1812.08650">arXiv:1812.08650</a> <span> [<a href="https://arxiv.org/pdf/1812.08650">pdf</a>, <a href="https://arxiv.org/format/1812.08650">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 Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Measuring the atmospheric neutrino oscillation parameters and constraining the 3+1 neutrino model with ten years of ANTARES data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/hep-ex?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</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="1812.08650v3-abstract-short" style="display: inline;"> The ANTARES neutrino telescope has an energy threshold of a few tens of GeV. This allows to study the phenomenon of atmospheric muon neutrino disappearance due to neutrino oscillations. In a similar way, constraints on the 3+1 neutrino model, which foresees the existence of one sterile neutrino, can be inferred. Using data collected by the ANTARES neutrino telescope from 2007 to 2016, a new measur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.08650v3-abstract-full').style.display = 'inline'; document.getElementById('1812.08650v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.08650v3-abstract-full" style="display: none;"> The ANTARES neutrino telescope has an energy threshold of a few tens of GeV. This allows to study the phenomenon of atmospheric muon neutrino disappearance due to neutrino oscillations. In a similar way, constraints on the 3+1 neutrino model, which foresees the existence of one sterile neutrino, can be inferred. Using data collected by the ANTARES neutrino telescope from 2007 to 2016, a new measurement of $螖m^2_{32}$ and $胃_{23}$ has been performed - which is consistent with world best-fit values - and constraints on the 3+1 neutrino model have been derived. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.08650v3-abstract-full').style.display = 'none'; document.getElementById('1812.08650v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.07831">arXiv:1812.07831</a> <span> [<a href="https://arxiv.org/pdf/1812.07831">pdf</a>, <a href="https://arxiv.org/format/1812.07831">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Beyond the Standard Model Physics at the HL-LHC and HE-LHC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Vidal%2C+X+C">X. Cid Vidal</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Onofrio%2C+M">M. D'Onofrio</a>, <a href="/search/hep-ex?searchtype=author&query=Fox%2C+P+J">P. J. Fox</a>, <a href="/search/hep-ex?searchtype=author&query=Torre%2C+R">R. Torre</a>, <a href="/search/hep-ex?searchtype=author&query=Ulmer%2C+K+A">K. A. Ulmer</a>, <a href="/search/hep-ex?searchtype=author&query=Aboubrahim%2C+A">A. Aboubrahim</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alimena%2C+J">J. Alimena</a>, <a href="/search/hep-ex?searchtype=author&query=Allanach%2C+B+C">B. C. Allanach</a>, <a href="/search/hep-ex?searchtype=author&query=Alpigiani%2C+C">C. Alpigiani</a>, <a href="/search/hep-ex?searchtype=author&query=Altakach%2C+M">M. Altakach</a>, <a href="/search/hep-ex?searchtype=author&query=Amoroso%2C+S">S. Amoroso</a>, <a href="/search/hep-ex?searchtype=author&query=Anders%2C+J+K">J. K. Anders</a>, <a href="/search/hep-ex?searchtype=author&query=Araz%2C+J+Y">J. Y. Araz</a>, <a href="/search/hep-ex?searchtype=author&query=Arbey%2C+A">A. Arbey</a>, <a href="/search/hep-ex?searchtype=author&query=Azzi%2C+P">P. Azzi</a>, <a href="/search/hep-ex?searchtype=author&query=Babounikau%2C+I">I. Babounikau</a>, <a href="/search/hep-ex?searchtype=author&query=Baer%2C+H">H. Baer</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+M+J">M. J. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Barducci%2C+D">D. Barducci</a>, <a href="/search/hep-ex?searchtype=author&query=Barger%2C+V">V. Barger</a>, <a href="/search/hep-ex?searchtype=author&query=Baron%2C+O">O. Baron</a>, <a href="/search/hep-ex?searchtype=author&query=Navarro%2C+L+B">L. Barranco Navarro</a>, <a href="/search/hep-ex?searchtype=author&query=Battaglia%2C+M">M. Battaglia</a>, <a href="/search/hep-ex?searchtype=author&query=Bay%2C+A">A. Bay</a> , et al. (272 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="1812.07831v4-abstract-short" style="display: inline;"> This is the third out of five chapters of the final report [1] of the Workshop on Physics at HL-LHC, and perspectives on HE-LHC [2]. It is devoted to the study of the potential, in the search for Beyond the Standard Model (BSM) physics, of the High Luminosity (HL) phase of the LHC, defined as $3~\mathrm{ab}^{-1}$ of data taken at a centre-of-mass energy of $14~\mathrm{TeV}$, and of a possible futu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.07831v4-abstract-full').style.display = 'inline'; document.getElementById('1812.07831v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.07831v4-abstract-full" style="display: none;"> This is the third out of five chapters of the final report [1] of the Workshop on Physics at HL-LHC, and perspectives on HE-LHC [2]. It is devoted to the study of the potential, in the search for Beyond the Standard Model (BSM) physics, of the High Luminosity (HL) phase of the LHC, defined as $3~\mathrm{ab}^{-1}$ of data taken at a centre-of-mass energy of $14~\mathrm{TeV}$, and of a possible future upgrade, the High Energy (HE) LHC, defined as $15~\mathrm{ab}^{-1}$ of data at a centre-of-mass energy of $27~\mathrm{TeV}$. We consider a large variety of new physics models, both in a simplified model fashion and in a more model-dependent one. A long list of contributions from the theory and experimental (ATLAS, CMS, LHCb) communities have been collected and merged together to give a complete, wide, and consistent view of future prospects for BSM physics at the considered colliders. On top of the usual standard candles, such as supersymmetric simplified models and resonances, considered for the evaluation of future collider potentials, this report contains results on dark matter and dark sectors, long lived particles, leptoquarks, sterile neutrinos, axion-like particles, heavy scalars, vector-like quarks, and more. Particular attention is placed, especially in the study of the HL-LHC prospects, to the detector upgrades, the assessment of the future systematic uncertainties, and new experimental techniques. The general conclusion is that the HL-LHC, on top of allowing to extend the present LHC mass and coupling reach by $20-50\%$ on most new physics scenarios, will also be able to constrain, and potentially discover, new physics that is presently unconstrained. Moreover, compared to the HL-LHC, the reach in most observables will generally more than double at the HE-LHC, which may represent a good candidate future facility for a final test of TeV-scale new physics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.07831v4-abstract-full').style.display = 'none'; document.getElementById('1812.07831v4-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Report from Working Group 3 on the Physics of the HL-LHC, and Perspectives at the HE-LHC; v2: final version updated with the latest contributions and summaries; 239 pages + refs; v3: typos and character misprint in Fig. 7.2 fixed; v4: added one missing author</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> CERN-LPCC-2018-05 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.09420">arXiv:1810.09420</a> <span> [<a href="https://arxiv.org/pdf/1810.09420">pdf</a>, <a href="https://arxiv.org/format/1810.09420">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 Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> LHC Dark Matter Working Group: Next-generation spin-0 dark matter models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+T">Tomohiro Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Afik%2C+Y">Yoav Afik</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">Andreas Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Anelli%2C+C+R">Christopher R. Anelli</a>, <a href="/search/hep-ex?searchtype=author&query=Barak%2C+L">Liron Barak</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+M">Martin Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Behr%2C+J+K">J. Katharina Behr</a>, <a href="/search/hep-ex?searchtype=author&query=Bell%2C+N+F">Nicole F. Bell</a>, <a href="/search/hep-ex?searchtype=author&query=Boveia%2C+A">Antonio Boveia</a>, <a href="/search/hep-ex?searchtype=author&query=Brandt%2C+O">Oleg Brandt</a>, <a href="/search/hep-ex?searchtype=author&query=Busoni%2C+G">Giorgio Busoni</a>, <a href="/search/hep-ex?searchtype=author&query=Carpenter%2C+L+M">Linda M. Carpenter</a>, <a href="/search/hep-ex?searchtype=author&query=Chen%2C+Y">Yu-Heng Chen</a>, <a href="/search/hep-ex?searchtype=author&query=Doglioni%2C+C">Caterina Doglioni</a>, <a href="/search/hep-ex?searchtype=author&query=Elliot%2C+A">Alison Elliot</a>, <a href="/search/hep-ex?searchtype=author&query=Fujiwara%2C+M">Motoko Fujiwara</a>, <a href="/search/hep-ex?searchtype=author&query=Genest%2C+M">Marie-Helene Genest</a>, <a href="/search/hep-ex?searchtype=author&query=Gerosa%2C+R">Raffaele Gerosa</a>, <a href="/search/hep-ex?searchtype=author&query=Gori%2C+S">Stefania Gori</a>, <a href="/search/hep-ex?searchtype=author&query=Gramling%2C+J">Johanna Gramling</a>, <a href="/search/hep-ex?searchtype=author&query=Grohsjean%2C+A">Alexander Grohsjean</a>, <a href="/search/hep-ex?searchtype=author&query=Gustavino%2C+G">Giuliano Gustavino</a>, <a href="/search/hep-ex?searchtype=author&query=Hahn%2C+K">Kristian Hahn</a>, <a href="/search/hep-ex?searchtype=author&query=Haisch%2C+U">Ulrich Haisch</a>, <a href="/search/hep-ex?searchtype=author&query=Henkelmann%2C+L">Lars Henkelmann</a> , et al. (28 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="1810.09420v2-abstract-short" style="display: inline;"> Dark matter (DM) simplified models are by now commonly used by the ATLAS and CMS Collaborations to interpret searches for missing transverse energy ($E_T^\mathrm{miss}$). The coherent use of these models sharpened the LHC DM search program, especially in the presentation of its results and their comparison to DM direct-detection (DD) and indirect-detection (ID) experiments. However, the community… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.09420v2-abstract-full').style.display = 'inline'; document.getElementById('1810.09420v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.09420v2-abstract-full" style="display: none;"> Dark matter (DM) simplified models are by now commonly used by the ATLAS and CMS Collaborations to interpret searches for missing transverse energy ($E_T^\mathrm{miss}$). The coherent use of these models sharpened the LHC DM search program, especially in the presentation of its results and their comparison to DM direct-detection (DD) and indirect-detection (ID) experiments. However, the community has been aware of the limitations of the DM simplified models, in particular the lack of theoretical consistency of some of them and their restricted phenomenology leading to the relevance of only a small subset of $E_T^\mathrm{miss}$ signatures. This document from the LHC Dark Matter Working Group identifies an example of a next-generation DM model, called $\textrm{2HDM+a}$, that provides the simplest theoretically consistent extension of the DM pseudoscalar simplified model. A comprehensive study of the phenomenology of the $\textrm{2HDM+a}$ model is presented, including a discussion of the rich and intricate pattern of mono-$X$ signatures and the relevance of other DM as well as non-DM experiments. Based on our discussions, a set of recommended scans are proposed to explore the parameter space of the $\textrm{2HDM+a}$ model through LHC searches. The exclusion limits obtained from the proposed scans can be consistently compared to the constraints on the $\textrm{2HDM+a}$ model that derive from DD, ID and the DM relic density. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.09420v2-abstract-full').style.display = 'none'; document.getElementById('1810.09420v2-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 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Change of CERN report ID in v2</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> CERN-LPCC-2018-02 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.11815">arXiv:1807.11815</a> <span> [<a href="https://arxiv.org/pdf/1807.11815">pdf</a>, <a href="https://arxiv.org/format/1807.11815">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/10.1140/epjc/s10052-018-6451-3">10.1140/epjc/s10052-018-6451-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The cosmic ray shadow of the Moon observed with the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%ADt%2C+J">J. Barrios-Mart铆t</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/hep-ex?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nza%2C+H">H. Br芒nza</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a> , et al. (102 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="1807.11815v1-abstract-short" style="display: inline;"> One of the main objectives of the ANTARES telescope is the search for point-like neutrino sources. Both the pointing accuracy and the angular resolution of the detector are important in this context and a reliable way to evaluate this performance is needed. In order to measure the pointing accuracy of the detector, one possibility is to study the shadow of the Moon, i.e. the deficit of the atmosph… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.11815v1-abstract-full').style.display = 'inline'; document.getElementById('1807.11815v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.11815v1-abstract-full" style="display: none;"> One of the main objectives of the ANTARES telescope is the search for point-like neutrino sources. Both the pointing accuracy and the angular resolution of the detector are important in this context and a reliable way to evaluate this performance is needed. In order to measure the pointing accuracy of the detector, one possibility is to study the shadow of the Moon, i.e. the deficit of the atmospheric muon flux from the direction of the Moon induced by the absorption of cosmic rays. Analysing the data taken between 2007 and 2016, the Moon shadow is observed with $3.5蟽$ statistical significance. The detector angular resolution for downward-going muons is 0.73$^{\circ}\pm0.14^{\circ}.$ The resulting pointing performance is consistent with the expectations. An independent check of the telescope pointing accuracy is realised with the data collected by a shower array detector onboard of a ship temporarily moving around the ANTARES location. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.11815v1-abstract-full').style.display = 'none'; document.getElementById('1807.11815v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 9 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/1711.01496">arXiv:1711.01496</a> <span> [<a href="https://arxiv.org/pdf/1711.01496">pdf</a>, <a href="https://arxiv.org/format/1711.01496">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> <p class="title is-5 mathjax"> The ANTARES Collaboration: Contributions to ICRC 2017 Part III: Searches for dark matter and exotics, neutrino oscillations and detector calibration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Celli%2C+S">S. Celli</a> , et al. (103 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="1711.01496v1-abstract-short" style="display: inline;"> Papers on the searches for dark matter and exotics, neutrino oscillations and detector calibration, prepared for the 35th International Cosmic Ray Conference (ICRC 2017, Busan, South Korea) by the ANTARES Collaboration </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.01496v1-abstract-full" style="display: none;"> Papers on the searches for dark matter and exotics, neutrino oscillations and detector calibration, prepared for the 35th International Cosmic Ray Conference (ICRC 2017, Busan, South Korea) by the ANTARES Collaboration <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.01496v1-abstract-full').style.display = 'none'; document.getElementById('1711.01496v1-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 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.02572">arXiv:1708.02572</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="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> HAWC Contributions to the 35th International Cosmic Ray Conference (ICRC2017) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abeysekara%2C+A+U">A. U. Abeysekara</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/hep-ex?searchtype=author&query=Alvarez%2C+C">C. Alvarez</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%81lvarez%2C+J+D">J. D. 脕lvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Arceo%2C+R">R. Arceo</a>, <a href="/search/hep-ex?searchtype=author&query=Arteaga-Vel%C3%A1zquez%2C+J+C">J. C. Arteaga-Vel谩zquez</a>, <a href="/search/hep-ex?searchtype=author&query=Rojas%2C+D+A">D. Avila Rojas</a>, <a href="/search/hep-ex?searchtype=author&query=Solares%2C+H+A+A">H. A. Ayala Solares</a>, <a href="/search/hep-ex?searchtype=author&query=Barber%2C+A+S">A. S. Barber</a>, <a href="/search/hep-ex?searchtype=author&query=Gonzalez%2C+J+B">J. Becerra Gonzalez</a>, <a href="/search/hep-ex?searchtype=author&query=Becerril%2C+A">A. Becerril</a>, <a href="/search/hep-ex?searchtype=author&query=Belmont-Moreno%2C+E">E. Belmont-Moreno</a>, <a href="/search/hep-ex?searchtype=author&query=BenZvi%2C+S+Y">S. Y. BenZvi</a>, <a href="/search/hep-ex?searchtype=author&query=Berley%2C+D">D. Berley</a>, <a href="/search/hep-ex?searchtype=author&query=Bernal%2C+A">A. Bernal</a>, <a href="/search/hep-ex?searchtype=author&query=Brisbois%2C+C">C. Brisbois</a>, <a href="/search/hep-ex?searchtype=author&query=Caballero-Mora%2C+K+S">K. S. Caballero-Mora</a>, <a href="/search/hep-ex?searchtype=author&query=Capistr%C3%A1n%2C+T">T. Capistr谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Carrami%C3%B1ana%2C+A">A. Carrami帽ana</a>, <a href="/search/hep-ex?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/hep-ex?searchtype=author&query=Castillo%2C+M">M. Castillo</a>, <a href="/search/hep-ex?searchtype=author&query=Cotti%2C+U">U. Cotti</a>, <a href="/search/hep-ex?searchtype=author&query=Cotzomi%2C+J">J. Cotzomi</a>, <a href="/search/hep-ex?searchtype=author&query=de+Le%C3%B3n%2C+S+C">S. Couti帽o de Le贸n</a> , et al. (101 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="1708.02572v2-abstract-short" style="display: inline;"> List of proceedings from the HAWC Collaboration presented at the 35th International Cosmic Ray Conference, 12 July - 20 July 2017, Bexco, Busan, Korea. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.02572v2-abstract-full" style="display: none;"> List of proceedings from the HAWC Collaboration presented at the 35th International Cosmic Ray Conference, 12 July - 20 July 2017, Bexco, Busan, Korea. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.02572v2-abstract-full').style.display = 'none'; document.getElementById('1708.02572v2-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 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2017. </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">List of proceedings from the HAWC Collaboration presented at ICRC2017. Corrected typos in the index of the previous version. Follow the "HTML" link to access the list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.01857">arXiv:1706.01857</a> <span> [<a href="https://arxiv.org/pdf/1706.01857">pdf</a>, <a href="https://arxiv.org/format/1706.01857">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.96.082001">10.1103/PhysRevD.96.082001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First all-flavour Neutrino Point-like Source Search with the ANTARES Neutrino Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Celli%2C+S">S. Celli</a> , et al. (104 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="1706.01857v2-abstract-short" style="display: inline;"> A search for cosmic neutrino sources using the data collected with the ANTARES neutrino telescope between early 2007 and the end of 2015 is performed. For the first time, all neutrino interactions --charged and neutral current interactions of all flavours-- are considered in a search for point-like sources with the ANTARES detector. In previous analyses, only muon neutrino charged current interact… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.01857v2-abstract-full').style.display = 'inline'; document.getElementById('1706.01857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.01857v2-abstract-full" style="display: none;"> A search for cosmic neutrino sources using the data collected with the ANTARES neutrino telescope between early 2007 and the end of 2015 is performed. For the first time, all neutrino interactions --charged and neutral current interactions of all flavours-- are considered in a search for point-like sources with the ANTARES detector. In previous analyses, only muon neutrino charged current interactions were used. This is achieved by using a novel reconstruction algorithm for shower-like events in addition to the standard muon track reconstruction. The shower channel contributes about 23\% of all signal events for an $E^{-2}$ energy spectrum. No significant excess over background is found. The most signal-like cluster of events is located at $(伪,未) = (343.8^\circ, 23.5^\circ)$ with a significance of $1.9蟽$. The neutrino flux sensitivity of the search is about $E^2 d\varPhi/dE = 6\cdot10^{-9} GeV cm^{-2} s^{-1}$ for declinations from $-90^\circ$ up to $-42^\circ$, and below $10^{-8} GeV cm^{-2} s^{-1}$ for declinations up to $5^{\circ}$. The directions of 106 source candidates and of 13 muon track events from the IceCube HESE sample are investigated for a possible neutrino signal and upper limits on the signal flux are determined. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.01857v2-abstract-full').style.display = 'none'; document.getElementById('1706.01857v2-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 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </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, 12 figures, submitted to Physical Review D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 96, 082001 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.05703">arXiv:1703.05703</a> <span> [<a href="https://arxiv.org/pdf/1703.05703">pdf</a>, <a href="https://arxiv.org/format/1703.05703">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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"> Recommendations of the LHC Dark Matter Working Group: Comparing LHC searches for heavy mediators of dark matter production in visible and invisible decay channels </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">Andreas Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Backovic%2C+M">Mihailo Backovic</a>, <a href="/search/hep-ex?searchtype=author&query=Boveia%2C+A">Antonio Boveia</a>, <a href="/search/hep-ex?searchtype=author&query=Buchmueller%2C+O">Oliver Buchmueller</a>, <a href="/search/hep-ex?searchtype=author&query=Busoni%2C+G">Giorgio Busoni</a>, <a href="/search/hep-ex?searchtype=author&query=De+Roeck%2C+A">Albert De Roeck</a>, <a href="/search/hep-ex?searchtype=author&query=Doglioni%2C+C">Caterina Doglioni</a>, <a href="/search/hep-ex?searchtype=author&query=DuPree%2C+T">Tristan DuPree</a>, <a href="/search/hep-ex?searchtype=author&query=Fairbairn%2C+M">Malcolm Fairbairn</a>, <a href="/search/hep-ex?searchtype=author&query=Genest%2C+M">Marie-Helene Genest</a>, <a href="/search/hep-ex?searchtype=author&query=Gori%2C+S">Stefania Gori</a>, <a href="/search/hep-ex?searchtype=author&query=Gustavino%2C+G">Giuliano Gustavino</a>, <a href="/search/hep-ex?searchtype=author&query=Hahn%2C+K">Kristian Hahn</a>, <a href="/search/hep-ex?searchtype=author&query=Haisch%2C+U">Ulrich Haisch</a>, <a href="/search/hep-ex?searchtype=author&query=Harris%2C+P+C">Philip C. Harris</a>, <a href="/search/hep-ex?searchtype=author&query=Hayden%2C+D">Dan Hayden</a>, <a href="/search/hep-ex?searchtype=author&query=Ippolito%2C+V">Valerio Ippolito</a>, <a href="/search/hep-ex?searchtype=author&query=John%2C+I">Isabelle John</a>, <a href="/search/hep-ex?searchtype=author&query=Kahlhoefer%2C+F">Felix Kahlhoefer</a>, <a href="/search/hep-ex?searchtype=author&query=Kulkarni%2C+S">Suchita Kulkarni</a>, <a href="/search/hep-ex?searchtype=author&query=Landsberg%2C+G">Greg Landsberg</a>, <a href="/search/hep-ex?searchtype=author&query=Lowette%2C+S">Steven Lowette</a>, <a href="/search/hep-ex?searchtype=author&query=Mawatari%2C+K">Kentarou Mawatari</a>, <a href="/search/hep-ex?searchtype=author&query=Riotto%2C+A">Antonio Riotto</a>, <a href="/search/hep-ex?searchtype=author&query=Shepherd%2C+W">William Shepherd</a> , et al. (5 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="1703.05703v2-abstract-short" style="display: inline;"> Weakly-coupled TeV-scale particles may mediate the interactions between normal matter and dark matter. If so, the LHC would produce dark matter through these mediators, leading to the familiar "mono-X" search signatures, but the mediators would also produce signals without missing momentum via the same vertices involved in their production. This document from the LHC Dark Matter Working Group sugg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.05703v2-abstract-full').style.display = 'inline'; document.getElementById('1703.05703v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.05703v2-abstract-full" style="display: none;"> Weakly-coupled TeV-scale particles may mediate the interactions between normal matter and dark matter. If so, the LHC would produce dark matter through these mediators, leading to the familiar "mono-X" search signatures, but the mediators would also produce signals without missing momentum via the same vertices involved in their production. This document from the LHC Dark Matter Working Group suggests how to compare searches for these two types of signals in case of vector and axial-vector mediators, based on a workshop that took place on September 19/20, 2016 and subsequent discussions. These suggestions include how to extend the spin-1 mediated simplified models already in widespread use to include lepton couplings. This document also provides analytic calculations of the relic density in the simplified models and reports an issue that arose when ATLAS and CMS first began to use preliminary numerical calculations of the dark matter relic density in these models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.05703v2-abstract-full').style.display = 'none'; document.getElementById('1703.05703v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </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, 4 figures; v2: author list and LaTeX problem fixed</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> CERN-LPCC-2017-01 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.06792">arXiv:1612.06792</a> <span> [<a href="https://arxiv.org/pdf/1612.06792">pdf</a>, <a href="https://arxiv.org/format/1612.06792">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 Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Search for Dark Matter Annihilation in the Earth using the ANTARES Neutrino Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Celli%2C+S">S. Celli</a>, <a href="/search/hep-ex?searchtype=author&query=Chiarusi%2C+T">T. Chiarusi</a>, <a href="/search/hep-ex?searchtype=author&query=Circella%2C+M">M. Circella</a> , et al. (104 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="1612.06792v2-abstract-short" style="display: inline;"> A search for a neutrino signal from WIMP pair annihilations in the centre of the Earth has been performed with the data collected with the ANTARES neutrino telescope from 2007 to 2012. The event selection criteria have been developed and tuned to maximise the sensitivity of the experiment to such a neutrino signal. No significant excess of neutrinos over the expected background has been observed.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.06792v2-abstract-full').style.display = 'inline'; document.getElementById('1612.06792v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.06792v2-abstract-full" style="display: none;"> A search for a neutrino signal from WIMP pair annihilations in the centre of the Earth has been performed with the data collected with the ANTARES neutrino telescope from 2007 to 2012. The event selection criteria have been developed and tuned to maximise the sensitivity of the experiment to such a neutrino signal. No significant excess of neutrinos over the expected background has been observed. Upper limits at $90\%$ C.L. on the WIMP annihilation rate in the Earth and the spin independent scattering cross-section of WIMPs to nucleons $蟽^{SI}_p$ were calculated for WIMP pair annihilations into either $蟿^{+}蟿^{-}$, $W^+W^-$, $b\overline{b}$ or the non-SUSY $谓_渭\bar谓_渭$ as a function of the WIMP mass (between $25\,\mathrm{GeV/c^2}$ and $1000\,\mathrm{GeV/c^2}$) and as a function of the thermally averaged annihilation cross section times velocity $\langle蟽_{A} v\rangle_{Earth}$ of the WIMPs in the centre of the Earth. For masses of the WIMP close to the mass of iron nuclei ($50\,\mathrm{GeV/c^2}$), the obtained limits on $蟽^{SI}_p$ are more stringent than those obtained by other indirect searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.06792v2-abstract-full').style.display = 'none'; document.getElementById('1612.06792v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </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">Revised version for journal submission</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.05621">arXiv:1612.05621</a> <span> [<a href="https://arxiv.org/pdf/1612.05621">pdf</a>, <a href="https://arxiv.org/format/1612.05621">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 Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - 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/10.1007/JHEP05(2017)008">10.1007/JHEP05(2017)008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Intrinsic limits on resolutions in muon- and electron-neutrino charged-current events in the KM3NeT/ORCA detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Ageron%2C+M">M. Ageron</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Anassontzis%2C+E+G">E. G. Anassontzis</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Barbarino%2C+G">G. Barbarino</a>, <a href="/search/hep-ex?searchtype=author&query=Barbarito%2C+E">E. Barbarito</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Belias%2C+A">A. Belias</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Berg%2C+A+v+d">A. van den Berg</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Beurthey%2C+S">S. Beurthey</a>, <a href="/search/hep-ex?searchtype=author&query=van+Beveren%2C+V">V. van Beveren</a>, <a href="/search/hep-ex?searchtype=author&query=Beverini%2C+N">N. Beverini</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Biagioni%2C+A">A. Biagioni</a> , et al. (228 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="1612.05621v2-abstract-short" style="display: inline;"> Studying atmospheric neutrino oscillations in the few-GeV range with a multimegaton detector promises to determine the neutrino mass hierarchy. This is the main science goal pursued by the future KM3NeT/ORCA water Cherenkov detector in the Mediterranean Sea. In this paper, the processes that limit the obtainable resolution in both energy and direction in charged-current neutrino events in the ORCA… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.05621v2-abstract-full').style.display = 'inline'; document.getElementById('1612.05621v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.05621v2-abstract-full" style="display: none;"> Studying atmospheric neutrino oscillations in the few-GeV range with a multimegaton detector promises to determine the neutrino mass hierarchy. This is the main science goal pursued by the future KM3NeT/ORCA water Cherenkov detector in the Mediterranean Sea. In this paper, the processes that limit the obtainable resolution in both energy and direction in charged-current neutrino events in the ORCA detector are investigated. These processes include the composition of the hadronic fragmentation products, the subsequent particle propagation and the photon-sampling fraction of the detector. GEANT simulations of neutrino interactions in seawater produced by GENIE are used to study the effects in the 1 - 20 GeV range. It is found that fluctuations in the hadronic cascade in conjunction with the variation of the inelasticity y are most detrimental to the resolutions. The effect of limited photon sampling in the detector is of significantly less importance. These results will therefore also be applicable to similar detectors/media, such as those in ice. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.05621v2-abstract-full').style.display = 'none'; document.getElementById('1612.05621v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </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">37 pages, 28 figures, JHEP published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The KM3NeT collaboration, Adri{谩}n-Mart{\'谋}nez, S., Ageron, M. et al. J. High Energ. Phys. (2017) 2017: 8 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.06680">arXiv:1607.06680</a> <span> [<a href="https://arxiv.org/pdf/1607.06680">pdf</a>, <a href="https://arxiv.org/format/1607.06680">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 Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Towards the next generation of simplified Dark Matter models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">Andreas Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+M">Martin Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Buchmueller%2C+O">Oliver Buchmueller</a>, <a href="/search/hep-ex?searchtype=author&query=Brooke%2C+J">Jim Brooke</a>, <a href="/search/hep-ex?searchtype=author&query=Cerdeno%2C+D+G">David G. Cerdeno</a>, <a href="/search/hep-ex?searchtype=author&query=Citron%2C+M">Matthew Citron</a>, <a href="/search/hep-ex?searchtype=author&query=Davies%2C+G">Gavin Davies</a>, <a href="/search/hep-ex?searchtype=author&query=de+Cosa%2C+A">Annapaola de Cosa</a>, <a href="/search/hep-ex?searchtype=author&query=De+Roeck%2C+A">Albert De Roeck</a>, <a href="/search/hep-ex?searchtype=author&query=De+Simone%2C+A">Andrea De Simone</a>, <a href="/search/hep-ex?searchtype=author&query=Pree%2C+T+D">Tristan Du Pree</a>, <a href="/search/hep-ex?searchtype=author&query=Ellis%2C+J">John Ellis</a>, <a href="/search/hep-ex?searchtype=author&query=Flaecher%2C+H">Henning Flaecher</a>, <a href="/search/hep-ex?searchtype=author&query=Fairbairn%2C+M">Malcolm Fairbairn</a>, <a href="/search/hep-ex?searchtype=author&query=Grohsjean%2C+A">Alexander Grohsjean</a>, <a href="/search/hep-ex?searchtype=author&query=Hahn%2C+K">Kristian Hahn</a>, <a href="/search/hep-ex?searchtype=author&query=Haisch%2C+U">Ulrich Haisch</a>, <a href="/search/hep-ex?searchtype=author&query=Harris%2C+P+C">Philip C. Harris</a>, <a href="/search/hep-ex?searchtype=author&query=Khoze%2C+V+V">Valentin V. Khoze</a>, <a href="/search/hep-ex?searchtype=author&query=Landsberg%2C+G">Greg Landsberg</a>, <a href="/search/hep-ex?searchtype=author&query=McCabe%2C+C">Christopher McCabe</a>, <a href="/search/hep-ex?searchtype=author&query=Penning%2C+B">Bjoern Penning</a>, <a href="/search/hep-ex?searchtype=author&query=Sanz%2C+V">Veronica Sanz</a>, <a href="/search/hep-ex?searchtype=author&query=Schwanenberger%2C+C">Christian Schwanenberger</a>, <a href="/search/hep-ex?searchtype=author&query=Scott%2C+P">Pat Scott</a> , et al. (1 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="1607.06680v3-abstract-short" style="display: inline;"> This White Paper is an input to the ongoing discussion about the extension and refinement of simplified Dark Matter (DM) models. Based on two concrete examples, we show how existing simplified DM models (SDMM) can be extended to provide a more accurate and comprehensive framework to interpret and characterise collider searches. In the first example we extend the canonical SDMM with a scalar mediat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.06680v3-abstract-full').style.display = 'inline'; document.getElementById('1607.06680v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.06680v3-abstract-full" style="display: none;"> This White Paper is an input to the ongoing discussion about the extension and refinement of simplified Dark Matter (DM) models. Based on two concrete examples, we show how existing simplified DM models (SDMM) can be extended to provide a more accurate and comprehensive framework to interpret and characterise collider searches. In the first example we extend the canonical SDMM with a scalar mediator to include mixing with the Higgs boson. We show that this approach not only provides a better description of the underlying kinematic properties that a complete model would possess, but also offers the option of using this more realistic class of scalar mixing models to compare and combine consistently searches based on different experimental signatures. The second example outlines how a new physics signal observed in a visible channel can be connected to DM by extending a simplified model including effective couplings. This discovery scenario uses the recently observed excess in the high-mass diphoton searches of ATLAS and CMS for a case study to show that such a pragmatic approach can aid the experimental search programme to verify/falsify a potential signal and to study its underlying nature. In the next part of the White Paper we outline other interesting options for SDMM that could be studied in more detail in the future. Finally, we discuss important aspects of supersymmetric models for DM and how these could help to develop of more complete SDMM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.06680v3-abstract-full').style.display = 'none'; document.getElementById('1607.06680v3-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 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.03349">arXiv:1604.03349</a> <span> [<a href="https://arxiv.org/pdf/1604.03349">pdf</a>, <a href="https://arxiv.org/ps/1604.03349">ps</a>, <a href="https://arxiv.org/format/1604.03349">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/10.1103/PhysRevD.93.082001">10.1103/PhysRevD.93.082001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the high-energy gamma-ray emission from the Moon with the Fermi Large Area Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/hep-ex?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Atwood%2C+W+B">W. B. Atwood</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+L">L. Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barbiellini%2C+G">G. Barbiellini</a>, <a href="/search/hep-ex?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/hep-ex?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/hep-ex?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/hep-ex?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/hep-ex?searchtype=author&query=Bonino%2C+R">R. Bonino</a>, <a href="/search/hep-ex?searchtype=author&query=Bottacini%2C+E">E. Bottacini</a>, <a href="/search/hep-ex?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/hep-ex?searchtype=author&query=Bruel%2C+P">P. Bruel</a>, <a href="/search/hep-ex?searchtype=author&query=Buehler%2C+R">R. Buehler</a>, <a href="/search/hep-ex?searchtype=author&query=Caliandro%2C+G+A">G. A. Caliandro</a>, <a href="/search/hep-ex?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/hep-ex?searchtype=author&query=Caragiulo%2C+M">M. Caragiulo</a>, <a href="/search/hep-ex?searchtype=author&query=Caraveo%2C+P+A">P. A. Caraveo</a>, <a href="/search/hep-ex?searchtype=author&query=Cavazzuti%2C+E">E. Cavazzuti</a>, <a href="/search/hep-ex?searchtype=author&query=Cecchi%2C+C">C. Cecchi</a>, <a href="/search/hep-ex?searchtype=author&query=Chekhtman%2C+A">A. Chekhtman</a>, <a href="/search/hep-ex?searchtype=author&query=Chiang%2C+J">J. Chiang</a>, <a href="/search/hep-ex?searchtype=author&query=Chiaro%2C+G">G. Chiaro</a>, <a href="/search/hep-ex?searchtype=author&query=Ciprini%2C+S">S. Ciprini</a> , et al. (90 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="1604.03349v2-abstract-short" style="display: inline;"> We have measured the gamma-ray emission spectrum of the Moon using the data collected by the Large Area Telescope onboard the Fermi satellite during its first 7 years of operation, in the energy range from 30 MeV up to a few GeV. We have also studied the time evolution of the flux, finding a correlation with the solar activity. We have developed a full Monte Carlo simulation describing the interac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.03349v2-abstract-full').style.display = 'inline'; document.getElementById('1604.03349v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.03349v2-abstract-full" style="display: none;"> We have measured the gamma-ray emission spectrum of the Moon using the data collected by the Large Area Telescope onboard the Fermi satellite during its first 7 years of operation, in the energy range from 30 MeV up to a few GeV. We have also studied the time evolution of the flux, finding a correlation with the solar activity. We have developed a full Monte Carlo simulation describing the interactions of cosmic rays with the lunar surface. The results of the present analysis can be explained in the framework of this model, where the production of gamma rays is due to the interactions of cosmic-ray proton and helium nuclei with the surface of the Moon. Finally, we have used our simulation to derive the cosmic-ray proton and helium spectra near Earth from the Moon gamma-ray data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.03349v2-abstract-full').style.display = 'none'; document.getElementById('1604.03349v2-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 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </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 by PRD, 16 pages, 11 figures, corresponding authors: F. Loparco and M. N. Mazziotta</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.02228">arXiv:1603.02228</a> <span> [<a href="https://arxiv.org/pdf/1603.02228">pdf</a>, <a href="https://arxiv.org/ps/1603.02228">ps</a>, <a href="https://arxiv.org/format/1603.02228">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/10.1016/j.physletb.2016.05.019">10.1016/j.physletb.2016.05.019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on Dark Matter Annihilation in the Sun using the ANTARES Neutrino Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+collaboration"> ANTARES collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Celli%2C+S">S. Celli</a>, <a href="/search/hep-ex?searchtype=author&query=Chiarusi%2C+T">T. Chiarusi</a>, <a href="/search/hep-ex?searchtype=author&query=Circella%2C+M">M. Circella</a>, <a href="/search/hep-ex?searchtype=author&query=Coleiro%2C+A">A. Coleiro</a> , et al. (95 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="1603.02228v2-abstract-short" style="display: inline;"> A search for muon neutrinos originating from dark matter annihilations in the Sun is performed using the data recorded by the ANTARES neutrino telescope from 2007 to 2012. In order to obtain the best possible sensitivities to dark matter signals, an optimisation of the event selection criteria is performed taking into account the background of atmospheric muons, atmospheric neutrinos and the energ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.02228v2-abstract-full').style.display = 'inline'; document.getElementById('1603.02228v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.02228v2-abstract-full" style="display: none;"> A search for muon neutrinos originating from dark matter annihilations in the Sun is performed using the data recorded by the ANTARES neutrino telescope from 2007 to 2012. In order to obtain the best possible sensitivities to dark matter signals, an optimisation of the event selection criteria is performed taking into account the background of atmospheric muons, atmospheric neutrinos and the energy spectra of the expected neutrino signals. No significant excess over the background is observed and $90\%$ C.L. upper limits on the neutrino flux, the spin--dependent and spin--independent WIMP-nucleon cross--sections are derived for WIMP masses ranging from $ \rm 50$ GeV to $\rm 5$ TeV for the annihilation channels $\rm WIMP + WIMP \to b \bar b, W^+ W^-$ and $\rm 蟿^+ 蟿^-$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.02228v2-abstract-full').style.display = 'none'; document.getElementById('1603.02228v2-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 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 4 figures, Submitted to Physics letters B</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 759, 10 August 2016, Pages 69 to 74 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.07000">arXiv:1602.07000</a> <span> [<a href="https://arxiv.org/pdf/1602.07000">pdf</a>, <a href="https://arxiv.org/format/1602.07000">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/10.1088/1475-7516/2016/05/016">10.1088/1475-7516/2016/05/016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for Secluded Dark Matter in the Sun with the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Bou-Cabo%2C+M">M. Bou-Cabo</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Celli%2C+S">S. Celli</a>, <a href="/search/hep-ex?searchtype=author&query=Chiarusi%2C+T">T. Chiarusi</a>, <a href="/search/hep-ex?searchtype=author&query=Circella%2C+M">M. Circella</a>, <a href="/search/hep-ex?searchtype=author&query=Coleiro%2C+A">A. Coleiro</a> , et al. (93 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="1602.07000v2-abstract-short" style="display: inline;"> A search for Secluded Dark Matter annihilation in the Sun using 2007-2012 data of the ANTARES neutrino telescope is presented. Three different cases are considered: a) detection of dimuons that result from the decay of the mediator, or neutrino detection from: b) mediator that decays into a dimuon and, in turn, into neutrinos, and c) mediator that decays directly into neutrinos. As no significant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.07000v2-abstract-full').style.display = 'inline'; document.getElementById('1602.07000v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.07000v2-abstract-full" style="display: none;"> A search for Secluded Dark Matter annihilation in the Sun using 2007-2012 data of the ANTARES neutrino telescope is presented. Three different cases are considered: a) detection of dimuons that result from the decay of the mediator, or neutrino detection from: b) mediator that decays into a dimuon and, in turn, into neutrinos, and c) mediator that decays directly into neutrinos. As no significant excess over background is observed, constraints are derived on the dark matter mass and the lifetime of the mediator. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.07000v2-abstract-full').style.display = 'none'; document.getElementById('1602.07000v2-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 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP05(2016)016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.07459">arXiv:1601.07459</a> <span> [<a href="https://arxiv.org/pdf/1601.07459">pdf</a>, <a href="https://arxiv.org/format/1601.07459">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 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> <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/10.1088/0954-3899/43/8/084001">10.1088/0954-3899/43/8/084001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Letter of Intent for KM3NeT 2.0 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Ageron%2C+M">M. Ageron</a>, <a href="/search/hep-ex?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Anassontzis%2C+E">E. Anassontzis</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Barbarino%2C+G">G. Barbarino</a>, <a href="/search/hep-ex?searchtype=author&query=Barbarito%2C+E">E. Barbarito</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/hep-ex?searchtype=author&query=Belias%2C+A">A. Belias</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Berg%2C+A+v+d">A. van den Berg</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Beurthey%2C+S">S. Beurthey</a>, <a href="/search/hep-ex?searchtype=author&query=van+Beveren%2C+V">V. van Beveren</a>, <a href="/search/hep-ex?searchtype=author&query=Beverini%2C+N">N. Beverini</a> , et al. (222 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="1601.07459v2-abstract-short" style="display: inline;"> The main objectives of the KM3NeT Collaboration are i) the discovery and subsequent observation of high-energy neutrino sources in the Universe and ii) the determination of the mass hierarchy of neutrinos. These objectives are strongly motivated by two recent important discoveries, namely: 1) The high-energy astrophysical neutrino signal reported by IceCube and 2) the sizable contribution of elect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.07459v2-abstract-full').style.display = 'inline'; document.getElementById('1601.07459v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.07459v2-abstract-full" style="display: none;"> The main objectives of the KM3NeT Collaboration are i) the discovery and subsequent observation of high-energy neutrino sources in the Universe and ii) the determination of the mass hierarchy of neutrinos. These objectives are strongly motivated by two recent important discoveries, namely: 1) The high-energy astrophysical neutrino signal reported by IceCube and 2) the sizable contribution of electron neutrinos to the third neutrino mass eigenstate as reported by Daya Bay, Reno and others. To meet these objectives, the KM3NeT Collaboration plans to build a new Research Infrastructure consisting of a network of deep-sea neutrino telescopes in the Mediterranean Sea. A phased and distributed implementation is pursued which maximises the access to regional funds, the availability of human resources and the synergetic opportunities for the earth and sea sciences community. Three suitable deep-sea sites are identified, namely off-shore Toulon (France), Capo Passero (Italy) and Pylos (Greece). The infrastructure will consist of three so-called building blocks. A building block comprises 115 strings, each string comprises 18 optical modules and each optical module comprises 31 photo-multiplier tubes. Each building block thus constitutes a 3-dimensional array of photo sensors that can be used to detect the Cherenkov light produced by relativistic particles emerging from neutrino interactions. Two building blocks will be configured to fully explore the IceCube signal with different methodology, improved resolution and complementary field of view, including the Galactic plane. One building block will be configured to precisely measure atmospheric neutrino oscillations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.07459v2-abstract-full').style.display = 'none'; document.getElementById('1601.07459v2-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 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2016. </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">119 pages, published version, revised Eq. 6, 7</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Physics G: Nuclear and Particle Physics, 43 (8), 084001, 2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.02149">arXiv:1511.02149</a> <span> [<a href="https://arxiv.org/pdf/1511.02149">pdf</a>, <a href="https://arxiv.org/format/1511.02149">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/10.3847/0004-637X/823/1/65">10.3847/0004-637X/823/1/65 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First combined search for neutrino point-sources in the Southern Hemisphere with the ANTARES and IceCube neutrino telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Chiarusi%2C+T">T. Chiarusi</a>, <a href="/search/hep-ex?searchtype=author&query=Circella%2C+M">M. Circella</a>, <a href="/search/hep-ex?searchtype=author&query=Coniglione%2C+R">R. Coniglione</a>, <a href="/search/hep-ex?searchtype=author&query=Costantini%2C+H">H. Costantini</a>, <a href="/search/hep-ex?searchtype=author&query=Coyle%2C+P">P. Coyle</a> , et al. (405 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="1511.02149v1-abstract-short" style="display: inline;"> We present the results of searches for point-like sources of neutrinos based on the first combined analysis of data from both the ANTARES and IceCube neutrino telescopes. The combination of both detectors which differ in size and location forms a window in the Southern sky where the sensitivity to point sources improves by up to a factor of two compared to individual analyses. Using data recorded… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02149v1-abstract-full').style.display = 'inline'; document.getElementById('1511.02149v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.02149v1-abstract-full" style="display: none;"> We present the results of searches for point-like sources of neutrinos based on the first combined analysis of data from both the ANTARES and IceCube neutrino telescopes. The combination of both detectors which differ in size and location forms a window in the Southern sky where the sensitivity to point sources improves by up to a factor of two compared to individual analyses. Using data recorded by ANTARES from 2007 to 2012, and by IceCube from 2008 to 2011, we search for sources of neutrino emission both across the Southern sky and from a pre-selected list of candidate objects. No significant excess over background has been found in these searches, and flux upper limits for the candidate sources are presented for $E^{-2.5}$ and $E^{-2}$ power-law spectra with different energy cut-offs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02149v1-abstract-full').style.display = 'none'; document.getElementById('1511.02149v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </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. Submitted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys. J. 823:65,2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.01561">arXiv:1510.01561</a> <span> [<a href="https://arxiv.org/pdf/1510.01561">pdf</a>, <a href="https://arxiv.org/format/1510.01561">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/10.1140/epjc/s10052-015-3868-9">10.1140/epjc/s10052-015-3868-9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The prototype detection unit of the KM3NeT detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KM3NeT+Collaboration"> KM3NeT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Ageron%2C+M">M. Ageron</a>, <a href="/search/hep-ex?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Anassontzis%2C+E+G">E. G. Anassontzis</a>, <a href="/search/hep-ex?searchtype=author&query=Androulakis%2C+G+C">G. C. Androulakis</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Anvar%2C+S">S. Anvar</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/hep-ex?searchtype=author&query=Balasi%2C+K">K. Balasi</a>, <a href="/search/hep-ex?searchtype=author&query=Band%2C+H">H. Band</a>, <a href="/search/hep-ex?searchtype=author&query=Barbarino%2C+G">G. Barbarino</a>, <a href="/search/hep-ex?searchtype=author&query=Barbarito%2C+E">E. Barbarito</a>, <a href="/search/hep-ex?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Baron%2C+S">S. Baron</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios%2C+J">J. Barrios</a>, <a href="/search/hep-ex?searchtype=author&query=Belias%2C+A">A. Belias</a>, <a href="/search/hep-ex?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/hep-ex?searchtype=author&query=Berg%2C+A+M+v+d">A. M. van den Berg</a> , et al. (224 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="1510.01561v2-abstract-short" style="display: inline;"> A prototype detection unit of the KM3NeT deep-sea neutrino telescope has been installed at 3500m depth 80km offshore the Italian coast. KM3NeT in its final configuration will contain several hundreds of detection units. Each detection unit is a mechanical structure anchored to the sea floor, held vertical by a submerged buoy and supporting optical modules for the detection of Cherenkov light emitt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.01561v2-abstract-full').style.display = 'inline'; document.getElementById('1510.01561v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.01561v2-abstract-full" style="display: none;"> A prototype detection unit of the KM3NeT deep-sea neutrino telescope has been installed at 3500m depth 80km offshore the Italian coast. KM3NeT in its final configuration will contain several hundreds of detection units. Each detection unit is a mechanical structure anchored to the sea floor, held vertical by a submerged buoy and supporting optical modules for the detection of Cherenkov light emitted by charged secondary particles emerging from neutrino interactions. This prototype string implements three optical modules with 31 photomultiplier tubes each. These optical modules were developed by the KM3NeT Collaboration to enhance the detection capability of neutrino interactions. The prototype detection unit was operated since its deployment in May 2014 until its decommissioning in July 2015. Reconstruction of the particle trajectories from the data requires a nanosecond accuracy in the time calibration. A procedure for relative time calibration of the photomultiplier tubes contained in each optical module is described. This procedure is based on the measured coincidences produced in the sea by the 40K background light and can easily be expanded to a detector with several thousands of optical modules. The time offsets between the different optical modules are obtained using LED nanobeacons mounted inside them. A set of data corresponding to 600 hours of livetime was analysed. The results show good agreement with Monte Carlo simulations of the expected optical background and the signal from atmospheric muons. An almost background-free sample of muons was selected by filtering the time correlated signals on all the three optical modules. The zenith angle of the selected muons was reconstructed with a precision of about 3掳. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.01561v2-abstract-full').style.display = 'none'; document.getElementById('1510.01561v2-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 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </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 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 (2016) 76:54 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.04182">arXiv:1507.04182</a> <span> [<a href="https://arxiv.org/pdf/1507.04182">pdf</a>, <a href="https://arxiv.org/ps/1507.04182">ps</a>, <a href="https://arxiv.org/format/1507.04182">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 Detectors">physics.ins-det</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/10.1016/j.astropartphys.2016.02.001">10.1016/j.astropartphys.2016.02.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bogazzi%2C+C">C. Bogazzi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Bou-Cabo%2C+M">M. Bou-Cabo</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Chiarusi%2C+T">T. Chiarusi</a>, <a href="/search/hep-ex?searchtype=author&query=Circella%2C+M">M. Circella</a>, <a href="/search/hep-ex?searchtype=author&query=Coniglione%2C+R">R. Coniglione</a>, <a href="/search/hep-ex?searchtype=author&query=Costantini%2C+H">H. Costantini</a> , et al. (105 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="1507.04182v1-abstract-short" style="display: inline;"> The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of $\sim$10 TeV the muon and the incident neutrino are almost c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.04182v1-abstract-full').style.display = 'inline'; document.getElementById('1507.04182v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.04182v1-abstract-full" style="display: none;"> The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of $\sim$10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.04182v1-abstract-full').style.display = 'none'; document.getElementById('1507.04182v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2015. </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 Astroparticle Physics (17 pages, 11 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/1503.02632">arXiv:1503.02632</a> <span> [<a href="https://arxiv.org/pdf/1503.02632">pdf</a>, <a href="https://arxiv.org/format/1503.02632">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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/809/1/L4">10.1088/2041-8205/809/1/L4 <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 Emission from DES Dwarf Spheroidal Galaxy Candidates with Fermi-LAT Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+F">The Fermi-LAT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/hep-ex?searchtype=author&query=Wood%2C+M">M. Wood</a>, <a href="/search/hep-ex?searchtype=author&query=Strigari%2C+L">L. Strigari</a>, <a href="/search/hep-ex?searchtype=author&query=Sanchez-Conde%2C+M">M. Sanchez-Conde</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+L">L. Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Essig%2C+R">R. Essig</a>, <a href="/search/hep-ex?searchtype=author&query=Cohen-Tanugi%2C+J">J. Cohen-Tanugi</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+B">B. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/hep-ex?searchtype=author&query=Bloom%2C+E+D">E. D. Bloom</a>, <a href="/search/hep-ex?searchtype=author&query=Caputo%2C+R">R. Caputo</a>, <a href="/search/hep-ex?searchtype=author&query=Cecchi%2C+C">C. Cecchi</a>, <a href="/search/hep-ex?searchtype=author&query=Charles%2C+E">E. Charles</a>, <a href="/search/hep-ex?searchtype=author&query=Chiang%2C+J">J. Chiang</a>, <a href="/search/hep-ex?searchtype=author&query=de+Angelis%2C+A">A. de Angelis</a>, <a href="/search/hep-ex?searchtype=author&query=Funk%2C+S">S. Funk</a>, <a href="/search/hep-ex?searchtype=author&query=Fusco%2C+P">P. Fusco</a>, <a href="/search/hep-ex?searchtype=author&query=Gargano%2C+F">F. Gargano</a>, <a href="/search/hep-ex?searchtype=author&query=Giglietto%2C+N">N. Giglietto</a>, <a href="/search/hep-ex?searchtype=author&query=Giordano%2C+F">F. Giordano</a> , et al. (102 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="1503.02632v3-abstract-short" style="display: inline;"> Due to their proximity, high dark-matter content, and apparent absence of non-thermal processes, Milky Way dwarf spheroidal satellite galaxies (dSphs) are excellent targets for the indirect detection of dark matter. Recently, eight new dSph candidates were discovered using the first year of data from the Dark Energy Survey (DES). We searched for gamma-ray emission coincident with the positions of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02632v3-abstract-full').style.display = 'inline'; document.getElementById('1503.02632v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.02632v3-abstract-full" style="display: none;"> Due to their proximity, high dark-matter content, and apparent absence of non-thermal processes, Milky Way dwarf spheroidal satellite galaxies (dSphs) are excellent targets for the indirect detection of dark matter. Recently, eight new dSph candidates were discovered using the first year of data from the Dark Energy Survey (DES). We searched for gamma-ray emission coincident with the positions of these new objects in six years of Fermi Large Area Telescope data. We found no significant excesses of gamma-ray emission. Under the assumption that the DES candidates are dSphs with dark matter halo properties similar to the known dSphs, we computed individual and combined limits on the velocity-averaged dark matter annihilation cross section for these new targets. If the estimated dark-matter content of these dSph candidates is confirmed, they will constrain the annihilation cross section to lie below the thermal relic cross section for dark matter particles with masses < 20 GeV annihilating via the b-bbar or tau+tau- channels. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02632v3-abstract-full').style.display = 'none'; document.getElementById('1503.02632v3-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 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 4 figures, 1 table. Updated to published version. Readers may be interested in the related work by Ackermann et al. arXiv:1503.02641 (The Fermi-LAT Collaboration), Bechtol, Drlica-Wagner, et al. arXiv:1503.02584 (The DES Collaboration), and Koposov, Belokurov, Torrealba, & Evans arXiv:1503.02079</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-15-082-AE </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 809 L4 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1402.6182">arXiv:1402.6182</a> <span> [<a href="https://arxiv.org/pdf/1402.6182">pdf</a>, <a href="https://arxiv.org/ps/1402.6182">ps</a>, <a href="https://arxiv.org/format/1402.6182">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="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/10.1088/2041-8205/786/1/L5">10.1088/2041-8205/786/1/L5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searches for Point-like and extended neutrino sources close to the Galactic Centre using the ANTARES neutrino Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bogazzi%2C+C">C. Bogazzi</a>, <a href="/search/hep-ex?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/hep-ex?searchtype=author&query=Bou-Cabo%2C+M">M. Bou-Cabo</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/hep-ex?searchtype=author&query=C%C3%A2rloganu%2C+C">C. C芒rloganu</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Chiarusi%2C+T">T. Chiarusi</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="1402.6182v1-abstract-short" style="display: inline;"> A search for cosmic neutrino sources using six years of data collected by the ANTARES neutrino telescope has been performed. Clusters of muon neutrinos over the expected atmospheric background have been looked for. No clear signal has been found. The most signal-like accumulation of events is located at equatorial coordinates RA=$-$46.8$^{\circ}$ and Dec=$-$64.9$^{\circ}$ and corresponds to a 2.2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.6182v1-abstract-full').style.display = 'inline'; document.getElementById('1402.6182v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1402.6182v1-abstract-full" style="display: none;"> A search for cosmic neutrino sources using six years of data collected by the ANTARES neutrino telescope has been performed. Clusters of muon neutrinos over the expected atmospheric background have been looked for. No clear signal has been found. The most signal-like accumulation of events is located at equatorial coordinates RA=$-$46.8$^{\circ}$ and Dec=$-$64.9$^{\circ}$ and corresponds to a 2.2$蟽$ background fluctuation. In addition, upper limits on the flux normalization of an E$^{-2}$ muon neutrino energy spectrum have been set for 50 pre-selected astrophysical objects. Finally, motivated by an accumulation of 7 events relatively close to the Galactic Centre in the recently reported neutrino sample of the IceCube telescope, a search for point sources in a broad region around this accumulation has been carried out. No indication of a neutrino signal has been found in the ANTARES data and upper limits on the flux normalization of an E$^{-2}$ energy spectrum of neutrinos from point sources in that region have been set. The 90% confidence level upper limits on the muon neutrino flux normalization vary between 3.5 and 5.1$\times$10$^{-8}$ GeV$\,$cm$^{-2}$s$^{-1}$, depending on the exact location of the source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.6182v1-abstract-full').style.display = 'none'; document.getElementById('1402.6182v1-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 February, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2014. </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 ApJL. 18 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/1310.0828">arXiv:1310.0828</a> <span> [<a href="https://arxiv.org/pdf/1310.0828">pdf</a>, <a href="https://arxiv.org/format/1310.0828">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/10.1103/PhysRevD.89.042001">10.1103/PhysRevD.89.042001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dark Matter Constraints from Observations of 25 Milky Way Satellite Galaxies with the Fermi Large Area Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+F">The Fermi-LAT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+B">B. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+L">L. Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Ballet%2C+J">J. Ballet</a>, <a href="/search/hep-ex?searchtype=author&query=Barbiellini%2C+G">G. Barbiellini</a>, <a href="/search/hep-ex?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/hep-ex?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/hep-ex?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/hep-ex?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/hep-ex?searchtype=author&query=Bloom%2C+E+D">E. D. Bloom</a>, <a href="/search/hep-ex?searchtype=author&query=Bonamente%2C+E">E. Bonamente</a>, <a href="/search/hep-ex?searchtype=author&query=Bouvier%2C+A">A. Bouvier</a>, <a href="/search/hep-ex?searchtype=author&query=Brandt%2C+T+J">T. J. Brandt</a>, <a href="/search/hep-ex?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a>, <a href="/search/hep-ex?searchtype=author&query=Brigida%2C+M">M. Brigida</a>, <a href="/search/hep-ex?searchtype=author&query=Bruel%2C+P">P. Bruel</a>, <a href="/search/hep-ex?searchtype=author&query=Buehler%2C+R">R. Buehler</a>, <a href="/search/hep-ex?searchtype=author&query=Buson%2C+S">S. Buson</a>, <a href="/search/hep-ex?searchtype=author&query=Caliandro%2C+G+A">G. A. Caliandro</a>, <a href="/search/hep-ex?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/hep-ex?searchtype=author&query=Caragiulo%2C+M">M. Caragiulo</a>, <a href="/search/hep-ex?searchtype=author&query=Caraveo%2C+P+A">P. A. Caraveo</a> , et al. (98 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="1310.0828v2-abstract-short" style="display: inline;"> The dwarf spheroidal satellite galaxies of the Milky Way are some of the most dark-matter-dominated objects known. Due to their proximity, high dark matter content, and lack of astrophysical backgrounds, dwarf spheroidal galaxies are widely considered to be among the most promising targets for the indirect detection of dark matter via gamma rays. Here we report on gamma-ray observations of 25 Milk… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.0828v2-abstract-full').style.display = 'inline'; document.getElementById('1310.0828v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.0828v2-abstract-full" style="display: none;"> The dwarf spheroidal satellite galaxies of the Milky Way are some of the most dark-matter-dominated objects known. Due to their proximity, high dark matter content, and lack of astrophysical backgrounds, dwarf spheroidal galaxies are widely considered to be among the most promising targets for the indirect detection of dark matter via gamma rays. Here we report on gamma-ray observations of 25 Milky Way dwarf spheroidal satellite galaxies based on 4 years of Fermi Large Area Telescope (LAT) data. None of the dwarf galaxies are significantly detected in gamma rays, and we present gamma-ray flux upper limits between 500 MeV and 500 GeV. We determine the dark matter content of 18 dwarf spheroidal galaxies from stellar kinematic data and combine LAT observations of 15 dwarf galaxies to constrain the dark matter annihilation cross section. We set some of the tightest constraints to date on the the annihilation of dark matter particles with masses between 2 GeV and 10 TeV into prototypical Standard Model channels. We find these results to be robust against systematic uncertainties in the LAT instrument performance, diffuse gamma-ray background modeling, and assumed dark matter density profile. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.0828v2-abstract-full').style.display = 'none'; document.getElementById('1310.0828v2-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 February, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2013. </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">47 pages, 8 figure, and 8 tables. Contact authors: Johann Cohen-Tanugi, Jan Conrad, Alex Drlica-Wagner, Maja Llena Garde, and Nicola Mazziotta</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 89, 042001 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.3105">arXiv:1207.3105</a> <span> [<a href="https://arxiv.org/pdf/1207.3105">pdf</a>, <a href="https://arxiv.org/ps/1207.3105">ps</a>, <a href="https://arxiv.org/format/1207.3105">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/10.1088/0004-637X/760/1/53">10.1088/0004-637X/760/1/53 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Cosmic Neutrino Point Sources with Four Years of Data from the ANTARES Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+Collaboration"> ANTARES Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/hep-ex?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Anvar%2C+S">S. Anvar</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Astraatmadja%2C+T">T. Astraatmadja</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/hep-ex?searchtype=author&query=Bogazzi%2C+C">C. Bogazzi</a>, <a href="/search/hep-ex?searchtype=author&query=Bou-Cabo%2C+M">M. Bou-Cabo</a>, <a href="/search/hep-ex?searchtype=author&query=Bouhou%2C+B">B. Bouhou</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Carloganu%2C+C">C. Carloganu</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a> , et al. (132 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="1207.3105v2-abstract-short" style="display: inline;"> In this paper, a time integrated search for point sources of cosmic neutrinos is presented using the data collected from 2007 to 2010 by the ANTARES neutrino telescope. No statistically significant signal has been found and upper limits on the neutrino flux have been obtained. Assuming an $E_谓^{-2}$ spectrum, these flux limits are at $1-10\times10^{-8}$ GeV cm$^{-2}$ s$^{-1}$ for declinations rang… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.3105v2-abstract-full').style.display = 'inline'; document.getElementById('1207.3105v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.3105v2-abstract-full" style="display: none;"> In this paper, a time integrated search for point sources of cosmic neutrinos is presented using the data collected from 2007 to 2010 by the ANTARES neutrino telescope. No statistically significant signal has been found and upper limits on the neutrino flux have been obtained. Assuming an $E_谓^{-2}$ spectrum, these flux limits are at $1-10\times10^{-8}$ GeV cm$^{-2}$ s$^{-1}$ for declinations ranging from $-90^{\circ}$ to 40$^{\circ}$. Limits for specific models of RX J1713.7-3946 and Vela X, which include information on the source morphology and spectrum, are also given. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.3105v2-abstract-full').style.display = 'none'; document.getElementById('1207.3105v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </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">30 pages, 13 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1206.0645">arXiv:1206.0645</a> <span> [<a href="https://arxiv.org/pdf/1206.0645">pdf</a>, <a href="https://arxiv.org/ps/1206.0645">ps</a>, <a href="https://arxiv.org/format/1206.0645">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> </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.2012.07.002">10.1016/j.physletb.2012.07.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of Atmospheric Neutrino Oscillations with the ANTARES Neutrino Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=ANTARES+collaboration"> ANTARES collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Adrian-Martinez%2C+S">S. Adrian-Martinez</a>, <a href="/search/hep-ex?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Anvar%2C+S">S. Anvar</a>, <a href="/search/hep-ex?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/hep-ex?searchtype=author&query=Astraatmadja%2C+T">T. Astraatmadja</a>, <a href="/search/hep-ex?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/hep-ex?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/hep-ex?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/hep-ex?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/hep-ex?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/hep-ex?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/hep-ex?searchtype=author&query=Bogazzi%2C+C">C. Bogazzi</a>, <a href="/search/hep-ex?searchtype=author&query=Bou-Cabo%2C+M">M. Bou-Cabo</a>, <a href="/search/hep-ex?searchtype=author&query=Bouhou%2C+B">B. Bouhou</a>, <a href="/search/hep-ex?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/hep-ex?searchtype=author&query=Carloganu%2C+C">C. Carloganu</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+J">J. Carr</a> , et al. (135 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="1206.0645v2-abstract-short" style="display: inline;"> The data taken with the ANTARES neutrino telescope from 2007 to 2010, a total live time of 863 days, are used to measure the oscillation parameters of atmospheric neutrinos. Muon tracks are reconstructed with energies as low as 20 GeV. Neutrino oscillations will cause a suppression of vertical upgoing muon neutrinos of such energies crossing the Earth. The parameters determining the oscillation of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.0645v2-abstract-full').style.display = 'inline'; document.getElementById('1206.0645v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1206.0645v2-abstract-full" style="display: none;"> The data taken with the ANTARES neutrino telescope from 2007 to 2010, a total live time of 863 days, are used to measure the oscillation parameters of atmospheric neutrinos. Muon tracks are reconstructed with energies as low as 20 GeV. Neutrino oscillations will cause a suppression of vertical upgoing muon neutrinos of such energies crossing the Earth. The parameters determining the oscillation of atmospheric neutrinos are extracted by fitting the event rate as a function of the ratio of the estimated neutrino energy and reconstructed flight path through the Earth. Measurement contours of the oscillation parameters in a two-flavour approximation are derived. Assuming maximum mixing, a mass difference of $螖m_{32}^2=(3.1\pm 0.9)\cdot 10^{-3}$ eV$^2$ is obtained, in good agreement with the world average value. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.0645v2-abstract-full').style.display = 'none'; document.getElementById('1206.0645v2-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 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 June, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1205.2739">arXiv:1205.2739</a> <span> [<a href="https://arxiv.org/pdf/1205.2739">pdf</a>, <a href="https://arxiv.org/format/1205.2739">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.86.022002">10.1103/PhysRevD.86.022002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fermi LAT Search for Dark Matter in Gamma-ray Lines and the Inclusive Photon Spectrum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+F">Fermi-LAT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/hep-ex?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+L">L. Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barbiellini%2C+G">G. Barbiellini</a>, <a href="/search/hep-ex?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/hep-ex?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/hep-ex?searchtype=author&query=Berenji%2C+B">B. Berenji</a>, <a href="/search/hep-ex?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/hep-ex?searchtype=author&query=Bloom%2C+E+D">E. D. Bloom</a>, <a href="/search/hep-ex?searchtype=author&query=Bonamente%2C+E">E. Bonamente</a>, <a href="/search/hep-ex?searchtype=author&query=Borgland%2C+A+W">A. W. Borgland</a>, <a href="/search/hep-ex?searchtype=author&query=Brigida%2C+M">M. Brigida</a>, <a href="/search/hep-ex?searchtype=author&query=Buehler%2C+R">R. Buehler</a>, <a href="/search/hep-ex?searchtype=author&query=Buson%2C+S">S. Buson</a>, <a href="/search/hep-ex?searchtype=author&query=Caliandro%2C+G+A">G. A. Caliandro</a>, <a href="/search/hep-ex?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/hep-ex?searchtype=author&query=Caraveo%2C+P+A">P. A. Caraveo</a>, <a href="/search/hep-ex?searchtype=author&query=Casandjian%2C+J+M">J. M. Casandjian</a>, <a href="/search/hep-ex?searchtype=author&query=Cecchi%2C+C">C. Cecchi</a>, <a href="/search/hep-ex?searchtype=author&query=Charles%2C+E">E. Charles</a>, <a href="/search/hep-ex?searchtype=author&query=Chekhtman%2C+A">A. Chekhtman</a>, <a href="/search/hep-ex?searchtype=author&query=Chiang%2C+J">J. Chiang</a> , et al. (96 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="1205.2739v1-abstract-short" style="display: inline;"> Dark matter particle annihilation or decay can produce monochromatic gamma-ray lines and contribute to the diffuse gamma-ray background. Flux upper limits are presented for gamma-ray spectral lines from 7 to 200 GeV and for the diffuse gamma-ray background from 4.8 GeV to 264 GeV obtained from two years of Fermi Large Area Telescope data integrated over most of the sky. We give cross section upper… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.2739v1-abstract-full').style.display = 'inline'; document.getElementById('1205.2739v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1205.2739v1-abstract-full" style="display: none;"> Dark matter particle annihilation or decay can produce monochromatic gamma-ray lines and contribute to the diffuse gamma-ray background. Flux upper limits are presented for gamma-ray spectral lines from 7 to 200 GeV and for the diffuse gamma-ray background from 4.8 GeV to 264 GeV obtained from two years of Fermi Large Area Telescope data integrated over most of the sky. We give cross section upper limits and decay lifetime lower limits for dark matter models that produce gamma-ray lines or contribute to the diffuse spectrum, including models proposed as explanations of the PAMELA and Fermi cosmic-ray data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.2739v1-abstract-full').style.display = 'none'; document.getElementById('1205.2739v1-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 May, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2012. </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 Physical Review D</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" 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