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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.17002">arXiv:2502.17002</a> <span> [<a href="https://arxiv.org/pdf/2502.17002">pdf</a>, <a href="https://arxiv.org/format/2502.17002">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> <p class="title is-5 mathjax"> Neutron multiplicity measurement in muon capture on oxygen nuclei in the Gd-loaded 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=Miki%2C+S">S. Miki</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=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>, <a href="/search/hep-ex?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a> , et al. (265 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.17002v1-abstract-short" style="display: inline;"> In recent neutrino detectors, neutrons produced in neutrino reactions play an important role. Muon capture on oxygen nuclei is one of the processes that produce neutrons in water Cherenkov detectors. We measured neutron multiplicity in the process using cosmic ray muons that stop in the gadolinium-loaded Super-Kamiokande detector. For this measurement, neutron detection efficiency is obtained with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17002v1-abstract-full').style.display = 'inline'; document.getElementById('2502.17002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.17002v1-abstract-full" style="display: none;"> In recent neutrino detectors, neutrons produced in neutrino reactions play an important role. Muon capture on oxygen nuclei is one of the processes that produce neutrons in water Cherenkov detectors. We measured neutron multiplicity in the process using cosmic ray muons that stop in the gadolinium-loaded Super-Kamiokande detector. For this measurement, neutron detection efficiency is obtained with the muon capture events followed by gamma rays to be $50.2^{+2.0}_{-2.1}\%$. By fitting the observed multiplicity considering the detection efficiency, we measure neutron multiplicity in muon capture as $P(0)=24\pm3\%$, $P(1)=70^{+3}_{-2}\%$, $P(2)=6.1\pm0.5\%$, $P(3)=0.38\pm0.09\%$. This is the first measurement of the multiplicity of neutrons associated with muon capture without neutron energy threshold. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17002v1-abstract-full').style.display = 'none'; document.getElementById('2502.17002v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2308.16606">arXiv:2308.16606</a> <span> [<a href="https://arxiv.org/pdf/2308.16606">pdf</a>, <a href="https://arxiv.org/ps/2308.16606">ps</a>, <a href="https://arxiv.org/format/2308.16606">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.108.092009">10.1103/PhysRevD.108.092009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of the $谓_渭$ and $\bar谓_渭$-induced Coherent Charged Pion Production Cross Sections on $^{12}C$ by the T2K experiment </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=Monsalve%2C+S+A">S. Alonso Monsalve</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=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=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=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=Berardi%2C+V">V. Berardi</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=Blanchet%2C+A">A. Blanchet</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=Bonus%2C+T">T. Bonus</a> , et al. (359 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.16606v2-abstract-short" style="display: inline;"> We report an updated measurement of the $谓_渭$-induced, and the first measurement of the $\bar谓_渭$-induced coherent charged pion production cross section on $^{12}C$ nuclei in the T2K experiment. This is measured in a restricted region of the final-state phase space for which $p_{渭,蟺} > 0.2$ GeV, $\cos(胃_渭) > 0.8$ and $\cos(胃_蟺) > 0.6$, and at a mean (anti)neutrino energy of 0.85 GeV using the T2K… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16606v2-abstract-full').style.display = 'inline'; document.getElementById('2308.16606v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.16606v2-abstract-full" style="display: none;"> We report an updated measurement of the $谓_渭$-induced, and the first measurement of the $\bar谓_渭$-induced coherent charged pion production cross section on $^{12}C$ nuclei in the T2K experiment. This is measured in a restricted region of the final-state phase space for which $p_{渭,蟺} > 0.2$ GeV, $\cos(胃_渭) > 0.8$ and $\cos(胃_蟺) > 0.6$, and at a mean (anti)neutrino energy of 0.85 GeV using the T2K near detector. The measured $谓_渭$ CC coherent pion production flux-averaged cross section on $^{12}C$ is $(2.98 \pm 0.37 (stat.) \pm 0.31 (syst.) \substack{ +0.49 \\ -0.00 } \mathrm{ (Q^2\,model)}) \times 10^{-40}~\mathrm{cm}^{2}$. The new measurement of the $\bar谓_渭$-induced cross section on $^{12}{C}$ is $(3.05 \pm 0.71 (stat.) \pm 0.39 (syst.) \substack{ +0.74 \\ -0.00 } \mathrm{(Q^2\,model)}) \times 10^{-40}~\mathrm{cm}^{2}$. The results are compatible with both the NEUT 5.4.0 Berger-Sehgal (2009) and GENIE 2.8.0 Rein-Sehgal (2007) model predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16606v2-abstract-full').style.display = 'none'; document.getElementById('2308.16606v2-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D 108 (2023) 9, 092009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.09916">arXiv:2305.09916</a> <span> [<a href="https://arxiv.org/pdf/2305.09916">pdf</a>, <a href="https://arxiv.org/format/2305.09916">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"> Updated T2K measurements of muon neutrino and antineutrino disappearance using 3.6 $\times$ 10$^{21}$ 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=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=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=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=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=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=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>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Blanchet%2C+A">A. Blanchet</a> , et al. (385 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="2305.09916v2-abstract-short" style="display: inline;"> Muon neutrino and antineutrino disappearance probabilities are identical in the standard three-flavor neutrino oscillation framework, but CPT violation and non-standard interactions can violate this symmetry. In this work we report the measurements of $\sin^{2} 胃_{23}$ and $螖m_{32}^2$ independently for neutrinos and antineutrinos. The aforementioned symmetry violation would manifest as an inconsis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.09916v2-abstract-full').style.display = 'inline'; document.getElementById('2305.09916v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.09916v2-abstract-full" style="display: none;"> Muon neutrino and antineutrino disappearance probabilities are identical in the standard three-flavor neutrino oscillation framework, but CPT violation and non-standard interactions can violate this symmetry. In this work we report the measurements of $\sin^{2} 胃_{23}$ and $螖m_{32}^2$ independently for neutrinos and antineutrinos. The aforementioned symmetry violation would manifest as an inconsistency in the neutrino and antineutrino oscillation parameters. The analysis discussed here uses a total of 1.97$\times$10$^{21}$ and 1.63$\times$10$^{21}$ protons on target taken with a neutrino and antineutrino beam respectively, and benefits from improved flux and cross-section models, new near detector samples and more than double the data reducing the overall uncertainty of the result. No significant deviation is observed, consistent with the standard neutrino oscillation picture. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.09916v2-abstract-full').style.display = 'none'; document.getElementById('2305.09916v2-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 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/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/2303.14228">arXiv:2303.14228</a> <span> [<a href="https://arxiv.org/pdf/2303.14228">pdf</a>, <a href="https://arxiv.org/format/2303.14228">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.108.112009">10.1103/PhysRevD.108.112009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First measurement of muon neutrino charged-current interactions on hydrocarbon without pions in the final state using multiple detectors with correlated energy spectra 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=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=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=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=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=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=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>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Blanchet%2C+A">A. Blanchet</a> , et al. (380 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="2303.14228v2-abstract-short" style="display: inline;"> This paper reports the first measurement of muon neutrino charged-current interactions without pions in the final state using multiple detectors with correlated energy spectra at T2K. The data was collected on hydrocarbon targets using the off-axis T2K near detector (ND280) and the on-axis T2K near detector (INGRID) with neutrino energy spectra peaked at 0.6 GeV and 1.1 GeV respectively. The corre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14228v2-abstract-full').style.display = 'inline'; document.getElementById('2303.14228v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.14228v2-abstract-full" style="display: none;"> This paper reports the first measurement of muon neutrino charged-current interactions without pions in the final state using multiple detectors with correlated energy spectra at T2K. The data was collected on hydrocarbon targets using the off-axis T2K near detector (ND280) and the on-axis T2K near detector (INGRID) with neutrino energy spectra peaked at 0.6 GeV and 1.1 GeV respectively. The correlated neutrino flux presents an opportunity to reduce the impact of the flux uncertainty and to study the energy dependence of neutrino interactions. The extracted double-differential cross sections are compared to several Monte Carlo neutrino-nucleus interaction event generators showing the agreement between both detectors individually and with the correlated result. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14228v2-abstract-full').style.display = 'none'; document.getElementById('2303.14228v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Updated discussion in Sec. V-A; Updated author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.04481">arXiv:2303.04481</a> <span> [<a href="https://arxiv.org/pdf/2303.04481">pdf</a>, <a href="https://arxiv.org/format/2303.04481">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"> Characterization of Charge Spreading and Gain of Encapsulated Resistive Micromegas Detectors for the Upgrade of the T2K Near Detector Time Projection Chambers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Attie%2C+D">D. Attie</a>, <a href="/search/hep-ex?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/hep-ex?searchtype=author&query=Batkiewicz-Kwasnia%2C+M">M. Batkiewicz-Kwasnia</a>, <a href="/search/hep-ex?searchtype=author&query=Billoir%2C+P">P. Billoir</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=Boullon%2C+R">R. Boullon</a>, <a href="/search/hep-ex?searchtype=author&query=Calvet%2C+D">D. Calvet</a>, <a href="/search/hep-ex?searchtype=author&query=Casado%2C+M+P">M. P. Casado</a>, <a href="/search/hep-ex?searchtype=author&query=Catanesi%2C+M+G">M. G. Catanesi</a>, <a href="/search/hep-ex?searchtype=author&query=Cicerchia%2C+M">M. Cicerchia</a>, <a href="/search/hep-ex?searchtype=author&query=Cogo%2C+G">G. Cogo</a>, <a href="/search/hep-ex?searchtype=author&query=Colas%2C+P">P. Colas</a>, <a href="/search/hep-ex?searchtype=author&query=Collazuol%2C+G">G. Collazuol</a>, <a href="/search/hep-ex?searchtype=author&query=Ago%2C+D+D">D. D Ago</a>, <a href="/search/hep-ex?searchtype=author&query=Dalmazzon%2C+C">C. Dalmazzon</a>, <a href="/search/hep-ex?searchtype=author&query=Daret%2C+T">T. Daret</a>, <a href="/search/hep-ex?searchtype=author&query=Delbart%2C+A">A. Delbart</a>, <a href="/search/hep-ex?searchtype=author&query=De+Lorenzis%2C+A">A. De Lorenzis</a>, <a href="/search/hep-ex?searchtype=author&query=de+Oliveira%2C+R">R. de Oliveira</a>, <a href="/search/hep-ex?searchtype=author&query=Dolan%2C+S">S. Dolan</a>, <a href="/search/hep-ex?searchtype=author&query=Dygnarowiczi%2C+K">K. Dygnarowiczi</a>, <a href="/search/hep-ex?searchtype=author&query=Dumarchez%2C+J">J. Dumarchez</a>, <a href="/search/hep-ex?searchtype=author&query=Emery-Schren%2C+S">S. Emery-Schren</a>, <a href="/search/hep-ex?searchtype=author&query=Ershova%2C+A">A. Ershova</a> , et al. (70 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="2303.04481v1-abstract-short" style="display: inline;"> An upgrade of the near detector of the T2K long baseline neutrino oscillation experiment is currently being conducted. This upgrade will include two new Time Projection Chambers, each equipped with 16 charge readout resistive Micromegas modules. A procedure to validate the performance of the detectors at different stages of production has been developed and implemented to ensure a proper and relia… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.04481v1-abstract-full').style.display = 'inline'; document.getElementById('2303.04481v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.04481v1-abstract-full" style="display: none;"> An upgrade of the near detector of the T2K long baseline neutrino oscillation experiment is currently being conducted. This upgrade will include two new Time Projection Chambers, each equipped with 16 charge readout resistive Micromegas modules. A procedure to validate the performance of the detectors at different stages of production has been developed and implemented to ensure a proper and reliable operation of the detectors once installed. A dedicated X-ray test bench is used to characterize the detectors by scanning each pad individually and to precisely measure the uniformity of the gain and the deposited energy resolution over the pad plane. An energy resolution of about 10% is obtained. A detailed physical model has been developed to describe the charge dispersion phenomena in the resistive Micromegas anode. The detailed physical description includes initial ionization, electron drift, diffusion effects and the readout electronics effects. The model provides an excellent characterization of the charge spreading of the experimental measurements and allowed the simultaneous extraction of gain and RC information of the modules. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.04481v1-abstract-full').style.display = 'none'; document.getElementById('2303.04481v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.03222">arXiv:2303.03222</a> <span> [<a href="https://arxiv.org/pdf/2303.03222">pdf</a>, <a href="https://arxiv.org/format/2303.03222">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-023-11819-x">10.1140/epjc/s10052-023-11819-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of neutrino oscillation parameters from the T2K experiment using $3.6\times10^{21}$ protons on target </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+T2K+Collaboration"> The 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=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=Monsalve%2C+S+A">S. Alonso Monsalve</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=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=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=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=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>, <a href="/search/hep-ex?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/hep-ex?searchtype=author&query=Blanchet%2C+A">A. Blanchet</a>, <a href="/search/hep-ex?searchtype=author&query=Blondel%2C+A">A. Blondel</a> , et al. (376 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="2303.03222v3-abstract-short" style="display: inline;"> The T2K experiment presents new measurements of neutrino oscillation parameters using $19.7(16.3)\times10^{20}$ protons on target (POT) in (anti-)neutrino mode at the far detector (FD). Compared to the previous analysis, an additional $4.7\times10^{20}$ POT neutrino data was collected at the FD. Significant improvements were made to the analysis methodology, with the near-detector analysis introdu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03222v3-abstract-full').style.display = 'inline'; document.getElementById('2303.03222v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.03222v3-abstract-full" style="display: none;"> The T2K experiment presents new measurements of neutrino oscillation parameters using $19.7(16.3)\times10^{20}$ protons on target (POT) in (anti-)neutrino mode at the far detector (FD). Compared to the previous analysis, an additional $4.7\times10^{20}$ POT neutrino data was collected at the FD. Significant improvements were made to the analysis methodology, with the near-detector analysis introducing new selections and using more than double the data. Additionally, this is the first T2K oscillation analysis to use NA61/SHINE data on a replica of the T2K target to tune the neutrino flux model, and the neutrino interaction model was improved to include new nuclear effects and calculations. Frequentist and Bayesian analyses are presented, including results on $\sin^2胃_{13}$ and the impact of priors on the $未_\mathrm{CP}$ measurement. Both analyses prefer the normal mass ordering and upper octant of $\sin^2胃_{23}$ with a nearly maximally CP-violating phase. Assuming the normal ordering and using the constraint on $\sin^2胃_{13}$ from reactors, $\sin^2胃_{23}=0.561^{+0.021}_{-0.032}$ using Feldman--Cousins corrected intervals, and $螖m^2_{32}=2.494_{-0.058}^{+0.041}\times10^{-3}~\mathrm{eV^2}$ using constant $螖蠂^{2}$ intervals. The CP-violating phase is constrained to $未_\mathrm{CP}=-1.97_{-0.70}^{+0.97}$ using Feldman--Cousins corrected intervals, and $未_\mathrm{CP}=0,蟺$ is excluded at more than 90% confidence level. A Jarlskog invariant of zero is excluded at more than $2蟽$ credible level using a flat prior in $未_\mathrm{CP}$, and just below $2蟽$ using a flat prior in $\sin未_\mathrm{CP}$. When the external constraint on $\sin^2胃_{13}$ is removed, $\sin^2胃_{13}=28.0^{+2.8}_{-6.5}\times10^{-3}$, in agreement with measurements from reactor experiments. These results are consistent with previous T2K analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03222v3-abstract-full').style.display = 'none'; document.getElementById('2303.03222v3-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 83, 782 (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> </ol> <div class="is-hidden-tablet">  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