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class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.01996">arXiv:2410.01996</a> <span> [<a href="https://arxiv.org/pdf/2410.01996">pdf</a>, <a href="https://arxiv.org/format/2410.01996">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Limits on the Low-Energy Electron Antineutrino Flux from the Brightest GRB of All Time </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Araki%2C+T">T. Araki</a>, <a href="/search/?searchtype=author&query=Chauhan%2C+S">S. Chauhan</a>, <a href="/search/?searchtype=author&query=Chiba%2C+K">K. Chiba</a>, <a href="/search/?searchtype=author&query=Eda%2C+T">T. Eda</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Funahashi%2C+Y">Y. Funahashi</a>, <a href="/search/?searchtype=author&query=Furuto%2C+A">A. Furuto</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Goto%2C+S">S. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Marthe%2C+A">A. Marthe</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+Y">Y. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Morita%2C+D">D. Morita</a> , et al. (48 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.01996v2-abstract-short" style="display: inline;"> The electron antinuetrino flux limits are presented for the brightest gamma-ray burst (GRB) of all time, GRB221009A, over a range of 1.8-200 MeV using the Kamioka Liquid Scintillator Anti Neutrino Detector (KamLAND). Using a variety of time windows to search for electron antineutrinos coincident with the GRB, we set an upper limit on the flux under the assumption of various neutrino source spectra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01996v2-abstract-full').style.display = 'inline'; document.getElementById('2410.01996v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.01996v2-abstract-full" style="display: none;"> The electron antinuetrino flux limits are presented for the brightest gamma-ray burst (GRB) of all time, GRB221009A, over a range of 1.8-200 MeV using the Kamioka Liquid Scintillator Anti Neutrino Detector (KamLAND). Using a variety of time windows to search for electron antineutrinos coincident with the GRB, we set an upper limit on the flux under the assumption of various neutrino source spectra. No excess was observed in any time windows ranging from seconds to days around the event trigger time. The limits are compared to the results presented by IceCube. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01996v2-abstract-full').style.display = 'none'; document.getElementById('2410.01996v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 3 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.11438">arXiv:2406.11438</a> <span> [<a href="https://arxiv.org/pdf/2406.11438">pdf</a>, <a href="https://arxiv.org/format/2406.11438">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 Majorana Neutrinos with the Complete KamLAND-Zen Dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Araki%2C+T">T. Araki</a>, <a href="/search/?searchtype=author&query=Chiba%2C+K">K. Chiba</a>, <a href="/search/?searchtype=author&query=Eda%2C+T">T. Eda</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Funahashi%2C+Y">Y. Funahashi</a>, <a href="/search/?searchtype=author&query=Furuto%2C+A">A. Furuto</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Goto%2C+S">S. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Marthe%2C+A">A. Marthe</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+Y">Y. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a> , et al. (48 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="2406.11438v1-abstract-short" style="display: inline;"> We present a search for neutrinoless double-beta ($0谓尾尾$) decay of $^{136}$Xe using the full KamLAND-Zen 800 dataset with 745 kg of enriched xenon, corresponding to an exposure of $2.097$ ton yr of $^{136}$Xe. This updated search benefits from a more than twofold increase in exposure, recovery of photo-sensor gain, and reduced background from muon-induced spallation of xenon. Combining with the se… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.11438v1-abstract-full').style.display = 'inline'; document.getElementById('2406.11438v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.11438v1-abstract-full" style="display: none;"> We present a search for neutrinoless double-beta ($0谓尾尾$) decay of $^{136}$Xe using the full KamLAND-Zen 800 dataset with 745 kg of enriched xenon, corresponding to an exposure of $2.097$ ton yr of $^{136}$Xe. This updated search benefits from a more than twofold increase in exposure, recovery of photo-sensor gain, and reduced background from muon-induced spallation of xenon. Combining with the search in the previous KamLAND-Zen phase, we obtain a lower limit for the $0谓尾尾$ decay half-life of $T_{1/2}^{0谓} > 3.8 \times 10^{26}$ yr at 90% C.L., a factor of 1.7 improvement over the previous limit. The corresponding upper limits on the effective Majorana neutrino mass are in the range 28-122 meV using phenomenological nuclear matrix element calculations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.11438v1-abstract-full').style.display = 'none'; document.getElementById('2406.11438v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">arXiv admin note: text overlap with arXiv:2203.02139</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/?searchtype=author&query=KamLAND"> KamLAND</a>, <a href="/search/?searchtype=author&query=Collaborations%2C+S">Super-Kamiokande Collaborations</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Seisho Abe</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">Minori Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">Sawako Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">Azusa Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Yoshihito Gando</a>, <a href="/search/?searchtype=author&query=Goto%2C+S">Shun Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">Takahiko Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">Kazumi Hata</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">Koichi Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">Sei Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">Haruo Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">Kunio Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">Koji Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Yuto Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">Nanami Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Yasuhiro Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">Masayuki Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">Maho Kurasawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">Tadao Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">Haruhiko Miyake</a>, <a href="/search/?searchtype=author&query=Morita%2C+D">Daisuke Morita</a>, <a href="/search/?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/2311.09676">arXiv:2311.09676</a> <span> [<a href="https://arxiv.org/pdf/2311.09676">pdf</a>, <a href="https://arxiv.org/format/2311.09676">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2024.138846">10.1016/j.physletb.2024.138846 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Charged Excited States of Dark Matter with KamLAND-Zen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=collaboration%2C+K">KamLAND-Zen collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Goto%2C+S">S. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Morita%2C+D">D. Morita</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+T">T. Nakahata</a> , et al. (44 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="2311.09676v2-abstract-short" style="display: inline;"> Particle dark matter could belong to a multiplet that includes an electrically charged state. WIMP dark matter ($蠂^{0}$) accompanied by a negatively charged excited state ($蠂^{-}$) with a small mass difference (e.g. $<$ 20 MeV) can form a bound-state with a nucleus such as xenon. This bound-state formation is rare and the released energy is $\mathcal{O}(1-10$) MeV depending on the nucleus, making… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.09676v2-abstract-full').style.display = 'inline'; document.getElementById('2311.09676v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.09676v2-abstract-full" style="display: none;"> Particle dark matter could belong to a multiplet that includes an electrically charged state. WIMP dark matter ($蠂^{0}$) accompanied by a negatively charged excited state ($蠂^{-}$) with a small mass difference (e.g. $<$ 20 MeV) can form a bound-state with a nucleus such as xenon. This bound-state formation is rare and the released energy is $\mathcal{O}(1-10$) MeV depending on the nucleus, making large liquid scintillator detectors suitable for detection. We searched for bound-state formation events with xenon in two experimental phases of the KamLAND-Zen experiment, a xenon-doped liquid scintillator detector. No statistically significant events were observed. For a benchmark parameter set of WIMP mass $m_{蠂^{0}} = 1$ TeV and mass difference $螖m = 17$ MeV, we set the most stringent upper limits on the recombination cross section times velocity $\langle蟽v\rangle$ and the decay-width of $蠂^{-}$ to $9.2 \times 10^{-30}$ ${\rm cm^3/s}$ and $8.7 \times 10^{-14}$ GeV, respectively at 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.09676v2-abstract-full').style.display = 'none'; document.getElementById('2311.09676v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 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">Journal ref:</span> Phys. Lett. B 855 (2024) 138846 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.09307">arXiv:2301.09307</a> <span> [<a href="https://arxiv.org/pdf/2301.09307">pdf</a>, <a href="https://arxiv.org/format/2301.09307">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <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"> Measurement of cosmic-ray muon spallation products in a xenon-loaded liquid scintillator with KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a> , et al. (42 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="2301.09307v1-abstract-short" style="display: inline;"> Cosmic-ray muons produce various radioisotopes when passing through material. These spallation products can be backgrounds for rare event searches such as in solar neutrino, double-beta decay, and dark matter search experiments. The KamLAND-Zen experiment searches for neutrinoless double-beta decay in 745kg of xenon dissolved in liquid scintillator. The experiment includes dead-time-free electroni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09307v1-abstract-full').style.display = 'inline'; document.getElementById('2301.09307v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.09307v1-abstract-full" style="display: none;"> Cosmic-ray muons produce various radioisotopes when passing through material. These spallation products can be backgrounds for rare event searches such as in solar neutrino, double-beta decay, and dark matter search experiments. The KamLAND-Zen experiment searches for neutrinoless double-beta decay in 745kg of xenon dissolved in liquid scintillator. The experiment includes dead-time-free electronics with a high efficiency for detecting muon-induced neutrons. The production yields of different radioisotopes are measured with a combination of delayed coincidence techniques, newly developed muon reconstruction and xenon spallation identification methods. The observed xenon spallation products are consistent with results from the FLUKA and Geant4 simulation codes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09307v1-abstract-full').style.display = 'none'; document.getElementById('2301.09307v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.13911">arXiv:2211.13911</a> <span> [<a href="https://arxiv.org/pdf/2211.13911">pdf</a>, <a href="https://arxiv.org/format/2211.13911">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.107.072006">10.1103/PhysRevD.107.072006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First measurement of the strange axial coupling constant using neutral-current quasielastic interactions of atmospheric neutrinos at KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+T">T. Nakahata</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a> , et al. (39 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.13911v2-abstract-short" style="display: inline;"> We report a measurement of the strange axial coupling constant $g_A^s$ using atmospheric neutrino data at KamLAND. This constant is a component of the axial form factor of the neutral-current quasielastic (NCQE) interaction. The value of $g_A^s$ significantly changes the ratio of proton and neutron NCQE cross sections. KamLAND is suitable for measuring NCQE interactions as it can detect nucleon re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.13911v2-abstract-full').style.display = 'inline'; document.getElementById('2211.13911v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.13911v2-abstract-full" style="display: none;"> We report a measurement of the strange axial coupling constant $g_A^s$ using atmospheric neutrino data at KamLAND. This constant is a component of the axial form factor of the neutral-current quasielastic (NCQE) interaction. The value of $g_A^s$ significantly changes the ratio of proton and neutron NCQE cross sections. KamLAND is suitable for measuring NCQE interactions as it can detect nucleon recoils with low-energy thresholds and measure neutron multiplicity with high efficiency. KamLAND data, including the information on neutron multiplicity associated with the NCQE interactions, makes it possible to measure $g_A^s$ with a suppressed dependence on the axial mass $M_A$, which has not yet been determined. For a comprehensive prediction of the neutron emission associated with neutrino interactions, we establish a simulation of particle emission via nuclear deexcitation of $^{12}$C, a process not considered in existing neutrino Monte Carlo event generators. Energy spectrum fitting for each neutron multiplicity gives $g_A^s =-0.14^{+0.25}_{-0.26}$, which is the most stringent limit obtained using NCQE interactions without $M_A$ constraints. The two-body current contribution considered in this analysis relies on a theoretically effective model and electron scattering experiments and requires future verification by direct measurements and future model improvement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.13911v2-abstract-full').style.display = 'none'; document.getElementById('2211.13911v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 107,072006 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.14934">arXiv:2205.14934</a> <span> [<a href="https://arxiv.org/pdf/2205.14934">pdf</a>, <a href="https://arxiv.org/format/2205.14934">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</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/10.1029/2022GL099566">10.1029/2022GL099566 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Abundances of uranium and thorium elements in Earth estimated by geoneutrino spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+T">T. Nakahata</a> , et al. (43 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.14934v2-abstract-short" style="display: inline;"> The decay of the primordial isotopes $^{238}\mathrm{U}$, $^{235}\mathrm{U}$, $^{232}\mathrm{Th}$, and $^{40}\mathrm{K}$ have contributed to the terrestrial heat budget throughout the Earth's history. Hence the individual abundance of those isotopes are key parameters in reconstructing contemporary Earth model. The geoneutrinos produced by the radioactive decays of uranium and thorium have been obs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.14934v2-abstract-full').style.display = 'inline'; document.getElementById('2205.14934v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.14934v2-abstract-full" style="display: none;"> The decay of the primordial isotopes $^{238}\mathrm{U}$, $^{235}\mathrm{U}$, $^{232}\mathrm{Th}$, and $^{40}\mathrm{K}$ have contributed to the terrestrial heat budget throughout the Earth's history. Hence the individual abundance of those isotopes are key parameters in reconstructing contemporary Earth model. The geoneutrinos produced by the radioactive decays of uranium and thorium have been observed with the Kamioka Liquid-Scintillator Antineutrino Detector (KamLAND). Those measurements have been improved with more than 18-year observation time, and improvements in detector background levels mainly by an 8-year almost rector-free period now permit spectroscopy with geoneutrinos. Our results yield the first constraint on both uranium and thorium heat contributions. Herein the KamLAND result is consistent with geochemical estimations based on elemental abundances of chondritic meteorites and mantle peridotites. The High-Q model is disfavored at 99.76% C.L. and a fully radiogenic model is excluded at 5.2$蟽$ assuming a homogeneous heat producing element distribution in the mantle. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.14934v2-abstract-full').style.display = 'none'; document.getElementById('2205.14934v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 2 figures, accepted for publication in Geophysical Research Letters on Aug 4th, 2022</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Geophysical Research Letters, Volume 49, Issue 16, e2022GL099566 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.12065">arXiv:2204.12065</a> <span> [<a href="https://arxiv.org/pdf/2204.12065">pdf</a>, <a href="https://arxiv.org/format/2204.12065">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac7a3f">10.3847/1538-4357/ac7a3f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for supernova neutrinos and constraint on the galactic star formation rate with the KamLAND data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+T">T. Nakahata</a> , et al. (42 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="2204.12065v3-abstract-short" style="display: inline;"> We present the results of a search for core-collapse supernova neutrinos, using long-term KamLAND data from 2002 March 9 to 2020 April 25. We focus on the electron antineutrinos emitted from supernovae in the energy range of 1.8--111 MeV. Supernovae will make a neutrino event cluster with the duration of $\sim$10 s in the KamLAND data. We find no neutrino clusters and give the upper limit on the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12065v3-abstract-full').style.display = 'inline'; document.getElementById('2204.12065v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.12065v3-abstract-full" style="display: none;"> We present the results of a search for core-collapse supernova neutrinos, using long-term KamLAND data from 2002 March 9 to 2020 April 25. We focus on the electron antineutrinos emitted from supernovae in the energy range of 1.8--111 MeV. Supernovae will make a neutrino event cluster with the duration of $\sim$10 s in the KamLAND data. We find no neutrino clusters and give the upper limit on the supernova rate as to be 0.15 yr$^{-1}$ with a 90% confidence level. The detectable range, which corresponds to a >95% detection probability, is 40--59 kpc and 65--81 kpc for core-collapse supernovae and failed core-collapse supernovae, respectively. This paper proposes to convert the supernova rate obtained by the neutrino observation to the Galactic star formation rate. Assuming a modified Salpeter-type initial mass function, the upper limit on the Galactic star formation rate is <(17.5--22.7) $M_{\odot} \mathrm{yr}^{-1}$ with a 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12065v3-abstract-full').style.display = 'none'; document.getElementById('2204.12065v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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, 4 figures, accepted for publication in Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 934, Number 1, Page 85 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.02139">arXiv:2203.02139</a> <span> [<a href="https://arxiv.org/pdf/2203.02139">pdf</a>, <a href="https://arxiv.org/format/2203.02139">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.130.051801">10.1103/PhysRevLett.130.051801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for the Majorana Nature of Neutrinos in the Inverted Mass Ordering Region with KamLAND-Zen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a> , et al. (50 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.02139v2-abstract-short" style="display: inline;"> The KamLAND-Zen experiment has provided stringent constraints on the neutrinoless double-beta ($0谓尾尾$) decay half-life in $^{136}$Xe using a xenon-loaded liquid scintillator. We report an improved search using an upgraded detector with almost double the amount of xenon and an ultralow radioactivity container, corresponding to an exposure of 970 kg yr of $^{136}$Xe. These new data provide valuable… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02139v2-abstract-full').style.display = 'inline'; document.getElementById('2203.02139v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.02139v2-abstract-full" style="display: none;"> The KamLAND-Zen experiment has provided stringent constraints on the neutrinoless double-beta ($0谓尾尾$) decay half-life in $^{136}$Xe using a xenon-loaded liquid scintillator. We report an improved search using an upgraded detector with almost double the amount of xenon and an ultralow radioactivity container, corresponding to an exposure of 970 kg yr of $^{136}$Xe. These new data provide valuable insight into backgrounds, especially from cosmic muon spallation of xenon, and have required the use of novel background rejection techniques. We obtain a lower limit for the $0谓尾尾$ decay half-life of $T_{1/2}^{0谓} > 2.3 \times 10^{26}$ yr at 90% C.L., corresponding to upper limits on the effective Majorana neutrino mass of 36-156 meV using commonly adopted nuclear matrix element calculations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02139v2-abstract-full').style.display = 'none'; document.getElementById('2203.02139v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 130, 051801 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.07345">arXiv:2202.07345</a> <span> [<a href="https://arxiv.org/pdf/2202.07345">pdf</a>, <a href="https://arxiv.org/format/2202.07345">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2022.102758">10.1016/j.astropartphys.2022.102758 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KamLAND's search for correlated low-energy electron antineutrinos with astrophysical neutrinos from IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.07345v2-abstract-short" style="display: inline;"> We report the results of a search for MeV-scale astrophysical neutrinos in KamLAND presented as an excess in the number of coincident neutrino interactions associated with the publicly available high-energy neutrino datasets from the IceCube Neutrino Observatory. We find no statistically significant excess in the number of observed low-energy electron antineutrinos in KamLAND, given a coincidence… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.07345v2-abstract-full').style.display = 'inline'; document.getElementById('2202.07345v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.07345v2-abstract-full" style="display: none;"> We report the results of a search for MeV-scale astrophysical neutrinos in KamLAND presented as an excess in the number of coincident neutrino interactions associated with the publicly available high-energy neutrino datasets from the IceCube Neutrino Observatory. We find no statistically significant excess in the number of observed low-energy electron antineutrinos in KamLAND, given a coincidence time window of $\pm$500s, $\pm$1,000s, $\pm$3,600s, and $\pm$10,000s around each of the IceCube neutrinos. We use this observation to present limits from 1.8 MeV to 100 MeV on the electron antineutrino fluence, assuming a mono-energetic flux. We then compare the results to several astrophysical measurements performed by IceCube and place a limit at the 90% confidence level on the electron antineutrino isotropic thermal luminosity from the TXS 0506+056 blazar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.07345v2-abstract-full').style.display = 'none'; document.getElementById('2202.07345v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.04918">arXiv:2112.04918</a> <span> [<a href="https://arxiv.org/pdf/2112.04918">pdf</a>, <a href="https://arxiv.org/format/2112.04918">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac4e7e">10.3847/1538-4357/ac4e7e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for correlated low-energy electron antineutrinos in KamLAND with gamma-ray bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+R">R. Nakamura</a> , et al. (43 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.04918v2-abstract-short" style="display: inline;"> We present the results of a time-coincident event search for low-energy electron antineutrinos in the KamLAND detector with gamma-ray bursts from the Gamma-ray Coordinates Network and Fermi Gamma-ray Burst Monitor. Using a variable coincidence time window of $\pm$500s plus the duration of each gamma-ray burst, no statistically significant excess above background is observed. We place the world's m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04918v2-abstract-full').style.display = 'inline'; document.getElementById('2112.04918v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.04918v2-abstract-full" style="display: none;"> We present the results of a time-coincident event search for low-energy electron antineutrinos in the KamLAND detector with gamma-ray bursts from the Gamma-ray Coordinates Network and Fermi Gamma-ray Burst Monitor. Using a variable coincidence time window of $\pm$500s plus the duration of each gamma-ray burst, no statistically significant excess above background is observed. We place the world's most stringent 90% confidence level upper limit on the electron antineutrino fluence below 17.5 MeV. Assuming a Fermi-Dirac neutrino energy spectrum from the gamma-ray burst source, we use the available redshift data to constrain the electron antineutrino luminosity and effective temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04918v2-abstract-full').style.display = 'none'; document.getElementById('2112.04918v2-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 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/2108.08527">arXiv:2108.08527</a> <span> [<a href="https://arxiv.org/pdf/2108.08527">pdf</a>, <a href="https://arxiv.org/format/2108.08527">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac32c1">10.3847/1538-4357/ac32c1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on astrophysical antineutrinos with the KamLAND experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.08527v3-abstract-short" style="display: inline;"> We report on a search for electron antineutrinos ($\bar谓_e$) from astrophysical sources in the neutrino energy range 8.3 to 30.8 MeV with the KamLAND detector. In an exposure of 6.72 kton-year of the liquid scintillator, we observe 18 candidate events via the inverse beta decay reaction. Although there is a large background uncertainty from neutral current atmospheric neutrino interactions, we fin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.08527v3-abstract-full').style.display = 'inline'; document.getElementById('2108.08527v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.08527v3-abstract-full" style="display: none;"> We report on a search for electron antineutrinos ($\bar谓_e$) from astrophysical sources in the neutrino energy range 8.3 to 30.8 MeV with the KamLAND detector. In an exposure of 6.72 kton-year of the liquid scintillator, we observe 18 candidate events via the inverse beta decay reaction. Although there is a large background uncertainty from neutral current atmospheric neutrino interactions, we find no significant excess over background model predictions. Assuming several supernova relic neutrino spectra, we give upper flux limits of 60--110 cm$^{-2}$ s$^{-1}$ (90% CL) in the analysis range and present a model-independent flux. We also set limits on the annihilation rates for light dark matter pairs to neutrino pairs. These data improves on the upper probability limit of $^{8}$B solar neutrinos converting into $\bar谓_e$'s, $P_{谓_e \rightarrow \bar谓_e} < 3.5\times10^{-5}$ (90% CL) assuming an undistorted $\bar谓_e$ shape. This corresponds to a solar $\bar谓_e$ flux of 60 cm$^{-2}$ s$^{-1}$ (90% CL) in the analysis energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.08527v3-abstract-full').style.display = 'none'; document.getElementById('2108.08527v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 9 figures, 4 tables, accepted for publication in Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 925, Number 1, Page 14 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.02458">arXiv:2105.02458</a> <span> [<a href="https://arxiv.org/pdf/2105.02458">pdf</a>, <a href="https://arxiv.org/format/2105.02458">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/ac35d1">10.3847/1538-4357/ac35d1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Solar Flare Neutrinos with the KamLAND detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a> , et al. (44 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="2105.02458v2-abstract-short" style="display: inline;"> We report the result of a search for neutrinos in coincidence with solar flares from the GOES flare database. The search was performed on a 10.8 kton-year exposure of KamLAND collected from 2002 to 2019. This large exposure allows us to explore previously unconstrained parameter space for solar flare neutrinos. We found no statistical excess of neutrinos and established 90% confidence level upper… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.02458v2-abstract-full').style.display = 'inline'; document.getElementById('2105.02458v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.02458v2-abstract-full" style="display: none;"> We report the result of a search for neutrinos in coincidence with solar flares from the GOES flare database. The search was performed on a 10.8 kton-year exposure of KamLAND collected from 2002 to 2019. This large exposure allows us to explore previously unconstrained parameter space for solar flare neutrinos. We found no statistical excess of neutrinos and established 90% confidence level upper limits of $8.4 \times 10^7$ cm$^{-2}$ ($3.0 \times 10^{9}$ cm$^{-2}$) on electron anti-neutrino (electron neutrino) fluence at 20 MeV normalized to the X12 flare, assuming that the neutrino fluence is proportional to the X-ray intensity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.02458v2-abstract-full').style.display = 'none'; document.getElementById('2105.02458v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 9 figures, accepted October 27, 2021</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 924, Number 2, Page 103 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.10452">arXiv:2104.10452</a> <span> [<a href="https://arxiv.org/pdf/2104.10452">pdf</a>, <a href="https://arxiv.org/format/2104.10452">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/16/08/p08023">10.1088/1748-0221/16/08/p08023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The nylon balloon for xenon loaded liquid scintillator in KamLAND-Zen 800 neutrinoless double-beta decay search experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=collaboration%2C+K">KamLAND-Zen collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Nakada%2C+T">T. Nakada</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Ozaki%2C+H">H. Ozaki</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hayashi%2C+A">A. Hayashi</a>, <a href="/search/?searchtype=author&query=Honda%2C+Y">Y. Honda</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+S">S. Ishikawa</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kamizawa%2C+K">K. Kamizawa</a> , et al. (49 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.10452v3-abstract-short" style="display: inline;"> The KamLAND-Zen 800 experiment is searching for the neutrinoless double-beta decay of $^{136}$Xe by using $^{136}$Xe-loaded liquid scintillator. The liquid scintillator is enclosed inside a balloon made of thin, transparent, low-radioactivity film that we call Inner Balloon (IB). The IB, apart from guaranteeing the liquid containment, also allows to minimize the background from cosmogenic muon-spa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10452v3-abstract-full').style.display = 'inline'; document.getElementById('2104.10452v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.10452v3-abstract-full" style="display: none;"> The KamLAND-Zen 800 experiment is searching for the neutrinoless double-beta decay of $^{136}$Xe by using $^{136}$Xe-loaded liquid scintillator. The liquid scintillator is enclosed inside a balloon made of thin, transparent, low-radioactivity film that we call Inner Balloon (IB). The IB, apart from guaranteeing the liquid containment, also allows to minimize the background from cosmogenic muon-spallation products and $^{8}$B solar neutrinos. Indeed these events could contribute to the total counts in the region of interest around the Q-value of the double-beta decay of $^{136}$Xe. In this paper, we present an overview of the IB and describe the various steps of its commissioning minimizing the radioactive contaminations, from the material selection, to the fabrication of the balloon and its installation inside the KamLAND detector. Finally, we show the impact of the IB on the KamLAND background as measured by the KamLAND detector itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10452v3-abstract-full').style.display = 'none'; document.getElementById('2104.10452v3-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 16 figures, to be submitted to JINST</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2021 JINST 16 P08023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.06049">arXiv:2101.06049</a> <span> [<a href="https://arxiv.org/pdf/2101.06049">pdf</a>, <a href="https://arxiv.org/ps/2101.06049">ps</a>, <a href="https://arxiv.org/format/2101.06049">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"> A Search for Charged Excitation of Dark Matter with the KamLAND-Zen Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+R">R. Nakamura</a> , et al. (47 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.06049v1-abstract-short" style="display: inline;"> There are many theories where a dark matter particle is part of a multiplet with an electrically charged state. If WIMP dark matter ($蠂^{0}$) is accompanied by a charged excited state ($蠂^{-}$) separated by a small mass difference, it can form a stable bound state with a nucleus. In supersymmetric models, the $蠂^{0}$ and the $蠂^{-}$ could be the neutralino and a charged slepton, such as the neutra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.06049v1-abstract-full').style.display = 'inline'; document.getElementById('2101.06049v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.06049v1-abstract-full" style="display: none;"> There are many theories where a dark matter particle is part of a multiplet with an electrically charged state. If WIMP dark matter ($蠂^{0}$) is accompanied by a charged excited state ($蠂^{-}$) separated by a small mass difference, it can form a stable bound state with a nucleus. In supersymmetric models, the $蠂^{0}$ and the $蠂^{-}$ could be the neutralino and a charged slepton, such as the neutralino-stau degenerate model. The formation binding process is expected to result in an energy deposition of {\it O}(1--10 MeV), making it suitable for detection in large liquid scintillator detectors. We describe new constraints on the bound state formation with a xenon nucleus using the KamLAND-Zen 400 Phase-II dataset. In order to enlarge the searchable parameter space, all xenon isotopes in the detector were used. For a benchmark parameter set of $m_{蠂^{0}} = 100$ GeV and $螖m = 10$ MeV, this study sets the most stringent upper limits on the recombination cross section $\langle蟽v\rangle$ and the decay-width of $蠂^{-}$ of $2.0 \times 10^{-31}$ ${\rm cm^3/s}$ and $1.1 \times 10^{-18}$ GeV, respectively (90\% confidence level). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.06049v1-abstract-full').style.display = 'none'; document.getElementById('2101.06049v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.12053">arXiv:2012.12053</a> <span> [<a href="https://arxiv.org/pdf/2012.12053">pdf</a>, <a href="https://arxiv.org/format/2012.12053">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abd5bc">10.3847/1538-4357/abd5bc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Low-energy Electron Antineutrinos in KamLAND Associated with Gravitational Wave Events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a> , et al. (44 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.12053v1-abstract-short" style="display: inline;"> We present the results of a search for MeV-scale electron antineutrino events in KamLAND in coincident with the 60 gravitational wave events/candidates reported by the LIGO/Virgo collaboration during their second and third observing runs. We find no significant coincident signals within a $\pm$ 500 s timing window from each gravitational wave and present 90% C.L. upper limits on the electron antin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12053v1-abstract-full').style.display = 'inline'; document.getElementById('2012.12053v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.12053v1-abstract-full" style="display: none;"> We present the results of a search for MeV-scale electron antineutrino events in KamLAND in coincident with the 60 gravitational wave events/candidates reported by the LIGO/Virgo collaboration during their second and third observing runs. We find no significant coincident signals within a $\pm$ 500 s timing window from each gravitational wave and present 90% C.L. upper limits on the electron antineutrino fluence between $10^{8}$-$10^{13}\,{\mathrm cm^2}$ for neutrino energies in the energy range of 1.8-111 MeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12053v1-abstract-full').style.display = 'none'; document.getElementById('2012.12053v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 2 figures, 2 tables, Accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 909, Number 2 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.07155">arXiv:1606.07155</a> <span> [<a href="https://arxiv.org/pdf/1606.07155">pdf</a>, <a href="https://arxiv.org/ps/1606.07155">ps</a>, <a href="https://arxiv.org/format/1606.07155">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> </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/10.3847/2041-8205/829/2/L34">10.3847/2041-8205/829/2/L34 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for electron antineutrinos associated with gravitational wave events GW150914 and GW151226 using KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashi%2C+A">A. Hayashi</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Karino%2C+Y">Y. Karino</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/?searchtype=author&query=Ozaki%2C+H">H. Ozaki</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takai%2C+T">T. Takai</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Teraoka%2C+Y">Y. Teraoka</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a> , et al. (23 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="1606.07155v2-abstract-short" style="display: inline;"> We present a search for low energy antineutrino events coincident with the gravitational wave events GW150914 and GW151226, and the candidate event LVT151012 using KamLAND, a kiloton-scale antineutrino detector. We find no inverse beta-decay neutrino events within $\pm 500$ seconds of either gravitational wave signal. This non-detection is used to constrain the electron antineutrino fluence and th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.07155v2-abstract-full').style.display = 'inline'; document.getElementById('1606.07155v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.07155v2-abstract-full" style="display: none;"> We present a search for low energy antineutrino events coincident with the gravitational wave events GW150914 and GW151226, and the candidate event LVT151012 using KamLAND, a kiloton-scale antineutrino detector. We find no inverse beta-decay neutrino events within $\pm 500$ seconds of either gravitational wave signal. This non-detection is used to constrain the electron antineutrino fluence and the luminosity of the astrophysical sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.07155v2-abstract-full').style.display = 'none'; document.getElementById('1606.07155v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 4 figures, as published in ApJL. Updated to replace power law spectrum with Fermi Dirac spectrum</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.829, L34, 2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.03724">arXiv:1509.03724</a> <span> [<a href="https://arxiv.org/pdf/1509.03724">pdf</a>, <a href="https://arxiv.org/ps/1509.03724">ps</a>, <a href="https://arxiv.org/format/1509.03724">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nuclphysa.2015.11.011">10.1016/j.nuclphysa.2015.11.011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for double-beta decay of 136Xe to excited states of 136Ba with the KamLAND-Zen experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Asakura%2C+K">K. Asakura</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+T">T. Ishikawa</a>, <a href="/search/?searchtype=author&query=Ishio%2C+S">S. Ishio</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Otani%2C+M">M. Otani</a>, <a href="/search/?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Tachibana%2C+H">H. Tachibana</a> , et al. (21 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="1509.03724v2-abstract-short" style="display: inline;"> A search for double-beta decays of 136Xe to excited states of 136Ba has been performed with the first phase data set of the KamLAND-Zen experiment. The 0+1, 2+1 and 2+2 transitions of 0谓\{beta}\{beta} decay were evaluated in an exposure of 89.5kg-yr of 136Xe, while the same transitions of 2谓\{beta}\{beta} decay were evaluated in an exposure of 61.8kg-yr. No excess over background was found for all… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.03724v2-abstract-full').style.display = 'inline'; document.getElementById('1509.03724v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.03724v2-abstract-full" style="display: none;"> A search for double-beta decays of 136Xe to excited states of 136Ba has been performed with the first phase data set of the KamLAND-Zen experiment. The 0+1, 2+1 and 2+2 transitions of 0谓\{beta}\{beta} decay were evaluated in an exposure of 89.5kg-yr of 136Xe, while the same transitions of 2谓\{beta}\{beta} decay were evaluated in an exposure of 61.8kg-yr. No excess over background was found for all decay modes. The lower half-life limits of the 2+1 state transitions of 0谓\{beta}\{beta} and 2谓\{beta}\{beta} decay were improved to T(0谓, 0+ \rightarrow 2+) > 2.6\times10^25 yr and T(2谓, 0+ \rightarrow 2+) > 4.6\times10^23 yr (90% C.L.), respectively. We report on the first experimental lower half-life limits for the transitions to the 0+1 state of 136Xe for 0谓\{beta}\{beta} and 2谓\{beta}\{beta} decay. They are T (0谓, 0+ \rightarrow 0+) > 2.4\times10^25 yr and T(2谓, 0+ \rightarrow 0+) > 8.3\times10^23 yr (90% C.L.). The transitions to the 2+2 states are also evaluated for the first time to be T(0谓, 0+ \rightarrow 2+) > 2.6\times10^25 yr and T(2谓, 0+ \rightarrow 2+) > 9.0\times10^23 yr (90% C.L.). These results are compared to recent theoretical predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.03724v2-abstract-full').style.display = 'none'; document.getElementById('1509.03724v2-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 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 4 figures. Published in Nuclear Physics A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1506.01175">arXiv:1506.01175</a> <span> [<a href="https://arxiv.org/pdf/1506.01175">pdf</a>, <a href="https://arxiv.org/ps/1506.01175">ps</a>, <a href="https://arxiv.org/format/1506.01175">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="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/10.3847/0004-637X/818/1/91">10.3847/0004-637X/818/1/91 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Asakura%2C+K">K. Asakura</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+T">T. Ishikawa</a>, <a href="/search/?searchtype=author&query=Ishio%2C+S">S. Ishio</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Tachibana%2C+H">H. Tachibana</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a> , et al. (22 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="1506.01175v4-abstract-short" style="display: inline;"> In the late stages of nuclear burning for massive stars ($M>8~M_{\sun}$), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01175v4-abstract-full').style.display = 'inline'; document.getElementById('1506.01175v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.01175v4-abstract-full" style="display: none;"> In the late stages of nuclear burning for massive stars ($M>8~M_{\sun}$), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta decay on free hydrogen. This is the golden channel for liquid scintillator detectors because the coincidence signature allows for significant reductions in background signals. We find that the kiloton-scale liquid scintillator detector KamLAND can detect these pre-supernova neutrinos from a star with a mass of $25~M_{\sun}$ at a distance less than 690~pc with 3$蟽$ significance before the supernova. This limit is dependent on the neutrino mass ordering and background levels. KamLAND takes data continuously and can provide a supernova alert to the community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01175v4-abstract-full').style.display = 'none'; document.getElementById('1506.01175v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 6 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.02137">arXiv:1503.02137</a> <span> [<a href="https://arxiv.org/pdf/1503.02137">pdf</a>, <a href="https://arxiv.org/ps/1503.02137">ps</a>, <a href="https://arxiv.org/format/1503.02137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/806/1/87">10.1088/0004-637X/806/1/87 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of electron anti-neutrinos associated with gamma-ray bursts using KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Asakura%2C+K">K. Asakura</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+T">T. Ishikawa</a>, <a href="/search/?searchtype=author&query=Ishio%2C+S">S. Ishio</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Tachibana%2C+H">H. Tachibana</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1503.02137v2-abstract-short" style="display: inline;"> We search for electron anti-neutrinos ($\overline谓_e$) from long and short-duration gamma-ray bursts~(GRBs) using data taken by the KamLAND detector from August 2002 to June 2013. No statistically significant excess over the background level is found. We place the tightest upper limits on $\overline谓_e$ fluence from GRBs below 7 MeV and place first constraints on the relation between… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02137v2-abstract-full').style.display = 'inline'; document.getElementById('1503.02137v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.02137v2-abstract-full" style="display: none;"> We search for electron anti-neutrinos ($\overline谓_e$) from long and short-duration gamma-ray bursts~(GRBs) using data taken by the KamLAND detector from August 2002 to June 2013. No statistically significant excess over the background level is found. We place the tightest upper limits on $\overline谓_e$ fluence from GRBs below 7 MeV and place first constraints on the relation between $\overline谓_e$ luminosity and effective temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02137v2-abstract-full').style.display = 'none'; document.getElementById('1503.02137v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages and 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 806 87 2015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.0413">arXiv:1407.0413</a> <span> [<a href="https://arxiv.org/pdf/1407.0413">pdf</a>, <a href="https://arxiv.org/format/1407.0413">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2014.09.068">10.1016/j.nima.2014.09.068 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A compact ultra-clean system for deploying radioactive sources inside the KamLAND detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Banks%2C+T+I">T. I. Banks</a>, <a href="/search/?searchtype=author&query=Freedman%2C+S+J">S. J. Freedman</a>, <a href="/search/?searchtype=author&query=Wallig%2C+J">J. Wallig</a>, <a href="/search/?searchtype=author&query=Ybarrolaza%2C+N">N. Ybarrolaza</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takemoto%2C+Y">Y. Takemoto</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Xu%2C+B+D">B. D. Xu</a>, <a href="/search/?searchtype=author&query=Yoshida%2C+H">H. Yoshida</a>, <a href="/search/?searchtype=author&query=Yoshida%2C+S">S. Yoshida</a>, <a href="/search/?searchtype=author&query=Kozlov%2C+A">A. Kozlov</a>, <a href="/search/?searchtype=author&query=Grant%2C+C">C. Grant</a>, <a href="/search/?searchtype=author&query=Keefer%2C+G">G. Keefer</a> , et al. (32 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="1407.0413v2-abstract-short" style="display: inline;"> We describe a compact, ultra-clean device used to deploy radioactive sources along the vertical axis of the KamLAND liquid-scintillator neutrino detector for purposes of calibration. The device worked by paying out and reeling in precise lengths of a hanging, small-gauge wire rope (cable); an assortment of interchangeable radioactive sources could be attached to a weight at the end of the cable. A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.0413v2-abstract-full').style.display = 'inline'; document.getElementById('1407.0413v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.0413v2-abstract-full" style="display: none;"> We describe a compact, ultra-clean device used to deploy radioactive sources along the vertical axis of the KamLAND liquid-scintillator neutrino detector for purposes of calibration. The device worked by paying out and reeling in precise lengths of a hanging, small-gauge wire rope (cable); an assortment of interchangeable radioactive sources could be attached to a weight at the end of the cable. All components exposed to the radiopure liquid scintillator were made of chemically compatible UHV-cleaned materials, primarily stainless steel, in order to avoid contaminating or degrading the scintillator. To prevent radon intrusion, the apparatus was enclosed in a hermetically sealed housing inside a glove box, and both volumes were regularly flushed with purified nitrogen gas. An infrared camera attached to the side of the housing permitted real-time visual monitoring of the cable's motion, and the system was controlled via a graphical user interface. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.0413v2-abstract-full').style.display = 'none'; document.getElementById('1407.0413v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Revised author affiliations, corrected typos, made minor improvements to text, and revised references</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Instruments and Methods in Physics Research Section A, Volume 769, 1 January 2015, pages 88-96 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.6190">arXiv:1405.6190</a> <span> [<a href="https://arxiv.org/pdf/1405.6190">pdf</a>, <a href="https://arxiv.org/ps/1405.6190">ps</a>, <a href="https://arxiv.org/format/1405.6190">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.92.055808">10.1103/PhysRevC.92.055808 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 7Be Solar Neutrino Measurement with KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hanakago%2C+H">H. Hanakago</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+H">H. Ishikawa</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+R">R. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakajima%2C+K">K. Nakajima</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obata%2C+A">A. Obata</a>, <a href="/search/?searchtype=author&query=Oki%2C+A">A. Oki</a>, <a href="/search/?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/?searchtype=author&query=Otani%2C+M">M. Otani</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a> , et al. (46 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="1405.6190v2-abstract-short" style="display: inline;"> We report a measurement of the neutrino-electron elastic scattering rate of 862 keV 7Be solar neutrinos based on a 165.4 kton-day exposure of KamLAND. The observed rate is 582 +/- 90 (kton-day)^-1, which corresponds to a 862 keV 7Be solar neutrino flux of (3.26 +/- 0.50) x 10^9 cm^-2s^-1, assuming a pure electron flavor flux. Comparing this flux with the standard solar model prediction and further… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.6190v2-abstract-full').style.display = 'inline'; document.getElementById('1405.6190v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.6190v2-abstract-full" style="display: none;"> We report a measurement of the neutrino-electron elastic scattering rate of 862 keV 7Be solar neutrinos based on a 165.4 kton-day exposure of KamLAND. The observed rate is 582 +/- 90 (kton-day)^-1, which corresponds to a 862 keV 7Be solar neutrino flux of (3.26 +/- 0.50) x 10^9 cm^-2s^-1, assuming a pure electron flavor flux. Comparing this flux with the standard solar model prediction and further assuming three flavor mixing, a nu_e survival probability of 0.66 +/- 0.14 is determined from the KamLAND data. Utilizing a global three flavor oscillation analysis, we obtain a total 7Be solar neutrino flux of (5.82 +/- 0.98) x 10^9 cm^-2s^-1, which is consistent with the standard solar model predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.6190v2-abstract-full').style.display = 'none'; document.getElementById('1405.6190v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 6 figures, submitted to Phys. Rev. C</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.0977">arXiv:1312.0977</a> <span> [<a href="https://arxiv.org/pdf/1312.0977">pdf</a>, <a href="https://arxiv.org/format/1312.0977">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Laboratory Studies on the Removal of Radon-Born Lead from KamLAND's Organic Liquid Scintillator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Keefer%2C+G">G. Keefer</a>, <a href="/search/?searchtype=author&query=Grant%2C+C">C. Grant</a>, <a href="/search/?searchtype=author&query=Piepke%2C+A">A. Piepke</a>, <a href="/search/?searchtype=author&query=Ebihara%2C+T">T. Ebihara</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Kibe%2C+Y">Y. Kibe</a>, <a href="/search/?searchtype=author&query=Koseki%2C+Y">Y. Koseki</a>, <a href="/search/?searchtype=author&query=Ogawa%2C+M">M. Ogawa</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Takeuchi%2C+S">S. Takeuchi</a>, <a href="/search/?searchtype=author&query=Mauger%2C+C">C. Mauger</a>, <a href="/search/?searchtype=author&query=Zhang%2C+C">C. Zhang</a>, <a href="/search/?searchtype=author&query=Schweitzer%2C+G">G. Schweitzer</a>, <a href="/search/?searchtype=author&query=Berger%2C+B+E">B. E. Berger</a>, <a href="/search/?searchtype=author&query=Dazeley%2C+S">S. Dazeley</a>, <a href="/search/?searchtype=author&query=Decowski%2C+M+P">M. P. Decowski</a>, <a href="/search/?searchtype=author&query=Detwiler%2C+J+A">J. A. Detwiler</a>, <a href="/search/?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/?searchtype=author&query=Dwyer%2C+D+A">D. A. Dwyer</a>, <a href="/search/?searchtype=author&query=Efremenko%2C+Y">Y. Efremenko</a>, <a href="/search/?searchtype=author&query=Enomoto%2C+S">S. Enomoto</a>, <a href="/search/?searchtype=author&query=Freedman%2C+S+J">S. J. Freedman</a>, <a href="/search/?searchtype=author&query=Fujikawa%2C+B+K">B. K. Fujikawa</a>, <a href="/search/?searchtype=author&query=Furuno%2C+K">K. Furuno</a> , et al. (43 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="1312.0977v1-abstract-short" style="display: inline;"> The removal of radioactivity from liquid scintillator has been studied in preparation of a low background phase of KamLAND. This paper describes the methods and techniques developed to measure and efficiently extract radon decay products from liquid scintillator. We report the radio-isotope reduction factors obtained when applying various extraction methods. During this study, distillation was ide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0977v1-abstract-full').style.display = 'inline'; document.getElementById('1312.0977v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.0977v1-abstract-full" style="display: none;"> The removal of radioactivity from liquid scintillator has been studied in preparation of a low background phase of KamLAND. This paper describes the methods and techniques developed to measure and efficiently extract radon decay products from liquid scintillator. We report the radio-isotope reduction factors obtained when applying various extraction methods. During this study, distillation was identified as the most efficient method for removing radon daughters from liquid scintillator. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0977v1-abstract-full').style.display = 'none'; document.getElementById('1312.0977v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-05 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.0896">arXiv:1312.0896</a> <span> [<a href="https://arxiv.org/pdf/1312.0896">pdf</a>, <a href="https://arxiv.org/format/1312.0896">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"> CeLAND: search for a 4th light neutrino state with a 3 PBq 144Ce-144Pr electron antineutrino generator in KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+H">H. Ishikawa</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+R">R. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/?searchtype=author&query=Otani%2C+M">M. Otani</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suekane%2C+F">F. Suekane</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takemoto%2C+Y">Y. Takemoto</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Xu%2C+B+D">B. D. Xu</a>, <a href="/search/?searchtype=author&query=Yamada%2C+S">S. Yamada</a> , et al. (41 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="1312.0896v2-abstract-short" style="display: inline;"> The reactor neutrino and gallium anomalies can be tested with a 3-4 PBq (75-100 kCi scale) 144Ce-144Pr antineutrino beta-source deployed at the center or next to a large low-background liquid scintillator detector. The antineutrino generator will be produced by the Russian reprocessing plant PA Mayak as early as 2014, transported to Japan, and deployed in the Kamioka Liquid Scintillator Anti-Neutr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0896v2-abstract-full').style.display = 'inline'; document.getElementById('1312.0896v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.0896v2-abstract-full" style="display: none;"> The reactor neutrino and gallium anomalies can be tested with a 3-4 PBq (75-100 kCi scale) 144Ce-144Pr antineutrino beta-source deployed at the center or next to a large low-background liquid scintillator detector. The antineutrino generator will be produced by the Russian reprocessing plant PA Mayak as early as 2014, transported to Japan, and deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND) as early as 2015. KamLAND's 13 m diameter target volume provides a suitable environment to measure the energy and position dependence of the detected neutrino flux. A characteristic oscillation pattern would be visible for a baseline of about 10 m or less, providing a very clean signal of neutrino disappearance into a yet-unknown, sterile neutrino state. This will provide a comprehensive test of the electron dissaperance neutrino anomalies and could lead to the discovery of a 4th neutrino state for Delta_m^2 > 0.1 eV^2 and sin^2(2theta) > 0.05. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0896v2-abstract-full').style.display = 'none'; document.getElementById('1312.0896v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">67 pages, 50 figures. Th. Lasserre thanks the European Research Council for support under the Starting Grant StG-307184</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.6805">arXiv:1309.6805</a> <span> [<a href="https://arxiv.org/pdf/1309.6805">pdf</a>, <a href="https://arxiv.org/format/1309.6805">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"> White paper: CeLAND - Investigation of the reactor antineutrino anomaly with an intense 144Ce-144Pr antineutrino source in KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+H">H. Ishikawa</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+R">R. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/?searchtype=author&query=Otani%2C+M">M. Otani</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suekane%2C+F">F. Suekane</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takemoto%2C+Y">Y. Takemoto</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Xu%2C+B+D">B. D. Xu</a>, <a href="/search/?searchtype=author&query=Yamada%2C+S">S. Yamada</a> , et al. (35 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="1309.6805v2-abstract-short" style="display: inline;"> We propose to test for short baseline neutrino oscillations, implied by the recent reevaluation of the reactor antineutrino flux and by anomalous results from the gallium solar neutrino detectors. The test will consist of producing a 75 kCi 144Ce - 144Pr antineutrino source to be deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND). KamLAND's 13m diameter target volume prov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.6805v2-abstract-full').style.display = 'inline'; document.getElementById('1309.6805v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.6805v2-abstract-full" style="display: none;"> We propose to test for short baseline neutrino oscillations, implied by the recent reevaluation of the reactor antineutrino flux and by anomalous results from the gallium solar neutrino detectors. The test will consist of producing a 75 kCi 144Ce - 144Pr antineutrino source to be deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND). KamLAND's 13m diameter target volume provides a suitable environment to measure energy and position dependence of the detected neutrino flux. A characteristic oscillation pattern would be visible for a baseline of about 10 m or less, providing a very clean signal of neutrino disappearance into a yet-unknown, "sterile" state. Such a measurement will be free of any reactor-related uncertainties. After 1.5 years of data taking the Reactor Antineutrino Anomaly parameter space will be tested at > 95% C.L. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.6805v2-abstract-full').style.display = 'none'; document.getElementById('1309.6805v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">White paper prepared for Snowmass-2013; slightly different 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/1205.6372">arXiv:1205.6372</a> <span> [<a href="https://arxiv.org/pdf/1205.6372">pdf</a>, <a href="https://arxiv.org/ps/1205.6372">ps</a>, <a href="https://arxiv.org/format/1205.6372">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.86.021601">10.1103/PhysRevC.86.021601 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on Majoron-emitting double-beta decays of Xe-136 in the KamLAND-Zen experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hanakago%2C+H">H. Hanakago</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Kato%2C+R">R. Kato</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Nakada%2C+T">T. Nakada</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obata%2C+A">A. Obata</a>, <a href="/search/?searchtype=author&query=Oki%2C+A">A. Oki</a>, <a href="/search/?searchtype=author&query=Ono%2C+Y">Y. Ono</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takemoto%2C+Y">Y. Takemoto</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Xu%2C+B+D">B. D. Xu</a>, <a href="/search/?searchtype=author&query=Yamada%2C+S">S. Yamada</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1205.6372v2-abstract-short" style="display: inline;"> We present limits on Majoron-emitting neutrinoless double-beta decay modes based on an exposure of 112.3 days with 125 kg of Xe-136. In particular, a lower limit on the ordinary (spectral index n = 1) Majoron-emitting decay half-life of Xe-136 is obtained as T_{1/2}^{0谓蠂^{0}} > 2.6 x 10^{24} yr at 90% C.L., a factor of five more stringent than previous limits. The corresponding upper limit on the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.6372v2-abstract-full').style.display = 'inline'; document.getElementById('1205.6372v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1205.6372v2-abstract-full" style="display: none;"> We present limits on Majoron-emitting neutrinoless double-beta decay modes based on an exposure of 112.3 days with 125 kg of Xe-136. In particular, a lower limit on the ordinary (spectral index n = 1) Majoron-emitting decay half-life of Xe-136 is obtained as T_{1/2}^{0谓蠂^{0}} > 2.6 x 10^{24} yr at 90% C.L., a factor of five more stringent than previous limits. The corresponding upper limit on the effective Majoron-neutrino coupling, using a range of available nuclear matrix calculations, is <g_{ee}> < (0.8 - 1.6) x 10^{-5}. This excludes a previously unconstrained region of parameter space and strongly limits the possible contribution of ordinary Majoron emission modes to 0谓尾尾decay for neutrino masses in the inverted hierarchy scheme. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.6372v2-abstract-full').style.display = 'none'; document.getElementById('1205.6372v2-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 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 May, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 3 figures (1 figure added). Published version in PRC rapid communication</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C86:021601,2012 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1106.0861">arXiv:1106.0861</a> <span> [<a href="https://arxiv.org/pdf/1106.0861">pdf</a>, <a href="https://arxiv.org/ps/1106.0861">ps</a>, <a href="https://arxiv.org/format/1106.0861">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.84.035804">10.1103/PhysRevC.84.035804 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the 8B Solar Neutrino Flux with the KamLAND Liquid Scintillator Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Furuno%2C+K">K. Furuno</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Kibe%2C+Y">Y. Kibe</a>, <a href="/search/?searchtype=author&query=Kimura%2C+W">W. Kimura</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Minekawa%2C+Y">Y. Minekawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Morikawa%2C+T">T. Morikawa</a>, <a href="/search/?searchtype=author&query=Nagai%2C+N">N. Nagai</a>, <a href="/search/?searchtype=author&query=Nakajima%2C+K">K. Nakajima</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+M">M. Nakamura</a>, <a href="/search/?searchtype=author&query=Narita%2C+K">K. Narita</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+Y">Y. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suekane%2C+F">F. Suekane</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a> , et al. (55 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="1106.0861v3-abstract-short" style="display: inline;"> We report a measurement of the neutrino-electron elastic scattering rate from 8B solar neutrinos based on a 123 kton-day exposure of KamLAND. The background-subtracted electron recoil rate, above a 5.5 MeV analysis threshold is 1.49+/-0.14(stat)+/-0.17(syst) events per kton-day. Interpreted as due to a pure electron flavor flux with a 8B neutrino spectrum, this corresponds to a spectrum integrated… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.0861v3-abstract-full').style.display = 'inline'; document.getElementById('1106.0861v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1106.0861v3-abstract-full" style="display: none;"> We report a measurement of the neutrino-electron elastic scattering rate from 8B solar neutrinos based on a 123 kton-day exposure of KamLAND. The background-subtracted electron recoil rate, above a 5.5 MeV analysis threshold is 1.49+/-0.14(stat)+/-0.17(syst) events per kton-day. Interpreted as due to a pure electron flavor flux with a 8B neutrino spectrum, this corresponds to a spectrum integrated flux of 2.77+/-0.26(stat)+/-0.32(syst) x 10^6 cm^-2s^-1. The analysis threshold is driven by 208Tl present in the liquid scintillator, and the main source of systematic uncertainty is due to background from cosmogenic 11Be. The measured rate is consistent with existing measurements and with Standard Solar Model predictions which include matter enhanced neutrino oscillation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.0861v3-abstract-full').style.display = 'none'; document.getElementById('1106.0861v3-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 August, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 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/hep-ex/0404025">arXiv:hep-ex/0404025</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0404025">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0404025">ps</a>, <a href="https://arxiv.org/format/hep-ex/0404025">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="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.70.083523">10.1103/PhysRevD.70.083523 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </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.70.109901">10.1103/PhysRevD.70.109901 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Dark Matter WIMPs using Upward Through-going Muons in Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/?searchtype=author&query=Ashie%2C+Y">Y. Ashie</a>, <a href="/search/?searchtype=author&query=Fukuda%2C+S">S. Fukuda</a>, <a href="/search/?searchtype=author&query=Fukuda%2C+Y">Y. Fukuda</a>, <a href="/search/?searchtype=author&query=Ishihara%2C+K">K. Ishihara</a>, <a href="/search/?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/?searchtype=author&query=Koshio%2C+Y">Y. Koshio</a>, <a href="/search/?searchtype=author&query=Minamino%2C+A">A. Minamino</a>, <a href="/search/?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/?searchtype=author&query=Namba%2C+T">T. Namba</a>, <a href="/search/?searchtype=author&query=Nambu%2C+R">R. Nambu</a>, <a href="/search/?searchtype=author&query=Obayashi%2C+Y">Y. Obayashi</a>, <a href="/search/?searchtype=author&query=Sakurai%2C+N">N. Sakurai</a>, <a href="/search/?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a>, <a href="/search/?searchtype=author&query=Takeuchi%2C+H">H. Takeuchi</a>, <a href="/search/?searchtype=author&query=Takeuchi%2C+Y">Y. Takeuchi</a>, <a href="/search/?searchtype=author&query=Yamada%2C+S">S. Yamada</a>, <a href="/search/?searchtype=author&query=Ishitsuka%2C+M">M. Ishitsuka</a>, <a href="/search/?searchtype=author&query=Kajita%2C+T">T. Kajita</a>, <a href="/search/?searchtype=author&query=Kaneyuki%2C+K">K. Kaneyuki</a> , et al. (112 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="hep-ex/0404025v2-abstract-short" style="display: inline;"> We present the results of indirect searches for Weakly Interacting Massive Particles (WIMPs) with 1679.6 live days of data from the Super-Kamiokande detector using neutrino-induced upward through-going muons. The search is performed by looking for an excess of high energy muon neutrinos from WIMP annihilations in the Sun, the core of the Earth, and the Galactic Center, as compared to the number… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0404025v2-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0404025v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0404025v2-abstract-full" style="display: none;"> We present the results of indirect searches for Weakly Interacting Massive Particles (WIMPs) with 1679.6 live days of data from the Super-Kamiokande detector using neutrino-induced upward through-going muons. The search is performed by looking for an excess of high energy muon neutrinos from WIMP annihilations in the Sun, the core of the Earth, and the Galactic Center, as compared to the number expected from the atmospheric neutrino background. No statistically significant excess was seen. We calculate flux limits in various angular cones around each of the above celestial objects. We obtain conservative model-independent upper limits on WIMP-nucleon cross-section as a function of WIMP mass and compare these results with the corresponding results from direct dark matter detection experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0404025v2-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0404025v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 July, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 April, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2004. </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, 14 figures, Submitted to Phys. Rev. D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D70:083523,2004; Erratum-ibid.D70:109901,2004 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 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