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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/2404.09920">arXiv:2404.09920</a> <span> [<a href="https://arxiv.org/pdf/2404.09920">pdf</a>, <a href="https://arxiv.org/format/2404.09920">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad5fee">10.3847/1538-4357/ad5fee <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combined Pre-Supernova Alert System with Kamland and Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KamLAND"> KamLAND</a>, <a href="/search/hep-ex?searchtype=author&query=Collaborations%2C+S">Super-Kamiokande Collaborations</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+S">Seisho Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Eizuka%2C+M">Minori Eizuka</a>, <a href="/search/hep-ex?searchtype=author&query=Futagi%2C+S">Sawako Futagi</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">Azusa Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Yoshihito Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Goto%2C+S">Shun Goto</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">Takahiko Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hata%2C+K">Kazumi Hata</a>, <a href="/search/hep-ex?searchtype=author&query=Ichimura%2C+K">Koichi Ichimura</a>, <a href="/search/hep-ex?searchtype=author&query=Ieki%2C+S">Sei Ieki</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">Haruo Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">Kunio Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">Koji Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Kamei%2C+Y">Yuto Kamei</a>, <a href="/search/hep-ex?searchtype=author&query=Kawada%2C+N">Nanami Kawada</a>, <a href="/search/hep-ex?searchtype=author&query=Kishimoto%2C+Y">Yasuhiro Kishimoto</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">Masayuki Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Kurasawa%2C+M">Maho Kurasawa</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">Tadao Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Miyake%2C+H">Haruhiko Miyake</a>, <a href="/search/hep-ex?searchtype=author&query=Morita%2C+D">Daisuke Morita</a>, <a href="/search/hep-ex?searchtype=author&query=Nakahata%2C+T">Takeshi Nakahata</a> , et al. (290 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.09920v3-abstract-short" style="display: inline;"> Preceding a core-collapse supernova, various processes produce an increasing amount of neutrinos of all flavors characterized by mounting energies from the interior of massive stars. Among them, the electron antineutrinos are potentially detectable by terrestrial neutrino experiments such as KamLAND and Super-Kamiokande via inverse beta decay interactions. Once these pre-supernova neutrinos are ob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09920v3-abstract-full').style.display = 'inline'; document.getElementById('2404.09920v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.09920v3-abstract-full" style="display: none;"> Preceding a core-collapse supernova, various processes produce an increasing amount of neutrinos of all flavors characterized by mounting energies from the interior of massive stars. Among them, the electron antineutrinos are potentially detectable by terrestrial neutrino experiments such as KamLAND and Super-Kamiokande via inverse beta decay interactions. Once these pre-supernova neutrinos are observed, an early warning of the upcoming core-collapse supernova can be provided. In light of this, KamLAND and Super-Kamiokande, both located in the Kamioka mine in Japan, have been monitoring pre-supernova neutrinos since 2015 and 2021, respectively. Recently, we performed a joint study between KamLAND and Super-Kamiokande on pre-supernova neutrino detection. A pre-supernova alert system combining the KamLAND detector and the Super-Kamiokande detector was developed and put into operation, which can provide a supernova alert to the astrophysics community. Fully leveraging the complementary properties of these two detectors, the combined alert is expected to resolve a pre-supernova neutrino signal from a 15 M$_{\odot}$ star within 510 pc of the Earth, at a significance level corresponding to a false alarm rate of no more than 1 per century. For a Betelgeuse-like model with optimistic parameters, it can provide early warnings up to 12 hours in advance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09920v3-abstract-full').style.display = 'none'; document.getElementById('2404.09920v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Resubmitted to ApJ. 22 pages, 16 figures, for more information about the combined pre-supernova alert system, see https://www.lowbg.org/presnalarm/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/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/hep-ex?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</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=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashi%2C+A">A. Hayashi</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashida%2C+S">S. Hayashida</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=Karino%2C+Y">Y. Karino</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/hep-ex?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/hep-ex?searchtype=author&query=Ozaki%2C+H">H. Ozaki</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/hep-ex?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/hep-ex?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/hep-ex?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/hep-ex?searchtype=author&query=Takai%2C+T">T. Takai</a>, <a href="/search/hep-ex?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/hep-ex?searchtype=author&query=Teraoka%2C+Y">Y. Teraoka</a>, <a href="/search/hep-ex?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/1505.03612">arXiv:1505.03612</a> <span> [<a href="https://arxiv.org/pdf/1505.03612">pdf</a>, <a href="https://arxiv.org/ps/1505.03612">ps</a>, <a href="https://arxiv.org/format/1505.03612">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/PhysRevD.92.052006">10.1103/PhysRevD.92.052006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for the proton decay mode $p \rightarrow \overline谓 K^{+}$ with KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1505.03612v3-abstract-short" style="display: inline;"> We present a search for the proton decay mode $p \rightarrow \overline谓 K^{+}$ based on an exposure of 8.97 kton-years in the KamLAND experiment. The liquid scintillator detector is sensitive to successive signals from $p \rightarrow \overline谓 K^{+}$ with unique kinematics, which allow us to achieve a detection efficiency of 44%, higher than previous searches in water Cherenkov detectors. We find… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.03612v3-abstract-full').style.display = 'inline'; document.getElementById('1505.03612v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1505.03612v3-abstract-full" style="display: none;"> We present a search for the proton decay mode $p \rightarrow \overline谓 K^{+}$ based on an exposure of 8.97 kton-years in the KamLAND experiment. The liquid scintillator detector is sensitive to successive signals from $p \rightarrow \overline谓 K^{+}$ with unique kinematics, which allow us to achieve a detection efficiency of 44%, higher than previous searches in water Cherenkov detectors. We find no evidence of proton decays for this mode. The expected background, which is dominated by atmospheric neutrinos, is $0.9 \pm 0.2$ events. The nonbackground-subtracted limit on the partial proton lifetime is $蟿/ B(p \rightarrow \overline谓 K^{+}) > 5.4 \times 10^{32}$ years at 90% C.L. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.03612v3-abstract-full').style.display = 'none'; document.getElementById('1505.03612v3-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 May, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D92:052006,2015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1303.4667">arXiv:1303.4667</a> <span> [<a href="https://arxiv.org/pdf/1303.4667">pdf</a>, <a href="https://arxiv.org/ps/1303.4667">ps</a>, <a href="https://arxiv.org/format/1303.4667">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="Geophysics">physics.geo-ph</span> </div> </div> <p class="title is-5 mathjax"> Reactor On-Off Antineutrino Measurement with KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+KamLAND+Collaboration"> The KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1303.4667v2-abstract-short" style="display: inline;"> The recent long-term shutdown of Japanese nuclear reactors has resulted in a significantly reduced reactor $\bar{nu}_{e}$ flux at KamLAND. This running condition provides a unique opportunity to confirm and constrain backgrounds for the reactor $\bar{nu}_{e}$ oscillation analysis. The data set also has improved sensitivity for other $\bar{nu}_{e}$ signals, in particular $\bar{nu}_{e}$'s produced i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1303.4667v2-abstract-full').style.display = 'inline'; document.getElementById('1303.4667v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1303.4667v2-abstract-full" style="display: none;"> The recent long-term shutdown of Japanese nuclear reactors has resulted in a significantly reduced reactor $\bar{nu}_{e}$ flux at KamLAND. This running condition provides a unique opportunity to confirm and constrain backgrounds for the reactor $\bar{nu}_{e}$ oscillation analysis. The data set also has improved sensitivity for other $\bar{nu}_{e}$ signals, in particular $\bar{nu}_{e}$'s produced in $尾$-decays from $^{238}$U and $^{232}$Th within the Earth's interior, whose energy spectrum overlaps with that of reactor $\bar{nu}_{e}$'s. Including constraints on $胃_{13}$ from accelerator and short-baseline reactor neutrino experiments, a combined three-flavor analysis of solar and KamLAND data gives fit values for the oscillation parameters of $tan^{2} 胃_{12} = 0.436^{+0.029}_{-0.025}$, $螖m^{2}_{21} = 7.53^{+0.18}_{-0.18} \times 10^{-5} {eV}^{2}$, and $sin^{2} 胃_{13} = 0.023^{+0.002}_{-0.002}$. Assuming a chondritic Th/U mass ratio, we obtain $116^{+28}_{-27}$ $\bar{nu}_{e}$ events from $^{238}$U and $^{232}$Th, corresponding to a geo $\bar{nu}_{e}$ flux of $3.4^{+0.8}_{-0.8} \times 10^{6} {cm^{-2}s^{-1}}$ at the KamLAND location. We evaluate various bulk silicate Earth composition models using the observed geo $\bar{nu}_{e}$ rate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1303.4667v2-abstract-full').style.display = 'none'; document.getElementById('1303.4667v2-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 March, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 March, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">9 pages, 8 figures. Fig.4 (b) has been replaced with the corrected version</span> </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/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=Furuno%2C+K">K. Furuno</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=Ichimura%2C+K">K. Ichimura</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=Kibe%2C+Y">Y. Kibe</a>, <a href="/search/hep-ex?searchtype=author&query=Kimura%2C+W">W. Kimura</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=Minekawa%2C+Y">Y. Minekawa</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Morikawa%2C+T">T. Morikawa</a>, <a href="/search/hep-ex?searchtype=author&query=Nagai%2C+N">N. Nagai</a>, <a href="/search/hep-ex?searchtype=author&query=Nakajima%2C+K">K. Nakajima</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+M">M. Nakamura</a>, <a href="/search/hep-ex?searchtype=author&query=Narita%2C+K">K. Narita</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+Y">Y. Shimizu</a>, <a href="/search/hep-ex?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/hep-ex?searchtype=author&query=Suekane%2C+F">F. Suekane</a>, <a href="/search/hep-ex?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/1105.3516">arXiv:1105.3516</a> <span> [<a href="https://arxiv.org/pdf/1105.3516">pdf</a>, <a href="https://arxiv.org/ps/1105.3516">ps</a>, <a href="https://arxiv.org/format/1105.3516">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/10.1088/0004-637X/745/2/193">10.1088/0004-637X/745/2/193 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for extraterrestrial antineutrino sources with the KamLAND detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+KamLAND+Collaboration"> The KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1105.3516v2-abstract-short" style="display: inline;"> We present the results of a search for extraterrestrial electron antineutrinos ($\bar谓_{e}$'s) in the energy range $8.3 MeV < E_{\bar谓_{e}} < 31.8 MeV$ using the KamLAND detector. In an exposure of 4.53 kton-year, we identify 25 candidate events. All of the candidate events can be attributed to background, most importantly neutral current atmospheric neutrino interactions, setting an upper limit o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.3516v2-abstract-full').style.display = 'inline'; document.getElementById('1105.3516v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1105.3516v2-abstract-full" style="display: none;"> We present the results of a search for extraterrestrial electron antineutrinos ($\bar谓_{e}$'s) in the energy range $8.3 MeV < E_{\bar谓_{e}} < 31.8 MeV$ using the KamLAND detector. In an exposure of 4.53 kton-year, we identify 25 candidate events. All of the candidate events can be attributed to background, most importantly neutral current atmospheric neutrino interactions, setting an upper limit on the probability of $^{8}$B solar $谓_{e}$'s converting into $\bar谓_{e}$'s at $5.3 \times 10^{-5}$ (90% C.L.), if we assume an undistorted $\bar谓_{e}$ shape. This limit corresponds to a solar $\bar谓_{e}$ flux of $93 cm^{-2} s^{-1}$ or an event rate of $1.6 events (kton-year)^{-1}$ above the energy threshold $(E_{\bar谓_{e}} > 8.3 MeV)$. The present data also allows us to set more stringent limits on the diffuse supernova neutrino flux and on the annihilation rates for light dark matter particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.3516v2-abstract-full').style.display = 'none'; document.getElementById('1105.3516v2-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 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">22 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.745:193,2012 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1009.4771">arXiv:1009.4771</a> <span> [<a href="https://arxiv.org/pdf/1009.4771">pdf</a>, <a href="https://arxiv.org/ps/1009.4771">ps</a>, <a href="https://arxiv.org/format/1009.4771">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="Geophysics">physics.geo-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.83.052002">10.1103/PhysRevD.83.052002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on $胃_{13}$ from A Three-Flavor Oscillation Analysis of Reactor Antineutrinos at KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+KamLAND+Collaboration"> The KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1009.4771v3-abstract-short" style="display: inline;"> We present new constraints on the neutrino oscillation parameters $/textyen Delta m^{2}_{21}$, $/textyen theta_{12}$, and $/textyen theta_{13}$ from a three-flavor analysis of solar and KamLAND data. The KamLAND data set includes data acquired following a radiopurity upgrade and amounts to a total exposure of $3.49 \textyen times 10^{32}$ target-proton-year. Under the assumption of {\textyen it CP… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.4771v3-abstract-full').style.display = 'inline'; document.getElementById('1009.4771v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1009.4771v3-abstract-full" style="display: none;"> We present new constraints on the neutrino oscillation parameters $/textyen Delta m^{2}_{21}$, $/textyen theta_{12}$, and $/textyen theta_{13}$ from a three-flavor analysis of solar and KamLAND data. The KamLAND data set includes data acquired following a radiopurity upgrade and amounts to a total exposure of $3.49 \textyen times 10^{32}$ target-proton-year. Under the assumption of {\textyen it CPT} invariance, a two-flavor analysis (/textyen mbox{$\textyen theta_{13} = 0$}) of the KamLAND and solar data yields the best-fit values $\textyen tan^{2} \textyen theta_{12} = 0.444^{+0.036}_{-0.030}$ and $\textyen Delta m^{2}_{21} = 7.50^{+0.19}_{-0.20} \textyen times 10^{-5} ~ {\textyen rm eV}^{2}$; a three-flavor analysis with $\textyen theta_{13}$ as a free parameter yields the best-fit values $\textyen tan^{2} \textyen theta_{12} = 0.452^{+0.035}_{-0.033}$, $\textyen Delta m^{2}_{21} = 7.50^{+0.19}_{-0.20} \textyen times 10^{-5} ~ {\textyen rm eV}^{2}$, and $\textyen sin^{2} \textyen theta_{13} = 0.020^{+0.016}_{-0.016}$. This $\textyen theta_{13}$ interval is consistent with other recent work combining the CHOOZ, atmospheric and long-baseline accelerator experiments. We also present a new global $\textyen theta_{13}$ analysis, incorporating the CHOOZ, atmospheric and accelerator data, which indicates $\textyen sin^{2} \textyen theta_{13} = 0.009^{+0.013}_{-0.007}$. A nonzero value is suggested, but only at the 79\textyen% C.L. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.4771v3-abstract-full').style.display = 'none'; document.getElementById('1009.4771v3-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 March, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 September, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2010. </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, 7 figures. Version as published in PRD. The dChi2-map and prompt energy spectrum for this analysis are available at http://www.awa.tohoku.ac.jp/KamLAND/4th_result_data_release/4th_result_data_release.html</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D83:052002,2011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0907.0066">arXiv:0907.0066</a> <span> [<a href="https://arxiv.org/pdf/0907.0066">pdf</a>, <a href="https://arxiv.org/ps/0907.0066">ps</a>, <a href="https://arxiv.org/format/0907.0066">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.81.025807">10.1103/PhysRevC.81.025807 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Production of Radioactive Isotopes through Cosmic Muon Spallation in KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+KamLAND+Collaboration"> The KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0907.0066v2-abstract-short" style="display: inline;"> Radioactive isotopes produced through cosmic muon spallation are a background for rare-event detection in $谓$ detectors, double-$尾$-decay experiments, and dark-matter searches. Understanding the nature of cosmogenic backgrounds is particularly important for future experiments aiming to determine the pep and CNO solar neutrino fluxes, for which the background is dominated by the spallation produc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.0066v2-abstract-full').style.display = 'inline'; document.getElementById('0907.0066v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.0066v2-abstract-full" style="display: none;"> Radioactive isotopes produced through cosmic muon spallation are a background for rare-event detection in $谓$ detectors, double-$尾$-decay experiments, and dark-matter searches. Understanding the nature of cosmogenic backgrounds is particularly important for future experiments aiming to determine the pep and CNO solar neutrino fluxes, for which the background is dominated by the spallation production of $^{11}$C. Data from the Kamioka liquid-scintillator antineutrino detector (KamLAND) provides valuable information for better understanding these backgrounds, especially in liquid scintillators, and for checking estimates from current simulations based upon MUSIC, FLUKA, and GEANT4. Using the time correlation between detected muons and neutron captures, the neutron production yield in the KamLAND liquid scintillator is measured to be $(2.8 \pm 0.3) \times 10^{-4} 渭^{-1} g^{-1} cm^{2}$. For other isotopes, the production yield is determined from the observed time correlation related to known isotope lifetimes. We find some yields are inconsistent with extrapolations based on an accelerator muon beam experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.0066v2-abstract-full').style.display = 'none'; document.getElementById('0907.0066v2-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 March, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2009. </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, 20 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C81:025807,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0903.0441">arXiv:0903.0441</a> <span> [<a href="https://arxiv.org/pdf/0903.0441">pdf</a>, <a href="https://arxiv.org/format/0903.0441">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/10.1088/1748-0221/4/04/P04017">10.1088/1748-0221/4/04/P04017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The KamLAND Full-Volume Calibration System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+KamLAND+Collaboration"> The KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0903.0441v1-abstract-short" style="display: inline;"> We have successfully built and operated a source deployment system for the KamLAND detector. This system was used to position radioactive sources throughout the delicate 1-kton liquid scintillator volume, while meeting stringent material cleanliness, material compatibility, and safety requirements. The calibration data obtained with this device were used to fully characterize detector position a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0903.0441v1-abstract-full').style.display = 'inline'; document.getElementById('0903.0441v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0903.0441v1-abstract-full" style="display: none;"> We have successfully built and operated a source deployment system for the KamLAND detector. This system was used to position radioactive sources throughout the delicate 1-kton liquid scintillator volume, while meeting stringent material cleanliness, material compatibility, and safety requirements. The calibration data obtained with this device were used to fully characterize detector position and energy reconstruction biases. As a result, the uncertainty in the size of the detector fiducial volume was reduced by a factor of two. Prior to calibration with this system, the fiducial volume was the largest source of systematic uncertainty in measuring the number of anti-neutrinos detected by KamLAND. This paper describes the design, operation and performance of this unique calibration system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0903.0441v1-abstract-full').style.display = 'none'; document.getElementById('0903.0441v1-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 March, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 22 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> JINST 4:P04017,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0801.4589">arXiv:0801.4589</a> <span> [<a href="https://arxiv.org/pdf/0801.4589">pdf</a>, <a href="https://arxiv.org/ps/0801.4589">ps</a>, <a href="https://arxiv.org/format/0801.4589">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="Geophysics">physics.geo-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/PhysRevLett.100.221803">10.1103/PhysRevLett.100.221803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precision Measurement of Neutrino Oscillation Parameters with KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+KamLAND+Collaboration"> The KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0801.4589v3-abstract-short" style="display: inline;"> The KamLAND experiment has determined a precise value for the neutrino oscillation parameter $螖m^{2}_{21}$ and stringent constraints on $胃_{12}$. The exposure to nuclear reactor anti-neutrinos is increased almost fourfold over previous results to 2.44$\times10^{32}$ proton-yr due to longer livetime and an enlarged fiducial volume. An undistorted reactor $\bar谓_{e}$ energy spectrum is now rejecte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0801.4589v3-abstract-full').style.display = 'inline'; document.getElementById('0801.4589v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0801.4589v3-abstract-full" style="display: none;"> The KamLAND experiment has determined a precise value for the neutrino oscillation parameter $螖m^{2}_{21}$ and stringent constraints on $胃_{12}$. The exposure to nuclear reactor anti-neutrinos is increased almost fourfold over previous results to 2.44$\times10^{32}$ proton-yr due to longer livetime and an enlarged fiducial volume. An undistorted reactor $\bar谓_{e}$ energy spectrum is now rejected at >5$蟽$. Extending the analysis down to the inverse beta decay energy threshold, and incorporating geo-neutrinos, gives a best-fit at $螖m^{2}_{21}$= $7.58^{+0.14}_{-0.13}(stat)^{+0.15}_{-0.15}(syst)\times10^{-5}$ eV$^{2}$ and $\tan^2 胃_{12}$=$0.56^{+0.10}_{0.07}(stat)^{+0.10}_{-0.06}(syst)$. Local $螖蠂^2$-minima at higher and lower $螖m^{2}_{21}$ are disfavored at >4$蟽$. Combining with solar neutrino data, we obtain $螖m^{2}_{21}$= $7.59^{+0.21}_{-0.21}\times10^{-5}$ eV$^{2}$ and $\tan^2 胃_{12}$=$0.47^{+0.06}_{-0.05}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0801.4589v3-abstract-full').style.display = 'none'; document.getElementById('0801.4589v3-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 June, 2008; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 January, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2008. </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">Version as published in PRL. Revised Fig. 2 (allowed contours) due to an error in the figure generating code (numbers or conclusions did not change). The full dChi2-map for this analysis is available at http://www.awa.tohoku.ac.jp/KamLAND/chi2map_3rdresult/chi2map.html . Fig. 3 (low E spectrum) was dropped due to space limitations</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.100:221803,2008 </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/0512059">arXiv:hep-ex/0512059</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0512059">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0512059">ps</a>, <a href="https://arxiv.org/format/hep-ex/0512059">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.96.101802">10.1103/PhysRevLett.96.101802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for the Invisible Decay of Neutrons with KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+KamLAND+collaboration"> The KamLAND collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="hep-ex/0512059v2-abstract-short" style="display: inline;"> The Kamioka Liquid scintillator Anti-Neutrino Detector (KamLAND) is used in a search for single neutron or two neutron intra-nuclear disappearance that would produce holes in the $\it{s}$-shell energy level of $^{12}$C nuclei. Such holes could be created as a result of nucleon decay into invisible modes ($inv$), e.g. $n \to 3谓$ or $nn \to 2谓$. The de-excitation of the corresponding daughter nucl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0512059v2-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0512059v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0512059v2-abstract-full" style="display: none;"> The Kamioka Liquid scintillator Anti-Neutrino Detector (KamLAND) is used in a search for single neutron or two neutron intra-nuclear disappearance that would produce holes in the $\it{s}$-shell energy level of $^{12}$C nuclei. Such holes could be created as a result of nucleon decay into invisible modes ($inv$), e.g. $n \to 3谓$ or $nn \to 2谓$. The de-excitation of the corresponding daughter nucleus results in a sequence of space and time correlated events observable in the liquid scintillator detector. We report on new limits for one- and two-neutron disappearance: $蟿(n\to inv)> 5.8\times 10^{29}$ years and $蟿(nn \to inv)> 1.4 \times 10^{30}$ years at 90% CL. These results represent an improvement of factors of $\sim$3 and $>10^4$ over previous experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0512059v2-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0512059v2-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 February, 2006; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 December, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 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.96:101802,2006 </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/0406035">arXiv:hep-ex/0406035</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0406035">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0406035">ps</a>, <a href="https://arxiv.org/format/hep-ex/0406035">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.94.081801">10.1103/PhysRevLett.94.081801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+KamLAND+Collaboration"> The KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="hep-ex/0406035v3-abstract-short" style="display: inline;"> We present results of a study of neutrino oscillation based on a 766 ton-year exposure of KamLAND to reactor anti-neutrinos. We observe 258 \nuebar\ candidate events with energies above 3.4 MeV compared to 365.2 events expected in the absence of neutrino oscillation. Accounting for 17.8 expected background events, the statistical significance for reactor \nuebar disappearance is 99.998%. The obs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0406035v3-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0406035v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0406035v3-abstract-full" style="display: none;"> We present results of a study of neutrino oscillation based on a 766 ton-year exposure of KamLAND to reactor anti-neutrinos. We observe 258 \nuebar\ candidate events with energies above 3.4 MeV compared to 365.2 events expected in the absence of neutrino oscillation. Accounting for 17.8 expected background events, the statistical significance for reactor \nuebar disappearance is 99.998%. The observed energy spectrum disagrees with the expected spectral shape in the absence of neutrino oscillation at 99.6% significance and prefers the distortion expected from \nuebar oscillation effects. A two-neutrino oscillation analysis of the KamLAND data gives \DeltaMSq = 7.9$^{+0.6}_{-0.5}\times10^{-5}$ eV$^2$. A global analysis of data from KamLAND and solar neutrino experiments yields \DeltaMSq = 7.9$^{+0.6}_{-0.5}\times10^{-5}$ eV$^2$ and \ThetaParam = 0.40$^{+0.10}_{-0.07}$, the most precise determination to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0406035v3-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0406035v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 June, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">5 pages, 4 figures; submitted to Phys.Rev.Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.94:081801,2005 </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/0310047">arXiv:hep-ex/0310047</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0310047">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0310047">ps</a>, <a href="https://arxiv.org/format/hep-ex/0310047">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.92.071301">10.1103/PhysRevLett.92.071301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A High Sensitivity Search for $\bar谓_{e}$'s from the Sun and Other Sources 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> </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/0310047v3-abstract-short" style="display: inline;"> Data corresponding to a KamLAND detector exposure of 0.28 kton-year has been used to search for $\bar谓_e$'s in the energy range 8.3 MeV $<$ E$_{\bar谓_e}$ $<$ 14.8 MeV. No candidates were found for an expected background of $1.1{\pm}0.4$ events. This result can be used to obtain a limit on $\bar谓_{e}$ fluxes of any origin. Assuming that all $\bar谓_e$ flux has its origin in the Sun and has the cha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0310047v3-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0310047v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0310047v3-abstract-full" style="display: none;"> Data corresponding to a KamLAND detector exposure of 0.28 kton-year has been used to search for $\bar谓_e$'s in the energy range 8.3 MeV $<$ E$_{\bar谓_e}$ $<$ 14.8 MeV. No candidates were found for an expected background of $1.1{\pm}0.4$ events. This result can be used to obtain a limit on $\bar谓_{e}$ fluxes of any origin. Assuming that all $\bar谓_e$ flux has its origin in the Sun and has the characteristic $^8$B solar $谓_e$ energy spectrum, we obtain an upper limit of 3.7 \times 10$^2$ cm$^{-2}$ s$^{-1}$ (90% C.L.) on the $\bar谓_e$ flux. We interpret this limit, corresponding to $2.8{\times}10^{-4}$ of the Standard Solar Model $^8$B $谓_e$ flux, in the framework of spin--flavor precession and neutrino decay models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0310047v3-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0310047v3-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, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 October, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures. New version has changes in text for sake of clarity per PRL referee Comments</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.92:071301,2004 </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/0212021">arXiv:hep-ex/0212021</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0212021">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0212021">ps</a>, <a href="https://arxiv.org/format/hep-ex/0212021">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/PhysRevLett.90.021802">10.1103/PhysRevLett.90.021802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Results from KamLAND: Evidence for Reactor Anti-Neutrino Disappearance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="hep-ex/0212021v1-abstract-short" style="display: inline;"> KamLAND has been used to measure the flux of $\bar谓_e$'s from distant nuclear reactors. In an exposure of 162 ton$\cdot$yr (145.1 days) the ratio of the number of observed inverse $尾$-decay events to the expected number of events without disappearance is $0.611\pm 0.085 {\rm (stat)} \pm 0.041 {\rm (syst)} $ for $\bar谓_e$ energies $>$ 3.4 MeV. The deficit of events is inconsistent with the expect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0212021v1-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0212021v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0212021v1-abstract-full" style="display: none;"> KamLAND has been used to measure the flux of $\bar谓_e$'s from distant nuclear reactors. In an exposure of 162 ton$\cdot$yr (145.1 days) the ratio of the number of observed inverse $尾$-decay events to the expected number of events without disappearance is $0.611\pm 0.085 {\rm (stat)} \pm 0.041 {\rm (syst)} $ for $\bar谓_e$ energies $>$ 3.4 MeV. The deficit of events is inconsistent with the expected rate for standard $\bar谓_e$ propagation at the 99.95% confidence level. In the context of two-flavor neutrino oscillations with CPT invariance, these results exclude all oscillation solutions but the `Large Mixing Angle' solution to the solar neutrino problem using reactor $\bar谓_e$ sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0212021v1-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0212021v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 December, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2002. </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, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.90:021802,2003 </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 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 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