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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=Anthony%2C+L&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Anthony%2C+L&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Anthony%2C+L&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/2409.19633">arXiv:2409.19633</a> <span> [<a href="https://arxiv.org/pdf/2409.19633">pdf</a>, <a href="https://arxiv.org/format/2409.19633">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 proton decay via $p\rightarrow{e^+畏}$ and $p\rightarrow{渭^+畏}$ with a 0.37 Mton-year exposure of Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Taniuchi%2C+N">N. Taniuchi</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Harada%2C+M">M. Harada</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a> , et al. (267 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="2409.19633v1-abstract-short" style="display: inline;"> A search for proton decay into $e^+/渭^+$ and a $畏$ meson has been performed using data from a 0.373 Mton$\cdot$year exposure (6050.3 live days) of Super-Kamiokande. Compared to previous searches this work introduces an improved model of the intranuclear $畏$ interaction cross section, resulting in a factor of two reduction in uncertainties from this source and $\sim$10\% increase in signal efficien… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19633v1-abstract-full').style.display = 'inline'; document.getElementById('2409.19633v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.19633v1-abstract-full" style="display: none;"> A search for proton decay into $e^+/渭^+$ and a $畏$ meson has been performed using data from a 0.373 Mton$\cdot$year exposure (6050.3 live days) of Super-Kamiokande. Compared to previous searches this work introduces an improved model of the intranuclear $畏$ interaction cross section, resulting in a factor of two reduction in uncertainties from this source and $\sim$10\% increase in signal efficiency. No significant data excess was found above the expected number of atmospheric neutrino background events resulting in no indication of proton decay into either mode. Lower limits on the proton partial lifetime of $1.4\times\mathrm{10^{34}~years}$ for $p\rightarrow e^+畏$ and $7.3\times\mathrm{10^{33}~years}$ for $p\rightarrow 渭^+畏$ at the 90$\%$ C.L. were set. These limits are around 1.5 times longer than our previous study and are the most stringent to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19633v1-abstract-full').style.display = 'none'; document.getElementById('2409.19633v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.12488">arXiv:2405.12488</a> <span> [<a href="https://arxiv.org/pdf/2405.12488">pdf</a>, <a href="https://arxiv.org/format/2405.12488">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"> First joint oscillation analysis of Super-Kamiokande atmospheric and T2K accelerator neutrino data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Super-Kamiokande"> Super-Kamiokande</a>, <a href="/search/hep-ex?searchtype=author&query=collaborations%2C+T">T2K collaborations</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akhlaq%2C+N">N. Akhlaq</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Alarakia-Charles%2C+H">H. Alarakia-Charles</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Hakim%2C+Y+I+A">Y. I. Alj Hakim</a>, <a href="/search/hep-ex?searchtype=author&query=Monsalve%2C+S+A">S. Alonso Monsalve</a>, <a href="/search/hep-ex?searchtype=author&query=Amanai%2C+S">S. Amanai</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L+H+V">L. H. V. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Apte%2C+K+A">K. A. Apte</a>, <a href="/search/hep-ex?searchtype=author&query=Arai%2C+T">T. Arai</a>, <a href="/search/hep-ex?searchtype=author&query=Arihara%2C+T">T. Arihara</a>, <a href="/search/hep-ex?searchtype=author&query=Arimoto%2C+S">S. Arimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/hep-ex?searchtype=author&query=Asaka%2C+R">R. Asaka</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Babu%2C+N">N. Babu</a> , et al. (524 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.12488v2-abstract-short" style="display: inline;"> The Super-Kamiokande and T2K collaborations present a joint measurement of neutrino oscillation parameters from their atmospheric and beam neutrino data. It uses a common interaction model for events overlapping in neutrino energy and correlated detector systematic uncertainties between the two datasets, which are found to be compatible. Using 3244.4 days of atmospheric data and a beam exposure of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12488v2-abstract-full').style.display = 'inline'; document.getElementById('2405.12488v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12488v2-abstract-full" style="display: none;"> The Super-Kamiokande and T2K collaborations present a joint measurement of neutrino oscillation parameters from their atmospheric and beam neutrino data. It uses a common interaction model for events overlapping in neutrino energy and correlated detector systematic uncertainties between the two datasets, which are found to be compatible. Using 3244.4 days of atmospheric data and a beam exposure of $19.7(16.3) \times 10^{20}$ protons on target in (anti)neutrino mode, the analysis finds a 1.9$蟽$ exclusion of CP-conservation (defined as $J_{CP}=0$) and a preference for the normal mass ordering. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12488v2-abstract-full').style.display = 'none'; document.getElementById('2405.12488v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 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/2404.09920">arXiv:2404.09920</a> <span> [<a href="https://arxiv.org/pdf/2404.09920">pdf</a>, <a href="https://arxiv.org/format/2404.09920">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 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/10.3847/1538-4357/ad5fee">10.3847/1538-4357/ad5fee <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combined Pre-Supernova Alert System with Kamland and Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KamLAND"> KamLAND</a>, <a href="/search/hep-ex?searchtype=author&query=Collaborations%2C+S">Super-Kamiokande Collaborations</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+S">Seisho Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Eizuka%2C+M">Minori Eizuka</a>, <a href="/search/hep-ex?searchtype=author&query=Futagi%2C+S">Sawako Futagi</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">Azusa Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Yoshihito Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+S">Shun Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">Takahiko Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">Kazumi Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">Koichi Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">Sei Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">Haruo Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">Kunio Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">Koji Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Yuto Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">Nanami Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Yasuhiro Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">Masayuki Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Kurasawa%2C+M">Maho Kurasawa</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">Tadao Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">Haruhiko Miyake</a>, <a href="/search/hep-ex?searchtype=author&query=Morita%2C+D">Daisuke Morita</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+T">Takeshi Nakahata</a> , et al. (290 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.09920v3-abstract-short" style="display: inline;"> Preceding a core-collapse supernova, various processes produce an increasing amount of neutrinos of all flavors characterized by mounting energies from the interior of massive stars. Among them, the electron antineutrinos are potentially detectable by terrestrial neutrino experiments such as KamLAND and Super-Kamiokande via inverse beta decay interactions. Once these pre-supernova neutrinos are ob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09920v3-abstract-full').style.display = 'inline'; document.getElementById('2404.09920v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.09920v3-abstract-full" style="display: none;"> Preceding a core-collapse supernova, various processes produce an increasing amount of neutrinos of all flavors characterized by mounting energies from the interior of massive stars. Among them, the electron antineutrinos are potentially detectable by terrestrial neutrino experiments such as KamLAND and Super-Kamiokande via inverse beta decay interactions. Once these pre-supernova neutrinos are observed, an early warning of the upcoming core-collapse supernova can be provided. In light of this, KamLAND and Super-Kamiokande, both located in the Kamioka mine in Japan, have been monitoring pre-supernova neutrinos since 2015 and 2021, respectively. Recently, we performed a joint study between KamLAND and Super-Kamiokande on pre-supernova neutrino detection. A pre-supernova alert system combining the KamLAND detector and the Super-Kamiokande detector was developed and put into operation, which can provide a supernova alert to the astrophysics community. Fully leveraging the complementary properties of these two detectors, the combined alert is expected to resolve a pre-supernova neutrino signal from a 15 M$_{\odot}$ star within 510 pc of the Earth, at a significance level corresponding to a false alarm rate of no more than 1 per century. For a Betelgeuse-like model with optimistic parameters, it can provide early warnings up to 12 hours in advance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09920v3-abstract-full').style.display = 'none'; document.getElementById('2404.09920v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Resubmitted to ApJ. 22 pages, 16 figures, for more information about the combined pre-supernova alert system, see https://www.lowbg.org/presnalarm/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.08725">arXiv:2404.08725</a> <span> [<a href="https://arxiv.org/pdf/2404.08725">pdf</a>, <a href="https://arxiv.org/format/2404.08725">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="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/10.1093/ptep/ptae128">10.1093/ptep/ptae128 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Development of a data overflow protection system for Super-Kamiokande to maximize data from nearby supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Mori%2C+M">M. Mori</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiba%2C+H">H. Shiba</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+K">K. Shimizu</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="2404.08725v2-abstract-short" style="display: inline;"> Neutrinos from very nearby supernovae, such as Betelgeuse, are expected to generate more than ten million events over 10\,s in Super-Kamokande (SK). At such large event rates, the buffers of the SK analog-to-digital conversion board (QBEE) will overflow, causing random loss of data that is critical for understanding the dynamics of the supernova explosion mechanism. In order to solve this problem,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08725v2-abstract-full').style.display = 'inline'; document.getElementById('2404.08725v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.08725v2-abstract-full" style="display: none;"> Neutrinos from very nearby supernovae, such as Betelgeuse, are expected to generate more than ten million events over 10\,s in Super-Kamokande (SK). At such large event rates, the buffers of the SK analog-to-digital conversion board (QBEE) will overflow, causing random loss of data that is critical for understanding the dynamics of the supernova explosion mechanism. In order to solve this problem, two new DAQ modules were developed to aid in the observation of very nearby supernovae. The first of these, the SN module, is designed to save only the number of hit PMTs during a supernova burst and the second, the Veto module, prescales the high rate neutrino events to prevent the QBEE from overflowing based on information from the SN module. In the event of a very nearby supernova, these modules allow SK to reconstruct the time evolution of the neutrino event rate from beginning to end using both QBEE and SN module data. This paper presents the development and testing of these modules together with an analysis of supernova-like data generated with a flashing laser diode. We demonstrate that the Veto module successfully prevents DAQ overflows for Betelgeuse-like supernovae as well as the long-term stability of the new modules. During normal running the Veto module is found to issue DAQ vetos a few times per month resulting in a total dead time less than 1\,ms, and does not influence ordinary operations. Additionally, using simulation data we find that supernovae closer than 800~pc will trigger Veto module resulting in a prescaling of the observed neutrino data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08725v2-abstract-full').style.display = 'none'; document.getElementById('2404.08725v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 18 figures. Submitted to PTEP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.08619">arXiv:2403.08619</a> <span> [<a href="https://arxiv.org/pdf/2403.08619">pdf</a>, <a href="https://arxiv.org/format/2403.08619">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/10.1103/PhysRevD.110.082008">10.1103/PhysRevD.110.082008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of the charge ratio and polarization of cosmic-ray muons with the Super-Kamiokande detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Kitagawa%2C+H">H. Kitagawa</a>, <a href="/search/hep-ex?searchtype=author&query=Tada%2C+T">T. Tada</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a> , et al. (231 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="2403.08619v2-abstract-short" style="display: inline;"> We present the results of the charge ratio ($R$) and polarization ($P^渭_{0}$) measurements using the decay electron events collected from 2008 September to 2022 June by the Super-Kamiokande detector. Because of its underground location and long operation, we performed high precision measurements by accumulating cosmic-ray muons. We measured the muon charge ratio to be $R=1.32 \pm 0.02$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.08619v2-abstract-full').style.display = 'inline'; document.getElementById('2403.08619v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.08619v2-abstract-full" style="display: none;"> We present the results of the charge ratio ($R$) and polarization ($P^渭_{0}$) measurements using the decay electron events collected from 2008 September to 2022 June by the Super-Kamiokande detector. Because of its underground location and long operation, we performed high precision measurements by accumulating cosmic-ray muons. We measured the muon charge ratio to be $R=1.32 \pm 0.02$ $(\mathrm{stat.}{+}\mathrm{syst.})$ at $E_渭\cos 胃_{\mathrm{Zenith}}=0.7^{+0.3}_{-0.2}$ $\mathrm{TeV}$, where $E_渭$ is the muon energy and $胃_{\mathrm{Zenith}}$ is the zenith angle of incoming cosmic-ray muons. This result is consistent with the Honda flux model while this suggests a tension with the $蟺K$ model of $1.9蟽$. We also measured the muon polarization at the production location to be $P^渭_{0}=0.52 \pm 0.02$ $(\mathrm{stat.}{+}\mathrm{syst.})$ at the muon momentum of $0.9^{+0.6}_{-0.1}$ $\mathrm{TeV}/c$ at the surface of the mountain; this also suggests a tension with the Honda flux model of $1.5蟽$. This is the most precise measurement ever to experimentally determine the cosmic-ray muon polarization near $1~\mathrm{TeV}/c$. These measurement results are useful to improve the atmospheric neutrino simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.08619v2-abstract-full').style.display = 'none'; document.getElementById('2403.08619v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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, 45 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 110, 082008 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.12907">arXiv:2312.12907</a> <span> [<a href="https://arxiv.org/pdf/2312.12907">pdf</a>, <a href="https://arxiv.org/ps/2312.12907">ps</a>, <a href="https://arxiv.org/format/2312.12907">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/10.1103/PhysRevD.109.092001">10.1103/PhysRevD.109.092001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solar neutrino measurements using the full data period of Super-Kamiokande-IV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a> , et al. (305 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="2312.12907v2-abstract-short" style="display: inline;"> An analysis of solar neutrino data from the fourth phase of Super-Kamiokande~(SK-IV) from October 2008 to May 2018 is performed and the results are presented. The observation time of the data set of SK-IV corresponds to $2970$~days and the total live time for all four phases is $5805$~days. For more precise solar neutrino measurements, several improvements are applied in this analysis: lowering th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12907v2-abstract-full').style.display = 'inline'; document.getElementById('2312.12907v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.12907v2-abstract-full" style="display: none;"> An analysis of solar neutrino data from the fourth phase of Super-Kamiokande~(SK-IV) from October 2008 to May 2018 is performed and the results are presented. The observation time of the data set of SK-IV corresponds to $2970$~days and the total live time for all four phases is $5805$~days. For more precise solar neutrino measurements, several improvements are applied in this analysis: lowering the data acquisition threshold in May 2015, further reduction of the spallation background using neutron clustering events, precise energy reconstruction considering the time variation of the PMT gain. The observed number of solar neutrino events in $3.49$--$19.49$ MeV electron kinetic energy region during SK-IV is $65,443^{+390}_{-388}\,(\mathrm{stat.})\pm 925\,(\mathrm{syst.})$ events. Corresponding $\mathrm{^{8}B}$ solar neutrino flux is $(2.314 \pm 0.014\, \rm{(stat.)} \pm 0.040 \, \rm{(syst.)}) \times 10^{6}~\mathrm{cm^{-2}\,s^{-1}}$, assuming a pure electron-neutrino flavor component without neutrino oscillations. The flux combined with all SK phases up to SK-IV is $(2.336 \pm 0.011\, \rm{(stat.)} \pm 0.043 \, \rm{(syst.)}) \times 10^{6}~\mathrm{cm^{-2}\,s^{-1}}$. Based on the neutrino oscillation analysis from all solar experiments, including the SK $5805$~days data set, the best-fit neutrino oscillation parameters are $\rm{sin^{2} 胃_{12,\,solar}} = 0.306 \pm 0.013 $ and $螖m^{2}_{21,\,\mathrm{solar}} = (6.10^{+ 0.95}_{-0.81}) \times 10^{-5}~\rm{eV}^{2}$, with a deviation of about 1.5$蟽$ from the $螖m^{2}_{21}$ parameter obtained by KamLAND. The best-fit neutrino oscillation parameters obtained from all solar experiments and KamLAND are $\sin^{2} 胃_{12,\,\mathrm{global}} = 0.307 \pm 0.012 $ and $螖m^{2}_{21,\,\mathrm{global}} = (7.50^{+ 0.19}_{-0.18}) \times 10^{-5}~\rm{eV}^{2}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12907v2-abstract-full').style.display = 'none'; document.getElementById('2312.12907v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">47 pages, 61 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 109, 092001 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.05105">arXiv:2311.05105</a> <span> [<a href="https://arxiv.org/pdf/2311.05105">pdf</a>, <a href="https://arxiv.org/format/2311.05105">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/10.1103/PhysRevD.109.072014">10.1103/PhysRevD.109.072014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Atmospheric neutrino oscillation analysis with neutron tagging and an expanded fiducial volume in Super-Kamiokande I-V </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Wester%2C+T">T. Wester</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a> , et al. (212 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.05105v1-abstract-short" style="display: inline;"> We present a measurement of neutrino oscillation parameters with the Super-Kamiokande detector using atmospheric neutrinos from the complete pure-water SK I-V (April 1996-July 2020) data set, including events from an expanded fiducial volume. The data set corresponds to 6511.3 live days and an exposure of 484.2 kiloton-years. Measurements of the neutrino oscillation parameters $螖m^2_{32}$,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.05105v1-abstract-full').style.display = 'inline'; document.getElementById('2311.05105v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.05105v1-abstract-full" style="display: none;"> We present a measurement of neutrino oscillation parameters with the Super-Kamiokande detector using atmospheric neutrinos from the complete pure-water SK I-V (April 1996-July 2020) data set, including events from an expanded fiducial volume. The data set corresponds to 6511.3 live days and an exposure of 484.2 kiloton-years. Measurements of the neutrino oscillation parameters $螖m^2_{32}$, $\sin^2胃_{23}$, $\sin^2 胃_{13}$, $未_{CP}$, and the preference for the neutrino mass ordering are presented with atmospheric neutrino data alone, and with constraints on $\sin^2 胃_{13}$ from reactor neutrino experiments. Our analysis including constraints on $\sin^2 胃_{13}$ favors the normal mass ordering at the 92.3% level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.05105v1-abstract-full').style.display = 'none'; document.getElementById('2311.05105v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 18 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/2311.03842">arXiv:2311.03842</a> <span> [<a href="https://arxiv.org/pdf/2311.03842">pdf</a>, <a href="https://arxiv.org/ps/2311.03842">ps</a>, <a href="https://arxiv.org/format/2311.03842">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 the neutrino-oxygen neutral-current quasielastic cross section using atmospheric neutrinos in the SK-Gd experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Sakai%2C+S">S. Sakai</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiba%2C+H">H. Shiba</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+K">K. Shimizu</a> , et al. (211 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.03842v1-abstract-short" style="display: inline;"> We report the first measurement of the atmospheric neutrino-oxygen neutral-current quasielastic (NCQE) cross section in the gadolinium-loaded Super-Kamiokande (SK) water Cherenkov detector. In June 2020, SK began a new experimental phase, named SK-Gd, by loading 0.011% by mass of gadolinium into the ultrapure water of the SK detector. The introduction of gadolinium to ultrapure water has the effec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03842v1-abstract-full').style.display = 'inline'; document.getElementById('2311.03842v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.03842v1-abstract-full" style="display: none;"> We report the first measurement of the atmospheric neutrino-oxygen neutral-current quasielastic (NCQE) cross section in the gadolinium-loaded Super-Kamiokande (SK) water Cherenkov detector. In June 2020, SK began a new experimental phase, named SK-Gd, by loading 0.011% by mass of gadolinium into the ultrapure water of the SK detector. The introduction of gadolinium to ultrapure water has the effect of improving the neutron-tagging efficiency. Using a 552.2 day data set from August 2020 to June 2022, we measure the NCQE cross section to be 0.74 $\pm$ 0.22(stat.) $^{+0.85}_{-0.15}$ (syst.) $\times$ 10$^{-38}$ cm$^{2}$/oxygen in the energy range from 160 MeV to 10 GeV, which is consistent with the atmospheric neutrino-flux-averaged theoretical NCQE cross section and the measurement in the SK pure-water phase within the uncertainties. Furthermore, we compare the models of the nucleon-nucleus interactions in water and find that the Binary Cascade model and the Liege Intranuclear Cascade model provide a somewhat better fit to the observed data than the Bertini Cascade model. Since the atmospheric neutrino-oxygen NCQE reactions are one of the main backgrounds in the search for diffuse supernova neutrino background (DSNB), these new results will contribute to future studies - and the potential discovery - of the DSNB in SK. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03842v1-abstract-full').style.display = 'none'; document.getElementById('2311.03842v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.01159">arXiv:2311.01159</a> <span> [<a href="https://arxiv.org/pdf/2311.01159">pdf</a>, <a href="https://arxiv.org/format/2311.01159">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 Periodic Time Variations of the Solar $^8$B Neutrino Flux between 1996 and 2018 in Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiba%2C+H">H. Shiba</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+K">K. Shimizu</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a> , et al. (211 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.01159v2-abstract-short" style="display: inline;"> We report a search for time variations of the solar $^8$B neutrino flux using 5804 live days of Super-Kamiokande data collected between May 31, 1996, and May 30, 2018. Super-Kamiokande measured the precise time of each solar neutrino interaction over 22 calendar years to search for solar neutrino flux modulations with unprecedented precision. Periodic modulations are searched for in a dataset comp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01159v2-abstract-full').style.display = 'inline'; document.getElementById('2311.01159v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.01159v2-abstract-full" style="display: none;"> We report a search for time variations of the solar $^8$B neutrino flux using 5804 live days of Super-Kamiokande data collected between May 31, 1996, and May 30, 2018. Super-Kamiokande measured the precise time of each solar neutrino interaction over 22 calendar years to search for solar neutrino flux modulations with unprecedented precision. Periodic modulations are searched for in a dataset comprising five-day interval solar neutrino flux measurements with a maximum likelihood method. We also applied the Lomb-Scargle method to this dataset to compare it with previous reports. The only significant modulation found is due to the elliptic orbit of the Earth around the Sun. The observed modulation is consistent with astronomical data: we measured an eccentricity of (1.53$\pm$0.35)\%, and a perihelion shift of ($-$1.5$\pm$13.5) days. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01159v2-abstract-full').style.display = 'none'; document.getElementById('2311.01159v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures, 2 tables, and data file: "sksolartimevariation5804d.txt" (the data file updated with additional 3 columns -- R^2 correction, upper-error, lower-error)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett 132, 241803 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.05135">arXiv:2305.05135</a> <span> [<a href="https://arxiv.org/pdf/2305.05135">pdf</a>, <a href="https://arxiv.org/format/2305.05135">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="Nuclear Experiment">nucl-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/10.3847/2041-8213/acdc9e">10.3847/2041-8213/acdc9e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for astrophysical electron antineutrinos in Super-Kamiokande with 0.01wt% gadolinium-loaded water </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Harada%2C+M">M. Harada</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiba%2C+H">H. Shiba</a> , et al. (216 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.05135v2-abstract-short" style="display: inline;"> We report the first search result for the flux of astrophysical electron antineutrinos for energies O(10) MeV in the gadolinium-loaded Super-Kamiokande (SK) detector. In June 2020, gadolinium was introduced to the ultra-pure water of the SK detector in order to detect neutrons more efficiently. In this new experimental phase, SK-Gd, we can search for electron antineutrinos via inverse beta decay w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05135v2-abstract-full').style.display = 'inline'; document.getElementById('2305.05135v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.05135v2-abstract-full" style="display: none;"> We report the first search result for the flux of astrophysical electron antineutrinos for energies O(10) MeV in the gadolinium-loaded Super-Kamiokande (SK) detector. In June 2020, gadolinium was introduced to the ultra-pure water of the SK detector in order to detect neutrons more efficiently. In this new experimental phase, SK-Gd, we can search for electron antineutrinos via inverse beta decay with efficient background rejection and higher signal efficiency thanks to the high efficiency of the neutron tagging technique. In this paper, we report the result for the initial stage of SK-Gd with a $22.5\times552$ $\rm kton\cdot day$ exposure at 0.01% Gd mass concentration. No significant excess over the expected background in the observed events is found for the neutrino energies below 31.3 MeV. Thus, the flux upper limits are placed at the 90% confidence level. The limits and sensitivities are already comparable with the previous SK result with pure-water ($22.5 \times 2970 \rm kton\cdot day$) owing to the enhanced neutron tagging. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05135v2-abstract-full').style.display = 'none'; document.getElementById('2305.05135v2-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.10801">arXiv:2212.10801</a> <span> [<a href="https://arxiv.org/pdf/2212.10801">pdf</a>, <a href="https://arxiv.org/format/2212.10801">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 the cosmogenic neutron yield in Super-Kamiokande with gadolinium loaded water </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Shinoki%2C+M">M. Shinoki</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</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="2212.10801v3-abstract-short" style="display: inline;"> Cosmic-ray muons that enter the Super-Kamiokande detector cause hadronic showers due to spallation in water, producing neutrons and radioactive isotopes. Those are a major background source for studies of MeV-scale neutrinos and searches for rare events. Since 2020, gadolinium was introduced in the ultra-pure water in the Super-Kamiokande detector to improve the detection efficiency of neutrons. I… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10801v3-abstract-full').style.display = 'inline'; document.getElementById('2212.10801v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.10801v3-abstract-full" style="display: none;"> Cosmic-ray muons that enter the Super-Kamiokande detector cause hadronic showers due to spallation in water, producing neutrons and radioactive isotopes. Those are a major background source for studies of MeV-scale neutrinos and searches for rare events. Since 2020, gadolinium was introduced in the ultra-pure water in the Super-Kamiokande detector to improve the detection efficiency of neutrons. In this study, the cosmogenic neutron yield was measured using data acquired during the period after the gadolinium loading. The yield was found to be $(2.76 \pm 0.02\,\mathrm{(stat.) \pm 0.19\,\mathrm{(syst.)}}) \times 10^{-4}\,渭^{-1} \mathrm{g^{-1} cm^{2}}$ at 259 GeV of average muon energy at the Super-Kamiokande detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10801v3-abstract-full').style.display = 'none'; document.getElementById('2212.10801v3-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">10 pages, 10 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.12948">arXiv:2210.12948</a> <span> [<a href="https://arxiv.org/pdf/2210.12948">pdf</a>, <a href="https://arxiv.org/format/2210.12948">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Searching for neutrinos from solar flares across solar cycles 23 and 24 with the Super-Kamiokande detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+Y">Y. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+K">K. Shimizu</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a> , et al. (220 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.12948v2-abstract-short" style="display: inline;"> Neutrinos associated with solar flares (solar-flare neutrinos) provide information on particle acceleration mechanisms during the impulsive phase of solar flares. We searched using the Super-Kamiokande detector for neutrinos from solar flares that occurred during solar cycles $23$ and $24$, including the largest solar flare (X28.0) on November 4th, 2003. In order to minimize the background rate we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12948v2-abstract-full').style.display = 'inline'; document.getElementById('2210.12948v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.12948v2-abstract-full" style="display: none;"> Neutrinos associated with solar flares (solar-flare neutrinos) provide information on particle acceleration mechanisms during the impulsive phase of solar flares. We searched using the Super-Kamiokande detector for neutrinos from solar flares that occurred during solar cycles $23$ and $24$, including the largest solar flare (X28.0) on November 4th, 2003. In order to minimize the background rate we searched for neutrino interactions within narrow time windows coincident with $纬$-rays and soft X-rays recorded by satellites. In addition, we performed the first attempt to search for solar-flare neutrinos from solar flares on the invisible side of the Sun by using the emission time of coronal mass ejections (CMEs). By selecting twenty powerful solar flares above X5.0 on the visible side and eight CMEs whose emission speed exceeds $2000$ $\mathrm{km \, s^{-1}}$ on the invisible side from 1996 to 2018, we found two (six) neutrino events coincident with solar flares occurring on the visible (invisible) side of the Sun, with a typical background rate of $0.10$ ($0.62$) events per flare in the MeV-GeV energy range. No significant solar-flare neutrino signal above the estimated background rate was observed. As a result we set the following upper limit on neutrino fluence at the Earth $\mathit桅<1.1\times10^{6}$ $\mathrm{cm^{-2}}$ at the $90\%$ confidence level for the largest solar flare. The resulting fluence limits allow us to constrain some of the theoretical models for solar-flare neutrino emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12948v2-abstract-full').style.display = 'none'; document.getElementById('2210.12948v2-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 18 figures, 9 tables (Figure 12 was replaced because it was incorrect in version 1.)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.14968">arXiv:2209.14968</a> <span> [<a href="https://arxiv.org/pdf/2209.14968">pdf</a>, <a href="https://arxiv.org/format/2209.14968">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/10.1103/PhysRevLett.130.031802">10.1103/PhysRevLett.130.031802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Cosmic-ray Boosted Sub-GeV Dark Matter using Recoil Protons at Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+S">The Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiba%2C+H">H. Shiba</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+K">K. Shimizu</a> , et al. (197 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="2209.14968v4-abstract-short" style="display: inline;"> We report a search for cosmic-ray boosted dark matter with protons using the 0.37 megaton$\times$years data collected at Super-Kamiokande experiment during the 1996-2018 period (SKI-IV phase). We searched for an excess of proton recoils above the atmospheric neutrino background from the vicinity of the Galactic Center. No such excess is observed, and limits are calculated for two reference models… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.14968v4-abstract-full').style.display = 'inline'; document.getElementById('2209.14968v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.14968v4-abstract-full" style="display: none;"> We report a search for cosmic-ray boosted dark matter with protons using the 0.37 megaton$\times$years data collected at Super-Kamiokande experiment during the 1996-2018 period (SKI-IV phase). We searched for an excess of proton recoils above the atmospheric neutrino background from the vicinity of the Galactic Center. No such excess is observed, and limits are calculated for two reference models of dark matter with either a constant interaction cross-section or through a scalar mediator. This is the first experimental search for boosted dark matter with hadrons using directional information. The results present the most stringent limits on cosmic-ray boosted dark matter and exclude the dark matter-nucleon elastic scattering cross-section between $10^{-33}\text{ cm}^{2}$ and $10^{-27}\text{ cm}^{2}$ for dark matter mass from 10 MeV/$c^2$ to 1 GeV/$c^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.14968v4-abstract-full').style.display = 'none'; document.getElementById('2209.14968v4-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">With 1-page appendix. A bug was found in July 2023. This version is updated to match the erratum</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 130 (2023) 031802 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.08609">arXiv:2209.08609</a> <span> [<a href="https://arxiv.org/pdf/2209.08609">pdf</a>, <a href="https://arxiv.org/format/2209.08609">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="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/10.1088/1748-0221/17/10/P10029">10.1088/1748-0221/17/10/P10029 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron Tagging following Atmospheric Neutrino Events in a Water Cherenkov Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Haga%2C+Y">Y. Haga</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+T">T. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a> , et al. (281 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="2209.08609v2-abstract-short" style="display: inline;"> We present the development of neutron-tagging techniques in Super-Kamiokande IV using a neural network analysis. The detection efficiency of neutron capture on hydrogen is estimated to be 26%, with a mis-tag rate of 0.016 per neutrino event. The uncertainty of the tagging efficiency is estimated to be 9.0%. Measurement of the tagging efficiency with data from an Americium-Beryllium calibration agr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.08609v2-abstract-full').style.display = 'inline'; document.getElementById('2209.08609v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.08609v2-abstract-full" style="display: none;"> We present the development of neutron-tagging techniques in Super-Kamiokande IV using a neural network analysis. The detection efficiency of neutron capture on hydrogen is estimated to be 26%, with a mis-tag rate of 0.016 per neutrino event. The uncertainty of the tagging efficiency is estimated to be 9.0%. Measurement of the tagging efficiency with data from an Americium-Beryllium calibration agrees with this value within 10%. The tagging procedure was performed on 3,244.4 days of SK-IV atmospheric neutrino data, identifying 18,091 neutrons in 26,473 neutrino events. The fitted neutron capture lifetime was measured as 218 \pm 9 渭s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.08609v2-abstract-full').style.display = 'none'; document.getElementById('2209.08609v2-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">Journal ref:</span> JINST 17 P10029 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.13188">arXiv:2208.13188</a> <span> [<a href="https://arxiv.org/pdf/2208.13188">pdf</a>, <a href="https://arxiv.org/format/2208.13188">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 proton decay via $p\rightarrow 渭^+K^0$ in 0.37 megaton-years exposure of Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Matsumoto%2C+R">R. Matsumoto</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiba%2C+H">H. Shiba</a> , et al. (208 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.13188v1-abstract-short" style="display: inline;"> We searched for proton decay via $p\to渭^+K^0$ in 0.37\,Mton$\cdot$years of data collected between 1996 and 2018 from the Super-Kamiokande water Cherenkov experiment. The selection criteria were defined separately for $K^0_S$ and $K^0_L$ channels. No significant event excess has been observed. As a result of this analysis, which extends the previous search by an additional 0.2\,Mton$\cdot$years of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.13188v1-abstract-full').style.display = 'inline'; document.getElementById('2208.13188v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.13188v1-abstract-full" style="display: none;"> We searched for proton decay via $p\to渭^+K^0$ in 0.37\,Mton$\cdot$years of data collected between 1996 and 2018 from the Super-Kamiokande water Cherenkov experiment. The selection criteria were defined separately for $K^0_S$ and $K^0_L$ channels. No significant event excess has been observed. As a result of this analysis, which extends the previous search by an additional 0.2\,Mton$\cdot$years of exposure and uses an improved event reconstruction, we set a lower limit of $3.6\times10^{33}$ years on the proton lifetime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.13188v1-abstract-full').style.display = 'none'; document.getElementById('2208.13188v1-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 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/2206.01380">arXiv:2206.01380</a> <span> [<a href="https://arxiv.org/pdf/2206.01380">pdf</a>, <a href="https://arxiv.org/format/2206.01380">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/10.3847/1538-4357/ac8f41">10.3847/1538-4357/ac8f41 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for supernova bursts in Super-Kamiokande IV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=collaboration%2C+T+S">The Super-Kamiokande collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Mori%2C+M">M. Mori</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</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="2206.01380v1-abstract-short" style="display: inline;"> Super-Kamiokande has been searching for neutrino bursts characteristic of core-collapse supernovae continuously, in real time, since the start of operations in 1996. The present work focuses on detecting more distant supernovae whose event rate may be too small to trigger in real time, but may be identified using an offline approach. The analysis of data collected from 2008 to 2018 found no eviden… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.01380v1-abstract-full').style.display = 'inline'; document.getElementById('2206.01380v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.01380v1-abstract-full" style="display: none;"> Super-Kamiokande has been searching for neutrino bursts characteristic of core-collapse supernovae continuously, in real time, since the start of operations in 1996. The present work focuses on detecting more distant supernovae whose event rate may be too small to trigger in real time, but may be identified using an offline approach. The analysis of data collected from 2008 to 2018 found no evidence of distant supernovae bursts. This establishes an upper limit of 0.29 year$^{-1}$ on the rate of core-collapse supernovae out to 100 kpc at 90% C.L.. For supernovae that fail to explode and collapse directly to black holes the limit reaches to 300 kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.01380v1-abstract-full').style.display = 'none'; document.getElementById('2206.01380v1-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">originally announced</span> June 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.09881">arXiv:2205.09881</a> <span> [<a href="https://arxiv.org/pdf/2205.09881">pdf</a>, <a href="https://arxiv.org/format/2205.09881">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 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/10.3847/1538-4357/ac7f9c">10.3847/1538-4357/ac7f9c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pre-Supernova Alert System for Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Machado%2C+L+N">L. N. Machado</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/hep-ex?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiba%2C+H">H. Shiba</a> , et al. (202 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.09881v2-abstract-short" style="display: inline;"> In 2020, the Super-Kamiokande (SK) experiment moved to a new stage (SK-Gd) in which gadolinium (Gd) sulfate octahydrate was added to the water in the detector, enhancing the efficiency to detect thermal neutrons and consequently improving the sensitivity to low energy electron anti-neutrinos from inverse beta decay (IBD) interactions. SK-Gd has the potential to provide early alerts of incipient co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09881v2-abstract-full').style.display = 'inline'; document.getElementById('2205.09881v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.09881v2-abstract-full" style="display: none;"> In 2020, the Super-Kamiokande (SK) experiment moved to a new stage (SK-Gd) in which gadolinium (Gd) sulfate octahydrate was added to the water in the detector, enhancing the efficiency to detect thermal neutrons and consequently improving the sensitivity to low energy electron anti-neutrinos from inverse beta decay (IBD) interactions. SK-Gd has the potential to provide early alerts of incipient core-collapse supernovae through detection of electron anti-neutrinos from thermal and nuclear processes responsible for the cooling of massive stars before the gravitational collapse of their cores. These pre-supernova neutrinos emitted during the silicon burning phase can exceed the energy threshold for IBD reactions. We present the sensitivity of SK-Gd to pre-supernova stars and the techniques used for the development of a pre-supernova alarm based on the detection of these neutrinos in SK, as well as prospects for future SK-Gd phases with higher concentrations of Gd. For the current SK-Gd phase, high-confidence alerts for Betelgeuse could be issued up to nine hours in advance of the core-collapse itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09881v2-abstract-full').style.display = 'none'; document.getElementById('2205.09881v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 935, Number 1 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.11772">arXiv:2203.11772</a> <span> [<a href="https://arxiv.org/pdf/2203.11772">pdf</a>, <a href="https://arxiv.org/format/2203.11772">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Testing Non-Standard Interactions Between Solar Neutrinos and Quarks with Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Weatherly%2C+P">P. Weatherly</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a> , et al. (248 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="2203.11772v1-abstract-short" style="display: inline;"> Non-Standard Interactions (NSI) between neutrinos and matter affect the neutrino flavor oscillations. Due to the high matter density in the core of the Sun, solar neutrinos are suited to probe these interactions. Using the $277$ kton-yr exposure of Super-Kamiokande to $^{8}$B solar neutrinos, we search for the presence of NSI. Our data favors the presence of NSI with down quarks at 1.8$蟽$, and wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.11772v1-abstract-full').style.display = 'inline'; document.getElementById('2203.11772v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.11772v1-abstract-full" style="display: none;"> Non-Standard Interactions (NSI) between neutrinos and matter affect the neutrino flavor oscillations. Due to the high matter density in the core of the Sun, solar neutrinos are suited to probe these interactions. Using the $277$ kton-yr exposure of Super-Kamiokande to $^{8}$B solar neutrinos, we search for the presence of NSI. Our data favors the presence of NSI with down quarks at 1.8$蟽$, and with up quarks at 1.6$蟽$, with the best fit NSI parameters being ($蔚_{11}^{d},蔚_{12}^{d}$) = (-3.3, -3.1) for $d$-quarks and ($蔚_{11}^{u},蔚_{12}^{u}$) = (-2.5, -3.1) for $u$-quarks. After combining with data from the Sudbury Neutrino Observatory and Borexino, the significance increases by 0.1$蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.11772v1-abstract-full').style.display = 'none'; document.getElementById('2203.11772v1-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> <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">Author: Pierce Weatherly 25 pages. To be submitted to Physical Review D</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.00092">arXiv:2112.00092</a> <span> [<a href="https://arxiv.org/pdf/2112.00092">pdf</a>, <a href="https://arxiv.org/format/2112.00092">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> <p class="title is-5 mathjax"> New Methods and Simulations for Cosmogenic Induced Spallation Removal in Super-Kamiokande-IV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Locke%2C+S">S. Locke</a>, <a href="/search/hep-ex?searchtype=author&query=Coffani%2C+A">A. Coffani</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Ito%2C+H">H. Ito</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/hep-ex?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a> , et al. (196 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="2112.00092v1-abstract-short" style="display: inline;"> Radioactivity induced by cosmic muon spallation is a dominant source of backgrounds for $\mathcal{O}(10)~$MeV neutrino interactions in water Cherenkov detectors. In particular, it is crucial to reduce backgrounds to measure the solar neutrino spectrum and find neutrino interactions from distant supernovae. In this paper we introduce new techniques to locate muon-induced hadronic showers and effici… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.00092v1-abstract-full').style.display = 'inline'; document.getElementById('2112.00092v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.00092v1-abstract-full" style="display: none;"> Radioactivity induced by cosmic muon spallation is a dominant source of backgrounds for $\mathcal{O}(10)~$MeV neutrino interactions in water Cherenkov detectors. In particular, it is crucial to reduce backgrounds to measure the solar neutrino spectrum and find neutrino interactions from distant supernovae. In this paper we introduce new techniques to locate muon-induced hadronic showers and efficiently reject spallation backgrounds. Applying these techniques to the solar neutrino analysis with an exposure of $2790\times22.5$~kton.day increases the signal efficiency by $12.6\%$, approximately corresponding to an additional year of detector running. Furthermore, we present the first spallation simulation at SK, where we model hadronic interactions using FLUKA. The agreement between the isotope yields and shower pattern in this simulation and in the data gives confidence in the accuracy of this simulation, and thus opens the door to use it to optimize muon spallation removal in new data with gadolinium-enhanced neutron capture detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.00092v1-abstract-full').style.display = 'none'; document.getElementById('2112.00092v1-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">originally announced</span> December 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.11174">arXiv:2109.11174</a> <span> [<a href="https://arxiv.org/pdf/2109.11174">pdf</a>, <a href="https://arxiv.org/format/2109.11174">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.104.122002">10.1103/PhysRevD.104.122002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Diffuse Supernova Neutrino Background Search at Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/hep-ex?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a>, <a href="/search/hep-ex?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a> , et al. (197 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.11174v2-abstract-short" style="display: inline;"> A new search for the diffuse supernova neutrino background (DSNB) flux has been conducted at Super-Kamiokande (SK), with a $22.5\times2970$-kton$\cdot$day exposure from its fourth operational phase IV. The new analysis improves on the existing background reduction techniques and systematic uncertainties and takes advantage of an improved neutron tagging algorithm to lower the energy threshold comp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.11174v2-abstract-full').style.display = 'inline'; document.getElementById('2109.11174v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.11174v2-abstract-full" style="display: none;"> A new search for the diffuse supernova neutrino background (DSNB) flux has been conducted at Super-Kamiokande (SK), with a $22.5\times2970$-kton$\cdot$day exposure from its fourth operational phase IV. The new analysis improves on the existing background reduction techniques and systematic uncertainties and takes advantage of an improved neutron tagging algorithm to lower the energy threshold compared to the previous phases of SK. This allows for setting the world's most stringent upper limit on the extraterrestrial $\bar谓_e$ flux, for neutrino energies below 31.3 MeV. The SK-IV results are combined with the ones from the first three phases of SK to perform a joint analysis using $22.5\times5823$ kton$\cdot$days of data. This analysis has the world's best sensitivity to the DSNB $\bar谓_e$ flux, comparable to the predictions from various models. For neutrino energies larger than 17.3 MeV, the new combined $90\%$ C.L. upper limits on the DSNB $\bar谓_e$ flux lie around $2.7$ cm$^{-2}$$\cdot$$\text{sec}^{-1}$, strongly disfavoring the most optimistic predictions. Finally, potentialities of the gadolinium phase of SK and the future Hyper-Kamiokande experiment are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.11174v2-abstract-full').style.display = 'none'; document.getElementById('2109.11174v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">42 pages, 37 figures, 14 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.09196">arXiv:2104.09196</a> <span> [<a href="https://arxiv.org/pdf/2104.09196">pdf</a>, <a href="https://arxiv.org/format/2104.09196">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/10.3847/1538-4357/ac0d5a">10.3847/1538-4357/ac0d5a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for neutrinos in coincidence with gravitational wave events from the LIGO-Virgo O3a Observing Run with the Super-Kamiokande detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=collaboration%2C+T+S">The Super-Kamiokande collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/hep-ex?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a>, <a href="/search/hep-ex?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a>, <a href="/search/hep-ex?searchtype=author&query=Takeda%2C+A">A. Takeda</a> , et al. (189 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="2104.09196v2-abstract-short" style="display: inline;"> The Super-Kamiokande detector can be used to search for neutrinos in time coincidence with gravitational waves detected by the LIGO-Virgo Collaboration (LVC). Both low-energy ($7-100$ MeV) and high-energy ($0.1-10^5$ GeV) samples were analyzed in order to cover a very wide neutrino spectrum. Follow-ups of 36 (out of 39) gravitational waves reported in the GWTC-2 catalog were examined; no significa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.09196v2-abstract-full').style.display = 'inline'; document.getElementById('2104.09196v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.09196v2-abstract-full" style="display: none;"> The Super-Kamiokande detector can be used to search for neutrinos in time coincidence with gravitational waves detected by the LIGO-Virgo Collaboration (LVC). Both low-energy ($7-100$ MeV) and high-energy ($0.1-10^5$ GeV) samples were analyzed in order to cover a very wide neutrino spectrum. Follow-ups of 36 (out of 39) gravitational waves reported in the GWTC-2 catalog were examined; no significant excess above the background was observed, with 10 (24) observed neutrinos compared with 4.8 (25.0) expected events in the high-energy (low-energy) samples. A statistical approach was used to compute the significance of potential coincidences. For each observation, p-values were estimated using neutrino direction and LVC sky map ; the most significant event (GW190602_175927) is associated with a post-trial p-value of $7.8\%$ ($1.4蟽$). Additionally, flux limits were computed independently for each sample and by combining the samples. The energy emitted as neutrinos by the identified gravitational wave sources was constrained, both for given flavors and for all-flavors assuming equipartition between the different flavors, independently for each trigger and by combining sources of the same nature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.09196v2-abstract-full').style.display = 'none'; document.getElementById('2104.09196v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">16 pages, 5 figures. v2: adding corrections from The Astrophysical Journal review</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 918, Number 2 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.05269">arXiv:2101.05269</a> <span> [<a href="https://arxiv.org/pdf/2101.05269">pdf</a>, <a href="https://arxiv.org/format/2101.05269">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/10.3847/1538-4357/abf7c4">10.3847/1538-4357/abf7c4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supernova Model Discrimination with Hyper-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+H">Hyper-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Adrich%2C+P">P. Adrich</a>, <a href="/search/hep-ex?searchtype=author&query=Aihara%2C+H">H. Aihara</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Alekseev%2C+I">I. Alekseev</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Anghel%2C+I">I. Anghel</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L+H+V">L. H. V. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Araya%2C+A">A. Araya</a>, <a href="/search/hep-ex?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Aushev%2C+V">V. Aushev</a>, <a href="/search/hep-ex?searchtype=author&query=Ballester%2C+F">F. Ballester</a>, <a href="/search/hep-ex?searchtype=author&query=Bandac%2C+I">I. Bandac</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">M. Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a> , et al. (478 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="2101.05269v2-abstract-short" style="display: inline;"> Core-collapse supernovae are among the most magnificent events in the observable universe. They produce many of the chemical elements necessary for life to exist and their remnants -- neutron stars and black holes -- are interesting astrophysical objects in their own right. However, despite millennia of observations and almost a century of astrophysical study, the explosion mechanism of core-colla… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05269v2-abstract-full').style.display = 'inline'; document.getElementById('2101.05269v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05269v2-abstract-full" style="display: none;"> Core-collapse supernovae are among the most magnificent events in the observable universe. They produce many of the chemical elements necessary for life to exist and their remnants -- neutron stars and black holes -- are interesting astrophysical objects in their own right. However, despite millennia of observations and almost a century of astrophysical study, the explosion mechanism of core-collapse supernovae is not yet well understood. Hyper-Kamiokande is a next-generation neutrino detector that will be able to observe the neutrino flux from the next galactic core-collapse supernova in unprecedented detail. We focus on the first 500 ms of the neutrino burst, corresponding to the accretion phase, and use a newly-developed, high-precision supernova event generator to simulate Hyper-Kamiokande's response to five different supernova models. We show that Hyper-Kamiokande will be able to distinguish between these models with high accuracy for a supernova at a distance of up to 100 kpc. Once the next galactic supernova happens, this ability will be a powerful tool for guiding simulations towards a precise reproduction of the explosion mechanism observed in nature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05269v2-abstract-full').style.display = 'none'; document.getElementById('2101.05269v2-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">21 pages, 7 figures. Article based on thesis published as arXiv:2002.01649. v2: added references and some explanations in response to reviewer comments</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 916 (2021) 15 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.03480">arXiv:2101.03480</a> <span> [<a href="https://arxiv.org/pdf/2101.03480">pdf</a>, <a href="https://arxiv.org/format/2101.03480">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"> Search for Tens of MeV Neutrinos associated with Gamma-Ray Bursts in Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+S">The Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Ito%2C+H">H. Ito</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/hep-ex?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a> , et al. (195 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.03480v2-abstract-short" style="display: inline;"> A search for neutrinos produced in coincidence with Gamma-Ray Bursts(GRB) was conducted with the Super-Kamiokande (SK) detector. Between December 2008 and March 2017, the Gamma-ray Coordinates Network recorded 2208 GRBs that occurred during normal SK operation. Several time windows around each GRB were used to search for coincident neutrino events. No statistically significant signal in excess of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03480v2-abstract-full').style.display = 'inline'; document.getElementById('2101.03480v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.03480v2-abstract-full" style="display: none;"> A search for neutrinos produced in coincidence with Gamma-Ray Bursts(GRB) was conducted with the Super-Kamiokande (SK) detector. Between December 2008 and March 2017, the Gamma-ray Coordinates Network recorded 2208 GRBs that occurred during normal SK operation. Several time windows around each GRB were used to search for coincident neutrino events. No statistically significant signal in excess of the estimated backgrounds was detected. The $\bar谓_e$ fluence in the range from 8 MeV to 100 MeV in positron total energy for $\bar谓_e+p\rightarrow e^{+}+n$ was found to be less than $\rm 5.07\times10^5$ cm$^{-2}$ per GRB in 90\% C.L. Upper bounds on the fluence as a function of neutrino energy were also obtained. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03480v2-abstract-full').style.display = 'none'; document.getElementById('2101.03480v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">29 pages, 16 figures, 5 tables, accepted by PTEP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.03807">arXiv:2012.03807</a> <span> [<a href="https://arxiv.org/pdf/2012.03807">pdf</a>, <a href="https://arxiv.org/ps/2012.03807">ps</a>, <a href="https://arxiv.org/format/2012.03807">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 Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2022.102702">10.1016/j.astropartphys.2022.102702 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for solar electron anti-neutrinos due to spin-flavor precession in the Sun with Super-Kamiokande-IV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Ito%2C+H">H. Ito</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/hep-ex?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a>, <a href="/search/hep-ex?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a>, <a href="/search/hep-ex?searchtype=author&query=Takeda%2C+A">A. Takeda</a> , et al. (177 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.03807v3-abstract-short" style="display: inline;"> Due to a very low production rate of electron anti-neutrinos ($\bar谓_e$) via nuclear fusion in the Sun, a flux of solar $\bar谓_e$ is unexpected. An appearance of $\bar谓_e$ in solar neutrino flux opens a new window for the new physics beyond the standard model. In particular, a spin-flavor precession process is expected to convert an electron neutrino into an electron anti-neutrino (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.03807v3-abstract-full').style.display = 'inline'; document.getElementById('2012.03807v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.03807v3-abstract-full" style="display: none;"> Due to a very low production rate of electron anti-neutrinos ($\bar谓_e$) via nuclear fusion in the Sun, a flux of solar $\bar谓_e$ is unexpected. An appearance of $\bar谓_e$ in solar neutrino flux opens a new window for the new physics beyond the standard model. In particular, a spin-flavor precession process is expected to convert an electron neutrino into an electron anti-neutrino (${谓_e\to\bar谓_e}$) when neutrino has a finite magnetic moment. In this work, we have searched for solar $\bar谓_e$ in the Super-Kamiokande experiment, using neutron tagging to identify their inverse beta decay signature. We identified 78 $\bar谓_e$ candidates for neutrino energies of 9.3 to 17.3 MeV in 2970.1 live days with a fiducial volume of 22.5 kiloton water (183.0 kton$\cdot$year exposure). The energy spectrum has been consistent with background predictions and we thus derived a 90% confidence level upper limit of ${4.7\times10^{-4}}$ on the $谓_e\to\bar谓_e$ conversion probability in the Sun. We used this result to evaluate the sensitivity of future experiments, notably the Super-Kamiokande Gadolinium (SK-Gd) upgrade. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.03807v3-abstract-full').style.display = 'none'; document.getElementById('2012.03807v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">16 pages, 10 figures, 7 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 139 (2022) 102702 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02607">arXiv:2012.02607</a> <span> [<a href="https://arxiv.org/pdf/2012.02607">pdf</a>, <a href="https://arxiv.org/ps/2012.02607">ps</a>, <a href="https://arxiv.org/format/2012.02607">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/10.1103/PhysRevD.103.012008">10.1103/PhysRevD.103.012008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron-Antineutron Oscillation Search using a 0.37 Megaton$\cdot$Year Exposure of Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Ito%2C+H">H. Ito</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/hep-ex?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a>, <a href="/search/hep-ex?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a>, <a href="/search/hep-ex?searchtype=author&query=Takeda%2C+A">A. Takeda</a> , et al. (176 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.02607v1-abstract-short" style="display: inline;"> As a baryon number violating process with $螖B=2$, neutron-antineutron oscillation ($n\to\bar n$) provides a unique test of baryon number conservation. We have performed a search for $n\to\bar n$ oscillation with bound neutrons in Super-Kamiokande, with the full data set from its first four run periods, representing an exposure of 0.37~Mton-years. The search used a multivariate analysis trained on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02607v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02607v1-abstract-full" style="display: none;"> As a baryon number violating process with $螖B=2$, neutron-antineutron oscillation ($n\to\bar n$) provides a unique test of baryon number conservation. We have performed a search for $n\to\bar n$ oscillation with bound neutrons in Super-Kamiokande, with the full data set from its first four run periods, representing an exposure of 0.37~Mton-years. The search used a multivariate analysis trained on simulated $n\to\bar n$ events and atmospheric neutrino backgrounds and resulted in 11 candidate events with an expected background of 9.3 events. In the absence of statistically significant excess, we derived a lower limit on $\bar n$ appearance lifetime in $^{16}$O nuclei of $3.6\times{10}^{32}$ years and on the neutron-antineutron oscillation time of $蟿_{n\to\bar n} > 4.7\times10^{8}$~s at 90\% C.L.. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02607v1-abstract-full').style.display = 'none'; document.getElementById('2012.02607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 103, 012008 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.16098">arXiv:2010.16098</a> <span> [<a href="https://arxiv.org/pdf/2010.16098">pdf</a>, <a href="https://arxiv.org/format/2010.16098">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/10.1103/PhysRevD.102.112011">10.1103/PhysRevD.102.112011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for proton decay via $p\to e^+蟺^0$ and $p\to 渭^+蟺^0$ with an enlarged fiducial volume in Super-Kamiokande I-IV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Takenaka%2C+A">A. Takenaka</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Ito%2C+H">H. Ito</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Marti%2C+L">Ll. Marti</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a> , et al. (191 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.16098v2-abstract-short" style="display: inline;"> We have searched for proton decay via $p\to e^+蟺^0$ and $p\to 渭^+蟺^0$ modes with the enlarged fiducial volume data of Super-Kamiokande from April 1996 to May 2018, which corresponds to 450 kton$\cdot$years exposure. We have accumulated about 25% more livetime and enlarged the fiducial volume of the Super-Kamiokande detector from 22.5 kton to 27.2 kton for this analysis, so that 144 kton$\cdot$year… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.16098v2-abstract-full').style.display = 'inline'; document.getElementById('2010.16098v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.16098v2-abstract-full" style="display: none;"> We have searched for proton decay via $p\to e^+蟺^0$ and $p\to 渭^+蟺^0$ modes with the enlarged fiducial volume data of Super-Kamiokande from April 1996 to May 2018, which corresponds to 450 kton$\cdot$years exposure. We have accumulated about 25% more livetime and enlarged the fiducial volume of the Super-Kamiokande detector from 22.5 kton to 27.2 kton for this analysis, so that 144 kton$\cdot$years of data, including 78 kton$\cdot$years of additional fiducial volume data, has been newly analyzed. No candidates have been found for $p\to e^+蟺^0$ and one candidate remains for $p\to 渭^+蟺^0$ in the conventional 22.5 kton fiducial volume and it is consistent with the atmospheric neutrino background prediction. We set lower limits on the partial lifetime for each of these modes: $蟿/B(p\to e^+蟺^0) > 2.4 \times 10^{34}$ years and $蟿/B(p\to 渭^+蟺^0) > 1.6 \times 10^{34}$ years at 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.16098v2-abstract-full').style.display = 'none'; document.getElementById('2010.16098v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 102, 112011 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.00794">arXiv:2009.00794</a> <span> [<a href="https://arxiv.org/pdf/2009.00794">pdf</a>, <a href="https://arxiv.org/ps/2009.00794">ps</a>, <a href="https://arxiv.org/format/2009.00794">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> <p class="title is-5 mathjax"> The Hyper-Kamiokande Experiment -- Snowmass LOI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+H">Hyper-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Adrich%2C+P">P. Adrich</a>, <a href="/search/hep-ex?searchtype=author&query=Aihara%2C+H">H. Aihara</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Alekseev%2C+I">I. Alekseev</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L+H+V">L. H. V. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Araya%2C+A">A. Araya</a>, <a href="/search/hep-ex?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/hep-ex?searchtype=author&query=Aushev%2C+V">V. Aushev</a>, <a href="/search/hep-ex?searchtype=author&query=Bandac%2C+I">I. Bandac</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">M. Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+L">L. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bian%2C+J">J. Bian</a>, <a href="/search/hep-ex?searchtype=author&query=Blanchet%2C+A">A. Blanchet</a> , et al. (366 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="2009.00794v1-abstract-short" style="display: inline;"> Hyper-Kamiokande is the next generation underground water Cherenkov detector that builds on the highly successful Super-Kamiokande experiment. The detector which has an 8.4~times larger effective volume than its predecessor will be located along the T2K neutrino beamline and utilize an upgraded J-PARC beam with 2.6~times beam power. Hyper-K's low energy threshold combined with the very large fiduc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.00794v1-abstract-full').style.display = 'inline'; document.getElementById('2009.00794v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.00794v1-abstract-full" style="display: none;"> Hyper-Kamiokande is the next generation underground water Cherenkov detector that builds on the highly successful Super-Kamiokande experiment. The detector which has an 8.4~times larger effective volume than its predecessor will be located along the T2K neutrino beamline and utilize an upgraded J-PARC beam with 2.6~times beam power. Hyper-K's low energy threshold combined with the very large fiducial volume make the detector unique, that is expected to acquire an unprecedented exposure of 3.8~Mton$\cdot$year over a period of 20~years of operation. Hyper-Kamiokande combines an extremely diverse science program including nucleon decays, long-baseline neutrino oscillations, atmospheric neutrinos, and neutrinos from astrophysical origins. The scientific scope of this program is highly complementary to liquid-argon detectors for example in sensitivity to nucleon decay channels or supernova detection modes. Hyper-Kamiokande construction has started in early 2020 and the experiment is expected to start operations in 2027. The Hyper-Kamiokande collaboration is presently being formed amongst groups from 19 countries including the United States, whose community has a long history of making significant contributions to the neutrino physics program in Japan. US physicists have played leading roles in the Kamiokande, Super-Kamiokande, EGADS, K2K, and T2K programs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.00794v1-abstract-full').style.display = 'none'; document.getElementById('2009.00794v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">6 pages, prepared as Snowmass2021 LOI</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.05109">arXiv:2005.05109</a> <span> [<a href="https://arxiv.org/pdf/2005.05109">pdf</a>, <a href="https://arxiv.org/format/2005.05109">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/10.1103/PhysRevD.102.072002">10.1103/PhysRevD.102.072002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Indirect Search for Dark Matter from the Galactic Center and Halo with the Super-Kamiokande Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Haga%2C+Y">Y. Haga</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Ito%2C+H">H. Ito</a>, <a href="/search/hep-ex?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Marti%2C+L">Ll. Marti</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+T">T. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a> , et al. (249 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.05109v2-abstract-short" style="display: inline;"> We present a search for an excess of neutrino interactions due to dark matter in the form of Weakly Interacting Massive Particles (WIMPs) annihilating in the galactic center or halo based on the data set of Super-Kamiokande-I, -II, -III and -IV taken from 1996 to 2016. We model the neutrino flux, energy, and flavor distributions assuming WIMP self-annihilation is dominant to $谓\overline谓$,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05109v2-abstract-full').style.display = 'inline'; document.getElementById('2005.05109v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.05109v2-abstract-full" style="display: none;"> We present a search for an excess of neutrino interactions due to dark matter in the form of Weakly Interacting Massive Particles (WIMPs) annihilating in the galactic center or halo based on the data set of Super-Kamiokande-I, -II, -III and -IV taken from 1996 to 2016. We model the neutrino flux, energy, and flavor distributions assuming WIMP self-annihilation is dominant to $谓\overline谓$, $渭^+渭^-$, $b\overline{b}$, or $W^+W^-$. The excess is in comparison to atmospheric neutrino interactions which are modeled in detail and fit to data. Limits on the self-annihilation cross section $\langle 蟽_{A} V \rangle$ are derived for WIMP masses in the range 1 GeV to 10 TeV, reaching as low as $9.6 \times10^{-23}$ cm$^3$ s$^{-1}$ for 5 GeV WIMPs in $b\bar b$ mode and $1.2 \times10^{-24}$ cm$^3$ s$^{-1}$ for 1 GeV WIMPs in $谓\bar 谓$ mode. The obtained sensitivity of the Super-Kamiokande detector to WIMP masses below several tens of GeV is the best among similar indirect searches to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05109v2-abstract-full').style.display = 'none'; document.getElementById('2005.05109v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">13 pages, 12 figures, Submitted to Phys. Rev. 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 102, 072002 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.13989">arXiv:2004.13989</a> <span> [<a href="https://arxiv.org/pdf/2004.13989">pdf</a>, <a href="https://arxiv.org/format/2004.13989">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/10.1093/ptep/ptab014">10.1093/ptep/ptab014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of $\bar谓_渭$ and $\bar谓_渭 + 谓_渭$ charged-current cross-sections without detected pions nor protons on water and hydrocarbon at mean antineutrino energy of 0.86 GeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akhlaq%2C+N">N. Akhlaq</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Arihara%2C+T">T. Arihara</a>, <a href="/search/hep-ex?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barrow%2C+D">D. Barrow</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a> , et al. (344 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="2004.13989v1-abstract-short" style="display: inline;"> We report measurements of the flux-integrated $\bar谓_渭$ and $\bar谓_渭+谓_渭$ charged-current cross-sections on water and hydrocarbon targets using the T2K anti-neutrino beam, with a mean neutrino energy of 0.86 GeV. The signal is defined as the (anti-)neutrino charged-current interaction with one induced $渭^\pm$ and no detected charged pion nor proton. These measurements are performed using a new WAG… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.13989v1-abstract-full').style.display = 'inline'; document.getElementById('2004.13989v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.13989v1-abstract-full" style="display: none;"> We report measurements of the flux-integrated $\bar谓_渭$ and $\bar谓_渭+谓_渭$ charged-current cross-sections on water and hydrocarbon targets using the T2K anti-neutrino beam, with a mean neutrino energy of 0.86 GeV. The signal is defined as the (anti-)neutrino charged-current interaction with one induced $渭^\pm$ and no detected charged pion nor proton. These measurements are performed using a new WAGASCI module recently added to the T2K setup in combination with the INGRID Proton module. The phase space of muons is restricted to the high-detection efficiency region, $p_渭>400~{\rm MeV}/c$ and $胃_渭<30^{\circ}$, in the laboratory frame. Absence of pions and protons in the detectable phase space of "$p_蟺>200~{\rm MeV}/c$ and $胃_蟺<70^{\circ}$", and "$p_{\rm p}>600~{\rm MeV}/c$ and $胃_{\rm p}<70^{\circ}$" is required. In this paper, both of the $\bar谓_渭$ cross-sections and $\bar谓_渭+谓_渭$ cross-sections on water and hydrocarbon targets, and their ratios are provided by using D'Agostini unfolding method. The results of the integrated $\bar谓_渭$ cross-section measurements over this phase space are $蟽_{\rm H_{2}O}\,=\,(1.082\pm0.068(\rm stat.)^{+0.145}_{-0.128}(\rm syst.)) \times 10^{-39}~{\rm cm^{2}/nucleon}$, $蟽_{\rm CH}\,=\,(1.096\pm0.054(\rm stat.)^{+0.132}_{-0.117}(\rm syst.)) \times 10^{-39}~{\rm cm^{2}/nucleon}$, and $蟽_{\rm H_{2}O}/蟽_{\rm CH} = 0.987\pm0.078(\rm stat.)^{+0.093}_{-0.090}(\rm syst.)$. The $\bar谓_渭+谓_渭$ cross-section is $蟽_{\rm H_{2}O} = (1.155\pm0.064(\rm stat.)^{+0.148}_{-0.129}(\rm syst.)) \times 10^{-39}~{\rm cm^{2}/nucleon}$, $蟽_{\rm CH}\,=\,(1.159\pm0.049(\rm stat.)^{+0.129}_{-0.115}(\rm syst.)) \times 10^{-39}~{\rm cm^{2}/nucleon}$, and $蟽_{\rm H_{2}O}/蟽_{\rm CH}\,=\,0.996\pm0.069(\rm stat.)^{+0.083}_{-0.078}(\rm syst.)$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.13989v1-abstract-full').style.display = 'none'; document.getElementById('2004.13989v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 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> Prog Theor Exp Phys (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.05434">arXiv:2004.05434</a> <span> [<a href="https://arxiv.org/pdf/2004.05434">pdf</a>, <a href="https://arxiv.org/format/2004.05434">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/10.1103/PhysRevD.101.112004">10.1103/PhysRevD.101.112004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simultaneous measurement of the muon neutrino charged-current cross section on oxygen and carbon without pions in the final state at T2K </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akhlaq%2C+N">N. Akhlaq</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Arihara%2C+T">T. Arihara</a>, <a href="/search/hep-ex?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barrow%2C+D">D. Barrow</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a> , et al. (308 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="2004.05434v2-abstract-short" style="display: inline;"> This paper reports the first simultaneous measurement of the double differential muon neutrino charged-current cross section on oxygen and carbon without pions in the final state as a function of the outgoing muon kinematics, made at the ND280 off-axis near detector of the T2K experiment. The ratio of the oxygen and carbon cross sections is also provided to help validate various models' ability to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.05434v2-abstract-full').style.display = 'inline'; document.getElementById('2004.05434v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.05434v2-abstract-full" style="display: none;"> This paper reports the first simultaneous measurement of the double differential muon neutrino charged-current cross section on oxygen and carbon without pions in the final state as a function of the outgoing muon kinematics, made at the ND280 off-axis near detector of the T2K experiment. The ratio of the oxygen and carbon cross sections is also provided to help validate various models' ability to extrapolate between carbon and oxygen nuclear targets, as is required in T2K oscillation analyses. The data are taken using a neutrino beam with an energy spectrum peaked at 0.6 GeV. The extracted measurement is compared with the prediction from different Monte Carlo neutrino-nucleus interaction event generators, showing particular model separation for very forward-going muons. Overall, of the models tested, the result is best described using Local Fermi Gas descriptions of the nuclear ground state with RPA suppression. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.05434v2-abstract-full').style.display = 'none'; document.getElementById('2004.05434v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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> Phys. Rev. D 101, 112004 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.11986">arXiv:2002.11986</a> <span> [<a href="https://arxiv.org/pdf/2002.11986">pdf</a>, <a href="https://arxiv.org/format/2002.11986">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/JHEP10(2020)114">10.1007/JHEP10(2020)114 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the charged-current electron (anti-)neutrino inclusive cross-sections at the T2K off-axis near detector ND280 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akhlaq%2C+N">N. Akhlaq</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Arihara%2C+T">T. Arihara</a>, <a href="/search/hep-ex?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barrow%2C+D">D. Barrow</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a> , et al. (344 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="2002.11986v2-abstract-short" style="display: inline;"> The electron (anti-)neutrino component of the T2K neutrino beam constitutes the largest background in the measurement of electron (anti-)neutrino appearance at the far detector. The electron neutrino scattering is measured directly with the T2K off-axis near detector, ND280. The selection of the electron (anti-)neutrino events in the plastic scintillator target from both neutrino and anti-neutrino… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.11986v2-abstract-full').style.display = 'inline'; document.getElementById('2002.11986v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.11986v2-abstract-full" style="display: none;"> The electron (anti-)neutrino component of the T2K neutrino beam constitutes the largest background in the measurement of electron (anti-)neutrino appearance at the far detector. The electron neutrino scattering is measured directly with the T2K off-axis near detector, ND280. The selection of the electron (anti-)neutrino events in the plastic scintillator target from both neutrino and anti-neutrino mode beams is discussed in this paper. The flux integrated single differential charged-current inclusive electron (anti-)neutrino cross-sections, $d蟽/dp$ and $d蟽/d\cos(胃)$, and the total cross-sections in a limited phase-space in momentum and scattering angle ($p > 300$ MeV/c and $胃\leq 45^{\circ}$) are measured using a binned maximum likelihood fit and compared to the neutrino Monte Carlo generator predictions, resulting in good agreement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.11986v2-abstract-full').style.display = 'none'; document.getElementById('2002.11986v2-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. High Energ. Phys. 2020, 114 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.09323">arXiv:2002.09323</a> <span> [<a href="https://arxiv.org/pdf/2002.09323">pdf</a>, <a href="https://arxiv.org/format/2002.09323">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/10.1103/PhysRevD.101.112001">10.1103/PhysRevD.101.112001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First combined measurement of the muon neutrino and antineutrino charged-current cross section without pions in the final state at T2K </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Arihara%2C+T">T. Arihara</a>, <a href="/search/hep-ex?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barrow%2C+D">D. Barrow</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a> , et al. (327 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="2002.09323v3-abstract-short" style="display: inline;"> This paper presents the first combined measurement of the double-differential muon neutrino and antineutrino charged-current cross sections with no pions in the final state on hydrocarbon at the off-axis near detector of the T2K experiment. The data analyzed in this work comprise 5.8$\times$10$^{20}$ and 6.3$\times$10$^{20}$ protons on target in neutrino and antineutrino mode respectively, at a be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.09323v3-abstract-full').style.display = 'inline'; document.getElementById('2002.09323v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.09323v3-abstract-full" style="display: none;"> This paper presents the first combined measurement of the double-differential muon neutrino and antineutrino charged-current cross sections with no pions in the final state on hydrocarbon at the off-axis near detector of the T2K experiment. The data analyzed in this work comprise 5.8$\times$10$^{20}$ and 6.3$\times$10$^{20}$ protons on target in neutrino and antineutrino mode respectively, at a beam energy peak of 0.6 GeV. Using the two measured cross sections, the sum, difference and asymmetry were calculated with the aim of better understanding the nuclear effects involved in such interactions. The extracted measurements have been compared with the prediction from different Monte Carlo generators and theoretical models showing that the difference between the two cross sections have interesting sensitivity to nuclear effects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.09323v3-abstract-full').style.display = 'none'; document.getElementById('2002.09323v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 112001 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.08011">arXiv:2001.08011</a> <span> [<a href="https://arxiv.org/pdf/2001.08011">pdf</a>, <a href="https://arxiv.org/format/2001.08011">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/10.1103/PhysRevD.101.052011">10.1103/PhysRevD.101.052011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for proton decay into three charged leptons in 0.37 megaton-years exposure of the Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Tanaka%2C+M">M. Tanaka</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/hep-ex?searchtype=author&query=Ito%2C+H">H. Ito</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Marti%2C+L">Ll. Marti</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a> , et al. (158 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.08011v2-abstract-short" style="display: inline;"> A search for proton decay into three charged leptons has been performed by using 0.37$\,$Mton$\cdot$years of data collected in Super-Kamiokande. All possible combinations of electrons, muons and their anti-particles consistent with charge conservation were considered as decay modes. No significant excess of events has been found over the background, and lower limits on the proton lifetime divided… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08011v2-abstract-full').style.display = 'inline'; document.getElementById('2001.08011v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08011v2-abstract-full" style="display: none;"> A search for proton decay into three charged leptons has been performed by using 0.37$\,$Mton$\cdot$years of data collected in Super-Kamiokande. All possible combinations of electrons, muons and their anti-particles consistent with charge conservation were considered as decay modes. No significant excess of events has been found over the background, and lower limits on the proton lifetime divided by the branching ratio have been obtained. The limits range between $9.2\times10^{33}$ to $3.4\times10^{34}$ years at 90$\,$% confidence level, improving by more than an order of magnitude upon limits from previous experiments. A first limit has been set for the $p\rightarrow渭^-e^+e^+$ mode. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08011v2-abstract-full').style.display = 'none'; document.getElementById('2001.08011v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 052011 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.07283">arXiv:1911.07283</a> <span> [<a href="https://arxiv.org/pdf/1911.07283">pdf</a>, <a href="https://arxiv.org/format/1911.07283">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/10.1103/PhysRevLett.124.161802">10.1103/PhysRevLett.124.161802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Electron Antineutrino Appearance in a Long-baseline Muon Antineutrino Beam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barrow%2C+D">D. Barrow</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a> , et al. (319 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="1911.07283v1-abstract-short" style="display: inline;"> Electron antineutrino appearance is measured by the T2K experiment in an accelerator-produced antineutrino beam, using additional neutrino beam operation to constrain parameters of the PMNS mixing matrix. T2K observes 15 candidate electron antineutrino events with a background expectation of 9.3 events. Including information from the kinematic distribution of observed events, the hypothesis of no… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.07283v1-abstract-full').style.display = 'inline'; document.getElementById('1911.07283v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.07283v1-abstract-full" style="display: none;"> Electron antineutrino appearance is measured by the T2K experiment in an accelerator-produced antineutrino beam, using additional neutrino beam operation to constrain parameters of the PMNS mixing matrix. T2K observes 15 candidate electron antineutrino events with a background expectation of 9.3 events. Including information from the kinematic distribution of observed events, the hypothesis of no electron antineutrino appearance is disfavored with a significance of 2.40蟽 and no discrepancy between data and PMNS predictions is found. A complementary analysis that introduces an additional free parameter which allows non-PMNS values of electron neutrino and antineutrino appearance also finds no discrepancy between data and PMNS predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.07283v1-abstract-full').style.display = 'none'; document.getElementById('1911.07283v1-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">arXiv admin note: text overlap with arXiv:1910.09439</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 124, 161802 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.09439">arXiv:1910.09439</a> <span> [<a href="https://arxiv.org/pdf/1910.09439">pdf</a>, <a href="https://arxiv.org/format/1910.09439">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/10.1103/PhysRevD.100.112009">10.1103/PhysRevD.100.112009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of neutrino and antineutrino neutral-current quasielastic-like interactions on oxygen by detecting nuclear de-excitation $纬$-rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a> , et al. (308 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.09439v2-abstract-short" style="display: inline;"> Neutrino- and antineutrino-oxygen neutral-current quasielastic-like interactions are measured at Super-Kamiokande using nuclear de-excitation $纬$-rays to identify signal-like interactions in data from a $14.94 \ (16.35)\times 10^{20}$ protons-on-target exposure of the T2K neutrino (antineutrino) beam. The measured flux-averaged cross sections on oxygen nuclei are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.09439v2-abstract-full').style.display = 'inline'; document.getElementById('1910.09439v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.09439v2-abstract-full" style="display: none;"> Neutrino- and antineutrino-oxygen neutral-current quasielastic-like interactions are measured at Super-Kamiokande using nuclear de-excitation $纬$-rays to identify signal-like interactions in data from a $14.94 \ (16.35)\times 10^{20}$ protons-on-target exposure of the T2K neutrino (antineutrino) beam. The measured flux-averaged cross sections on oxygen nuclei are $\langle 蟽_{谓{\rm -NCQE}} \rangle = 1.70 \pm 0.17 ({\rm stat.}) ^{+ {\rm 0.51}}_{- {\rm 0.38}} ({\rm syst.}) \times 10^{-38} \ {\rm cm^2/oxygen}$ with a flux-averaged energy of 0.82 GeV and $\langle 蟽_{\bar谓 {\rm -NCQE}} \rangle = 0.98 \pm 0.16 ({\rm stat.}) ^{+ {\rm 0.26}}_{- {\rm 0.19}} ({\rm syst.}) \times 10^{-38} \ {\rm cm^2/oxygen}$ with a flux-averaged energy of 0.68 GeV, for neutrinos and antineutrinos, respectively. These results are the most precise to date, and the antineutrino result is the first cross section measurement of this channel. They are compared with various theoretical predictions. The impact on evaluation of backgrounds to searches for supernova relic neutrinos at present and future water Cherenkov detectors is also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.09439v2-abstract-full').style.display = 'none'; document.getElementById('1910.09439v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 16 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 100, 112009 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.03887">arXiv:1910.03887</a> <span> [<a href="https://arxiv.org/pdf/1910.03887">pdf</a>, <a href="https://arxiv.org/format/1910.03887">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/10.1038/s41586-020-2177-0">10.1038/s41586-020-2177-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraint on the Matter-Antimatter Symmetry-Violating Phase in Neutrino Oscillations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a> , et al. (310 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.03887v3-abstract-short" style="display: inline;"> The current laws of physics do not explain the observed imbalance of matter and antimatter in the universe. Sakharov proposed that an explanation would require the violation of CP symmetry between matter and antimatter. The only CP violation observed so far is in the weak interactions of quarks, and it is too small to explain the matter-antimatter imbalance of the universe. It has been shown that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.03887v3-abstract-full').style.display = 'inline'; document.getElementById('1910.03887v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.03887v3-abstract-full" style="display: none;"> The current laws of physics do not explain the observed imbalance of matter and antimatter in the universe. Sakharov proposed that an explanation would require the violation of CP symmetry between matter and antimatter. The only CP violation observed so far is in the weak interactions of quarks, and it is too small to explain the matter-antimatter imbalance of the universe. It has been shown that CP violation in the lepton sector could generate the matter-antimatter disparity through the process called leptogenesis. The quantum mixing of neutrinos, the neutral leptons in the Standard Model, provides a potential source of CP violation through a complex phase dCP, which may have consequences for theoretical models of leptogenesis. This CP violation can be measured in muon neutrino to electron neutrino oscillations and the corresponding antineutrino oscillations, which are experimentally accessible with accelerator-produced beams as established by the T2K experiment. Until now, the value of dCP has not been significantly constrained by neutrino oscillation experiments. Here the T2K collaboration reports a measurement that favors large enhancement of the neutrino oscillation probability, excluding values of dCP which result in a large enhancement of the observed anti-neutrino oscillation probability at three standard deviations (3 sigma). The 3 sigma confidence level interval for dCP, which is cyclic and repeats every 2pi, is [-3.41,-0.03] for the so-called normal mass ordering, and [-2.54,-0.32] for the inverted mass ordering. Our results show an indication of CP violation in the lepton sector. Herein we establish methods for sensitive searches for matter-antimatter asymmetry in neutrino oscillations using accelerator-produced neutrino beams. Future measurements with larger data samples will determine whether the leptonic CP violation is larger than the quark sector CP violation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.03887v3-abstract-full').style.display = 'none'; document.getElementById('1910.03887v3-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature 580, 339-344 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.03936">arXiv:1909.03936</a> <span> [<a href="https://arxiv.org/pdf/1909.03936">pdf</a>, <a href="https://arxiv.org/format/1909.03936">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="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.101.012007">10.1103/PhysRevD.101.012007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the muon neutrino charged-current single $蟺^+$ production on hydrocarbon using the T2K off-axis near detector ND280 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Amey%2C+J">J. Amey</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Azuma%2C+Y">Y. Azuma</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berner%2C+R+M">R. M. Berner</a> , et al. (356 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="1909.03936v3-abstract-short" style="display: inline;"> We report the measurements of single and double differential cross section of muon neutrino charged-current interactions on carbon with a single positively charged pion in the final state at the T2K off-axis near detector using $5.56\times10^{20}$ protons on target. The analysis uses data control samples for the background subtraction and the cross section signal, defined as a single negatively ch… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.03936v3-abstract-full').style.display = 'inline'; document.getElementById('1909.03936v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.03936v3-abstract-full" style="display: none;"> We report the measurements of single and double differential cross section of muon neutrino charged-current interactions on carbon with a single positively charged pion in the final state at the T2K off-axis near detector using $5.56\times10^{20}$ protons on target. The analysis uses data control samples for the background subtraction and the cross section signal, defined as a single negatively charged muon and a single positively charged pion exiting from the target nucleus, is extracted using an unfolding method. The model dependent cross section, integrated over the T2K off-axis neutrino beam spectrum peaking at $0.6$~GeV, is measured to be $蟽= (11.76 \pm 0.44 \text{(stat)} \pm 2.39 \text{(syst)}) \times 10^{-40} \text{cm}^2$~$\text{nucleon}^{-1}$. Various differential cross sections are measured, including the first measurement of the Adler angles for single charged pion production in neutrino interactions with heavy nuclei target. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.03936v3-abstract-full').style.display = 'none'; document.getElementById('1909.03936v3-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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">Journal ref:</span> Phys. Rev. D 101, 012007 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.10249">arXiv:1908.10249</a> <span> [<a href="https://arxiv.org/pdf/1908.10249">pdf</a>, <a href="https://arxiv.org/format/1908.10249">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/10.1103/PhysRevD.102.012007">10.1103/PhysRevD.102.012007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Measurement of the Charged Current $\overline谓_渭$ Double Differential Cross Section on a Water Target without Pions in the final state </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Beloshapkin%2C+A">A. Beloshapkin</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a> , et al. (300 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="1908.10249v1-abstract-short" style="display: inline;"> This paper reports the first differential measurement of the charged-current $\overline谓_渭$ interaction cross section on water with no pions in the final state. The unfolded flux-averaged measurement using the T2K off-axis near detector is given in double differential bins of $渭^+$ momentum and angle. The integrated cross section in a restricted phase space is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.10249v1-abstract-full').style.display = 'inline'; document.getElementById('1908.10249v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.10249v1-abstract-full" style="display: none;"> This paper reports the first differential measurement of the charged-current $\overline谓_渭$ interaction cross section on water with no pions in the final state. The unfolded flux-averaged measurement using the T2K off-axis near detector is given in double differential bins of $渭^+$ momentum and angle. The integrated cross section in a restricted phase space is $蟽=\left(1.11\pm0.18\right)\times10^{-38}$ cm$^{2}$ per water molecule. Comparisons with several nuclear models are also presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.10249v1-abstract-full').style.display = 'none'; document.getElementById('1908.10249v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 102, 012007 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.09611">arXiv:1904.09611</a> <span> [<a href="https://arxiv.org/pdf/1904.09611">pdf</a>, <a href="https://arxiv.org/format/1904.09611">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 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/10.1093/ptep/ptz070">10.1093/ptep/ptz070 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the $谓_渭$ charged-current cross sections on water, hydrocarbon, iron, and their ratios with the T2K on-axis detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Azuma%2C+Y">Y. Azuma</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berner%2C+R+M">R. M. Berner</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a>, <a href="/search/hep-ex?searchtype=author&query=Blondely%2C+A">A. Blondely</a> , et al. (292 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.09611v1-abstract-short" style="display: inline;"> We report a measurement of the flux-integrated $谓_渭$ charged-current cross sections on water, hydrocarbon, and iron in the T2K on-axis neutrino beam with a mean neutrino energy of 1.5 GeV. The measured cross sections on water, hydrocarbon, and iron are $蟽^{\rm{H_{2}O}}_{\rm{CC}}$ = (0.840$\pm 0.010$(stat.)$^{+0.10}_{-0.08}$(syst.))$\times$10$^{-38}$cm$^2$/nucleon, $蟽^{\rm{CH}}_{\rm{CC}}$ = (0.817… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.09611v1-abstract-full').style.display = 'inline'; document.getElementById('1904.09611v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.09611v1-abstract-full" style="display: none;"> We report a measurement of the flux-integrated $谓_渭$ charged-current cross sections on water, hydrocarbon, and iron in the T2K on-axis neutrino beam with a mean neutrino energy of 1.5 GeV. The measured cross sections on water, hydrocarbon, and iron are $蟽^{\rm{H_{2}O}}_{\rm{CC}}$ = (0.840$\pm 0.010$(stat.)$^{+0.10}_{-0.08}$(syst.))$\times$10$^{-38}$cm$^2$/nucleon, $蟽^{\rm{CH}}_{\rm{CC}}$ = (0.817$\pm 0.007$(stat.)$^{+0.11}_{-0.08}$(syst.))$\times$10$^{-38}$cm$^2$/nucleon, and $蟽^{\rm{Fe}}_{\rm{CC}}$ = (0.859$\pm 0.003$(stat.) $^{+0.12}_{-0.10}$(syst.))$\times$10$^{-38}$cm$^2$/nucleon respectively, for a restricted phase space of induced muons: $胃_渭<45^{\circ}$ and $p_渭>$0.4 GeV/$c$ in the laboratory frame. The measured cross section ratios are ${蟽^{\rm{H_{2}O}}_{\rm{CC}}}/{蟽^{\rm{CH}}_{\rm{CC}}}$ = 1.028$\pm 0.016$(stat.)$\pm 0.053$(syst.), ${蟽^{\rm{Fe}}_{\rm{CC}}}/{蟽^{\rm{H_{2}O}}_{\rm{CC}}}$ = 1.023$\pm 0.012$(stat.)$\pm 0.058$(syst.), and ${蟽^{\rm{Fe}}_{\rm{CC}}}/{蟽^{\rm{CH}}_{\rm{CC}}}$ = 1.049$\pm 0.010$(stat.)$\pm 0.043$(syst.). These results, with an unprecedented precision for the measurements of neutrino cross sections on water in the studied energy region, show good agreement with the current neutrino interaction models used in the T2K oscillation analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.09611v1-abstract-full').style.display = 'none'; document.getElementById('1904.09611v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Prog Theor Exp Phys (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.07598">arXiv:1902.07598</a> <span> [<a href="https://arxiv.org/pdf/1902.07598">pdf</a>, <a href="https://arxiv.org/ps/1902.07598">ps</a>, <a href="https://arxiv.org/format/1902.07598">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/10.1103/PhysRevD.100.052006">10.1103/PhysRevD.100.052006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for heavy neutrinos with the T2K near detector ND280 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Azuma%2C+Y">Y. Azuma</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berner%2C+R+M">R. M. Berner</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a>, <a href="/search/hep-ex?searchtype=author&query=Blondel%2C+A">A. Blondel</a> , et al. (303 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="1902.07598v2-abstract-short" style="display: inline;"> This paper reports on the search for heavy neutrinos with masses in the range $140 < M_N < 493$ MeV/c$^2$ using the off-axis near detector ND280 of the T2K experiment. These particles can be produced from kaon decays in the standard neutrino beam and then subsequently decay in ND280. The decay modes under consideration are $N \to \ell^{\pm}_伪蟺^{\mp}$ and $N \to \ell^+_伪 \ell^-_尾谓(\bar谓)$ (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.07598v2-abstract-full').style.display = 'inline'; document.getElementById('1902.07598v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.07598v2-abstract-full" style="display: none;"> This paper reports on the search for heavy neutrinos with masses in the range $140 < M_N < 493$ MeV/c$^2$ using the off-axis near detector ND280 of the T2K experiment. These particles can be produced from kaon decays in the standard neutrino beam and then subsequently decay in ND280. The decay modes under consideration are $N \to \ell^{\pm}_伪蟺^{\mp}$ and $N \to \ell^+_伪 \ell^-_尾谓(\bar谓)$ ($伪,尾=e,渭$). A search for such events has been made using the Time Projection Chambers of ND280, where the background has been reduced to less than two events in the current dataset in all channels. No excess has been observed in the signal region. A combined Bayesian statistical approach has been applied to extract upper limits on the mixing elements of heavy neutrinos to electron-, muon- and tau- flavoured currents ($U_e^2$, $U_渭^2$, $U_蟿^2$) as a function of the heavy neutrino mass, e.g. $U_e^2 < 10^{-9}$ at $90\%$ C.L. for a mass of $390$ MeV/c$^2$. These constraints are competitive with previous experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.07598v2-abstract-full').style.display = 'none'; document.getElementById('1902.07598v2-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 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">9 pages, 7 figures Version submitted to PRD: https://journals.aps.org/prd/pdf/10.1103/PhysRevD.100.052006</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 100, 052006 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.06529">arXiv:1902.06529</a> <span> [<a href="https://arxiv.org/pdf/1902.06529">pdf</a>, <a href="https://arxiv.org/format/1902.06529">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/10.1103/PhysRevD.99.071103">10.1103/PhysRevD.99.071103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for light sterile neutrinos with the T2K far detector Super-Kamiokande at a baseline of 295 km </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Azuma%2C+Y">Y. Azuma</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berner%2C+R+M">R. M. Berner</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a>, <a href="/search/hep-ex?searchtype=author&query=Blondel%2C+A">A. Blondel</a> , et al. (296 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="1902.06529v3-abstract-short" style="display: inline;"> We perform a search for light sterile neutrinos using the data from the T2K far detector at a baseline of 295 km, with an exposure of 14.7 (7.6)$\times 10^{20}$ protons on target in neutrino (antineutrino) mode. A selection of neutral current interaction samples are also used to enhance the sensitivity to sterile mixing. No evidence of sterile neutrino mixing in the 3+1 model was found from a simu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.06529v3-abstract-full').style.display = 'inline'; document.getElementById('1902.06529v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.06529v3-abstract-full" style="display: none;"> We perform a search for light sterile neutrinos using the data from the T2K far detector at a baseline of 295 km, with an exposure of 14.7 (7.6)$\times 10^{20}$ protons on target in neutrino (antineutrino) mode. A selection of neutral current interaction samples are also used to enhance the sensitivity to sterile mixing. No evidence of sterile neutrino mixing in the 3+1 model was found from a simultaneous fit to the charged-current muon, electron and neutral current neutrino samples. We set the most stringent limit on the sterile oscillation amplitude $\sin^2胃_{24}$ for the sterile neutrino mass splitting $螖m^2_{41}<3\times 10^{-3}$ eV$^2/c^4$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.06529v3-abstract-full').style.display = 'none'; document.getElementById('1902.06529v3-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 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">9 pages, 4 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 99, 071103 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.03848">arXiv:1902.03848</a> <span> [<a href="https://arxiv.org/pdf/1902.03848">pdf</a>, <a href="https://arxiv.org/format/1902.03848">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/10.1088/1361-6471/ab227d">10.1088/1361-6471/ab227d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for neutral-current induced single photon production at the ND280 near detector in T2K </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Awataguchi%2C+Y">Y. Awataguchi</a>, <a href="/search/hep-ex?searchtype=author&query=Azuma%2C+Y">Y. Azuma</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berner%2C+R+M">R. M. Berner</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a>, <a href="/search/hep-ex?searchtype=author&query=Blondel%2C+A">A. Blondel</a> , et al. (292 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="1902.03848v1-abstract-short" style="display: inline;"> Neutrino neutral-current induced single photon production is a sub-leading order process for accelerator-based neutrino beam experiments including T2K. It is, however, an important process to understand because it is a background for electron (anti)neutrino appearance oscillation experiments. Here, we performed the first search of this process below 1 GeV using the fine-grained detector at the T2K… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.03848v1-abstract-full').style.display = 'inline'; document.getElementById('1902.03848v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.03848v1-abstract-full" style="display: none;"> Neutrino neutral-current induced single photon production is a sub-leading order process for accelerator-based neutrino beam experiments including T2K. It is, however, an important process to understand because it is a background for electron (anti)neutrino appearance oscillation experiments. Here, we performed the first search of this process below 1 GeV using the fine-grained detector at the T2K ND280 off-axis near detector. By reconstructing single photon kinematics from electron-positron pairs, we achieved 95\% pure gamma ray sample from 5.738$\times 10^{20}$ protons-on-targets neutrino mode data. We do not find positive evidence of neutral current induced single photon production in this sample. We set the model-dependent upper limit on the cross-section for this process, at 0.114$\times 10^{-38}$ cm$^2$ (90\% C.L.) per nucleon, using the J-PARC off-axis neutrino beam with an average energy of $\left<E_谓\right>\sim 0.6$ GeV. This is the first limit on this process below 1 GeV which is important for current and future oscillation experiments looking for electron neutrino appearance oscillation signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.03848v1-abstract-full').style.display = 'none'; document.getElementById('1902.03848v1-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 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">5 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Phys. G 46, 08LT01 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.05281">arXiv:1901.05281</a> <span> [<a href="https://arxiv.org/pdf/1901.05281">pdf</a>, <a href="https://arxiv.org/ps/1901.05281">ps</a>, <a href="https://arxiv.org/format/1901.05281">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/10.1103/PhysRevD.99.032005">10.1103/PhysRevD.99.032005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of neutrino-oxygen neutral-current quasi-elastic cross section using atmospheric neutrinos at Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Wan%2C+L">L. Wan</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Marti%2C+L">Ll. Marti</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a> , et al. (143 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="1901.05281v1-abstract-short" style="display: inline;"> Neutral current (NC) interactions of atmospheric neutrinos on oxygen form one of the major backgrounds in the search for supernova relic neutrinos with water-based Cherenkov detectors. The NC channel is dominated by neutrino quasi-elastic (NCQE) scattering off nucleons inside $^{16}$O nuclei. In this paper we report the first measurement of NCQE cross section using atmospheric neutrinos at Super-K… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.05281v1-abstract-full').style.display = 'inline'; document.getElementById('1901.05281v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.05281v1-abstract-full" style="display: none;"> Neutral current (NC) interactions of atmospheric neutrinos on oxygen form one of the major backgrounds in the search for supernova relic neutrinos with water-based Cherenkov detectors. The NC channel is dominated by neutrino quasi-elastic (NCQE) scattering off nucleons inside $^{16}$O nuclei. In this paper we report the first measurement of NCQE cross section using atmospheric neutrinos at Super-Kamiokande (SK). The measurement used 2,778 live days of SK-IV data with a fiducial volume of 22.5 kiloton water. Within the visible energy window of 7.5-29.5 MeV, we observed $117$ events compared to the expected $71.9$ NCQE signal and $53.1$ background events. Weighted by the atmospheric neutrino spectrum from 160 MeV to 10 GeV, the flux averaged NCQE cross section is measured to be $(1.01\pm0.17(\text{stat.})^{+0.78}_{-0.30}(\text{sys.}))\times10^{-38}$ cm$^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.05281v1-abstract-full').style.display = 'none'; document.getElementById('1901.05281v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 9 figures, submitted to PRD</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 99, 032005 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.03230">arXiv:1901.03230</a> <span> [<a href="https://arxiv.org/pdf/1901.03230">pdf</a>, <a href="https://arxiv.org/format/1901.03230">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/10.1093/ptep/ptz015">10.1093/ptep/ptz015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Atmospheric Neutrino Oscillation Analysis With Improved Event Reconstruction in Super-Kamiokande IV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Jiang%2C+M">M. Jiang</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Marti%2C+L">Ll. Marti</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a> , et al. (146 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="1901.03230v1-abstract-short" style="display: inline;"> A new event reconstruction algorithm based on a maximum likelihood method has been developed for Super-Kamiokande. Its improved kinematic and particle identification capabilities enable the analysis of atmospheric neutrino data in a detector volume 32% larger than previous analyses and increases sensitivity to the neutrino mass hierarchy. Analysis of a 253.9 kton-year exposure of the Super-Kamioka… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.03230v1-abstract-full').style.display = 'inline'; document.getElementById('1901.03230v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.03230v1-abstract-full" style="display: none;"> A new event reconstruction algorithm based on a maximum likelihood method has been developed for Super-Kamiokande. Its improved kinematic and particle identification capabilities enable the analysis of atmospheric neutrino data in a detector volume 32% larger than previous analyses and increases sensitivity to the neutrino mass hierarchy. Analysis of a 253.9 kton-year exposure of the Super-Kamiokande IV atmospheric neutrino data has yielded a weak preference for the normal hierarchy, disfavoring the inverted hierarchy at 74% assuming oscillations at the best fit of the analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.03230v1-abstract-full').style.display = 'none'; document.getElementById('1901.03230v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">42 pages, 28 figures, submitted to PTEP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Prog Theor Exp Phys (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.12430">arXiv:1811.12430</a> <span> [<a href="https://arxiv.org/pdf/1811.12430">pdf</a>, <a href="https://arxiv.org/format/1811.12430">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"> Dinucleon and Nucleon Decay to Two-Body Final States with no Hadrons in Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Sussman%2C+S">S. Sussman</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Marti%2C+L">Ll. Marti</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a> , et al. (146 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="1811.12430v1-abstract-short" style="display: inline;"> Using 0.37 megaton$\cdot$years of exposure from the Super-Kamiokande detector, we search for 10 dinucleon and nucleon decay modes that have a two-body final state with no hadrons. These baryon and lepton number violating modes have the potential to probe theories of unification and baryogenesis. For five of these modes the searches are novel, and for the other five modes we improve the limits by m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.12430v1-abstract-full').style.display = 'inline'; document.getElementById('1811.12430v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.12430v1-abstract-full" style="display: none;"> Using 0.37 megaton$\cdot$years of exposure from the Super-Kamiokande detector, we search for 10 dinucleon and nucleon decay modes that have a two-body final state with no hadrons. These baryon and lepton number violating modes have the potential to probe theories of unification and baryogenesis. For five of these modes the searches are novel, and for the other five modes we improve the limits by more than one order of magnitude. No significant evidence for dinucleon or nucleon decay is observed and we set lower limits on the partial lifetime of oxygen nuclei and on the nucleon partial lifetime that are above $4\times 10^{33}$ years for oxygen via the dinucleon decay modes and up to about $4 \times 10^{34}$ years for nucleons via the single nucleon decay modes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.12430v1-abstract-full').style.display = 'none'; document.getElementById('1811.12430v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.07891">arXiv:1807.07891</a> <span> [<a href="https://arxiv.org/pdf/1807.07891">pdf</a>, <a href="https://arxiv.org/format/1807.07891">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/10.1103/PhysRevLett.121.171802">10.1103/PhysRevLett.121.171802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for CP violation in Neutrino and Antineutrino Oscillations by the T2K experiment with $2.2\times10^{21}$ protons on target </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=Amey%2C+J">J. Amey</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Azuma%2C+Y">Y. Azuma</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz%2C+M">M. Batkiewicz</a>, <a href="/search/hep-ex?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berner%2C+R+M">R. M. Berner</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a>, <a href="/search/hep-ex?searchtype=author&query=Blondel%2C+A">A. Blondel</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="1807.07891v3-abstract-short" style="display: inline;"> The T2K experiment measures muon neutrino disappearance and electron neutrino appearance in accelerator-produced neutrino and antineutrino beams. With an exposure of $14.7(7.6)\times 10^{20}$ protons on target in neutrino (antineutrino) mode, 89 $谓_e$ candidates and 7 anti-$谓_e$ candidates were observed while 67.5 and 9.0 are expected for $未_{CP}=0$ and normal mass ordering. The obtained $2蟽$ conf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.07891v3-abstract-full').style.display = 'inline'; document.getElementById('1807.07891v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.07891v3-abstract-full" style="display: none;"> The T2K experiment measures muon neutrino disappearance and electron neutrino appearance in accelerator-produced neutrino and antineutrino beams. With an exposure of $14.7(7.6)\times 10^{20}$ protons on target in neutrino (antineutrino) mode, 89 $谓_e$ candidates and 7 anti-$谓_e$ candidates were observed while 67.5 and 9.0 are expected for $未_{CP}=0$ and normal mass ordering. The obtained $2蟽$ confidence interval for the $CP$ violating phase, $未_{CP}$, does not include the $CP$-conserving cases ($未_{CP}=0,蟺$). The best-fit values of other parameters are $\sin^2胃_{23} = 0.526^{+0.032}_{-0.036}$ and $螖m^2_{32}=2.463^{+0.071}_{-0.070}\times10^{-3} \mathrm{eV}^2/c^4$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.07891v3-abstract-full').style.display = 'none'; document.getElementById('1807.07891v3-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 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">9 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 121, 171802 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.04163">arXiv:1805.04163</a> <span> [<a href="https://arxiv.org/pdf/1805.04163">pdf</a>, <a href="https://arxiv.org/format/1805.04163">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="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> <p class="title is-5 mathjax"> Hyper-Kamiokande Design Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Proto-Collaboration%2C+H">Hyper-Kamiokande Proto-Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">Ke. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Aihara%2C+H">H. Aihara</a>, <a href="/search/hep-ex?searchtype=author&query=Aimi%2C+A">A. Aimi</a>, <a href="/search/hep-ex?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anghel%2C+I">I. Anghel</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L+H+V">L. H. V. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Aushev%2C+V">V. Aushev</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Berry%2C+T">T. Berry</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo-Bergu%C3%B1o%2C+D">D. Bravo-Bergu帽o</a>, <a href="/search/hep-ex?searchtype=author&query=Blaszczyk%2C+F+d+M">F. d. M. Blaszczyk</a> , et al. (291 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="1805.04163v2-abstract-short" style="display: inline;"> On the strength of a double Nobel prize winning experiment (Super)Kamiokande and an extremely successful long baseline neutrino programme, the third generation Water Cherenkov detector, Hyper-Kamiokande, is being developed by an international collaboration as a leading worldwide experiment based in Japan. The Hyper-Kamiokande detector will be hosted in the Tochibora mine, about 295 km away from th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.04163v2-abstract-full').style.display = 'inline'; document.getElementById('1805.04163v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.04163v2-abstract-full" style="display: none;"> On the strength of a double Nobel prize winning experiment (Super)Kamiokande and an extremely successful long baseline neutrino programme, the third generation Water Cherenkov detector, Hyper-Kamiokande, is being developed by an international collaboration as a leading worldwide experiment based in Japan. The Hyper-Kamiokande detector will be hosted in the Tochibora mine, about 295 km away from the J-PARC proton accelerator research complex in Tokai, Japan. The currently existing accelerator will be steadily upgraded to reach a MW beam by the start of the experiment. A suite of near detectors will be vital to constrain the beam for neutrino oscillation measurements. A new cavern will be excavated at the Tochibora mine to host the detector. The experiment will be the largest underground water Cherenkov detector in the world and will be instrumented with new technology photosensors, faster and with higher quantum efficiency than the ones in Super-Kamiokande. The science that will be developed will be able to shape the future theoretical framework and generations of experiments. Hyper-Kamiokande will be able to measure with the highest precision the leptonic CP violation that could explain the baryon asymmetry in the Universe. The experiment also has a demonstrated excellent capability to search for proton decay, providing a significant improvement in discovery sensitivity over current searches for the proton lifetime. The atmospheric neutrinos will allow to determine the neutrino mass ordering and, together with the beam, able to precisely test the three-flavour neutrino oscillation paradigm and search for new phenomena. A strong astrophysical programme will be carried out at the experiment that will detect supernova neutrinos and will measure precisely solar neutrino oscillation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.04163v2-abstract-full').style.display = 'none'; document.getElementById('1805.04163v2-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">325 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.05078">arXiv:1802.05078</a> <span> [<a href="https://arxiv.org/pdf/1802.05078">pdf</a>, <a href="https://arxiv.org/format/1802.05078">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/10.1103/PhysRevD.98.032003">10.1103/PhysRevD.98.032003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterisation of nuclear effects in muon-neutrino scattering on hydrocarbon with a measurement of final-state kinematics and correlations in charged-current pionless interactions at T2K </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Amey%2C+J">J. Amey</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Azuma%2C+Y">Y. Azuma</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz%2C+M">M. Batkiewicz</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berner%2C+R+M">R. M. Berner</a>, <a href="/search/hep-ex?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a>, <a href="/search/hep-ex?searchtype=author&query=Blondel%2C+A">A. Blondel</a>, <a href="/search/hep-ex?searchtype=author&query=Bolognesi%2C+S">S. Bolognesi</a>, <a href="/search/hep-ex?searchtype=author&query=Bordoni%2C+S">S. Bordoni</a>, <a href="/search/hep-ex?searchtype=author&query=Bourguille%2C+B">B. Bourguille</a> , et al. (280 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="1802.05078v3-abstract-short" style="display: inline;"> This paper reports measurements of final-state proton multiplicity, muon and proton kinematics, and their correlations in charged-current pionless neutrino interactions, measured by the T2K ND280 near detector in its plastic scintillator (C$_8$H$_8$) target. The data were taken between years 2010 and 2013, corresponding to approximately 6$\times10^{20}$ protons on target. Thanks to their explorati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.05078v3-abstract-full').style.display = 'inline'; document.getElementById('1802.05078v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.05078v3-abstract-full" style="display: none;"> This paper reports measurements of final-state proton multiplicity, muon and proton kinematics, and their correlations in charged-current pionless neutrino interactions, measured by the T2K ND280 near detector in its plastic scintillator (C$_8$H$_8$) target. The data were taken between years 2010 and 2013, corresponding to approximately 6$\times10^{20}$ protons on target. Thanks to their exploration of the proton kinematics and of kinematic imbalances between the proton and muon kinematics, the results offer a novel probe of the nuclear-medium effects most pertinent to the (sub-)GeV neutrino-nucleus interactions that are used in accelerator-based long-baseline neutrino oscillation measurements. These results are compared to many neutrino-nucleus interaction models which all fail to describe at least part of the observed phase space. In case of events without a proton above a detection threshold in the final state, a fully consistent implementation of the local Fermi gas model with multinucleon interactions gives the best description of the data. In the case of at least one proton in the final state the spectral function model agrees well with the data, most notably when measuring the kinematic imbalance between the muon and the proton in the plane transverse to the incoming neutrino. A clear indication of existence of multinucleon interactions is observed. The effect of final-state interactions is also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.05078v3-abstract-full').style.display = 'none'; document.getElementById('1802.05078v3-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 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">49 pages, 31 figures - version submitted to PRD following comments from referee</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 98, 032003 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.05148">arXiv:1801.05148</a> <span> [<a href="https://arxiv.org/pdf/1801.05148">pdf</a>, <a href="https://arxiv.org/format/1801.05148">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/10.1103/PhysRevD.98.012004">10.1103/PhysRevD.98.012004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of inclusive double-differential $谓_渭$ charged-current cross section with improved acceptance in the T2K off-axis near detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=T2K+Collaboration"> T2K Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Amey%2C+J">J. Amey</a>, <a href="/search/hep-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Anthony%2C+L">L. Anthony</a>, <a href="/search/hep-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ex?searchtype=author&query=Azuma%2C+Y">Y. Azuma</a>, <a href="/search/hep-ex?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/hep-ex?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/hep-ex?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/hep-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+C">C. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz%2C+M">M. Batkiewicz</a>, <a href="/search/hep-ex?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/hep-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/hep-ex?searchtype=author&query=Berner%2C+R+M">R. M. Berner</a>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Bienstock%2C+S">S. Bienstock</a>, <a href="/search/hep-ex?searchtype=author&query=Blondel%2C+A">A. Blondel</a>, <a href="/search/hep-ex?searchtype=author&query=Bolognesi%2C+S">S. Bolognesi</a>, <a href="/search/hep-ex?searchtype=author&query=Bordoni%2C+S">S. Bordoni</a>, <a href="/search/hep-ex?searchtype=author&query=Bourguille%2C+B">B. Bourguille</a> , et al. (280 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="1801.05148v2-abstract-short" style="display: inline;"> We report a measurement of the flux-integrated cross section for inclusive muon neutrino charged-current interactions on carbon. The double differential measurements are given as function of the muon momentum and angle. Relative to our previous publication on this topic, these results have an increased angular acceptance and higher statistics. The data sample presented here corresponds to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.05148v2-abstract-full').style.display = 'inline'; document.getElementById('1801.05148v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.05148v2-abstract-full" style="display: none;"> We report a measurement of the flux-integrated cross section for inclusive muon neutrino charged-current interactions on carbon. The double differential measurements are given as function of the muon momentum and angle. Relative to our previous publication on this topic, these results have an increased angular acceptance and higher statistics. The data sample presented here corresponds to $5.7 \times 10^{20}$ protons-on-target. The total flux-integrated cross section is measured to be $(6.950 \pm 0.662) \times 10^{-39}$ cm$^2$nucleon$^{-1}$ and is consistent with our simulation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.05148v2-abstract-full').style.display = 'none'; document.getElementById('1801.05148v2-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 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 98, 012004 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.09436">arXiv:1711.09436</a> <span> [<a href="https://arxiv.org/pdf/1711.09436">pdf</a>, <a href="https://arxiv.org/format/1711.09436">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/10.1103/PhysRevD.98.052006">10.1103/PhysRevD.98.052006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Measurement of the Tau Neutrino Cross Section in Atmospheric Neutrino Oscillations with Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Li%2C+Z">Z. Li</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/hep-ex?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/hep-ex?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/hep-ex?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Marti%2C+L">Ll. Marti</a>, <a href="/search/hep-ex?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/hep-ex?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/hep-ex?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/hep-ex?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/hep-ex?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/hep-ex?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/hep-ex?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/hep-ex?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/hep-ex?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a>, <a href="/search/hep-ex?searchtype=author&query=Takeda%2C+A">A. Takeda</a>, <a href="/search/hep-ex?searchtype=author&query=Takenaka%2C+A">A. Takenaka</a> , et al. (139 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="1711.09436v1-abstract-short" style="display: inline;"> Using 5,326 days of atmospheric neutrino data, a search for atmospheric tau neutrino appearance has been performed in the Super-Kamiokande experiment. Super-Kamiokande measures the tau normalization to be 1.47$\pm$0.32 under the assumption of normal neutrino hierarchy, relative to the expectation of unity with neutrino oscillation. The result excludes the hypothesis of no-tau-appearance with a sig… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.09436v1-abstract-full').style.display = 'inline'; document.getElementById('1711.09436v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.09436v1-abstract-full" style="display: none;"> Using 5,326 days of atmospheric neutrino data, a search for atmospheric tau neutrino appearance has been performed in the Super-Kamiokande experiment. Super-Kamiokande measures the tau normalization to be 1.47$\pm$0.32 under the assumption of normal neutrino hierarchy, relative to the expectation of unity with neutrino oscillation. The result excludes the hypothesis of no-tau-appearance with a significance level of 4.6$蟽$. The inclusive charged-current tau neutrino cross section averaged by the tau neutrino flux at Super-Kamiokande is measured to be $(0.94\pm0.20)\times 10^{-38}$ cm$^{2}$. The measurement is consistent with the Standard Model prediction, agreeing to within 1.5$蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.09436v1-abstract-full').style.display = 'none'; document.getElementById('1711.09436v1-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 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 98, 052006 (2018) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Anthony%2C+L&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Anthony%2C+L&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Anthony%2C+L&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> 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