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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Takeda%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Takeda%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Takeda%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Takeda%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.18005">arXiv:2502.18005</a> <span> [<a href="https://arxiv.org/pdf/2502.18005">pdf</a>, <a href="https://arxiv.org/format/2502.18005">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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"> WIMP Dark Matter Search using a 3.1 tonne $\times$ year Exposure of the XENONnT Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Armbruster%2C+S+R">S. R. Armbruster</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Ch%C3%A1vez%2C+A+P+C">A. P. Cimental Ch谩vez</a>, <a href="/search/physics?searchtype=author&query=Colijn%2C+A+P">A. P. Colijn</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J">J. Conrad</a> , et al. (153 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.18005v1-abstract-short" style="display: inline;"> We report on a search for weakly interacting massive particle (WIMP) dark matter (DM) via elastic DM-xenon-nucleus interactions in the XENONnT experiment. We combine datasets from the first and second science campaigns resulting in a total exposure of $3.1\;\text{tonne}\times\text{year}$. In a blind analysis of nuclear recoil events with energies above $3.8\,\mathrm{keV_{NR}}$, we find no signific… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.18005v1-abstract-full').style.display = 'inline'; document.getElementById('2502.18005v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.18005v1-abstract-full" style="display: none;"> We report on a search for weakly interacting massive particle (WIMP) dark matter (DM) via elastic DM-xenon-nucleus interactions in the XENONnT experiment. We combine datasets from the first and second science campaigns resulting in a total exposure of $3.1\;\text{tonne}\times\text{year}$. In a blind analysis of nuclear recoil events with energies above $3.8\,\mathrm{keV_{NR}}$, we find no significant excess above background. We set new upper limits on the spin-independent WIMP-nucleon scattering cross-section for WIMP masses above $10\,\mathrm{GeV}/c^2$ with a minimum of $1.7\,\times\,10^{-47}\,\mathrm{cm^2}$ at $90\,\%$ confidence level for a WIMP mass of $30\,\mathrm{GeV}/c^2$. We achieve a best median sensitivity of $1.4\,\times\,10^{-47}\,\mathrm{cm^2}$ for a $41\,\mathrm{GeV}/c^2$ WIMP. Compared to the result from the first XENONnT science dataset, we improve our sensitivity by a factor of up to 1.8. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.18005v1-abstract-full').style.display = 'none'; document.getElementById('2502.18005v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </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">Limits are included in the submission file</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.17002">arXiv:2502.17002</a> <span> [<a href="https://arxiv.org/pdf/2502.17002">pdf</a>, <a href="https://arxiv.org/format/2502.17002">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Neutron multiplicity measurement in muon capture on oxygen nuclei in the Gd-loaded Super-Kamiokande detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Collaboration%2C+T+S">The Super-Kamiokande Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</a>, <a href="/search/physics?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/physics?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/physics?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/physics?searchtype=author&query=Harada%2C+M">M. Harada</a>, <a href="/search/physics?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/physics?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/physics?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/physics?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/physics?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/physics?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/physics?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/physics?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/physics?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/physics?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/physics?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a> , et al. (265 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.17002v1-abstract-short" style="display: inline;"> In recent neutrino detectors, neutrons produced in neutrino reactions play an important role. Muon capture on oxygen nuclei is one of the processes that produce neutrons in water Cherenkov detectors. We measured neutron multiplicity in the process using cosmic ray muons that stop in the gadolinium-loaded Super-Kamiokande detector. For this measurement, neutron detection efficiency is obtained with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17002v1-abstract-full').style.display = 'inline'; document.getElementById('2502.17002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.17002v1-abstract-full" style="display: none;"> In recent neutrino detectors, neutrons produced in neutrino reactions play an important role. Muon capture on oxygen nuclei is one of the processes that produce neutrons in water Cherenkov detectors. We measured neutron multiplicity in the process using cosmic ray muons that stop in the gadolinium-loaded Super-Kamiokande detector. For this measurement, neutron detection efficiency is obtained with the muon capture events followed by gamma rays to be $50.2^{+2.0}_{-2.1}\%$. By fitting the observed multiplicity considering the detection efficiency, we measure neutron multiplicity in muon capture as $P(0)=24\pm3\%$, $P(1)=70^{+3}_{-2}\%$, $P(2)=6.1\pm0.5\%$, $P(3)=0.38\pm0.09\%$. This is the first measurement of the multiplicity of neutrons associated with muon capture without neutron energy threshold. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17002v1-abstract-full').style.display = 'none'; document.getElementById('2502.17002v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.04209">arXiv:2502.04209</a> <span> [<a href="https://arxiv.org/pdf/2502.04209">pdf</a>, <a href="https://arxiv.org/format/2502.04209">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Radon Removal in XENONnT down to the Solar Neutrino Level </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Ch%C3%A1vez%2C+A+P+C">A. P. Cimental Ch谩vez</a>, <a href="/search/physics?searchtype=author&query=Colijn%2C+A+P">A. P. Colijn</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J">J. Conrad</a>, <a href="/search/physics?searchtype=author&query=Cuenca-Garc%C3%ADa%2C+J+J">J. J. Cuenca-Garc铆a</a> , et al. (147 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.04209v1-abstract-short" style="display: inline;"> The XENONnT experiment has achieved an unprecedented reduction of the $^\text{222}$Rn activity concentration within its liquid xenon dual-phase time projection chamber to a level of (0.90$\,\pm\,$0.01$\,$stat.$\,\pm\,$0.07 sys.)$\,渭$Bq/kg, equivalent to about 1200 $^\text{222}$Rn atoms per cubic meter of liquid xenon. This represents a 15-fold improvement over the $^\text{222}$Rn levels encountere… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.04209v1-abstract-full').style.display = 'inline'; document.getElementById('2502.04209v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.04209v1-abstract-full" style="display: none;"> The XENONnT experiment has achieved an unprecedented reduction of the $^\text{222}$Rn activity concentration within its liquid xenon dual-phase time projection chamber to a level of (0.90$\,\pm\,$0.01$\,$stat.$\,\pm\,$0.07 sys.)$\,渭$Bq/kg, equivalent to about 1200 $^\text{222}$Rn atoms per cubic meter of liquid xenon. This represents a 15-fold improvement over the $^\text{222}$Rn levels encountered during XENON1T's main science runs and is a factor five lower compared to other currently operational multi-tonne liquid xenon detectors engaged in dark matter searches. This breakthrough enables the pursuit of various rare event searches that lie beyond the confines of the standard model of particle physics, with world-leading sensitivity. The ultra-low $^\text{222}$Rn levels have diminished the radon-induced background rate in the detector to a point where it is for the first time lower than the solar neutrino-induced background, which is poised to become the primary irreducible background in liquid xenon-based detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.04209v1-abstract-full').style.display = 'none'; document.getElementById('2502.04209v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.10451">arXiv:2412.10451</a> <span> [<a href="https://arxiv.org/pdf/2412.10451">pdf</a>, <a href="https://arxiv.org/format/2412.10451">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Low-Energy Nuclear Recoil Calibration of XENONnT with a $^{88}$YBe Photoneutron Source </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XENON+Collaboration"> XENON Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Ant%2C+D">D. Ant</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Ch%2C+A+P+C">A. P. Cimental Ch</a>, <a href="/search/physics?searchtype=author&query=Colijn%2C+A+P">A. P. Colijn</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J">J. Conrad</a> , et al. (147 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="2412.10451v1-abstract-short" style="display: inline;"> Characterizing low-energy (O(1keV)) nuclear recoils near the detector threshold is one of the major challenges for large direct dark matter detectors. To that end, we have successfully used a Yttrium-Beryllium photoneutron source that emits 152 keV neutrons for the calibration of the light and charge yields of the XENONnT experiment for the first time. After data selection, we accumulated 474 even… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.10451v1-abstract-full').style.display = 'inline'; document.getElementById('2412.10451v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.10451v1-abstract-full" style="display: none;"> Characterizing low-energy (O(1keV)) nuclear recoils near the detector threshold is one of the major challenges for large direct dark matter detectors. To that end, we have successfully used a Yttrium-Beryllium photoneutron source that emits 152 keV neutrons for the calibration of the light and charge yields of the XENONnT experiment for the first time. After data selection, we accumulated 474 events from 183 hours of exposure with this source. The expected background was $55 \pm 12$ accidental coincidence events, estimated using a dedicated 152 hour background calibration run with a Yttrium-PVC gamma-only source and data-driven modeling. From these calibrations, we extracted the light yield and charge yield for liquid xenon at our field strength of 23 V/cm between 0.5 keV$_{\rm NR}$ and 5.0 keV$_{\rm NR}$ (nuclear recoil energy in keV). This calibration is crucial for accurately measuring the solar $^8$B neutrino coherent elastic neutrino-nucleus scattering and searching for light dark matter particles with masses below 12 GeV/c$^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.10451v1-abstract-full').style.display = 'none'; document.getElementById('2412.10451v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.05264">arXiv:2412.05264</a> <span> [<a href="https://arxiv.org/pdf/2412.05264">pdf</a>, <a href="https://arxiv.org/format/2412.05264">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> The neutron veto of the XENONnT experiment: Results with demineralized water </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XENON+Collaboration"> XENON Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Ch%C3%A1vez%2C+A+P+C">A. P. Cimental Ch谩vez</a>, <a href="/search/physics?searchtype=author&query=Colijn%2C+A+P">A. P. Colijn</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J">J. Conrad</a> , et al. (145 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="2412.05264v3-abstract-short" style="display: inline;"> Radiogenic neutrons emitted by detector materials are one of the most challenging backgrounds for the direct search of dark matter in the form of weakly interacting massive particles (WIMPs). To mitigate this background, the XENONnT experiment is equipped with a novel gadolinium-doped water Cherenkov detector, which encloses the xenon dual-phase time projection chamber (TPC). The neutron veto (NV)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05264v3-abstract-full').style.display = 'inline'; document.getElementById('2412.05264v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.05264v3-abstract-full" style="display: none;"> Radiogenic neutrons emitted by detector materials are one of the most challenging backgrounds for the direct search of dark matter in the form of weakly interacting massive particles (WIMPs). To mitigate this background, the XENONnT experiment is equipped with a novel gadolinium-doped water Cherenkov detector, which encloses the xenon dual-phase time projection chamber (TPC). The neutron veto (NV) tags neutrons via their capture on gadolinium or hydrogen, which release $纬$-rays that are subsequently detected as Cherenkov light. In this work, we present the key features and the first results of the XENONnT NV when operated with demineralized water in the initial phase of the experiment. Its efficiency for detecting neutrons is $(82\pm 1)\,\%$, the highest neutron detection efficiency achieved in a water Cherenkov detector. This enables a high efficiency of $(53\pm 3)\,\%$ for the tagging of WIMP-like neutron signals, inside a tagging time window of $250\,\mathrm{渭s}$ between TPC and NV, leading to a livetime loss of $1.6\,\%$ during the first science run of XENONnT. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05264v3-abstract-full').style.display = 'none'; document.getElementById('2412.05264v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.19016">arXiv:2410.19016</a> <span> [<a href="https://arxiv.org/pdf/2410.19016">pdf</a>, <a href="https://arxiv.org/format/2410.19016">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Neutrinoless Double Beta Decay Sensitivity of the XLZD Rare Event Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/physics?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/physics?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/physics?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a> , et al. (419 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.19016v1-abstract-short" style="display: inline;"> The XLZD collaboration is developing a two-phase xenon time projection chamber with an active mass of 60 to 80 t capable of probing the remaining WIMP-nucleon interaction parameter space down to the so-called neutrino fog. In this work we show that, based on the performance of currently operating detectors using the same technology and a realistic reduction of radioactivity in detector materials,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19016v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19016v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19016v1-abstract-full" style="display: none;"> The XLZD collaboration is developing a two-phase xenon time projection chamber with an active mass of 60 to 80 t capable of probing the remaining WIMP-nucleon interaction parameter space down to the so-called neutrino fog. In this work we show that, based on the performance of currently operating detectors using the same technology and a realistic reduction of radioactivity in detector materials, such an experiment will also be able to competitively search for neutrinoless double beta decay in $^{136}$Xe using a natural-abundance xenon target. XLZD can reach a 3$蟽$ discovery potential half-life of 5.7$\times$10$^{27}$ yr (and a 90% CL exclusion of 1.3$\times$10$^{28}$ yr) with 10 years of data taking, corresponding to a Majorana mass range of 7.3-31.3 meV (4.8-20.5 meV). XLZD will thus exclude the inverted neutrino mass ordering parameter space and will start to probe the normal ordering region for most of the nuclear matrix elements commonly considered by the community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19016v1-abstract-full').style.display = 'none'; document.getElementById('2410.19016v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 7 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/2410.17137">arXiv:2410.17137</a> <span> [<a href="https://arxiv.org/pdf/2410.17137">pdf</a>, <a href="https://arxiv.org/format/2410.17137">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 Physics - Phenomenology">hep-ph</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"> The XLZD Design Book: Towards the Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/physics?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/physics?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/physics?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a> , et al. (419 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.17137v1-abstract-short" style="display: inline;"> This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60-80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17137v1-abstract-full').style.display = 'inline'; document.getElementById('2410.17137v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.17137v1-abstract-full" style="display: none;"> This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60-80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generation experiments, LZ and XENONnT. A baseline design and opportunities for further optimization of the individual detector components are discussed. The experiment envisaged here has the capability to explore parameter space for Weakly Interacting Massive Particle (WIMP) dark matter down to the neutrino fog, with a 3$蟽$ evidence potential for the spin-independent WIMP-nucleon cross sections as low as $3\times10^{-49}\rm cm^2$ (at 40 GeV/c$^2$ WIMP mass). The observatory is also projected to have a 3$蟽$ observation potential of neutrinoless double-beta decay of $^{136}$Xe at a half-life of up to $5.7\times 10^{27}$ years. Additionally, it is sensitive to astrophysical neutrinos from the atmosphere, sun, and galactic supernovae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17137v1-abstract-full').style.display = 'none'; document.getElementById('2410.17137v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 14 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/2410.00755">arXiv:2410.00755</a> <span> [<a href="https://arxiv.org/pdf/2410.00755">pdf</a>, <a href="https://arxiv.org/format/2410.00755">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> </div> </div> <p class="title is-5 mathjax"> Model-independent searches of new physics in DARWIN with a semi-supervised deep learning pipeline </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/physics?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/physics?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/physics?searchtype=author&query=Barberio%2C+E">E. Barberio</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bell%2C+N+F">N. F. Bell</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+Y">Y. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Boehm%2C+C">C. Boehm</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/physics?searchtype=author&query=Braun%2C+R">R. Braun</a> , et al. (209 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.00755v1-abstract-short" style="display: inline;"> We present a novel deep learning pipeline to perform a model-independent, likelihood-free search for anomalous (i.e., non-background) events in the proposed next generation multi-ton scale liquid Xenon-based direct detection experiment, DARWIN. We train an anomaly detector comprising a variational autoencoder and a classifier on extensive, high-dimensional simulated detector response data and cons… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00755v1-abstract-full').style.display = 'inline'; document.getElementById('2410.00755v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.00755v1-abstract-full" style="display: none;"> We present a novel deep learning pipeline to perform a model-independent, likelihood-free search for anomalous (i.e., non-background) events in the proposed next generation multi-ton scale liquid Xenon-based direct detection experiment, DARWIN. We train an anomaly detector comprising a variational autoencoder and a classifier on extensive, high-dimensional simulated detector response data and construct a one-dimensional anomaly score optimised to reject the background only hypothesis in the presence of an excess of non-background-like events. We benchmark the procedure with a sensitivity study that determines its power to reject the background-only hypothesis in the presence of an injected WIMP dark matter signal, outperforming the classical, likelihood-based background rejection test. We show that our neural networks learn relevant energy features of the events from low-level, high-dimensional detector outputs, without the need to compress this data into lower-dimensional observables, thus reducing computational effort and information loss. For the future, our approach lays the foundation for an efficient end-to-end pipeline that eliminates the need for many of the corrections and cuts that are traditionally part of the analysis chain, with the potential of achieving higher accuracy and significant reduction of analysis time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00755v1-abstract-full').style.display = 'none'; document.getElementById('2410.00755v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 Figures, 3 Tables, 23 Pages (incl. references)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.08778">arXiv:2409.08778</a> <span> [<a href="https://arxiv.org/pdf/2409.08778">pdf</a>, <a href="https://arxiv.org/format/2409.08778">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="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> XENONnT Analysis: Signal Reconstruction, Calibration and Event Selection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XENON+Collaboration"> XENON Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Ch%C3%A1vez%2C+A+P+C">A. P. Cimental Ch谩vez</a>, <a href="/search/physics?searchtype=author&query=Colijn%2C+A+P">A. P. Colijn</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J">J. Conrad</a>, <a href="/search/physics?searchtype=author&query=Cuenca-Garc%C3%ADa%2C+J+J">J. J. Cuenca-Garc铆a</a> , et al. (143 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.08778v1-abstract-short" style="display: inline;"> The XENONnT experiment, located at the INFN Laboratori Nazionali del Gran Sasso, Italy, features a 5.9 tonne liquid xenon time projection chamber surrounded by an instrumented neutron veto, all of which is housed within a muon veto water tank. Due to extensive shielding and advanced purification to mitigate natural radioactivity, an exceptionally low background level of (15.8 $\pm$ 1.3) events/(to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.08778v1-abstract-full').style.display = 'inline'; document.getElementById('2409.08778v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.08778v1-abstract-full" style="display: none;"> The XENONnT experiment, located at the INFN Laboratori Nazionali del Gran Sasso, Italy, features a 5.9 tonne liquid xenon time projection chamber surrounded by an instrumented neutron veto, all of which is housed within a muon veto water tank. Due to extensive shielding and advanced purification to mitigate natural radioactivity, an exceptionally low background level of (15.8 $\pm$ 1.3) events/(tonne$\cdot$year$\cdot$keV) in the (1, 30) keV region is reached in the inner part of the TPC. XENONnT is thus sensitive to a wide range of rare phenomena related to Dark Matter and Neutrino interactions, both within and beyond the Standard Model of particle physics, with a focus on the direct detection of Dark Matter in the form of weakly interacting massive particles (WIMPs). From May 2021 to December 2021, XENONnT accumulated data in rare-event search mode with a total exposure of one tonne $\cdot$ year. This paper provides a detailed description of the signal reconstruction methods, event selection procedure, and detector response calibration, as well as an overview of the detector performance in this time frame. This work establishes the foundational framework for the `blind analysis' methodology we are using when reporting XENONnT physics results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.08778v1-abstract-full').style.display = 'none'; document.getElementById('2409.08778v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">27 pages, 23 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/2408.02877">arXiv:2408.02877</a> <span> [<a href="https://arxiv.org/pdf/2408.02877">pdf</a>, <a href="https://arxiv.org/format/2408.02877">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-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="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.133.191002">10.1103/PhysRevLett.133.191002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Indication of Solar $^8$B Neutrinos via Coherent Elastic Neutrino-Nucleus Scattering with XENONnT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Ch%C3%A1vez%2C+A+P+C">A. P. Cimental Ch谩vez</a>, <a href="/search/physics?searchtype=author&query=Colijn%2C+A+P">A. P. Colijn</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J">J. Conrad</a>, <a href="/search/physics?searchtype=author&query=Cuenca-Garc%C3%ADa%2C+J+J">J. J. Cuenca-Garc铆a</a> , et al. (142 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="2408.02877v2-abstract-short" style="display: inline;"> We present the first measurement of nuclear recoils from solar $^8$B neutrinos via coherent elastic neutrino-nucleus scattering with the XENONnT dark matter experiment. The central detector of XENONnT is a low-background, two-phase time projection chamber with a 5.9 t sensitive liquid xenon target. A blind analysis with an exposure of 3.51 t$\times$yr resulted in 37 observed events above 0.5 keV,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.02877v2-abstract-full').style.display = 'inline'; document.getElementById('2408.02877v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.02877v2-abstract-full" style="display: none;"> We present the first measurement of nuclear recoils from solar $^8$B neutrinos via coherent elastic neutrino-nucleus scattering with the XENONnT dark matter experiment. The central detector of XENONnT is a low-background, two-phase time projection chamber with a 5.9 t sensitive liquid xenon target. A blind analysis with an exposure of 3.51 t$\times$yr resulted in 37 observed events above 0.5 keV, with ($26.4^{+1.4}_{-1.3}$) events expected from backgrounds. The background-only hypothesis is rejected with a statistical significance of 2.73 $蟽$. The measured $^8$B solar neutrino flux of $(4.7_{-2.3}^{+3.6})\times 10^6 \mathrm{cm}^{-2}\mathrm{s}^{-1}$ is consistent with results from the Sudbury Neutrino Observatory. The measured neutrino flux-weighted CE$谓$NS cross section on Xe of $(1.1^{+0.8}_{-0.5})\times10^{-39} \mathrm{cm}^2$ is consistent with the Standard Model prediction. This is the first direct measurement of nuclear recoils from solar neutrinos with a dark matter detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.02877v2-abstract-full').style.display = 'none'; document.getElementById('2408.02877v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 133, 191002 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.18507">arXiv:2407.18507</a> <span> [<a href="https://arxiv.org/pdf/2407.18507">pdf</a>, <a href="https://arxiv.org/ps/2407.18507">ps</a>, <a href="https://arxiv.org/format/2407.18507">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Atmospheric and Oceanic Physics">physics.ao-ph</span> </div> </div> <p class="title is-5 mathjax"> Feasibility study of upper atmosphere density measurement on the ISS by observations of the CXB transmitted through the Earth rim </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Kishimoto%2C+T">Takumi Kishimoto</a>, <a href="/search/physics?searchtype=author&query=Nobukawa%2C+K+K">Kumiko K. Nobukawa</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Ayaki Takeda</a>, <a href="/search/physics?searchtype=author&query=Tsuru%2C+T+G">Takeshi G. Tsuru</a>, <a href="/search/physics?searchtype=author&query=Katsuda%2C+S">Satoru Katsuda</a>, <a href="/search/physics?searchtype=author&query=Kazuhiro%2C+N">Nakazawa Kazuhiro</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+K">Koji Mori</a>, <a href="/search/physics?searchtype=author&query=Nobukawa%2C+M">Masayoshi Nobukawa</a>, <a href="/search/physics?searchtype=author&query=Uchida%2C+H">Hiroyuki Uchida</a>, <a href="/search/physics?searchtype=author&query=Kawabe%2C+Y">Yoshihisa Kawabe</a>, <a href="/search/physics?searchtype=author&query=Kuwano%2C+S">Satoru Kuwano</a>, <a href="/search/physics?searchtype=author&query=Kurogi%2C+E">Eisuke Kurogi</a>, <a href="/search/physics?searchtype=author&query=Ito%2C+Y">Yamato Ito</a>, <a href="/search/physics?searchtype=author&query=Aoki%2C+Y">Yuma Aoki</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="2407.18507v1-abstract-short" style="display: inline;"> Measurements of the upper atmosphere at ~100 km are important to investigate climate change, space weather forecasting, and the interaction between the Sun and the Earth. Atmospheric occultations of cosmic X-ray sources are an effective technique to measure the neutral density in the upper atmosphere. We are developing the instrument SUIM dedicated to continuous observations of atmospheric occulta… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.18507v1-abstract-full').style.display = 'inline'; document.getElementById('2407.18507v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.18507v1-abstract-full" style="display: none;"> Measurements of the upper atmosphere at ~100 km are important to investigate climate change, space weather forecasting, and the interaction between the Sun and the Earth. Atmospheric occultations of cosmic X-ray sources are an effective technique to measure the neutral density in the upper atmosphere. We are developing the instrument SUIM dedicated to continuous observations of atmospheric occultations. SUIM will be mounted on a platform on the exterior of the International Space Station for six months and pointed at the Earth's rim to observe atmospheric absorption of the cosmic X-ray background (CXB). In this paper, we conducted a feasibility study of SUIM by estimating the CXB statistics and the fraction of the non-X-ray background (NXB) in the observed data. The estimated CXB statistics are enough to evaluate the atmospheric absorption of CXB for every 15 km of altitude. On the other hand, the NXB will be dominant in the X-ray spectra of SUIM. Assuming that the NXB per detection area of SUIM is comparable to that of the soft X-ray Imager onboard Hitomi, the NXB level will be much higher than the CXB one and account for ~80% of the total SUIM spectra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.18507v1-abstract-full').style.display = 'none'; document.getElementById('2407.18507v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">5 pages, 5 figures, Proceedings of SPIE Astronomical Telescopes and Instrumentation 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.16922">arXiv:2407.16922</a> <span> [<a href="https://arxiv.org/pdf/2407.16922">pdf</a>, <a href="https://arxiv.org/ps/2407.16922">ps</a>, <a href="https://arxiv.org/format/2407.16922">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Atmospheric and Oceanic Physics">physics.ao-ph</span> </div> </div> <p class="title is-5 mathjax"> SUIM project: measuring the upper atmosphere from the ISS by observations of the CXB transmitted through the Earth rim </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Nobukawa%2C+K+K">Kumiko K. Nobukawa</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Ayaki Takeda</a>, <a href="/search/physics?searchtype=author&query=Katsuda%2C+S">Satoru Katsuda</a>, <a href="/search/physics?searchtype=author&query=Tsuru%2C+T+G">Takeshi G. Tsuru</a>, <a href="/search/physics?searchtype=author&query=Nakazawa%2C+K">Kazuhiro Nakazawa</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+K">Koji Mori</a>, <a href="/search/physics?searchtype=author&query=Uchida%2C+H">Hiroyuki Uchida</a>, <a href="/search/physics?searchtype=author&query=Nobukawa%2C+M">Masayoshi Nobukawa</a>, <a href="/search/physics?searchtype=author&query=Kurogi%2C+E">Eisuke Kurogi</a>, <a href="/search/physics?searchtype=author&query=Kishimoto%2C+T">Takumi Kishimoto</a>, <a href="/search/physics?searchtype=author&query=Matsui%2C+R">Reo Matsui</a>, <a href="/search/physics?searchtype=author&query=Aoki%2C+Y">Yuma Aoki</a>, <a href="/search/physics?searchtype=author&query=Ito%2C+Y">Yamato Ito</a>, <a href="/search/physics?searchtype=author&query=Kuwano%2C+S">Satoru Kuwano</a>, <a href="/search/physics?searchtype=author&query=Tanaka%2C+T">Tomitaka Tanaka</a>, <a href="/search/physics?searchtype=author&query=Uenomachi%2C+M">Mizuki Uenomachi</a>, <a href="/search/physics?searchtype=author&query=Matsuda%2C+M">Masamune Matsuda</a>, <a href="/search/physics?searchtype=author&query=Yamawaki%2C+T">Takaya Yamawaki</a>, <a href="/search/physics?searchtype=author&query=Kohmura%2C+T">Takayoshi Kohmura</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="2407.16922v1-abstract-short" style="display: inline;"> The upper atmosphere at the altitude of 60-110 km, the mesosphere and lower thermosphere (MLT), has the least observational data of all atmospheres due to the difficulties of in-situ observations. Previous studies demonstrated that atmospheric occultation of cosmic X-ray sources is an effective technique to investigate the MLT. Aiming to measure the atmospheric density of the MLT continuously, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16922v1-abstract-full').style.display = 'inline'; document.getElementById('2407.16922v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.16922v1-abstract-full" style="display: none;"> The upper atmosphere at the altitude of 60-110 km, the mesosphere and lower thermosphere (MLT), has the least observational data of all atmospheres due to the difficulties of in-situ observations. Previous studies demonstrated that atmospheric occultation of cosmic X-ray sources is an effective technique to investigate the MLT. Aiming to measure the atmospheric density of the MLT continuously, we are developing an X-ray camera, "Soipix for observing Upper atmosphere as Iss experiment Mission (SUIM)", dedicated to atmospheric observations. SUIM will be installed on the exposed area of the International Space Station (ISS) and face the ram direction of the ISS to point toward the Earth rim. Observing the cosmic X-ray background (CXB) transmitted through the atmosphere, we will measure the absorption column density via spectroscopy and thus obtain the density of the upper atmosphere. The X-ray camera is composed of a slit collimator and two X-ray SOI-CMOS pixel sensors (SOIPIX), and will stand on its own and make observations, controlled by a CPU-embedded FPGA "Zynq". We plan to install the SUIM payload on the ISS in 2025 during the solar maximum. In this paper, we report the overview and the development status of this project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16922v1-abstract-full').style.display = 'none'; document.getElementById('2407.16922v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">5 pages, 2 figures, Proceedings of SPIE Astronomical Telescopes and Instrumentation 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.13638">arXiv:2406.13638</a> <span> [<a href="https://arxiv.org/pdf/2406.13638">pdf</a>, <a href="https://arxiv.org/format/2406.13638">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <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"> XENONnT WIMP Search: Signal & Background Modeling and Statistical Inference </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XENON+Collaboration"> XENON Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Ch%C3%A1vez%2C+A+P+C">A. P. Cimental Ch谩vez</a>, <a href="/search/physics?searchtype=author&query=Colijn%2C+A+P">A. P. Colijn</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J">J. Conrad</a>, <a href="/search/physics?searchtype=author&query=Cuenca-Garc%C3%ADa%2C+J+J">J. J. Cuenca-Garc铆a</a>, <a href="/search/physics?searchtype=author&query=D%27Andrea%2C+V">V. D'Andrea</a> , et al. (139 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.13638v1-abstract-short" style="display: inline;"> The XENONnT experiment searches for weakly-interacting massive particle (WIMP) dark matter scattering off a xenon nucleus. In particular, XENONnT uses a dual-phase time projection chamber with a 5.9-tonne liquid xenon target, detecting both scintillation and ionization signals to reconstruct the energy, position, and type of recoil. A blind search for nuclear recoil WIMPs with an exposure of 1.1 t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.13638v1-abstract-full').style.display = 'inline'; document.getElementById('2406.13638v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.13638v1-abstract-full" style="display: none;"> The XENONnT experiment searches for weakly-interacting massive particle (WIMP) dark matter scattering off a xenon nucleus. In particular, XENONnT uses a dual-phase time projection chamber with a 5.9-tonne liquid xenon target, detecting both scintillation and ionization signals to reconstruct the energy, position, and type of recoil. A blind search for nuclear recoil WIMPs with an exposure of 1.1 tonne-years yielded no signal excess over background expectations, from which competitive exclusion limits were derived on WIMP-nucleon elastic scatter cross sections, for WIMP masses ranging from 6 GeV/$c^2$ up to the TeV/$c^2$ scale. This work details the modeling and statistical methods employed in this search. By means of calibration data, we model the detector response, which is then used to derive background and signal models. The construction and validation of these models is discussed, alongside additional purely data-driven backgrounds. We also describe the statistical inference framework, including the definition of the likelihood function and the construction of confidence intervals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.13638v1-abstract-full').style.display = 'none'; document.getElementById('2406.13638v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.09920">arXiv:2404.09920</a> <span> [<a href="https://arxiv.org/pdf/2404.09920">pdf</a>, <a href="https://arxiv.org/format/2404.09920">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad5fee">10.3847/1538-4357/ad5fee <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combined Pre-Supernova Alert System with Kamland and Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=KamLAND"> KamLAND</a>, <a href="/search/physics?searchtype=author&query=Collaborations%2C+S">Super-Kamiokande Collaborations</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+S">Seisho Abe</a>, <a href="/search/physics?searchtype=author&query=Eizuka%2C+M">Minori Eizuka</a>, <a href="/search/physics?searchtype=author&query=Futagi%2C+S">Sawako Futagi</a>, <a href="/search/physics?searchtype=author&query=Gando%2C+A">Azusa Gando</a>, <a href="/search/physics?searchtype=author&query=Gando%2C+Y">Yoshihito Gando</a>, <a href="/search/physics?searchtype=author&query=Goto%2C+S">Shun Goto</a>, <a href="/search/physics?searchtype=author&query=Hachiya%2C+T">Takahiko Hachiya</a>, <a href="/search/physics?searchtype=author&query=Hata%2C+K">Kazumi Hata</a>, <a href="/search/physics?searchtype=author&query=Ichimura%2C+K">Koichi Ichimura</a>, <a href="/search/physics?searchtype=author&query=Ieki%2C+S">Sei Ieki</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+H">Haruo Ikeda</a>, <a href="/search/physics?searchtype=author&query=Inoue%2C+K">Kunio Inoue</a>, <a href="/search/physics?searchtype=author&query=Ishidoshiro%2C+K">Koji Ishidoshiro</a>, <a href="/search/physics?searchtype=author&query=Kamei%2C+Y">Yuto Kamei</a>, <a href="/search/physics?searchtype=author&query=Kawada%2C+N">Nanami Kawada</a>, <a href="/search/physics?searchtype=author&query=Kishimoto%2C+Y">Yasuhiro Kishimoto</a>, <a href="/search/physics?searchtype=author&query=Koga%2C+M">Masayuki Koga</a>, <a href="/search/physics?searchtype=author&query=Kurasawa%2C+M">Maho Kurasawa</a>, <a href="/search/physics?searchtype=author&query=Mitsui%2C+T">Tadao Mitsui</a>, <a href="/search/physics?searchtype=author&query=Miyake%2C+H">Haruhiko Miyake</a>, <a href="/search/physics?searchtype=author&query=Morita%2C+D">Daisuke Morita</a>, <a href="/search/physics?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/2403.14878">arXiv:2403.14878</a> <span> [<a href="https://arxiv.org/pdf/2403.14878">pdf</a>, <a href="https://arxiv.org/format/2403.14878">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.110.012011">10.1103/PhysRevD.110.012011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Offline tagging of radon-induced backgrounds in XENON1T and applicability to other liquid xenon detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brookes%2C+E+J">E. J. Brookes</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Bui%2C+T+K">T. K. Bui</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Chavez%2C+A+P+C">A. P. Cimental Chavez</a>, <a href="/search/physics?searchtype=author&query=Colijn%2C+A+P">A. P. Colijn</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J">J. Conrad</a> , et al. (142 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.14878v2-abstract-short" style="display: inline;"> This paper details the first application of a software tagging algorithm to reduce radon-induced backgrounds in liquid noble element time projection chambers, such as XENON1T and XENONnT. The convection velocity field in XENON1T was mapped out using $^{222}\text{Rn}$ and $^{218}\text{Po}$ events, and the root-mean-square convection speed was measured to be $0.30 \pm 0.01$ cm/s. Given this velocity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14878v2-abstract-full').style.display = 'inline'; document.getElementById('2403.14878v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.14878v2-abstract-full" style="display: none;"> This paper details the first application of a software tagging algorithm to reduce radon-induced backgrounds in liquid noble element time projection chambers, such as XENON1T and XENONnT. The convection velocity field in XENON1T was mapped out using $^{222}\text{Rn}$ and $^{218}\text{Po}$ events, and the root-mean-square convection speed was measured to be $0.30 \pm 0.01$ cm/s. Given this velocity field, $^{214}\text{Pb}$ background events can be tagged when they are followed by $^{214}\text{Bi}$ and $^{214}\text{Po}$ decays, or preceded by $^{218}\text{Po}$ decays. This was achieved by evolving a point cloud in the direction of a measured convection velocity field, and searching for $^{214}\text{Bi}$ and $^{214}\text{Po}$ decays or $^{218}\text{Po}$ decays within a volume defined by the point cloud. In XENON1T, this tagging system achieved a $^{214}\text{Pb}$ background reduction of $6.2^{+0.4}_{-0.9}\%$ with an exposure loss of $1.8\pm 0.2 \%$, despite the timescales of convection being smaller than the relevant decay times. We show that the performance can be improved in XENONnT, and that the performance of such a software-tagging approach can be expected to be further improved in a diffusion-limited scenario. Finally, a similar method might be useful to tag the cosmogenic $^{137}\text{Xe}$ background, which is relevant to the search for neutrinoless double-beta decay. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14878v2-abstract-full').style.display = 'none'; document.getElementById('2403.14878v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 19 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D 110 (2024) 012011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.07796">arXiv:2403.07796</a> <span> [<a href="https://arxiv.org/pdf/2403.07796">pdf</a>, <a href="https://arxiv.org/format/2403.07796">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 Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2024.169480">10.1016/j.nima.2024.169480 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Second gadolinium loading to Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/physics?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/physics?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/physics?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/physics?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/physics?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/physics?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/physics?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/physics?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/physics?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/physics?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/physics?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/physics?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Shiba%2C+H">H. Shiba</a>, <a href="/search/physics?searchtype=author&query=Shimizu%2C+K">K. Shimizu</a>, <a href="/search/physics?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a> , et al. (225 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.07796v3-abstract-short" style="display: inline;"> The first loading of gadolinium (Gd) into Super-Kamiokande in 2020 was successful, and the neutron capture efficiency on Gd reached 50\%. To further increase the Gd neutron capture efficiency to 75\%, 26.1 tons of $\rm Gd_2(\rm SO_4)_3\cdot \rm 8H_2O$ was additionally loaded into Super-Kamiokande (SK) from May 31 to July 4, 2022. As the amount of loaded $\rm Gd_2(\rm SO_4)_3\cdot \rm 8H_2O$ was do… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07796v3-abstract-full').style.display = 'inline'; document.getElementById('2403.07796v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.07796v3-abstract-full" style="display: none;"> The first loading of gadolinium (Gd) into Super-Kamiokande in 2020 was successful, and the neutron capture efficiency on Gd reached 50\%. To further increase the Gd neutron capture efficiency to 75\%, 26.1 tons of $\rm Gd_2(\rm SO_4)_3\cdot \rm 8H_2O$ was additionally loaded into Super-Kamiokande (SK) from May 31 to July 4, 2022. As the amount of loaded $\rm Gd_2(\rm SO_4)_3\cdot \rm 8H_2O$ was doubled compared to the first loading, the capacity of the powder dissolving system was doubled. We also developed new batches of gadolinium sulfate with even further reduced radioactive impurities. In addition, a more efficient screening method was devised and implemented to evaluate these new batches of $\rm Gd_2(\rm SO_4)_3\cdot \rm 8H_2O$. Following the second loading, the Gd concentration in SK was measured to be $333.5\pm2.5$ ppm via an Atomic Absorption Spectrometer (AAS). From the mean neutron capture time constant of neutrons from an Am/Be calibration source, the Gd concentration was independently measured to be 332.7 $\pm$ 6.8(sys.) $\pm$ 1.1(stat.) ppm, consistent with the AAS result. Furthermore, during the loading the Gd concentration was monitored continually using the capture time constant of each spallation neutron produced by cosmic-ray muons,and the final neutron capture efficiency was shown to become 1.5 times higher than that of the first loaded phase, as expected. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07796v3-abstract-full').style.display = 'none'; document.getElementById('2403.07796v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">34 pages, 13 figures, submitted to Nuclear Inst. and Methods in Physics Research, A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Inst. and Methods in Physics Research, A 1065 (2024) 169480 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.10446">arXiv:2402.10446</a> <span> [<a href="https://arxiv.org/pdf/2402.10446">pdf</a>, <a href="https://arxiv.org/format/2402.10446">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> The XENONnT Dark Matter Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XENON+Collaboration"> XENON Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Balata%2C+M">M. Balata</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brookes%2C+E+J">E. J. Brookes</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Bui%2C+T+K">T. K. Bui</a> , et al. (170 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="2402.10446v1-abstract-short" style="display: inline;"> The multi-staged XENON program at INFN Laboratori Nazionali del Gran Sasso aims to detect dark matter with two-phase liquid xenon time projection chambers of increasing size and sensitivity. The XENONnT experiment is the latest detector in the program, planned to be an upgrade of its predecessor XENON1T. It features an active target of 5.9 tonnes of cryogenic liquid xenon (8.5 tonnes total mass in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10446v1-abstract-full').style.display = 'inline'; document.getElementById('2402.10446v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.10446v1-abstract-full" style="display: none;"> The multi-staged XENON program at INFN Laboratori Nazionali del Gran Sasso aims to detect dark matter with two-phase liquid xenon time projection chambers of increasing size and sensitivity. The XENONnT experiment is the latest detector in the program, planned to be an upgrade of its predecessor XENON1T. It features an active target of 5.9 tonnes of cryogenic liquid xenon (8.5 tonnes total mass in cryostat). The experiment is expected to extend the sensitivity to WIMP dark matter by more than an order of magnitude compared to XENON1T, thanks to the larger active mass and the significantly reduced background, improved by novel systems such as a radon removal plant and a neutron veto. This article describes the XENONnT experiment and its sub-systems in detail and reports on the detector performance during the first science run. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10446v1-abstract-full').style.display = 'none'; document.getElementById('2402.10446v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">32 pages, 19 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/2309.11996">arXiv:2309.11996</a> <span> [<a href="https://arxiv.org/pdf/2309.11996">pdf</a>, <a href="https://arxiv.org/format/2309.11996">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/10.1140/epjc/s10052-023-12296-y">10.1140/epjc/s10052-023-12296-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design and performance of the field cage for the XENONnT experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brookes%2C+E+J">E. J. Brookes</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Bui%2C+T+K">T. K. Bui</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Cichon%2C+D">D. Cichon</a> , et al. (139 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.11996v1-abstract-short" style="display: inline;"> The precision in reconstructing events detected in a dual-phase time projection chamber depends on an homogeneous and well understood electric field within the liquid target. In the XENONnT TPC the field homogeneity is achieved through a double-array field cage, consisting of two nested arrays of field shaping rings connected by an easily accessible resistor chain. Rather than being connected to t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.11996v1-abstract-full').style.display = 'inline'; document.getElementById('2309.11996v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.11996v1-abstract-full" style="display: none;"> The precision in reconstructing events detected in a dual-phase time projection chamber depends on an homogeneous and well understood electric field within the liquid target. In the XENONnT TPC the field homogeneity is achieved through a double-array field cage, consisting of two nested arrays of field shaping rings connected by an easily accessible resistor chain. Rather than being connected to the gate electrode, the topmost field shaping ring is independently biased, adding a degree of freedom to tune the electric field during operation. Two-dimensional finite element simulations were used to optimize the field cage, as well as its operation. Simulation results were compared to ${}^{83m}\mathrm{Kr}$ calibration data. This comparison indicates an accumulation of charge on the panels of the TPC which is constant over time, as no evolution of the reconstructed position distribution of events is observed. The simulated electric field was then used to correct the charge signal for the field dependence of the charge yield. This correction resolves the inconsistent measurement of the drift electron lifetime when using different calibrations sources and different field cage tuning voltages. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.11996v1-abstract-full').style.display = 'none'; document.getElementById('2309.11996v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 84, 138 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.11871">arXiv:2306.11871</a> <span> [<a href="https://arxiv.org/pdf/2306.11871">pdf</a>, <a href="https://arxiv.org/format/2306.11871">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Search for events in XENON1T associated with Gravitational Waves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XENON+Collaboration"> XENON Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Anto艅 Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brookes%2C+E+J">E. J. Brookes</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Bui%2C+T+K">T. K. Bui</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a> , et al. (138 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="2306.11871v2-abstract-short" style="display: inline;"> We perform a blind search for particle signals in the XENON1T dark matter detector that occur close in time to gravitational wave signals in the LIGO and Virgo observatories. No particle signal is observed in the nuclear recoil, electronic recoil, CE$谓$NS, and S2-only channels within $\pm$ 500 seconds of observations of the gravitational wave signals GW170104, GW170729, GW170817, GW170818, and GW1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11871v2-abstract-full').style.display = 'inline'; document.getElementById('2306.11871v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.11871v2-abstract-full" style="display: none;"> We perform a blind search for particle signals in the XENON1T dark matter detector that occur close in time to gravitational wave signals in the LIGO and Virgo observatories. No particle signal is observed in the nuclear recoil, electronic recoil, CE$谓$NS, and S2-only channels within $\pm$ 500 seconds of observations of the gravitational wave signals GW170104, GW170729, GW170817, GW170818, and GW170823. We use this null result to constrain mono-energetic neutrinos and Beyond Standard Model particles emitted in the closest coalescence GW170817, a binary neutron star merger. We set new upper limits on the fluence (time-integrated flux) of coincident neutrinos down to 17 keV at 90% confidence level. Furthermore, we constrain the product of coincident fluence and cross section of Beyond Standard Model particles to be less than $10^{-29}$ cm$^2$/cm$^2$ in the [5.5-210] keV energy range at 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11871v2-abstract-full').style.display = 'none'; document.getElementById('2306.11871v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.08716">arXiv:2306.08716</a> <span> [<a href="https://arxiv.org/pdf/2306.08716">pdf</a>, <a href="https://arxiv.org/format/2306.08716">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1109/TNS.2023.3287130">10.1109/TNS.2023.3287130 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radiation-Induced Degradation Mechanism of X-ray SOI Pixel Sensors with Pinned Depleted Diode Structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Hagino%2C+K">Kouichi Hagino</a>, <a href="/search/physics?searchtype=author&query=Kitajima%2C+M">Masatoshi Kitajima</a>, <a href="/search/physics?searchtype=author&query=Kohmura%2C+T">Takayoshi Kohmura</a>, <a href="/search/physics?searchtype=author&query=Kurachi%2C+I">Ikuo Kurachi</a>, <a href="/search/physics?searchtype=author&query=Tsuru%2C+T+G">Takeshi G. Tsuru</a>, <a href="/search/physics?searchtype=author&query=Yukumoto%2C+M">Masataka Yukumoto</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Ayaki Takeda</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+K">Koji Mori</a>, <a href="/search/physics?searchtype=author&query=Nishioka%2C+Y">Yusuke Nishioka</a>, <a href="/search/physics?searchtype=author&query=Tanaka%2C+T">Takaaki Tanaka</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="2306.08716v1-abstract-short" style="display: inline;"> The X-ray Silicon-On-Insulator (SOI) pixel sensor named XRPIX has been developed for the future X-ray astronomical satellite FORCE. XRPIX is capable of a wide-band X-ray imaging spectroscopy from below 1 keV to a few tens of keV with a good timing resolution of a few tens of $渭$s. However, it had a major issue with its radiation tolerance to the total ionizing dose (TID) effect because of its thic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.08716v1-abstract-full').style.display = 'inline'; document.getElementById('2306.08716v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.08716v1-abstract-full" style="display: none;"> The X-ray Silicon-On-Insulator (SOI) pixel sensor named XRPIX has been developed for the future X-ray astronomical satellite FORCE. XRPIX is capable of a wide-band X-ray imaging spectroscopy from below 1 keV to a few tens of keV with a good timing resolution of a few tens of $渭$s. However, it had a major issue with its radiation tolerance to the total ionizing dose (TID) effect because of its thick buried oxide layer due to the SOI structure. Although new device structures introducing pinned depleted diodes dramatically improved radiation tolerance, it remained unknown how radiation effects degrade the sensor performance. Thus, this paper reports the results of a study of the degradation mechanism of XRPIX due to radiation using device simulations. In particular, mechanisms of increases in dark current and readout noise are investigated by simulation, taking into account the positive charge accumulation in the oxide layer and the increase in the surface recombination velocity at the interface between the sensor layer and the oxide layer. As a result, it is found that the depletion of the buried p-well at the interface increases the dark current, and that the increase in the sense-node capacitance increases the readout noise. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.08716v1-abstract-full').style.display = 'none'; document.getElementById('2306.08716v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 10 figures, accepted for publication in IEEE-TNS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.05135">arXiv:2305.05135</a> <span> [<a href="https://arxiv.org/pdf/2305.05135">pdf</a>, <a href="https://arxiv.org/format/2305.05135">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acdc9e">10.3847/2041-8213/acdc9e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for astrophysical electron antineutrinos in Super-Kamiokande with 0.01wt% gadolinium-loaded water </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Harada%2C+M">M. Harada</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/physics?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/physics?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/physics?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/physics?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/physics?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/physics?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/physics?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/physics?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/physics?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/physics?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/physics?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/physics?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/physics?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Shiba%2C+H">H. Shiba</a> , et al. (216 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.05135v2-abstract-short" style="display: inline;"> We report the first search result for the flux of astrophysical electron antineutrinos for energies O(10) MeV in the gadolinium-loaded Super-Kamiokande (SK) detector. In June 2020, gadolinium was introduced to the ultra-pure water of the SK detector in order to detect neutrons more efficiently. In this new experimental phase, SK-Gd, we can search for electron antineutrinos via inverse beta decay w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05135v2-abstract-full').style.display = 'inline'; document.getElementById('2305.05135v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.05135v2-abstract-full" style="display: none;"> We report the first search result for the flux of astrophysical electron antineutrinos for energies O(10) MeV in the gadolinium-loaded Super-Kamiokande (SK) detector. In June 2020, gadolinium was introduced to the ultra-pure water of the SK detector in order to detect neutrons more efficiently. In this new experimental phase, SK-Gd, we can search for electron antineutrinos via inverse beta decay with efficient background rejection and higher signal efficiency thanks to the high efficiency of the neutron tagging technique. In this paper, we report the result for the initial stage of SK-Gd with a $22.5\times552$ $\rm kton\cdot day$ exposure at 0.01% Gd mass concentration. No significant excess over the expected background in the observed events is found for the neutrino energies below 31.3 MeV. Thus, the flux upper limits are placed at the 90% confidence level. The limits and sensitivities are already comparable with the previous SK result with pure-water ($22.5 \times 2970 \rm kton\cdot day$) owing to the enhanced neutron tagging. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05135v2-abstract-full').style.display = 'none'; document.getElementById('2305.05135v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.10931">arXiv:2304.10931</a> <span> [<a href="https://arxiv.org/pdf/2304.10931">pdf</a>, <a href="https://arxiv.org/format/2304.10931">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.130.261002">10.1103/PhysRevLett.130.261002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Heavy Dark Matter near the Planck Mass with XENON1T </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brookes%2C+E+J">E. J. Brookes</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Bui%2C+T+K">T. K. Bui</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Cichon%2C+D">D. Cichon</a> , et al. (142 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="2304.10931v1-abstract-short" style="display: inline;"> Multiple viable theoretical models predict heavy dark matter particles with a mass close to the Planck mass, a range relatively unexplored by current experimental measurements. We use 219.4 days of data collected with the XENON1T experiment to conduct a blind search for signals from Multiply-Interacting Massive Particles (MIMPs). Their unique track signature allows a targeted analysis with only 0.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.10931v1-abstract-full').style.display = 'inline'; document.getElementById('2304.10931v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.10931v1-abstract-full" style="display: none;"> Multiple viable theoretical models predict heavy dark matter particles with a mass close to the Planck mass, a range relatively unexplored by current experimental measurements. We use 219.4 days of data collected with the XENON1T experiment to conduct a blind search for signals from Multiply-Interacting Massive Particles (MIMPs). Their unique track signature allows a targeted analysis with only 0.05 expected background events from muons. Following unblinding, we observe no signal candidate events. This work places strong constraints on spin-independent interactions of dark matter particles with a mass between 1$\times$10$^{12}\,$GeV/c$^2$ and 2$\times$10$^{17}\,$GeV/c$^2$. In addition, we present the first exclusion limits on spin-dependent MIMP-neutron and MIMP-proton cross-sections for dark matter particles with masses close to the Planck scale. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.10931v1-abstract-full').style.display = 'none'; document.getElementById('2304.10931v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 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. 130, 261002 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.14729">arXiv:2303.14729</a> <span> [<a href="https://arxiv.org/pdf/2303.14729">pdf</a>, <a href="https://arxiv.org/format/2303.14729">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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.131.041003">10.1103/PhysRevLett.131.041003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XENON+Collaboration"> XENON Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brookes%2C+E+J">E. J. Brookes</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Bui%2C+T+K">T. K. Bui</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a> , et al. (141 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.14729v2-abstract-short" style="display: inline;"> We report on the first search for nuclear recoils from dark matter in the form of weakly interacting massive particles (WIMPs) with the XENONnT experiment which is based on a two-phase time projection chamber with a sensitive liquid xenon mass of $5.9$ t. During the approximately 1.1 tonne-year exposure used for this search, the intrinsic $^{85}$Kr and $^{222}$Rn concentrations in the liquid targe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14729v2-abstract-full').style.display = 'inline'; document.getElementById('2303.14729v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.14729v2-abstract-full" style="display: none;"> We report on the first search for nuclear recoils from dark matter in the form of weakly interacting massive particles (WIMPs) with the XENONnT experiment which is based on a two-phase time projection chamber with a sensitive liquid xenon mass of $5.9$ t. During the approximately 1.1 tonne-year exposure used for this search, the intrinsic $^{85}$Kr and $^{222}$Rn concentrations in the liquid target were reduced to unprecedentedly low levels, giving an electronic recoil background rate of $(15.8\pm1.3)~\mathrm{events}/(\mathrm{t\cdot y \cdot keV})$ in the region of interest. A blind analysis of nuclear recoil events with energies between $3.3$ keV and $60.5$ keV finds no significant excess. This leads to a minimum upper limit on the spin-independent WIMP-nucleon cross section of $2.58\times 10^{-47}~\mathrm{cm}^2$ for a WIMP mass of $28~\mathrm{GeV}/c^2$ at $90\%$ confidence level. Limits for spin-dependent interactions are also provided. Both the limit and the sensitivity for the full range of WIMP masses analyzed here improve on previous results obtained with the XENON1T experiment for the same exposure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14729v2-abstract-full').style.display = 'none'; document.getElementById('2303.14729v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Limit points are included in the submission file</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 131, 041003 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.11032">arXiv:2212.11032</a> <span> [<a href="https://arxiv.org/pdf/2212.11032">pdf</a>, <a href="https://arxiv.org/format/2212.11032">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div 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/10.1088/1748-0221/18/07/P07054">10.1088/1748-0221/18/07/P07054 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Triggerless Data Acquisition System of the XENONnT Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brookes%2C+E+J">E. J. Brookes</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Bui%2C+T+K">T. K. Bui</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a> , et al. (140 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.11032v1-abstract-short" style="display: inline;"> The XENONnT detector uses the latest and largest liquid xenon-based time projection chamber (TPC) operated by the XENON Collaboration, aimed at detecting Weakly Interacting Massive Particles and conducting other rare event searches. The XENONnT data acquisition (DAQ) system constitutes an upgraded and expanded version of the XENON1T DAQ system. For its operation, it relies predominantly on commerc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11032v1-abstract-full').style.display = 'inline'; document.getElementById('2212.11032v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.11032v1-abstract-full" style="display: none;"> The XENONnT detector uses the latest and largest liquid xenon-based time projection chamber (TPC) operated by the XENON Collaboration, aimed at detecting Weakly Interacting Massive Particles and conducting other rare event searches. The XENONnT data acquisition (DAQ) system constitutes an upgraded and expanded version of the XENON1T DAQ system. For its operation, it relies predominantly on commercially available hardware accompanied by open-source and custom-developed software. The three constituent subsystems of the XENONnT detector, the TPC (main detector), muon veto, and the newly introduced neutron veto, are integrated into a single DAQ, and can be operated both independently and as a unified system. In total, the DAQ digitizes the signals of 698 photomultiplier tubes (PMTs), of which 253 from the top PMT array of the TPC are digitized twice, at $\times10$ and $\times0.5$ gain. The DAQ for the most part is a triggerless system, reading out and storing every signal that exceeds the digitization thresholds. Custom-developed software is used to process the acquired data, making it available within $\mathcal{O}\left(10\text{ s}\right)$ for live data quality monitoring and online analyses. The entire system with all the three subsystems was successfully commissioned and has been operating continuously, comfortably withstanding readout rates that exceed $\sim500$ MB/s during calibration. Livetime during normal operation exceeds $99\%$ and is $\sim90\%$ during most high-rate calibrations. The combined DAQ system has collected more than 2 PB of both calibration and science data during the commissioning of XENONnT and the first science run. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11032v1-abstract-full').style.display = 'none'; document.getElementById('2212.11032v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.14191">arXiv:2211.14191</a> <span> [<a href="https://arxiv.org/pdf/2211.14191">pdf</a>, <a href="https://arxiv.org/format/2211.14191">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-023-11512-z">10.1140/epjc/s10052-023-11512-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-energy Calibration of XENON1T with an Internal $^{37}$Ar Source </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Alfonsi%2C+M">M. Alfonsi</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Bui%2C+T+K">T. K. Bui</a>, <a href="/search/physics?searchtype=author&query=Cai%2C+C">C. Cai</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a> , et al. (139 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.14191v3-abstract-short" style="display: inline;"> A low-energy electronic recoil calibration of XENON1T, a dual-phase xenon time projection chamber, with an internal $^{37}$Ar source was performed. This calibration source features a 35-day half-life and provides two mono-energetic lines at 2.82 keV and 0.27 keV. The photon yield and electron yield at 2.82 keV are measured to be (32.3$\pm$0.3) photons/keV and (40.6$\pm$0.5) electrons/keV, respecti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14191v3-abstract-full').style.display = 'inline'; document.getElementById('2211.14191v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.14191v3-abstract-full" style="display: none;"> A low-energy electronic recoil calibration of XENON1T, a dual-phase xenon time projection chamber, with an internal $^{37}$Ar source was performed. This calibration source features a 35-day half-life and provides two mono-energetic lines at 2.82 keV and 0.27 keV. The photon yield and electron yield at 2.82 keV are measured to be (32.3$\pm$0.3) photons/keV and (40.6$\pm$0.5) electrons/keV, respectively, in agreement with other measurements and with NEST predictions. The electron yield at 0.27 keV is also measured and it is (68.0$^{+6.3}_{-3.7}$) electrons/keV. The $^{37}$Ar calibration confirms that the detector is well-understood in the energy region close to the detection threshold, with the 2.82 keV line reconstructed at (2.83$\pm$0.02) keV, which further validates the model used to interpret the low-energy electronic recoil excess previously reported by XENON1T. The ability to efficiently remove argon with cryogenic distillation after the calibration proves that $^{37}$Ar can be considered as a regular calibration source for multi-tonne xenon detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14191v3-abstract-full').style.display = 'none'; document.getElementById('2211.14191v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 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> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.06204">arXiv:2211.06204</a> <span> [<a href="https://arxiv.org/pdf/2211.06204">pdf</a>, <a href="https://arxiv.org/format/2211.06204">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.108.083022">10.1103/PhysRevD.108.083022 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct dark matter searches with the full data set of XMASS-I </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XMASS+Collaboration"> XMASS Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Kato%2C+N">N. Kato</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+T">T. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">A. Takeda</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+B+S">B. S. Yang</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+N+Y">N. Y. Kim</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+Y+D">Y. D. Kim</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+Y+H">Y. H. Kim</a>, <a href="/search/physics?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/physics?searchtype=author&query=Martens%2C+K">K. Martens</a>, <a href="/search/physics?searchtype=author&query=Mason%2C+A">A. Mason</a>, <a href="/search/physics?searchtype=author&query=Yamashita%2C+M">M. Yamashita</a>, <a href="/search/physics?searchtype=author&query=Miuchi%2C+K">K. Miuchi</a>, <a href="/search/physics?searchtype=author&query=Takeuchi%2C+Y">Y. Takeuchi</a>, <a href="/search/physics?searchtype=author&query=Lee%2C+K+B">K. B. Lee</a>, <a href="/search/physics?searchtype=author&query=Lee%2C+M+K">M. K. Lee</a>, <a href="/search/physics?searchtype=author&query=Fukuda%2C+Y">Y. Fukuda</a>, <a href="/search/physics?searchtype=author&query=Ogawa%2C+H">H. Ogawa</a> , et al. (7 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="2211.06204v2-abstract-short" style="display: inline;"> Various WIMP dark matter searches using the full data set of XMASS-I, a single-phase liquid xenon detector, are reported in this paper. Stable XMASS-I data taking accumulated a total live time of 1590.9 days between November 20, 2013 and February 1, 2019 with an analysis threshold of ${\rm 1.0\,keV_{ee}}$. In the latter half of data taking a lower analysis threshold of ${\rm 0.5\,keV_{ee}}$ was al… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.06204v2-abstract-full').style.display = 'inline'; document.getElementById('2211.06204v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.06204v2-abstract-full" style="display: none;"> Various WIMP dark matter searches using the full data set of XMASS-I, a single-phase liquid xenon detector, are reported in this paper. Stable XMASS-I data taking accumulated a total live time of 1590.9 days between November 20, 2013 and February 1, 2019 with an analysis threshold of ${\rm 1.0\,keV_{ee}}$. In the latter half of data taking a lower analysis threshold of ${\rm 0.5\,keV_{ee}}$ was also available through a new low threshold trigger. Searching for a WIMP signal in the detector's 97~kg fiducial volume yielded a limit on the WIMP-nucleon scattering cross section of ${\rm 1.4\times 10^{-44}\, cm^{2}}$ for a ${\rm 60\,GeV/c^{2}}$ WIMP at the 90$\%$ confidence level. We also searched for WIMP induced annual modulation signatures in the detector's whole target volume, containing 832~kg of liquid xenon. For nuclear recoils of a ${\rm 8\,GeV/c^{2}}$ WIMP this analysis yielded a 90\% CL cross section limit of ${\rm 2.3\times 10^{-42}\, cm^{2}}$. At a WIMP mass of ${\rm 0.5\, GeV/c^{2}}$ the Migdal effect and Bremsstrahlung signatures were evaluated and lead to 90\% CL cross section limits of ${\rm 1.4\times 10^{-35}\, cm^{2}}$ and ${\rm 1.1\times 10^{-33}\, cm^{2}}$ respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.06204v2-abstract-full').style.display = 'none'; document.getElementById('2211.06204v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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 108, 083022 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.12948">arXiv:2210.12948</a> <span> [<a href="https://arxiv.org/pdf/2210.12948">pdf</a>, <a href="https://arxiv.org/format/2210.12948">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Searching for neutrinos from solar flares across solar cycles 23 and 24 with the Super-Kamiokande detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/physics?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/physics?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/physics?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/physics?searchtype=author&query=Kaneshima%2C+Y">Y. Kaneshima</a>, <a href="/search/physics?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/physics?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/physics?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/physics?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/physics?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/physics?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/physics?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/physics?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Shimizu%2C+K">K. Shimizu</a>, <a href="/search/physics?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a> , et al. (220 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.12948v2-abstract-short" style="display: inline;"> Neutrinos associated with solar flares (solar-flare neutrinos) provide information on particle acceleration mechanisms during the impulsive phase of solar flares. We searched using the Super-Kamiokande detector for neutrinos from solar flares that occurred during solar cycles $23$ and $24$, including the largest solar flare (X28.0) on November 4th, 2003. In order to minimize the background rate we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12948v2-abstract-full').style.display = 'inline'; document.getElementById('2210.12948v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.12948v2-abstract-full" style="display: none;"> Neutrinos associated with solar flares (solar-flare neutrinos) provide information on particle acceleration mechanisms during the impulsive phase of solar flares. We searched using the Super-Kamiokande detector for neutrinos from solar flares that occurred during solar cycles $23$ and $24$, including the largest solar flare (X28.0) on November 4th, 2003. In order to minimize the background rate we searched for neutrino interactions within narrow time windows coincident with $纬$-rays and soft X-rays recorded by satellites. In addition, we performed the first attempt to search for solar-flare neutrinos from solar flares on the invisible side of the Sun by using the emission time of coronal mass ejections (CMEs). By selecting twenty powerful solar flares above X5.0 on the visible side and eight CMEs whose emission speed exceeds $2000$ $\mathrm{km \, s^{-1}}$ on the invisible side from 1996 to 2018, we found two (six) neutrino events coincident with solar flares occurring on the visible (invisible) side of the Sun, with a typical background rate of $0.10$ ($0.62$) events per flare in the MeV-GeV energy range. No significant solar-flare neutrino signal above the estimated background rate was observed. As a result we set the following upper limit on neutrino fluence at the Earth $\mathit桅<1.1\times10^{6}$ $\mathrm{cm^{-2}}$ at the $90\%$ confidence level for the largest solar flare. The resulting fluence limits allow us to constrain some of the theoretical models for solar-flare neutrino emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12948v2-abstract-full').style.display = 'none'; document.getElementById('2210.12948v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 18 figures, 9 tables (Figure 12 was replaced because it was incorrect in version 1.)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.07231">arXiv:2210.07231</a> <span> [<a href="https://arxiv.org/pdf/2210.07231">pdf</a>, <a href="https://arxiv.org/format/2210.07231">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/10.1140/epjc/s10052-022-10913-w">10.1140/epjc/s10052-022-10913-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An approximate likelihood for nuclear recoil searches with XENON1T data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Alfonsi%2C+M">M. Alfonsi</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Cichon%2C+D">D. Cichon</a>, <a href="/search/physics?searchtype=author&query=Cimmino%2C+B">B. Cimmino</a> , et al. (129 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.07231v1-abstract-short" style="display: inline;"> The XENON collaboration has published stringent limits on specific dark matter -nucleon recoil spectra from dark matter recoiling on the liquid xenon detector target. In this paper, we present an approximate likelihood for the XENON1T 1 tonne-year nuclear recoil search applicable to any nuclear recoil spectrum. Alongside this paper, we publish data and code to compute upper limits using the method… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.07231v1-abstract-full').style.display = 'inline'; document.getElementById('2210.07231v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.07231v1-abstract-full" style="display: none;"> The XENON collaboration has published stringent limits on specific dark matter -nucleon recoil spectra from dark matter recoiling on the liquid xenon detector target. In this paper, we present an approximate likelihood for the XENON1T 1 tonne-year nuclear recoil search applicable to any nuclear recoil spectrum. Alongside this paper, we publish data and code to compute upper limits using the method we present. The approximate likelihood is constructed in bins of reconstructed energy, profiled along the signal expectation in each bin. This approach can be used to compute an approximate likelihood and therefore most statistical results for any nuclear recoil spectrum. Computing approximate results with this method is approximately three orders of magnitude faster than the likelihood used in the original publications of XENON1T, where limits were set for specific families of recoil spectra. Using this same method, we include toy Monte Carlo simulation-derived binwise likelihoods for the upcoming XENONnT experiment that can similarly be used to assess the sensitivity to arbitrary nuclear recoil signatures in its eventual 20 tonne-year exposure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.07231v1-abstract-full').style.display = 'none'; document.getElementById('2210.07231v1-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by European Physical Journal C</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.05049">arXiv:2210.05049</a> <span> [<a href="https://arxiv.org/pdf/2210.05049">pdf</a>, <a href="https://arxiv.org/format/2210.05049">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1117/1.JATIS.8.4.046001">10.1117/1.JATIS.8.4.046001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Single Event Tolerance of X-ray SOI Pixel Sensors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Hagino%2C+K">Kouichi Hagino</a>, <a href="/search/physics?searchtype=author&query=Hayashida%2C+M">Mitsuki Hayashida</a>, <a href="/search/physics?searchtype=author&query=Kohmura%2C+T">Takayoshi Kohmura</a>, <a href="/search/physics?searchtype=author&query=Doi%2C+T">Toshiki Doi</a>, <a href="/search/physics?searchtype=author&query=Tsunomachi%2C+S">Shun Tsunomachi</a>, <a href="/search/physics?searchtype=author&query=Kitajima%2C+M">Masatoshi Kitajima</a>, <a href="/search/physics?searchtype=author&query=Tsuru%2C+T+G">Takeshi G. Tsuru</a>, <a href="/search/physics?searchtype=author&query=Uchida%2C+H">Hiroyuki Uchida</a>, <a href="/search/physics?searchtype=author&query=Kayama%2C+K">Kazuho Kayama</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+K">Koji Mori</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Ayaki Takeda</a>, <a href="/search/physics?searchtype=author&query=Nishioka%2C+Y">Yusuke Nishioka</a>, <a href="/search/physics?searchtype=author&query=Yukumoto%2C+M">Masataka Yukumoto</a>, <a href="/search/physics?searchtype=author&query=Mieda%2C+K">Kira Mieda</a>, <a href="/search/physics?searchtype=author&query=Yonemura%2C+S">Syuto Yonemura</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+T">Tatsunori Ishida</a>, <a href="/search/physics?searchtype=author&query=Tanaka%2C+T">Takaaki Tanaka</a>, <a href="/search/physics?searchtype=author&query=Arai%2C+Y">Yasuo Arai</a>, <a href="/search/physics?searchtype=author&query=Kurachi%2C+I">Ikuo Kurachi</a>, <a href="/search/physics?searchtype=author&query=Kitamura%2C+H">Hisashi Kitamura</a>, <a href="/search/physics?searchtype=author&query=Kawahito%2C+S">Shoji Kawahito</a>, <a href="/search/physics?searchtype=author&query=Yasutomi%2C+K">Keita Yasutomi</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="2210.05049v1-abstract-short" style="display: inline;"> We evaluate the single event tolerance of the X-ray silicon-on-insulator (SOI) pixel sensor named XRPIX, developed for the future X-ray astronomical satellite FORCE. In this work, we measure the cross-section of single event upset (SEU) of the shift register on XRPIX by irradiating heavy ion beams with linear energy transfer (LET) ranging from 0.022 MeV/(mg/cm2) to 68 MeV/(mg/cm2). From the SEU cr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05049v1-abstract-full').style.display = 'inline'; document.getElementById('2210.05049v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.05049v1-abstract-full" style="display: none;"> We evaluate the single event tolerance of the X-ray silicon-on-insulator (SOI) pixel sensor named XRPIX, developed for the future X-ray astronomical satellite FORCE. In this work, we measure the cross-section of single event upset (SEU) of the shift register on XRPIX by irradiating heavy ion beams with linear energy transfer (LET) ranging from 0.022 MeV/(mg/cm2) to 68 MeV/(mg/cm2). From the SEU cross-section curve, the saturation cross-section and threshold LET are successfully obtained to be $3.4^{+2.9}_{-0.9}\times 10^{-10}~{\rm cm^2/bit}$ and $7.3^{+1.9}_{-3.5}~{\rm MeV/(mg/cm^2)}$, respectively. Using these values, the SEU rate in orbit is estimated to be $\lesssim$ 0.1 event/year primarily due to the secondary particles induced by cosmic-ray protons. This SEU rate of the shift register on XRPIX is negligible in the FORCE orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05049v1-abstract-full').style.display = 'none'; document.getElementById('2210.05049v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 5 figures, accepted for publication in JATIS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.08609">arXiv:2209.08609</a> <span> [<a href="https://arxiv.org/pdf/2209.08609">pdf</a>, <a href="https://arxiv.org/format/2209.08609">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/17/10/P10029">10.1088/1748-0221/17/10/P10029 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron Tagging following Atmospheric Neutrino Events in a Water Cherenkov Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Haga%2C+Y">Y. Haga</a>, <a href="/search/physics?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/physics?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/physics?searchtype=author&query=Iyogi%2C+K">K. Iyogi</a>, <a href="/search/physics?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/physics?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/physics?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/physics?searchtype=author&query=Kato%2C+Y">Y. Kato</a>, <a href="/search/physics?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/physics?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/physics?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/physics?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/physics?searchtype=author&query=Mochizuki%2C+T">T. Mochizuki</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Nakajima%2C+T">T. Nakajima</a>, <a href="/search/physics?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/physics?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/physics?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/physics?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a> , et al. (281 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.08609v2-abstract-short" style="display: inline;"> We present the development of neutron-tagging techniques in Super-Kamiokande IV using a neural network analysis. The detection efficiency of neutron capture on hydrogen is estimated to be 26%, with a mis-tag rate of 0.016 per neutrino event. The uncertainty of the tagging efficiency is estimated to be 9.0%. Measurement of the tagging efficiency with data from an Americium-Beryllium calibration agr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.08609v2-abstract-full').style.display = 'inline'; document.getElementById('2209.08609v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.08609v2-abstract-full" style="display: none;"> We present the development of neutron-tagging techniques in Super-Kamiokande IV using a neural network analysis. The detection efficiency of neutron capture on hydrogen is estimated to be 26%, with a mis-tag rate of 0.016 per neutrino event. The uncertainty of the tagging efficiency is estimated to be 9.0%. Measurement of the tagging efficiency with data from an Americium-Beryllium calibration agrees with this value within 10%. The tagging procedure was performed on 3,244.4 days of SK-IV atmospheric neutrino data, identifying 18,091 neutrons in 26,473 neutrino events. The fitted neutron capture lifetime was measured as 218 \pm 9 渭s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.08609v2-abstract-full').style.display = 'none'; document.getElementById('2209.08609v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 17 P10029 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12982">arXiv:2207.12982</a> <span> [<a href="https://arxiv.org/pdf/2207.12982">pdf</a>, <a href="https://arxiv.org/format/2207.12982">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Scintillator ageing of the T2K near detectors from 2010 to 2021 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+T2K+Collaboration"> The T2K Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Akhlaq%2C+N">N. Akhlaq</a>, <a href="/search/physics?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/physics?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/physics?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/physics?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/physics?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/physics?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/physics?searchtype=author&query=Arihara%2C+T">T. Arihara</a>, <a href="/search/physics?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/physics?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/physics?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/physics?searchtype=author&query=Ban%2C+S">S. Ban</a>, <a href="/search/physics?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/physics?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/physics?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/physics?searchtype=author&query=Barrow%2C+D">D. Barrow</a>, <a href="/search/physics?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/physics?searchtype=author&query=Bench%2C+F">F. Bench</a>, <a href="/search/physics?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/physics?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/physics?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/physics?searchtype=author&query=Blanchet%2C+A">A. Blanchet</a>, <a href="/search/physics?searchtype=author&query=Blondel%2C+A">A. Blondel</a> , et al. (333 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="2207.12982v1-abstract-short" style="display: inline;"> The T2K experiment widely uses plastic scintillator as a target for neutrino interactions and an active medium for the measurement of charged particles produced in neutrino interactions at its near detector complex. Over 10 years of operation the measured light yield recorded by the scintillator based subsystems has been observed to degrade by 0.9--2.2\% per year. Extrapolation of the degradation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12982v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12982v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12982v1-abstract-full" style="display: none;"> The T2K experiment widely uses plastic scintillator as a target for neutrino interactions and an active medium for the measurement of charged particles produced in neutrino interactions at its near detector complex. Over 10 years of operation the measured light yield recorded by the scintillator based subsystems has been observed to degrade by 0.9--2.2\% per year. Extrapolation of the degradation rate through to 2040 indicates the recorded light yield should remain above the lower threshold used by the current reconstruction algorithms for all subsystems. This will allow the near detectors to continue contributing to important physics measurements during the T2K-II and Hyper-Kamiokande eras. Additionally, work to disentangle the degradation of the plastic scintillator and wavelength shifting fibres shows that the reduction in light yield can be attributed to the ageing of the plastic scintillator. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12982v1-abstract-full').style.display = 'none'; document.getElementById('2207.12982v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">29 pages, 18 figures. Prepared for submission to JINST</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.13244">arXiv:2205.13244</a> <span> [<a href="https://arxiv.org/pdf/2205.13244">pdf</a>, <a href="https://arxiv.org/format/2205.13244">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1117/1.JATIS.8.2.026007">10.1117/1.JATIS.8.2.026007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray Radiation Damage Effects on Double-SOI Pixel Detectors for the Future Astronomical Satellite "FORCE" </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Kitajima%2C+M">Masatoshi Kitajima</a>, <a href="/search/physics?searchtype=author&query=Hagino%2C+K">Kouichi Hagino</a>, <a href="/search/physics?searchtype=author&query=Kohmura%2C+T">Takayoshi Kohmura</a>, <a href="/search/physics?searchtype=author&query=Hayashida%2C+M">Mitsuki Hayashida</a>, <a href="/search/physics?searchtype=author&query=Oono%2C+K">Kenji Oono</a>, <a href="/search/physics?searchtype=author&query=Negishi%2C+K">Kousuke Negishi</a>, <a href="/search/physics?searchtype=author&query=Yarita%2C+K">Keigo Yarita</a>, <a href="/search/physics?searchtype=author&query=Doi%2C+T">Toshiki Doi</a>, <a href="/search/physics?searchtype=author&query=Tsunomachi%2C+S">Shun Tsunomachi</a>, <a href="/search/physics?searchtype=author&query=Tsuru%2C+T+G">Takeshi G. Tsuru</a>, <a href="/search/physics?searchtype=author&query=Uchida%2C+H">Hiroyuki Uchida</a>, <a href="/search/physics?searchtype=author&query=Kayama%2C+K">Kazuho Kayama</a>, <a href="/search/physics?searchtype=author&query=Kodama%2C+R">Ryota Kodama</a>, <a href="/search/physics?searchtype=author&query=Tanaka%2C+T">Takaaki Tanaka</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+K">Koji Mori</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Ayaki Takeda</a>, <a href="/search/physics?searchtype=author&query=Nishioka%2C+Y">Yusuke Nishioka</a>, <a href="/search/physics?searchtype=author&query=Yukumoto%2C+M">Masataka Yukumoto</a>, <a href="/search/physics?searchtype=author&query=Mieda%2C+K">Kira Mieda</a>, <a href="/search/physics?searchtype=author&query=Yonemura%2C+S">Syuto Yonemura</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+T">Tatsunori Ishida</a>, <a href="/search/physics?searchtype=author&query=Arai%2C+Y">Yasuo Arai</a>, <a href="/search/physics?searchtype=author&query=Kurachi%2C+I">Ikuo Kurachi</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="2205.13244v1-abstract-short" style="display: inline;"> We have been developing the monolithic active pixel detector "XRPIX" onboard the future X-ray astronomical satellite "FORCE". XRPIX is composed of CMOS pixel circuits, SiO2 insulator, and Si sensor by utilizing the silicon-on-insulator (SOI) technology. When the semiconductor detector is operated in orbit, it suffers from radiation damage due to X-rays emitted from the celestial objects as well as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.13244v1-abstract-full').style.display = 'inline'; document.getElementById('2205.13244v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.13244v1-abstract-full" style="display: none;"> We have been developing the monolithic active pixel detector "XRPIX" onboard the future X-ray astronomical satellite "FORCE". XRPIX is composed of CMOS pixel circuits, SiO2 insulator, and Si sensor by utilizing the silicon-on-insulator (SOI) technology. When the semiconductor detector is operated in orbit, it suffers from radiation damage due to X-rays emitted from the celestial objects as well as cosmic rays. From previous studies, positive charges trapped in the SiO2 insulator are known to cause the degradation of the detector performance. To improve the radiation hardness, we developed XRPIX equipped with Double-SOI (D-SOI) structure, introducing an additional silicon layer in the SiO2 insulator. This structure is aimed at compensating for the effect of the trapped positive charges. Although the radiation hardness to cosmic rays of the D-SOI detectors has been evaluated, the radiation effect due to the X-ray irradiation has not been evaluated. Then, we conduct an X-ray irradiation experiment using an X-ray generator with a total dose of 10 krad at the SiO2 insulator, equivalent to 7 years in orbit. As a result of this experiment, the energy resolution in full-width half maximum for the 5.9 keV X-ray degrades by 17.8 $\pm$ 2.8% and the dark current increases by 89 $\pm$ 13%. We also investigate the physical mechanism of the increase in the dark current due to X-ray irradiation using TCAD simulation. It is found that the increase in the dark current can be explained by the increase in the interface state density at the Si/SiO2 interface. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.13244v1-abstract-full').style.display = 'none'; document.getElementById('2205.13244v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 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">15 pages, 12 figures, accepted for publication in Journal of Astronomical Telescopes, Instruments, and Systems</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.09881">arXiv:2205.09881</a> <span> [<a href="https://arxiv.org/pdf/2205.09881">pdf</a>, <a href="https://arxiv.org/format/2205.09881">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac7f9c">10.3847/1538-4357/ac7f9c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pre-Supernova Alert System for Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</a>, <a href="/search/physics?searchtype=author&query=Machado%2C+L+N">L. N. Machado</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/physics?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/physics?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/physics?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/physics?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/physics?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/physics?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/physics?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/physics?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nakano%2C+Y">Y. Nakano</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/physics?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/physics?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/physics?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Shiba%2C+H">H. Shiba</a> , et al. (202 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.09881v2-abstract-short" style="display: inline;"> In 2020, the Super-Kamiokande (SK) experiment moved to a new stage (SK-Gd) in which gadolinium (Gd) sulfate octahydrate was added to the water in the detector, enhancing the efficiency to detect thermal neutrons and consequently improving the sensitivity to low energy electron anti-neutrinos from inverse beta decay (IBD) interactions. SK-Gd has the potential to provide early alerts of incipient co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09881v2-abstract-full').style.display = 'inline'; document.getElementById('2205.09881v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.09881v2-abstract-full" style="display: none;"> In 2020, the Super-Kamiokande (SK) experiment moved to a new stage (SK-Gd) in which gadolinium (Gd) sulfate octahydrate was added to the water in the detector, enhancing the efficiency to detect thermal neutrons and consequently improving the sensitivity to low energy electron anti-neutrinos from inverse beta decay (IBD) interactions. SK-Gd has the potential to provide early alerts of incipient core-collapse supernovae through detection of electron anti-neutrinos from thermal and nuclear processes responsible for the cooling of massive stars before the gravitational collapse of their cores. These pre-supernova neutrinos emitted during the silicon burning phase can exceed the energy threshold for IBD reactions. We present the sensitivity of SK-Gd to pre-supernova stars and the techniques used for the development of a pre-supernova alarm based on the detection of these neutrinos in SK, as well as prospects for future SK-Gd phases with higher concentrations of Gd. For the current SK-Gd phase, high-confidence alerts for Betelgeuse could be issued up to nine hours in advance of the core-collapse itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09881v2-abstract-full').style.display = 'none'; document.getElementById('2205.09881v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 935, Number 1 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.05231">arXiv:2205.05231</a> <span> [<a href="https://arxiv.org/pdf/2205.05231">pdf</a>, <a href="https://arxiv.org/ps/2205.05231">ps</a>, <a href="https://arxiv.org/format/2205.05231">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2022.137355">10.1016/j.physletb.2022.137355 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for neutrinoless quadruple beta decay of $^{136}$Xe in XMASS-I </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XMASS+Collaboration"> XMASS Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/physics?searchtype=author&query=Kato%2C+N">N. Kato</a>, <a href="/search/physics?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/physics?searchtype=author&query=Kobayashi%2C+K">K. Kobayashi</a>, <a href="/search/physics?searchtype=author&query=Kobayashi%2C+M">M. Kobayashi</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+T">T. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">A. Takeda</a>, <a href="/search/physics?searchtype=author&query=Tasaka%2C+S">S. Tasaka</a>, <a href="/search/physics?searchtype=author&query=Yamashita%2C+M">M. Yamashita</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+B+S">B. S. Yang</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+N+Y">N. Y. Kim</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+Y+D">Y. D. Kim</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+Y+H">Y. H. Kim</a>, <a href="/search/physics?searchtype=author&query=Ishii%2C+R">R. Ishii</a>, <a href="/search/physics?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/physics?searchtype=author&query=Kanzawa%2C+K">K. Kanzawa</a>, <a href="/search/physics?searchtype=author&query=Masuda%2C+K">K. Masuda</a>, <a href="/search/physics?searchtype=author&query=Martens%2C+K">K. Martens</a> , et al. (12 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="2205.05231v2-abstract-short" style="display: inline;"> A search for the neutrinoless quadruple beta decay of $^{136}$Xe was conducted with the liquid-xenon detector XMASS-I using $\rm 327\; kg \times 800.0 \; days$ of the exposure. The pulse shape discrimination based on the scintillation decay time constant which distinguishes $纬$-rays including the signal and $尾$-rays was used to enhance the search sensitivity. No significant signal excess was obser… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.05231v2-abstract-full').style.display = 'inline'; document.getElementById('2205.05231v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.05231v2-abstract-full" style="display: none;"> A search for the neutrinoless quadruple beta decay of $^{136}$Xe was conducted with the liquid-xenon detector XMASS-I using $\rm 327\; kg \times 800.0 \; days$ of the exposure. The pulse shape discrimination based on the scintillation decay time constant which distinguishes $纬$-rays including the signal and $尾$-rays was used to enhance the search sensitivity. No significant signal excess was observed from the energy spectrum fitting with precise background evaluation, and we set a lower limit of the half life of 3.7 $\times$ 10$^{24}$ years at 90$\%$ confidence level. This is the first experimental constraint of the neutrinoless quadruple beta decay of $^{136}$Xe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.05231v2-abstract-full').style.display = 'none'; document.getElementById('2205.05231v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Journal ref:</span> Physics Letters B 833 (2022) 137355 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.03838">arXiv:2205.03838</a> <span> [<a href="https://arxiv.org/pdf/2205.03838">pdf</a>, <a href="https://arxiv.org/ps/2205.03838">ps</a>, <a href="https://arxiv.org/format/2205.03838">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> </div> </div> <p class="title is-5 mathjax"> Precision beam telescope based on SOI pixel sensor technology for electrons in the energy range of sub-GeV to GeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Suzuki%2C+H">Hisanori Suzuki</a>, <a href="/search/physics?searchtype=author&query=Omori%2C+T">Takumi Omori</a>, <a href="/search/physics?searchtype=author&query=Hara%2C+K">Kazuhiko Hara</a>, <a href="/search/physics?searchtype=author&query=Yamauchi%2C+H">Hiroki Yamauchi</a>, <a href="/search/physics?searchtype=author&query=Yamada%2C+M">Miho Yamada</a>, <a href="/search/physics?searchtype=author&query=Tsuboyama%2C+T">Toru Tsuboyama</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Ayaki Takeda</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="2205.03838v3-abstract-short" style="display: inline;"> We developed a beam telescope system comprising five layers of 300-$渭$m-thick INTPIX4NA monolithic pixel sensors with each pixel size of 17 $渭$m square. The sensors were fabricated using silicon-on-insulator (SOI) technology. The signal-to-noise ratio of 140--230 is realized at a bias voltage of 20~V. The tracker system was tested using a positron beam of 200--822 MeV/c, and various tracking metho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.03838v3-abstract-full').style.display = 'inline'; document.getElementById('2205.03838v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.03838v3-abstract-full" style="display: none;"> We developed a beam telescope system comprising five layers of 300-$渭$m-thick INTPIX4NA monolithic pixel sensors with each pixel size of 17 $渭$m square. The sensors were fabricated using silicon-on-insulator (SOI) technology. The signal-to-noise ratio of 140--230 is realized at a bias voltage of 20~V. The tracker system was tested using a positron beam of 200--822 MeV/c, and various tracking methods are examined to optimize spatial precision achievable at these energies. The best tracking precision including the precision of the sensor under test itself is 11.04 $\pm$ 0.10 $渭$m for 822-MeV/c positrons for an equidistant sensor spacing of 32 mm. The achieved precision results combined with the intrinsic spatial resolution value obtained for a similar system using 120 GeV protons are used to estimate the tracking performance of electrons in the GeV energy range; a tracking precision of 2.22 $渭$m is evaluated for 5-GeV electrons. The method to estimate the tracking performance is verified using a Geant4-based simulation. The developed high precision tracker system enables to map the detailed performance of the sensors with pixel sizes of $\mathcal{O}$(10 $渭$m), therefore will be a powerful system for development of devices targeting precision position resolutions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.03838v3-abstract-full').style.display = 'none'; document.getElementById('2205.03838v3-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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 figures and 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.02309">arXiv:2203.02309</a> <span> [<a href="https://arxiv.org/pdf/2203.02309">pdf</a>, <a href="https://arxiv.org/format/2203.02309">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1088/1361-6471/ac841a">10.1088/1361-6471/ac841a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Aerne%2C+V">V. Aerne</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/physics?searchtype=author&query=Akshat%2C+J">J. Akshat</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Amaro%2C+F+D">F. D. Amaro</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J">J. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a> , et al. (572 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="2203.02309v1-abstract-short" style="display: inline;"> The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for Weakly Interacting Massive Particles (WIMPs), while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neut… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02309v1-abstract-full').style.display = 'inline'; document.getElementById('2203.02309v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.02309v1-abstract-full" style="display: none;"> The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for Weakly Interacting Massive Particles (WIMPs), while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neutrinos through neutrinoless double-beta decay and through a variety of astrophysical sources. A next-generation xenon-based detector will therefore be a true multi-purpose observatory to significantly advance particle physics, nuclear physics, astrophysics, solar physics, and cosmology. This review article presents the science cases for such a detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02309v1-abstract-full').style.display = 'none'; document.getElementById('2203.02309v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 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">77 pages, 40 figures, 1262 references</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> INT-PUB-22-003 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Phys. G: Nucl. Part. Phys. 50 (2023) 013001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.12231">arXiv:2112.12231</a> <span> [<a href="https://arxiv.org/pdf/2112.12231">pdf</a>, <a href="https://arxiv.org/format/2112.12231">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/ptep/ptac074">10.1093/ptep/ptac074 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Application and modeling of an online distillation method to reduce krypton and argon in XENON1T </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Alfonsi%2C+M">M. Alfonsi</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Bernard%2C+A">A. Bernard</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Cichon%2C+D">D. Cichon</a>, <a href="/search/physics?searchtype=author&query=Cimmino%2C+B">B. Cimmino</a> , et al. (129 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="2112.12231v2-abstract-short" style="display: inline;"> A novel online distillation technique was developed for the XENON1T dark matter experiment to reduce intrinsic background components more volatile than xenon, such as krypton or argon, while the detector was operating. The method is based on a continuous purification of the gaseous volume of the detector system using the XENON1T cryogenic distillation column. A krypton-in-xenon concentration of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.12231v2-abstract-full').style.display = 'inline'; document.getElementById('2112.12231v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.12231v2-abstract-full" style="display: none;"> A novel online distillation technique was developed for the XENON1T dark matter experiment to reduce intrinsic background components more volatile than xenon, such as krypton or argon, while the detector was operating. The method is based on a continuous purification of the gaseous volume of the detector system using the XENON1T cryogenic distillation column. A krypton-in-xenon concentration of $(360 \pm 60)$ ppq was achieved. It is the lowest concentration measured in the fiducial volume of an operating dark matter detector to date. A model was developed and fit to the data to describe the krypton evolution in the liquid and gas volumes of the detector system for several operation modes over the time span of 550 days, including the commissioning and science runs of XENON1T. The online distillation was also successfully applied to remove Ar-37 after its injection for a low energy calibration in XENON1T. This makes the usage of Ar-37 as a regular calibration source possible in the future. The online distillation can be applied to next-generation experiments to remove krypton prior to, or during, any science run. The model developed here allows further optimization of the distillation strategy for future large scale detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.12231v2-abstract-full').style.display = 'none'; document.getElementById('2112.12231v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">Journal ref:</span> Prog Theor Exp Phys (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.12116">arXiv:2112.12116</a> <span> [<a href="https://arxiv.org/pdf/2112.12116">pdf</a>, <a href="https://arxiv.org/format/2112.12116">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.106.022001">10.1103/PhysRevD.106.022001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Emission of Single and Few Electrons in XENON1T and Limits on Light Dark Matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Alfonsi%2C+M">M. Alfonsi</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Bernard%2C+A">A. Bernard</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Cichon%2C+D">D. Cichon</a>, <a href="/search/physics?searchtype=author&query=Cimmino%2C+B">B. Cimmino</a> , et al. (130 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="2112.12116v3-abstract-short" style="display: inline;"> Delayed single- and few-electron emissions plague dual-phase time projection chambers, limiting their potential to search for light-mass dark matter. This paper examines the origins of these events in the XENON1T experiment. Characterization of the intensity of delayed electron backgrounds shows that the resulting emissions are correlated, in time and position, with high-energy events and can effe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.12116v3-abstract-full').style.display = 'inline'; document.getElementById('2112.12116v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.12116v3-abstract-full" style="display: none;"> Delayed single- and few-electron emissions plague dual-phase time projection chambers, limiting their potential to search for light-mass dark matter. This paper examines the origins of these events in the XENON1T experiment. Characterization of the intensity of delayed electron backgrounds shows that the resulting emissions are correlated, in time and position, with high-energy events and can effectively be vetoed. In this work we extend previous S2-only analyses down to a single electron. From this analysis, after removing the correlated backgrounds, we observe rates < 30 events/(electron*kg*day) in the region of interest spanning 1 to 5 electrons. We derive 90% confidence upper limits for dark matter-electron scattering, first direct limits on the electric dipole, magnetic dipole, and anapole interactions, and bosonic dark matter models, where we exclude new parameter space for dark photons and solar dark photons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.12116v3-abstract-full').style.display = 'none'; document.getElementById('2112.12116v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">20 pages, 17 figures, Updated to correct published Solar Dark Photon limit</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 106, 022001 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.05629">arXiv:2112.05629</a> <span> [<a href="https://arxiv.org/pdf/2112.05629">pdf</a>, <a href="https://arxiv.org/format/2112.05629">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-022-10345-6">10.1140/epjc/s10052-022-10345-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Material radiopurity control in the XENONnT experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Alfonsi%2C+M">M. Alfonsi</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A+L">A. L. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Cichon%2C+D">D. Cichon</a>, <a href="/search/physics?searchtype=author&query=Cimmino%2C+B">B. Cimmino</a>, <a href="/search/physics?searchtype=author&query=Clark%2C+M">M. Clark</a> , et al. (128 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="2112.05629v2-abstract-short" style="display: inline;"> The selection of low-radioactive construction materials is of the utmost importance for rare-event searches and thus critical to the XENONnT experiment. Results of an extensive radioassay program are reported, in which material samples have been screened with gamma-ray spectroscopy, mass spectrometry, and $^{222}$Rn emanation measurements. Furthermore, the cleanliness procedures applied to remove… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.05629v2-abstract-full').style.display = 'inline'; document.getElementById('2112.05629v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.05629v2-abstract-full" style="display: none;"> The selection of low-radioactive construction materials is of the utmost importance for rare-event searches and thus critical to the XENONnT experiment. Results of an extensive radioassay program are reported, in which material samples have been screened with gamma-ray spectroscopy, mass spectrometry, and $^{222}$Rn emanation measurements. Furthermore, the cleanliness procedures applied to remove or mitigate surface contamination of detector materials are described. Screening results, used as inputs for a XENONnT Monte Carlo simulation, predict a reduction of materials background ($\sim$17%) with respect to its predecessor XENON1T. Through radon emanation measurements, the expected $^{222}$Rn activity concentration in XENONnT is determined to be 4.2$\,(^{+0.5}_{-0.7})\,渭$Bq/kg, a factor three lower with respect to XENON1T. This radon concentration will be further suppressed by means of the novel radon distillation system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.05629v2-abstract-full').style.display = 'none'; document.getElementById('2112.05629v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.00360">arXiv:2109.00360</a> <span> [<a href="https://arxiv.org/pdf/2109.00360">pdf</a>, <a href="https://arxiv.org/format/2109.00360">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2021.166248">10.1016/j.nima.2021.166248 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Gadolinium Loading to Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/physics?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/physics?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/physics?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/physics?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/physics?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/physics?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/physics?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/physics?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/physics?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/physics?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/physics?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/physics?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">A. Takeda</a>, <a href="/search/physics?searchtype=author&query=Takemoto%2C+Y">Y. Takemoto</a> , et al. (192 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.00360v3-abstract-short" style="display: inline;"> In order to improve Super-Kamiokande's neutron detection efficiency and to thereby increase its sensitivity to the diffuse supernova neutrino background flux, 13 tons of $\rm Gd_2(\rm SO_4)_3\cdot \rm 8H_2O$ (gadolinium sulfate octahydrate) was dissolved into the detector's otherwise ultrapure water from July 14 to August 17, 2020, marking the start of the SK-Gd phase of operations. During the loa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.00360v3-abstract-full').style.display = 'inline'; document.getElementById('2109.00360v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.00360v3-abstract-full" style="display: none;"> In order to improve Super-Kamiokande's neutron detection efficiency and to thereby increase its sensitivity to the diffuse supernova neutrino background flux, 13 tons of $\rm Gd_2(\rm SO_4)_3\cdot \rm 8H_2O$ (gadolinium sulfate octahydrate) was dissolved into the detector's otherwise ultrapure water from July 14 to August 17, 2020, marking the start of the SK-Gd phase of operations. During the loading, water was continuously recirculated at a rate of 60 m$^3$/h, extracting water from the top of the detector and mixing it with concentrated $\rm Gd_2(\rm SO_4)_3\cdot \rm 8H_2O$ solution to create a 0.02% solution of the Gd compound before injecting it into the bottom of the detector. A clear boundary between the Gd-loaded and pure water was maintained through the loading, enabling monitoring of the loading itself and the spatial uniformity of the Gd concentration over the 35 days it took to reach the top of the detector. During the subsequent commissioning the recirculation rate was increased to 120 m$^3$/h, resulting in a constant and uniform distribution of Gd throughout the detector and water transparency equivalent to that of previous pure-water operation periods. Using an Am-Be neutron calibration source the mean neutron capture time was measured to be $115\pm1$ $渭$s, which corresponds to a Gd concentration of $111\pm2$ ppm, as expected for this level of Gd loading. This paper describes changes made to the water circulation system for this detector upgrade, the Gd loading procedure, detector commissioning, and the first neutron calibration measurements in SK-Gd. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.00360v3-abstract-full').style.display = 'none'; document.getElementById('2109.00360v3-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 19 Figures, Accepted for publication in Nucl. Instrum. Meth. A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Inst. and Methods in Physics Research, A 1027 (2022) 166248 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.05303">arXiv:2108.05303</a> <span> [<a href="https://arxiv.org/pdf/2108.05303">pdf</a>, <a href="https://arxiv.org/format/2108.05303">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1117/1.JATIS.7.3.036001">10.1117/1.JATIS.7.3.036001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Proton radiation hardness of X-ray SOI pixel sensors with pinned depleted diode structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Hayashida%2C+M">Mitsuki Hayashida</a>, <a href="/search/physics?searchtype=author&query=Hagino%2C+K">Kouichi Hagino</a>, <a href="/search/physics?searchtype=author&query=Kohmura%2C+T">Takayoshi Kohmura</a>, <a href="/search/physics?searchtype=author&query=Kitajima%2C+M">Masatoshi Kitajima</a>, <a href="/search/physics?searchtype=author&query=Yarita%2C+K">Keigo Yarita</a>, <a href="/search/physics?searchtype=author&query=Oono%2C+K">Kenji Oono</a>, <a href="/search/physics?searchtype=author&query=Negishi%2C+K">Kousuke Negishi</a>, <a href="/search/physics?searchtype=author&query=Tsuru%2C+T+G">Takeshi G. Tsuru</a>, <a href="/search/physics?searchtype=author&query=Tanaka%2C+T">Takaaki Tanaka</a>, <a href="/search/physics?searchtype=author&query=Uchida%2C+H">Hiroyuki Uchida</a>, <a href="/search/physics?searchtype=author&query=Kayama%2C+K">Kazuho Kayama</a>, <a href="/search/physics?searchtype=author&query=Kodama%2C+R">Ryota Kodama</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+K">Koji Mori</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Ayaki Takeda</a>, <a href="/search/physics?searchtype=author&query=Nishioka%2C+Y">Yusuke Nishioka</a>, <a href="/search/physics?searchtype=author&query=Hida%2C+T">Takahiro Hida</a>, <a href="/search/physics?searchtype=author&query=Yukumoto%2C+M">Masataka Yukumoto</a>, <a href="/search/physics?searchtype=author&query=Arai%2C+Y">Yasuo Arai</a>, <a href="/search/physics?searchtype=author&query=Kurachi%2C+I">Ikuo Kurachi</a>, <a href="/search/physics?searchtype=author&query=Kitamura%2C+H">Hisashi Kitamura</a>, <a href="/search/physics?searchtype=author&query=Kawahito%2C+S">Shoji Kawahito</a>, <a href="/search/physics?searchtype=author&query=Yasutomi%2C+K">Keita Yasutomi</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="2108.05303v1-abstract-short" style="display: inline;"> X-ray SOI pixel sensors, "XRPIX", are being developed for the next-generation X-ray astronomical satellite, "FORCE". The XRPIX are fabricated with the SOI technology, which makes it possible to integrate a high-resistivity Si sensor and a low-resistivity Si CMOS circuit. The CMOS circuit in each pixel is equipped with a trigger function, allowing us to read out outputs only from the pixels with X-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.05303v1-abstract-full').style.display = 'inline'; document.getElementById('2108.05303v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.05303v1-abstract-full" style="display: none;"> X-ray SOI pixel sensors, "XRPIX", are being developed for the next-generation X-ray astronomical satellite, "FORCE". The XRPIX are fabricated with the SOI technology, which makes it possible to integrate a high-resistivity Si sensor and a low-resistivity Si CMOS circuit. The CMOS circuit in each pixel is equipped with a trigger function, allowing us to read out outputs only from the pixels with X-ray signals at the timing of X-ray detection. This function thus realizes high throughput and high time resolution, which enables to employ anti-coincidence technique for background rejection. A new series of XRPIX named XRPIX6E developed with a pinned depleted diode (PDD) structure improves spectral performance by suppressing the interference between the sensor and circuit layers. When semiconductor X-ray sensors are used in space, their spectral performance is generally degraded owing to the radiation damage caused by high-energy protons. Therefore, before using an XRPIX in space, it is necessary to evaluate the extent of degradation of its spectral performance by radiation damage. Thus, we performed a proton irradiation experiment for XRPIX6E for the first time at HIMAC in the NIRS. We irradiated XRPIX6E with high-energy protons with a total dose of up to 40 krad, equivalent to 400 years of irradiation in orbit. The 40-krad irradiation degraded the energy resolution of XRPIX6E by 25 $\pm$ 3%, yielding an energy resolution of 260.1 $\pm$ 5.6 eV at the full width half maximum for 5.9 keV X-rays. However, the value satisfies the requirement for FORCE, 300 eV at 6 keV, even after the irradiation. It was also found that the PDD XRPIX has enhanced radiation hardness compared to previous XRPIX devices. In addition, we investigated the degradation of the energy resolution; it was shown that the degradation would be due to increasing energy-independent components, e.g., readout noise. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.05303v1-abstract-full').style.display = 'none'; document.getElementById('2108.05303v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 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">15 pages, 16 figures, accepted for publication in JATIS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.09921">arXiv:2101.09921</a> <span> [<a href="https://arxiv.org/pdf/2101.09921">pdf</a>, <a href="https://arxiv.org/format/2101.09921">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/ptep/ptab053">10.1093/ptep/ptab053 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direction-sensitive dark matter search with a low-background gaseous detector NEWAGE-0.3b'' </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ikeda%2C+T">Tomonori Ikeda</a>, <a href="/search/physics?searchtype=author&query=Nakamura%2C+K">Kiseki Nakamura</a>, <a href="/search/physics?searchtype=author&query=Shimada%2C+T">Takuya Shimada</a>, <a href="/search/physics?searchtype=author&query=Yakabe%2C+R">Ryota Yakabe</a>, <a href="/search/physics?searchtype=author&query=Hashimoto%2C+T">Takashi Hashimoto</a>, <a href="/search/physics?searchtype=author&query=Ishiura%2C+H">Hirohisa Ishiura</a>, <a href="/search/physics?searchtype=author&query=Nakamura%2C+T">Takuma Nakamura</a>, <a href="/search/physics?searchtype=author&query=Ito%2C+H">Hiroshi Ito</a>, <a href="/search/physics?searchtype=author&query=Ichimura%2C+K">Koichi Ichimura</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">Ko Abe</a>, <a href="/search/physics?searchtype=author&query=Kobayashi%2C+K">Kazuyoshi Kobayashi</a>, <a href="/search/physics?searchtype=author&query=Tanimori%2C+T">Toru Tanimori</a>, <a href="/search/physics?searchtype=author&query=Kubo%2C+H">Hidetoshi Kubo</a>, <a href="/search/physics?searchtype=author&query=Takada%2C+A">Atsushi Takada</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">Hiroyuki Sekiya</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Atsushi Takeda</a>, <a href="/search/physics?searchtype=author&query=Miuchi%2C+K">Kentaro Miuchi</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="2101.09921v2-abstract-short" style="display: inline;"> NEWAGE is a direction-sensitive dark matter search using a low-pressure gaseous time projection chamber. A low alpha-ray emission rate micro pixel chamber had been developed in order to reduce background for dark matter search. We conducted the dark matter search at the Kamioka Observatory in 2018. The total live time was 107.6 days corresponding to an exposure of 1.1 kg${\cdot}$days. Two events r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.09921v2-abstract-full').style.display = 'inline'; document.getElementById('2101.09921v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.09921v2-abstract-full" style="display: none;"> NEWAGE is a direction-sensitive dark matter search using a low-pressure gaseous time projection chamber. A low alpha-ray emission rate micro pixel chamber had been developed in order to reduce background for dark matter search. We conducted the dark matter search at the Kamioka Observatory in 2018. The total live time was 107.6 days corresponding to an exposure of 1.1 kg${\cdot}$days. Two events remained in the energy region of 50-60 keV which was consistent with 2.5 events of the expected background. A directional analysis was carried out and no significant forward-backward asymmetry derived from the WIMP-nucleus elastic scatterings was found. Thus a 90% confidence level upper limit on Spin-Dependent WIMP-proton cross section of 50 pb for a WIMP mass of 100 GeV/c2 was derived. This limit is the most stringent yet obtained from direction-sensitive dark matter search experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.09921v2-abstract-full').style.display = 'none'; document.getElementById('2101.09921v2-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Prog. Theor. Exp. Phys. 2021, 063F01 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.05269">arXiv:2101.05269</a> <span> [<a href="https://arxiv.org/pdf/2101.05269">pdf</a>, <a href="https://arxiv.org/format/2101.05269">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abf7c4">10.3847/1538-4357/abf7c4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supernova Model Discrimination with Hyper-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Collaboration%2C+H">Hyper-Kamiokande Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Adrich%2C+P">P. Adrich</a>, <a href="/search/physics?searchtype=author&query=Aihara%2C+H">H. Aihara</a>, <a href="/search/physics?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/physics?searchtype=author&query=Alekseev%2C+I">I. Alekseev</a>, <a href="/search/physics?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/physics?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/physics?searchtype=author&query=Anghel%2C+I">I. Anghel</a>, <a href="/search/physics?searchtype=author&query=Anthony%2C+L+H+V">L. H. V. Anthony</a>, <a href="/search/physics?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/physics?searchtype=author&query=Araya%2C+A">A. Araya</a>, <a href="/search/physics?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/physics?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/physics?searchtype=author&query=Aushev%2C+V">V. Aushev</a>, <a href="/search/physics?searchtype=author&query=Ballester%2C+F">F. Ballester</a>, <a href="/search/physics?searchtype=author&query=Bandac%2C+I">I. Bandac</a>, <a href="/search/physics?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/physics?searchtype=author&query=Barker%2C+G+J">G. J. Barker</a>, <a href="/search/physics?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/physics?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">M. Bellato</a>, <a href="/search/physics?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a> , et al. (478 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.05269v2-abstract-short" style="display: inline;"> Core-collapse supernovae are among the most magnificent events in the observable universe. They produce many of the chemical elements necessary for life to exist and their remnants -- neutron stars and black holes -- are interesting astrophysical objects in their own right. However, despite millennia of observations and almost a century of astrophysical study, the explosion mechanism of core-colla… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05269v2-abstract-full').style.display = 'inline'; document.getElementById('2101.05269v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05269v2-abstract-full" style="display: none;"> Core-collapse supernovae are among the most magnificent events in the observable universe. They produce many of the chemical elements necessary for life to exist and their remnants -- neutron stars and black holes -- are interesting astrophysical objects in their own right. However, despite millennia of observations and almost a century of astrophysical study, the explosion mechanism of core-collapse supernovae is not yet well understood. Hyper-Kamiokande is a next-generation neutrino detector that will be able to observe the neutrino flux from the next galactic core-collapse supernova in unprecedented detail. We focus on the first 500 ms of the neutrino burst, corresponding to the accretion phase, and use a newly-developed, high-precision supernova event generator to simulate Hyper-Kamiokande's response to five different supernova models. We show that Hyper-Kamiokande will be able to distinguish between these models with high accuracy for a supernova at a distance of up to 100 kpc. Once the next galactic supernova happens, this ability will be a powerful tool for guiding simulations towards a precise reproduction of the explosion mechanism observed in nature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05269v2-abstract-full').style.display = 'none'; document.getElementById('2101.05269v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 7 figures. Article based on thesis published as arXiv:2002.01649. v2: added references and some explanations in response to reviewer comments</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 916 (2021) 15 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.03807">arXiv:2012.03807</a> <span> [<a href="https://arxiv.org/pdf/2012.03807">pdf</a>, <a href="https://arxiv.org/ps/2012.03807">ps</a>, <a href="https://arxiv.org/format/2012.03807">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2022.102702">10.1016/j.astropartphys.2022.102702 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for solar electron anti-neutrinos due to spin-flavor precession in the Sun with Super-Kamiokande-IV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/physics?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/physics?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/physics?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/physics?searchtype=author&query=Ito%2C+H">H. Ito</a>, <a href="/search/physics?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/physics?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/physics?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nagao%2C+Y">Y. Nagao</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Nakajima%2C+Y">Y. Nakajima</a>, <a href="/search/physics?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/physics?searchtype=author&query=Okada%2C+T">T. Okada</a>, <a href="/search/physics?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a>, <a href="/search/physics?searchtype=author&query=Orii%2C+A">A. Orii</a>, <a href="/search/physics?searchtype=author&query=Pronost%2C+G">G. Pronost</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Shiozawa%2C+M">M. Shiozawa</a>, <a href="/search/physics?searchtype=author&query=Sonoda%2C+Y">Y. Sonoda</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">A. Takeda</a> , et al. (177 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.03807v3-abstract-short" style="display: inline;"> Due to a very low production rate of electron anti-neutrinos ($\bar谓_e$) via nuclear fusion in the Sun, a flux of solar $\bar谓_e$ is unexpected. An appearance of $\bar谓_e$ in solar neutrino flux opens a new window for the new physics beyond the standard model. In particular, a spin-flavor precession process is expected to convert an electron neutrino into an electron anti-neutrino (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.03807v3-abstract-full').style.display = 'inline'; document.getElementById('2012.03807v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.03807v3-abstract-full" style="display: none;"> Due to a very low production rate of electron anti-neutrinos ($\bar谓_e$) via nuclear fusion in the Sun, a flux of solar $\bar谓_e$ is unexpected. An appearance of $\bar谓_e$ in solar neutrino flux opens a new window for the new physics beyond the standard model. In particular, a spin-flavor precession process is expected to convert an electron neutrino into an electron anti-neutrino (${谓_e\to\bar谓_e}$) when neutrino has a finite magnetic moment. In this work, we have searched for solar $\bar谓_e$ in the Super-Kamiokande experiment, using neutron tagging to identify their inverse beta decay signature. We identified 78 $\bar谓_e$ candidates for neutrino energies of 9.3 to 17.3 MeV in 2970.1 live days with a fiducial volume of 22.5 kiloton water (183.0 kton$\cdot$year exposure). The energy spectrum has been consistent with background predictions and we thus derived a 90% confidence level upper limit of ${4.7\times10^{-4}}$ on the $谓_e\to\bar谓_e$ conversion probability in the Sun. We used this result to evaluate the sensitivity of future experiments, notably the Super-Kamiokande Gadolinium (SK-Gd) upgrade. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.03807v3-abstract-full').style.display = 'none'; document.getElementById('2012.03807v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures, 7 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 139 (2022) 102702 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.13981">arXiv:2009.13981</a> <span> [<a href="https://arxiv.org/pdf/2009.13981">pdf</a>, <a href="https://arxiv.org/format/2009.13981">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-020-08777-z">10.1140/epjc/s10052-020-08777-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> $^{222}$Rn emanation measurements for the XENON1T experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Alfonsi%2C+M">M. Alfonsi</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amaro%2C+F+D">F. D. Amaro</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Barge%2C+D">D. Barge</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bauermeister%2C+B">B. Bauermeister</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Benabderrahmane%2C+M+L">M. L. Benabderrahmane</a>, <a href="/search/physics?searchtype=author&query=Berger%2C+T">T. Berger</a>, <a href="/search/physics?searchtype=author&query=Breur%2C+P+A">P. A. Breur</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+E">E. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Cichon%2C+D">D. Cichon</a> , et al. (118 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.13981v3-abstract-short" style="display: inline;"> The selection of low-radioactive construction materials is of utmost importance for the success of low-energy rare event search experiments. Besides radioactive contaminants in the bulk, the emanation of radioactive radon atoms from material surfaces attains increasing relevance in the effort to further reduce the background of such experiments. In this work, we present the $^{222}$Rn emanation me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.13981v3-abstract-full').style.display = 'inline'; document.getElementById('2009.13981v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.13981v3-abstract-full" style="display: none;"> The selection of low-radioactive construction materials is of utmost importance for the success of low-energy rare event search experiments. Besides radioactive contaminants in the bulk, the emanation of radioactive radon atoms from material surfaces attains increasing relevance in the effort to further reduce the background of such experiments. In this work, we present the $^{222}$Rn emanation measurements performed for the XENON1T dark matter experiment. Together with the bulk impurity screening campaign, the results enabled us to select the radio-purest construction materials, targeting a $^{222}$Rn activity concentration of 10 $渭$Bq/kg in 3.2 t of xenon. The knowledge of the distribution of the $^{222}$Rn sources allowed us to selectively eliminate critical components in the course of the experiment. The predictions from the emanation measurements were compared to data of the $^{222}$Rn activity concentration in XENON1T. The final $^{222}$Rn activity concentration of (4.5 $\pm$ 0.1) $渭$Bq/kg in the target of XENON1T is the lowest ever achieved in a xenon dark matter experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.13981v3-abstract-full').style.display = 'none'; document.getElementById('2009.13981v3-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 81, 337 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.00794">arXiv:2009.00794</a> <span> [<a href="https://arxiv.org/pdf/2009.00794">pdf</a>, <a href="https://arxiv.org/ps/2009.00794">ps</a>, <a href="https://arxiv.org/format/2009.00794">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> The Hyper-Kamiokande Experiment -- Snowmass LOI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Collaboration%2C+H">Hyper-Kamiokande Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Adrich%2C+P">P. Adrich</a>, <a href="/search/physics?searchtype=author&query=Aihara%2C+H">H. Aihara</a>, <a href="/search/physics?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/physics?searchtype=author&query=Alekseev%2C+I">I. Alekseev</a>, <a href="/search/physics?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/physics?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/physics?searchtype=author&query=Anthony%2C+L+H+V">L. H. V. Anthony</a>, <a href="/search/physics?searchtype=author&query=Araya%2C+A">A. Araya</a>, <a href="/search/physics?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/physics?searchtype=author&query=Aushev%2C+V">V. Aushev</a>, <a href="/search/physics?searchtype=author&query=Bandac%2C+I">I. Bandac</a>, <a href="/search/physics?searchtype=author&query=Barbi%2C+M">M. Barbi</a>, <a href="/search/physics?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/physics?searchtype=author&query=Batkiewicz-Kwasniak%2C+M">M. Batkiewicz-Kwasniak</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">M. Bellato</a>, <a href="/search/physics?searchtype=author&query=Berardi%2C+V">V. Berardi</a>, <a href="/search/physics?searchtype=author&query=Bernard%2C+L">L. Bernard</a>, <a href="/search/physics?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/physics?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/physics?searchtype=author&query=Bhadra%2C+S">S. Bhadra</a>, <a href="/search/physics?searchtype=author&query=Bian%2C+J">J. Bian</a>, <a href="/search/physics?searchtype=author&query=Blanchet%2C+A">A. Blanchet</a> , et al. (366 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.00794v1-abstract-short" style="display: inline;"> Hyper-Kamiokande is the next generation underground water Cherenkov detector that builds on the highly successful Super-Kamiokande experiment. The detector which has an 8.4~times larger effective volume than its predecessor will be located along the T2K neutrino beamline and utilize an upgraded J-PARC beam with 2.6~times beam power. Hyper-K's low energy threshold combined with the very large fiduc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.00794v1-abstract-full').style.display = 'inline'; document.getElementById('2009.00794v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.00794v1-abstract-full" style="display: none;"> Hyper-Kamiokande is the next generation underground water Cherenkov detector that builds on the highly successful Super-Kamiokande experiment. The detector which has an 8.4~times larger effective volume than its predecessor will be located along the T2K neutrino beamline and utilize an upgraded J-PARC beam with 2.6~times beam power. Hyper-K's low energy threshold combined with the very large fiducial volume make the detector unique, that is expected to acquire an unprecedented exposure of 3.8~Mton$\cdot$year over a period of 20~years of operation. Hyper-Kamiokande combines an extremely diverse science program including nucleon decays, long-baseline neutrino oscillations, atmospheric neutrinos, and neutrinos from astrophysical origins. The scientific scope of this program is highly complementary to liquid-argon detectors for example in sensitivity to nucleon decay channels or supernova detection modes. Hyper-Kamiokande construction has started in early 2020 and the experiment is expected to start operations in 2027. The Hyper-Kamiokande collaboration is presently being formed amongst groups from 19 countries including the United States, whose community has a long history of making significant contributions to the neutrino physics program in Japan. US physicists have played leading roles in the Kamiokande, Super-Kamiokande, EGADS, K2K, and T2K programs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.00794v1-abstract-full').style.display = 'none'; document.getElementById('2009.00794v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, prepared as Snowmass2021 LOI</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.16046">arXiv:2007.16046</a> <span> [<a href="https://arxiv.org/pdf/2007.16046">pdf</a>, <a href="https://arxiv.org/ps/2007.16046">ps</a>, <a href="https://arxiv.org/format/2007.16046">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <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"> Search for event bursts in XMASS-I associated with gravitational-wave events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XMASS+Collaboration"> XMASS Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/physics?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/physics?searchtype=author&query=Kobayashi%2C+K">K. Kobayashi</a>, <a href="/search/physics?searchtype=author&query=Kobayashi%2C+M">M. Kobayashi</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Ogawa%2C+H">H. Ogawa</a>, <a href="/search/physics?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+T">T. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">A. Takeda</a>, <a href="/search/physics?searchtype=author&query=Tasaka%2C+S">S. Tasaka</a>, <a href="/search/physics?searchtype=author&query=Yamashita%2C+M">M. Yamashita</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+B+S">B. S. Yang</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+N+Y">N. Y. Kim</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+Y+D">Y. D. Kim</a>, <a href="/search/physics?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/physics?searchtype=author&query=Kanzawa%2C+K">K. Kanzawa</a>, <a href="/search/physics?searchtype=author&query=Masuda%2C+K">K. Masuda</a>, <a href="/search/physics?searchtype=author&query=Martens%2C+K">K. Martens</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+Y">Y. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Xu%2C+B+D">B. D. Xu</a> , et al. (12 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="2007.16046v2-abstract-short" style="display: inline;"> We performed a search for event bursts in the XMASS-I detector associated with 11 gravitational-wave events detected during LIGO/Virgo's O1 and O2 periods. Simple and loose cuts were applied to the data collected in the full 832 kg xenon volume around the detection time of each gravitational-wave event. The data were divided into four energy regions ranging from keV to MeV. Without assuming any pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.16046v2-abstract-full').style.display = 'inline'; document.getElementById('2007.16046v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.16046v2-abstract-full" style="display: none;"> We performed a search for event bursts in the XMASS-I detector associated with 11 gravitational-wave events detected during LIGO/Virgo's O1 and O2 periods. Simple and loose cuts were applied to the data collected in the full 832 kg xenon volume around the detection time of each gravitational-wave event. The data were divided into four energy regions ranging from keV to MeV. Without assuming any particular burst models, we looked for event bursts in sliding windows with various time width from 0.02 to 10 s. The search was conducted in a time window between $-$400 and $+$10,000 s from each gravitational-wave event. For the binary neutron star merger GW170817, no significant event burst was observed in the XMASS-I detector and we set 90% confidence level upper limits on neutrino fluence for the sum of all the neutrino flavors via coherent elastic neutrino-nucleus scattering. The obtained upper limit was (1.3-2.1)$\times 10^{11}$ cm$^{-2}$ under the assumption of a Fermi-Dirac spectrum with average neutrino energy of 20 MeV. The neutrino fluence limits for mono-energetic neutrinos in the energy range between 14 and 100 MeV were also calculated. Among the other 10 gravitational wave events detected as the binary black hole mergers, a burst candidate with a 3.0$蟽$ significance was found at 1801.95-1803.95 s in the analysis for GW151012. However, no significant deviation from the background in the reconstructed energy and position distributions was found. Considering the additional look-elsewhere effect of analyzing the 11 GW events, the significance of finding such a burst candidate associated with any of them is 2.1$蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.16046v2-abstract-full').style.display = 'none'; document.getElementById('2007.16046v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">8 pages, 12 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/2007.08796">arXiv:2007.08796</a> <span> [<a href="https://arxiv.org/pdf/2007.08796">pdf</a>, <a href="https://arxiv.org/format/2007.08796">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2020/11/031">10.1088/1475-7516/2020/11/031 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Projected WIMP Sensitivity of the XENONnT Dark Matter Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+XENON+collaboration"> The XENON collaboration</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Alfonsi%2C+M">M. Alfonsi</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amaro%2C+F+D">F. D. Amaro</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/physics?searchtype=author&query=Barge%2C+D">D. Barge</a>, <a href="/search/physics?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/physics?searchtype=author&query=Bauermeister%2C+B">B. Bauermeister</a>, <a href="/search/physics?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/physics?searchtype=author&query=Benabderrahmane%2C+M+L">M. L. Benabderrahmane</a>, <a href="/search/physics?searchtype=author&query=Berger%2C+T">T. Berger</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/physics?searchtype=author&query=Brown%2C+E">E. Brown</a>, <a href="/search/physics?searchtype=author&query=Bruenner%2C+S">S. Bruenner</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/physics?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/physics?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a>, <a href="/search/physics?searchtype=author&query=Cichon%2C+D">D. Cichon</a> , et al. (115 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="2007.08796v2-abstract-short" style="display: inline;"> XENONnT is a dark matter direct detection experiment, utilizing 5.9 t of instrumented liquid xenon, located at the INFN Laboratori Nazionali del Gran Sasso. In this work, we predict the experimental background and project the sensitivity of XENONnT to the detection of weakly interacting massive particles (WIMPs). The expected average differential background rate in the energy region of interest, c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.08796v2-abstract-full').style.display = 'inline'; document.getElementById('2007.08796v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.08796v2-abstract-full" style="display: none;"> XENONnT is a dark matter direct detection experiment, utilizing 5.9 t of instrumented liquid xenon, located at the INFN Laboratori Nazionali del Gran Sasso. In this work, we predict the experimental background and project the sensitivity of XENONnT to the detection of weakly interacting massive particles (WIMPs). The expected average differential background rate in the energy region of interest, corresponding to (1, 13) keV and (4, 50) keV for electronic and nuclear recoils, amounts to $12.3 \pm 0.6$ (keV t y)$^{-1}$ and $(2.2\pm 0.5)\times 10^{-3}$ (keV t y)$^{-1}$, respectively, in a 4 t fiducial mass. We compute unified confidence intervals using the profile construction method, in order to ensure proper coverage. With the exposure goal of 20 t$\,$y, the expected sensitivity to spin-independent WIMP-nucleon interactions reaches a cross-section of $1.4\times10^{-48}$ cm$^2$ for a 50 GeV/c$^2$ mass WIMP at 90% confidence level, more than one order of magnitude beyond the current best limit, set by XENON1T. In addition, we show that for a 50 GeV/c$^2$ WIMP with cross-sections above $2.6\times10^{-48}$ cm$^2$ ($5.0\times10^{-48}$ cm$^2$) the median XENONnT discovery significance exceeds 3$蟽$ (5$蟽$). The expected sensitivity to the spin-dependent WIMP coupling to neutrons (protons) reaches $2.2\times10^{-43}$ cm$^2$ ($6.0\times10^{-42}$ cm$^2$). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.08796v2-abstract-full').style.display = 'none'; document.getElementById('2007.08796v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP11(2020)031 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.08718">arXiv:2007.08718</a> <span> [<a href="https://arxiv.org/pdf/2007.08718">pdf</a>, <a href="https://arxiv.org/format/2007.08718">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2020.164435">10.1016/j.nima.2020.164435 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radiation Damage Effects on Double-SOI Pixel Sensors for X-ray Astronomy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Hagino%2C+K">Kouichi Hagino</a>, <a href="/search/physics?searchtype=author&query=Yarita%2C+K">Keigo Yarita</a>, <a href="/search/physics?searchtype=author&query=Negishi%2C+K">Kousuke Negishi</a>, <a href="/search/physics?searchtype=author&query=Oono%2C+K">Kenji Oono</a>, <a href="/search/physics?searchtype=author&query=Hayashida%2C+M">Mitsuki Hayashida</a>, <a href="/search/physics?searchtype=author&query=Kitajima%2C+M">Masatoshi Kitajima</a>, <a href="/search/physics?searchtype=author&query=Kohmura%2C+T">Takayoshi Kohmura</a>, <a href="/search/physics?searchtype=author&query=Tsuru%2C+T+G">Takeshi G. Tsuru</a>, <a href="/search/physics?searchtype=author&query=Tanaka%2C+T">Takaaki Tanaka</a>, <a href="/search/physics?searchtype=author&query=Uchida%2C+H">Hiroyuki Uchida</a>, <a href="/search/physics?searchtype=author&query=Kayama%2C+K">Kazuho Kayama</a>, <a href="/search/physics?searchtype=author&query=Amano%2C+Y">Yuki Amano</a>, <a href="/search/physics?searchtype=author&query=Kodama%2C+R">Ryota Kodama</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">Ayaki Takeda</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+K">Koji Mori</a>, <a href="/search/physics?searchtype=author&query=Nishioka%2C+Y">Yusuke Nishioka</a>, <a href="/search/physics?searchtype=author&query=Yukumoto%2C+M">Masataka Yukumoto</a>, <a href="/search/physics?searchtype=author&query=Hida%2C+T">Takahiro Hida</a>, <a href="/search/physics?searchtype=author&query=Arai%2C+Y">Yasuo Arai</a>, <a href="/search/physics?searchtype=author&query=Kurachi%2C+I">Ikuo Kurachi</a>, <a href="/search/physics?searchtype=author&query=Hamano%2C+T">Tsuyoshi Hamano</a>, <a href="/search/physics?searchtype=author&query=Kitamura%2C+H">Hisashi Kitamura</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="2007.08718v1-abstract-short" style="display: inline;"> The X-ray SOI pixel sensor onboard the FORCE satellite will be placed in the low earth orbit and will consequently suffer from the radiation effects mainly caused by geomagnetically trapped cosmic-ray protons. Based on previous studies on the effects of radiation on SOI pixel sensors, the positive charges trapped in the oxide layer significantly affect the performance of the sensor. To improve the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.08718v1-abstract-full').style.display = 'inline'; document.getElementById('2007.08718v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.08718v1-abstract-full" style="display: none;"> The X-ray SOI pixel sensor onboard the FORCE satellite will be placed in the low earth orbit and will consequently suffer from the radiation effects mainly caused by geomagnetically trapped cosmic-ray protons. Based on previous studies on the effects of radiation on SOI pixel sensors, the positive charges trapped in the oxide layer significantly affect the performance of the sensor. To improve the radiation hardness of the SOI pixel sensors, we introduced a double-SOI (D-SOI) structure containing an additional middle Si layer in the oxide layer. The negative potential applied on the middle Si layer compensates for the radiation effects, due to the trapped positive charges. Although the radiation hardness of the D-SOI pixel sensors for applications in high-energy accelerators has been evaluated, radiation effects for astronomical application in the D-SOI sensors has not been evaluated thus far. To evaluate the radiation effects of the D-SOI sensor, we perform an irradiation experiment using a 6-MeV proton beam with a total dose of ~ 5 krad, corresponding to a few tens of years of in-orbit operation. This experiment indicates an improvement in the radiation hardness of the X- ray D-SOI devices. On using an irradiation of 5 krad on the D-SOI device, the energy resolution in the full-width half maximum for the 5.9-keV X-ray increases by 7 $\pm$ 2%, and the chip output gain decreases by 0.35 $\pm$ 0.09%. The physical mechanism of the gain degradation is also investigated; it is found that the gain degradation is caused by an increase in the parasitic capacitance due to the enlarged buried n-well. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.08718v1-abstract-full').style.display = 'none'; document.getElementById('2007.08718v1-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">7 pages, 7 figures, accepted for publication in NIM A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.00922">arXiv:2006.00922</a> <span> [<a href="https://arxiv.org/pdf/2006.00922">pdf</a>, <a href="https://arxiv.org/ps/2006.00922">ps</a>, <a href="https://arxiv.org/format/2006.00922">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> </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/10.1088/1748-0221/15/09/P09027">10.1088/1748-0221/15/09/P09027 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Development of low-background photomultiplier tubes for liquid xenon detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XMASS+Collaboration"> XMASS Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Chen%2C+Y">Y. Chen</a>, <a href="/search/physics?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/physics?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/physics?searchtype=author&query=Imaizumi%2C+S">S. Imaizumi</a>, <a href="/search/physics?searchtype=author&query=Kato%2C+N">N. Kato</a>, <a href="/search/physics?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/physics?searchtype=author&query=Kobayashi%2C+K">K. Kobayashi</a>, <a href="/search/physics?searchtype=author&query=Kobayashi%2C+M">M. Kobayashi</a>, <a href="/search/physics?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/physics?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/physics?searchtype=author&query=Sato%2C+K">K. Sato</a>, <a href="/search/physics?searchtype=author&query=Sekiya%2C+H">H. Sekiya</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+T">T. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Takeda%2C+A">A. Takeda</a>, <a href="/search/physics?searchtype=author&query=Tasaka%2C+S">S. Tasaka</a>, <a href="/search/physics?searchtype=author&query=Yamashita%2C+M">M. Yamashita</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+B+S">B. S. Yang</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+N+Y">N. Y. Kim</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+Y+D">Y. D. Kim</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+Y+H">Y. H. Kim</a>, <a href="/search/physics?searchtype=author&query=Ishii%2C+R">R. Ishii</a>, <a href="/search/physics?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/physics?searchtype=author&query=Kanzawa%2C+K">K. Kanzawa</a> , et al. (14 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="2006.00922v2-abstract-short" style="display: inline;"> We successfully developed a new photomultiplier tube (PMT) with a three-inch diameter, convex-shaped photocathode, R13111. Its prominent features include good performance and ultra-low radioactivity. The convex-shaped photocathode realized a large photon acceptance and good timing resolution. Low radioactivity was achieved by three factors: (1) the glass material was synthesized using low-radioact… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.00922v2-abstract-full').style.display = 'inline'; document.getElementById('2006.00922v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.00922v2-abstract-full" style="display: none;"> We successfully developed a new photomultiplier tube (PMT) with a three-inch diameter, convex-shaped photocathode, R13111. Its prominent features include good performance and ultra-low radioactivity. The convex-shaped photocathode realized a large photon acceptance and good timing resolution. Low radioactivity was achieved by three factors: (1) the glass material was synthesized using low-radioactive-contamination material; (2) the photocathode was produced with $^{39}$K-enriched potassium; and (3) the purest grade of aluminum material was used for the vacuum seal. As a result each R13111 PMT contains only about 0.4 mBq of $^{226}$Ra, less than 2 mBq of $^{238}$U, 0.3 mBq of $^{228}$Ra, 2 mBq of $^{40}$K and 0.2 mBq of $^{60}$Co. We also examined and resolved the intrinsic leakage of Xe gas into PMTs that was observed in several older models. We thus succeeded in developing a PMT that has low background, large angular acceptance with high collection efficiency, good timing resolution, and long-term stable operation. These features are highly desirable for experiments searching for rare events beyond the standard model, such as dark matter particle interactions and neutrinoless double beta decay events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.00922v2-abstract-full').style.display = 'none'; document.getElementById('2006.00922v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Takeda%2C+A&start=50" 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