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type="radio" value="hide"> <label for="abstracts-1">Hide abstracts</label></li></ul> </div> <div class="box field is-grouped is-grouped-multiline level-item"> <div class="control"> <span class="select is-small"> <select id="size" name="size"><option value="25">25</option><option selected value="50">50</option><option value="100">100</option><option value="200">200</option></select> </span> <label for="size">results per page</label>. </div> <div class="control"> <label for="order">Sort results by</label> <span class="select is-small"> <select id="order" name="order"><option selected value="-announced_date_first">Announcement date (newest first)</option><option value="announced_date_first">Announcement date (oldest first)</option><option value="-submitted_date">Submission date (newest first)</option><option value="submitted_date">Submission date (oldest first)</option><option value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/hep-ex?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/hep-ex?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/hep-ex?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+T">T. Nakahata</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/hep-ex?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/hep-ex?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/hep-ex?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/hep-ex?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/hep-ex?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/hep-ex?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Kinoshita%2C+T">T. Kinoshita</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Maemura%2C+N">N. Maemura</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?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> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 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