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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=Piepke%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Piepke%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Piepke%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </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/2412.04854">arXiv:2412.04854</a> <span> [<a href="https://arxiv.org/pdf/2412.04854">pdf</a>, <a href="https://arxiv.org/format/2412.04854">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> First search for atmospheric millicharged particles with the LUX-ZEPLIN experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a> , et al. (193 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="2412.04854v2-abstract-short" style="display: inline;"> We report on a search for millicharged particles (mCPs) produced in cosmic ray proton atmospheric interactions using data collected during the first science run of the LUX-ZEPLIN experiment. The mCPs produced by two processes -- meson decay and proton bremsstrahlung -- are considered in this study. This search utilized a novel signature unique to liquid xenon (LXe) time projection chambers (TPCs),… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04854v2-abstract-full').style.display = 'inline'; document.getElementById('2412.04854v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.04854v2-abstract-full" style="display: none;"> We report on a search for millicharged particles (mCPs) produced in cosmic ray proton atmospheric interactions using data collected during the first science run of the LUX-ZEPLIN experiment. The mCPs produced by two processes -- meson decay and proton bremsstrahlung -- are considered in this study. This search utilized a novel signature unique to liquid xenon (LXe) time projection chambers (TPCs), allowing sensitivity to mCPs with masses ranging from 10 to 1000 MeV/c$^2$ and fractional charges between 0.001 and 0.02 of the electron charge e. With an exposure of 60 live days and a 5.5 tonne fiducial mass, we observed no significant excess over background. This represents the first experimental search for atmospheric mCPs and the first search for mCPs using an underground LXe experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04854v2-abstract-full').style.display = 'none'; document.getElementById('2412.04854v2-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 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/hep-ex?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/hep-ex?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/hep-ex?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/hep-ex?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/hep-ex?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/hep-ex?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/hep-ex?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/hep-ex?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/hep-ex?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/hep-ex?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/hep-ex?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/hep-ex?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/2410.17036">arXiv:2410.17036</a> <span> [<a href="https://arxiv.org/pdf/2410.17036">pdf</a>, <a href="https://arxiv.org/format/2410.17036">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Dark Matter Search Results from 4.2 Tonne-Years of Exposure of the LUX-ZEPLIN (LZ) Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a> , et al. (193 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="2410.17036v2-abstract-short" style="display: inline;"> We report results of a search for nuclear recoils induced by weakly interacting massive particle (WIMP) dark matter using the LUX-ZEPLIN (LZ) two-phase xenon time projection chamber. This analysis uses a total exposure of $4.2\pm0.1$ tonne-years from 280 live days of LZ operation, of which $3.3\pm0.1$ tonne-years and 220 live days are new. A technique to actively tag background electronic recoils… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17036v2-abstract-full').style.display = 'inline'; document.getElementById('2410.17036v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.17036v2-abstract-full" style="display: none;"> We report results of a search for nuclear recoils induced by weakly interacting massive particle (WIMP) dark matter using the LUX-ZEPLIN (LZ) two-phase xenon time projection chamber. This analysis uses a total exposure of $4.2\pm0.1$ tonne-years from 280 live days of LZ operation, of which $3.3\pm0.1$ tonne-years and 220 live days are new. A technique to actively tag background electronic recoils from $^{214}$Pb $尾$ decays is featured for the first time. Enhanced electron-ion recombination is observed in two-neutrino double electron capture decays of $^{124}$Xe, representing a noteworthy new background. After removal of artificial signal-like events injected into the data set to mitigate analyzer bias, we find no evidence for an excess over expected backgrounds. World-leading constraints are placed on spin-independent (SI) and spin-dependent WIMP-nucleon cross sections for masses $\geq$9 GeV/$c^2$. The strongest SI exclusion set is $2.1\times10^{-48}$ cm$^{2}$ at the 90% confidence level at a mass of 36 GeV/$c^2$, and the best SI median sensitivity achieved is $5.0\times10^{-48}$ cm$^{2}$ for a mass of 40 GeV/$c^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17036v2-abstract-full').style.display = 'none'; document.getElementById('2410.17036v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">9 pages, 7 figures. See https://www.hepdata.net/record/155182 for a data release related to this paper</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.12874">arXiv:2406.12874</a> <span> [<a href="https://arxiv.org/pdf/2406.12874">pdf</a>, <a href="https://arxiv.org/format/2406.12874">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/10.1088/1748-0221/19/08/P08027">10.1088/1748-0221/19/08/P08027 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Design, Implementation, and Performance of the LZ Calibration Systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a> , et al. (179 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="2406.12874v3-abstract-short" style="display: inline;"> LUX-ZEPLIN (LZ) is a tonne-scale experiment searching for direct dark matter interactions and other rare events. It is located at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, USA. The core of the LZ detector is a dual-phase xenon time projection chamber (TPC), designed with the primary goal of detecting Weakly Interacting Massive Particles (WIMPs) via their induced low e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12874v3-abstract-full').style.display = 'inline'; document.getElementById('2406.12874v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.12874v3-abstract-full" style="display: none;"> LUX-ZEPLIN (LZ) is a tonne-scale experiment searching for direct dark matter interactions and other rare events. It is located at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, USA. The core of the LZ detector is a dual-phase xenon time projection chamber (TPC), designed with the primary goal of detecting Weakly Interacting Massive Particles (WIMPs) via their induced low energy nuclear recoils. Surrounding the TPC, two veto detectors immersed in an ultra-pure water tank enable reducing background events to enhance the discovery potential. Intricate calibration systems are purposely designed to precisely understand the responses of these three detector volumes to various types of particle interactions and to demonstrate LZ's ability to discriminate between signals and backgrounds. In this paper, we present a comprehensive discussion of the key features, requirements, and performance of the LZ calibration systems, which play a crucial role in enabling LZ's WIMP-search and its broad science program. The thorough description of these calibration systems, with an emphasis on their novel aspects, is valuable for future calibration efforts in direct dark matter and other rare-event search experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12874v3-abstract-full').style.display = 'none'; document.getElementById('2406.12874v3-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 May, 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">Journal ref:</span> JINST 19 P08027 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.02441">arXiv:2406.02441</a> <span> [<a href="https://arxiv.org/pdf/2406.02441">pdf</a>, <a href="https://arxiv.org/format/2406.02441">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s42005-024-01774-8">10.1038/s42005-024-01774-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the Scalar WIMP-Pion Coupling with the first LUX-ZEPLIN data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Bishop%2C+E+J">E. J. Bishop</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a> , et al. (178 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="2406.02441v1-abstract-short" style="display: inline;"> Weakly interacting massive particles (WIMPs) may interact with a virtual pion that is exchanged between nucleons. This interaction channel is important to consider in models where the spin-independent isoscalar channel is suppressed. Using data from the first science run of the LUX-ZEPLIN dark matter experiment, containing 60 live days of data in a 5.5~tonne fiducial mass of liquid xenon, we repor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.02441v1-abstract-full').style.display = 'inline'; document.getElementById('2406.02441v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.02441v1-abstract-full" style="display: none;"> Weakly interacting massive particles (WIMPs) may interact with a virtual pion that is exchanged between nucleons. This interaction channel is important to consider in models where the spin-independent isoscalar channel is suppressed. Using data from the first science run of the LUX-ZEPLIN dark matter experiment, containing 60 live days of data in a 5.5~tonne fiducial mass of liquid xenon, we report the results on a search for WIMP-pion interactions. We observe no significant excess and set an upper limit of $1.5\times10^{-46}$~cm$^2$ at a 90\% confidence level for a WIMP mass of 33~GeV/c$^2$ for this interaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.02441v1-abstract-full').style.display = 'none'; document.getElementById('2406.02441v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 June, 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">Journal ref:</span> Commun Phys 7, 292 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.19419">arXiv:2405.19419</a> <span> [<a href="https://arxiv.org/pdf/2405.19419">pdf</a>, <a href="https://arxiv.org/format/2405.19419">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 - Phenomenology">hep-ph</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 Theory">nucl-th</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.110.093002">10.1103/PhysRevD.110.093002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supernova electron-neutrino interactions with xenon in the nEXO detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=nEXO+Collaboration"> nEXO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Hedges%2C+S">S. Hedges</a>, <a href="/search/hep-ex?searchtype=author&query=Kharusi%2C+S+A">S. Al Kharusi</a>, <a href="/search/hep-ex?searchtype=author&query=Angelico%2C+E">E. Angelico</a>, <a href="/search/hep-ex?searchtype=author&query=Brodsky%2C+J+P">J. P. Brodsky</a>, <a href="/search/hep-ex?searchtype=author&query=Richardson%2C+G">G. Richardson</a>, <a href="/search/hep-ex?searchtype=author&query=Wilde%2C+S">S. Wilde</a>, <a href="/search/hep-ex?searchtype=author&query=Amy%2C+A">A. Amy</a>, <a href="/search/hep-ex?searchtype=author&query=Anker%2C+A">A. Anker</a>, <a href="/search/hep-ex?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/hep-ex?searchtype=author&query=Arsenault%2C+P">P. Arsenault</a>, <a href="/search/hep-ex?searchtype=author&query=Atencio%2C+A">A. Atencio</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Bane%2C+J">J. Bane</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Bolotnikov%2C+A">A. Bolotnikov</a>, <a href="/search/hep-ex?searchtype=author&query=Breslin%2C+J">J. Breslin</a>, <a href="/search/hep-ex?searchtype=author&query=Breur%2C+P+A">P. A. Breur</a>, <a href="/search/hep-ex?searchtype=author&query=Brown%2C+E">E. Brown</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Caden%2C+E">E. Caden</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+L+Q">L. Q. Cao</a> , et al. (122 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.19419v2-abstract-short" style="display: inline;"> Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-$尾$ decay detector (~5 metric ton, 90% ${}^{136}$Xe, 10% ${}^{134}$Xe) to evaluate its sensitivity to supernova neutrinos. Predictions for event rates and detectable signatures were modeled using the Model of Argon Reaction Low Energy Yields (MARLEY) event generator. We find good agreement… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19419v2-abstract-full').style.display = 'inline'; document.getElementById('2405.19419v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.19419v2-abstract-full" style="display: none;"> Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-$尾$ decay detector (~5 metric ton, 90% ${}^{136}$Xe, 10% ${}^{134}$Xe) to evaluate its sensitivity to supernova neutrinos. Predictions for event rates and detectable signatures were modeled using the Model of Argon Reaction Low Energy Yields (MARLEY) event generator. We find good agreement between MARLEY's predictions and existing theoretical calculations of the inclusive cross sections at supernova neutrino energies. The interactions modeled by MARLEY were simulated within the nEXO simulation framework and were run through an example reconstruction algorithm to determine the detector's efficiency for reconstructing these events. The simulated data, incorporating the detector response, were used to study the ability of nEXO to reconstruct the incident electron-neutrino spectrum and these results were extended to a larger xenon detector of the same isotope enrichment. We estimate that nEXO will be able to observe electron-neutrino interactions with xenon from supernovae as far as 5-8 kpc from Earth, while the ability to reconstruct incident electron-neutrino spectrum parameters from observed interactions in nEXO is limited to closer supernovae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19419v2-abstract-full').style.display = 'none'; document.getElementById('2405.19419v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LLNL-JRNL-864783 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 110, 093002 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.14732">arXiv:2405.14732</a> <span> [<a href="https://arxiv.org/pdf/2405.14732">pdf</a>, <a href="https://arxiv.org/format/2405.14732">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 Data Acquisition System of the LZ Dark Matter Detector: FADR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a> , et al. (191 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.14732v3-abstract-short" style="display: inline;"> The Data Acquisition System (DAQ) for the LUX-ZEPLIN (LZ) dark matter detector is described. The signals from 745 PMTs, distributed across three subsystems, are sampled with 100-MHz 32-channel digitizers (DDC-32s). A basic waveform analysis is carried out on the on-board Field Programmable Gate Arrays (FPGAs) to extract information about the observed scintillation and electroluminescence signals.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14732v3-abstract-full').style.display = 'inline'; document.getElementById('2405.14732v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.14732v3-abstract-full" style="display: none;"> The Data Acquisition System (DAQ) for the LUX-ZEPLIN (LZ) dark matter detector is described. The signals from 745 PMTs, distributed across three subsystems, are sampled with 100-MHz 32-channel digitizers (DDC-32s). A basic waveform analysis is carried out on the on-board Field Programmable Gate Arrays (FPGAs) to extract information about the observed scintillation and electroluminescence signals. This information is used to determine if the digitized waveforms should be preserved for offline analysis. The system is designed around the Kintex-7 FPGA. In addition to digitizing the PMT signals and providing basic event selection in real time, the flexibility provided by the use of FPGAs allows us to monitor the performance of the detector and the DAQ in parallel to normal data acquisition. The hardware and software/firmware of this FPGA-based Architecture for Data acquisition and Realtime monitoring (FADR) are discussed and performance measurements are described. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14732v3-abstract-full').style.display = 'none'; document.getElementById('2405.14732v3-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 24 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/2404.17666">arXiv:2404.17666</a> <span> [<a href="https://arxiv.org/pdf/2404.17666">pdf</a>, <a href="https://arxiv.org/format/2404.17666">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.133.221801">10.1103/PhysRevLett.133.221801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints On Covariant WIMP-Nucleon Effective Field Theory Interactions from the First Science Run of the LUX-ZEPLIN Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Bishop%2C+E+J">E. J. Bishop</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a> , et al. (179 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="2404.17666v1-abstract-short" style="display: inline;"> The first science run of the LUX-ZEPLIN (LZ) experiment, a dual-phase xenon time project chamber operating in the Sanford Underground Research Facility in South Dakota, USA, has reported leading limits on spin-independent WIMP-nucleon interactions and interactions described from a non-relativistic effective field theory (NREFT). Using the same 5.5~t fiducial mass and 60 live days of exposure we re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17666v1-abstract-full').style.display = 'inline'; document.getElementById('2404.17666v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.17666v1-abstract-full" style="display: none;"> The first science run of the LUX-ZEPLIN (LZ) experiment, a dual-phase xenon time project chamber operating in the Sanford Underground Research Facility in South Dakota, USA, has reported leading limits on spin-independent WIMP-nucleon interactions and interactions described from a non-relativistic effective field theory (NREFT). Using the same 5.5~t fiducial mass and 60 live days of exposure we report on the results of a relativistic extension to the NREFT. We present constraints on couplings from covariant interactions arising from the coupling of vector, axial currents, and electric dipole moments of the nucleon to the magnetic and electric dipole moments of the WIMP which cannot be described by recasting previous results described by an NREFT. Using a profile-likelihood ratio analysis, in an energy region between 0~keV$_\text{nr}$ to 270~keV$_\text{nr}$, we report 90% confidence level exclusion limits on the coupling strength of five interactions in both the isoscalar and isovector bases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17666v1-abstract-full').style.display = 'none'; document.getElementById('2404.17666v1-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 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">7 pages, 4 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. 133, 221801 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.08865">arXiv:2402.08865</a> <span> [<a href="https://arxiv.org/pdf/2402.08865">pdf</a>, <a href="https://arxiv.org/format/2402.08865">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.112010">10.1103/PhysRevD.109.112010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New constraints on ultraheavy dark matter from the LZ experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/hep-ex?searchtype=author&query=Brew%2C+C+A+J">C. A. J. Brew</a> , et al. (174 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="2402.08865v1-abstract-short" style="display: inline;"> Searches for dark matter with liquid xenon time projection chamber experiments have traditionally focused on the region of the parameter space that is characteristic of weakly interacting massive particles, ranging from a few GeV/$c^2$ to a few TeV/$c^2$. Models of dark matter with a mass much heavier than this are well motivated by early production mechanisms different from the standard thermal f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08865v1-abstract-full').style.display = 'inline'; document.getElementById('2402.08865v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08865v1-abstract-full" style="display: none;"> Searches for dark matter with liquid xenon time projection chamber experiments have traditionally focused on the region of the parameter space that is characteristic of weakly interacting massive particles, ranging from a few GeV/$c^2$ to a few TeV/$c^2$. Models of dark matter with a mass much heavier than this are well motivated by early production mechanisms different from the standard thermal freeze-out, but they have generally been less explored experimentally. In this work, we present a re-analysis of the first science run (SR1) of the LZ experiment, with an exposure of $0.9$ tonne$\times$year, to search for ultraheavy particle dark matter. The signal topology consists of multiple energy deposits in the active region of the detector forming a straight line, from which the velocity of the incoming particle can be reconstructed on an event-by-event basis. Zero events with this topology were observed after applying the data selection calibrated on a simulated sample of signal-like events. New experimental constraints are derived, which rule out previously unexplored regions of the dark matter parameter space of spin-independent interactions beyond a mass of 10$^{17}$ GeV/$c^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08865v1-abstract-full').style.display = 'none'; document.getElementById('2402.08865v1-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 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">9 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109, 112010 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.02030">arXiv:2312.02030</a> <span> [<a href="https://arxiv.org/pdf/2312.02030">pdf</a>, <a href="https://arxiv.org/format/2312.02030">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.092003">10.1103/PhysRevD.109.092003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Constraints on WIMP-Nucleon Effective Field Theory Couplings in an Extended Energy Region From LUX-ZEPLIN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=LZ+Collaboration"> LZ Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a> , et al. (175 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.02030v2-abstract-short" style="display: inline;"> Following the first science results of the LUX-ZEPLIN (LZ) experiment, a dual-phase xenon time projection chamber operating from the Sanford Underground Research Facility in Lead, South Dakota, USA, we report the initial limits on a model-independent non-relativistic effective field theory describing the complete set of possible interactions of a weakly interacting massive particle (WIMP) with a n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.02030v2-abstract-full').style.display = 'inline'; document.getElementById('2312.02030v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.02030v2-abstract-full" style="display: none;"> Following the first science results of the LUX-ZEPLIN (LZ) experiment, a dual-phase xenon time projection chamber operating from the Sanford Underground Research Facility in Lead, South Dakota, USA, we report the initial limits on a model-independent non-relativistic effective field theory describing the complete set of possible interactions of a weakly interacting massive particle (WIMP) with a nucleon. These results utilize the same 5.5 t fiducial mass and 60 live days of exposure collected for the LZ spin-independent and spin-dependent analyses while extending the upper limit of the energy region of interest by a factor of 7.5 to 270 keVnr. No significant excess in this high energy region is observed. Using a profile-likelihood ratio analysis, we report 90% confidence level exclusion limits on the coupling of each individual non-relativistic WIMP-nucleon operator for both elastic and inelastic interactions in the isoscalar and isovector bases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.02030v2-abstract-full').style.display = 'none'; document.getElementById('2312.02030v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109, 092003 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.15753">arXiv:2307.15753</a> <span> [<a href="https://arxiv.org/pdf/2307.15753">pdf</a>, <a href="https://arxiv.org/format/2307.15753">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> </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.108.072006">10.1103/PhysRevD.108.072006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for new physics in low-energy electron recoils from the first LZ exposure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a> , et al. (178 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="2307.15753v2-abstract-short" style="display: inline;"> The LUX-ZEPLIN (LZ) experiment is a dark matter detector centered on a dual-phase xenon time projection chamber. We report searches for new physics appearing through few-keV-scale electron recoils, using the experiment's first exposure of 60 live days and a fiducial mass of 5.5t. The data are found to be consistent with a background-only hypothesis, and limits are set on models for new physics inc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.15753v2-abstract-full').style.display = 'inline'; document.getElementById('2307.15753v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.15753v2-abstract-full" style="display: none;"> The LUX-ZEPLIN (LZ) experiment is a dark matter detector centered on a dual-phase xenon time projection chamber. We report searches for new physics appearing through few-keV-scale electron recoils, using the experiment's first exposure of 60 live days and a fiducial mass of 5.5t. The data are found to be consistent with a background-only hypothesis, and limits are set on models for new physics including solar axion electron coupling, solar neutrino magnetic moment and millicharge, and electron couplings to galactic axion-like particles and hidden photons. Similar limits are set on weakly interacting massive particle (WIMP) dark matter producing signals through ionized atomic states from the Migdal effect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.15753v2-abstract-full').style.display = 'none'; document.getElementById('2307.15753v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">13 pages, 10 figures. See https://tinyurl.com/LZDataReleaseRun1ER for a data release related to this paper</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 108, 072006 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.06311">arXiv:2303.06311</a> <span> [<a href="https://arxiv.org/pdf/2303.06311">pdf</a>, <a href="https://arxiv.org/format/2303.06311">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="Machine Learning">cs.LG</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/10.1088/1748-0221/18/06/P06005">10.1088/1748-0221/18/06/P06005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Generative Adversarial Networks for Scintillation Signal Simulation in EXO-200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Li%2C+S">S. Li</a>, <a href="/search/hep-ex?searchtype=author&query=Ostrovskiy%2C+I">I. Ostrovskiy</a>, <a href="/search/hep-ex?searchtype=author&query=Li%2C+Z">Z. Li</a>, <a href="/search/hep-ex?searchtype=author&query=Yang%2C+L">L. Yang</a>, <a href="/search/hep-ex?searchtype=author&query=Kharusi%2C+S+A">S. Al Kharusi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Darroch%2C+L">L. Darroch</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a> , et al. (65 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="2303.06311v2-abstract-short" style="display: inline;"> Generative Adversarial Networks trained on samples of simulated or actual events have been proposed as a way of generating large simulated datasets at a reduced computational cost. In this work, a novel approach to perform the simulation of photodetector signals from the time projection chamber of the EXO-200 experiment is demonstrated. The method is based on a Wasserstein Generative Adversarial N… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.06311v2-abstract-full').style.display = 'inline'; document.getElementById('2303.06311v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.06311v2-abstract-full" style="display: none;"> Generative Adversarial Networks trained on samples of simulated or actual events have been proposed as a way of generating large simulated datasets at a reduced computational cost. In this work, a novel approach to perform the simulation of photodetector signals from the time projection chamber of the EXO-200 experiment is demonstrated. The method is based on a Wasserstein Generative Adversarial Network - a deep learning technique allowing for implicit non-parametric estimation of the population distribution for a given set of objects. Our network is trained on real calibration data using raw scintillation waveforms as input. We find that it is able to produce high-quality simulated waveforms an order of magnitude faster than the traditional simulation approach and, importantly, generalize from the training sample and discern salient high-level features of the data. In particular, the network correctly deduces position dependency of scintillation light response in the detector and correctly recognizes dead photodetector channels. The network output is then integrated into the EXO-200 analysis framework to show that the standard EXO-200 reconstruction routine processes the simulated waveforms to produce energy distributions comparable to that of real waveforms. Finally, the remaining discrepancies and potential ways to improve the approach further are highlighted. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.06311v2-abstract-full').style.display = 'none'; document.getElementById('2303.06311v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">As accepted by JINST</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 18 P06005 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.01103">arXiv:2303.01103</a> <span> [<a href="https://arxiv.org/pdf/2303.01103">pdf</a>, <a href="https://arxiv.org/format/2303.01103">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1674-1137/aceee3">10.1088/1674-1137/aceee3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Two-neutrino Double-Beta Decay of $^{136}\rm Xe$ to the $0^+_1$ excited state of $^{136}\rm Ba$ with the Complete EXO-200 Dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+E">EXO-200 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Kharusi%2C+S+A">S. Al Kharusi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Darroch%2C+L">L. Darroch</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Dilling%2C+J">J. Dilling</a> , et al. (83 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="2303.01103v2-abstract-short" style="display: inline;"> A new search for two-neutrino double-beta ($2谓尾尾$) decay of $^{136}\rm Xe$ to the $0^+_1$ excited state of $^{136}\rm Ba$ is performed with the full EXO-200 dataset. A deep learning-based convolutional neural network is used to discriminate signal from background events. Signal detection efficiency is increased relative to previous searches by EXO-200 by more than a factor of two. With the additio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.01103v2-abstract-full').style.display = 'inline'; document.getElementById('2303.01103v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.01103v2-abstract-full" style="display: none;"> A new search for two-neutrino double-beta ($2谓尾尾$) decay of $^{136}\rm Xe$ to the $0^+_1$ excited state of $^{136}\rm Ba$ is performed with the full EXO-200 dataset. A deep learning-based convolutional neural network is used to discriminate signal from background events. Signal detection efficiency is increased relative to previous searches by EXO-200 by more than a factor of two. With the addition of the Phase II dataset taken with an upgraded detector, the median 90$\%$ confidence level half-life sensitivity of $2谓尾尾$ decay to the $0^+_1$ state of $^{136}\rm Ba$ is $2.9 \times 10^{24}~\rm yr$ using a total $^{136}\rm Xe$ exposure of $234.1~\rm kg~yr$. No statistically significant evidence for $2谓尾尾$ decay to the $0^+_1$ state is observed, leading to a lower limit of $T^{2谓}_{1/2}(0^+ \rightarrow 0^+_1) > 1.4\times10^{24}~\rm yr$ at 90$\%$ confidence level, improved by 70$\%$ relative to the current world's best constraint. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.01103v2-abstract-full').style.display = 'none'; document.getElementById('2303.01103v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">9 pages, 7 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Chinese Physics C, Volume 47, Number 10, 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.01444">arXiv:2302.01444</a> <span> [<a href="https://arxiv.org/pdf/2302.01444">pdf</a>, <a href="https://arxiv.org/format/2302.01444">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/10.1088/1748-0221/18/05/P05006">10.1088/1748-0221/18/05/P05006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design and characterization of AmLi neutron sources for the LZ experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Sazzad%2C+A+B+M+R">A. B. M. R. Sazzad</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Piepke%2C+A">A. Piepke</a>, <a href="/search/hep-ex?searchtype=author&query=Poudel%2C+S">S. Poudel</a>, <a href="/search/hep-ex?searchtype=author&query=Trewin%2C+H">H. Trewin</a>, <a href="/search/hep-ex?searchtype=author&query=LeViness%2C+A">A. LeViness</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="2302.01444v2-abstract-short" style="display: inline;"> In this paper we describe the development, testing, and characterization of three low-emission rate AmLi neutron sources. The sources are used to calibrate the nuclear recoil response of the LUX-ZEPLIN (LZ) dark matter experiment. The sources' neutron emission rate was measured using $^{3}$He proportional tubes. The sources' gamma emissions were characterized using a high-purity germanium (HPGe) d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01444v2-abstract-full').style.display = 'inline'; document.getElementById('2302.01444v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.01444v2-abstract-full" style="display: none;"> In this paper we describe the development, testing, and characterization of three low-emission rate AmLi neutron sources. The sources are used to calibrate the nuclear recoil response of the LUX-ZEPLIN (LZ) dark matter experiment. The sources' neutron emission rate was measured using $^{3}$He proportional tubes. The sources' gamma emissions were characterized using a high-purity germanium (HPGe) detector. Source-validated GEANT4 Monte Carlo simulations allowed to calibrate the Ge and neutron detector responses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01444v2-abstract-full').style.display = 'none'; document.getElementById('2302.01444v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">20 pages, 13 figures, 4 tables, revised manuscripts after accommodating the reviewer's comments</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2023 JINST 18 P05006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.17120">arXiv:2211.17120</a> <span> [<a href="https://arxiv.org/pdf/2211.17120">pdf</a>, <a href="https://arxiv.org/format/2211.17120">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.108.012010">10.1103/PhysRevD.108.012010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Background Determination for the LUX-ZEPLIN (LZ) Dark Matter Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a> , et al. (178 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="2211.17120v2-abstract-short" style="display: inline;"> The LUX-ZEPLIN experiment recently reported limits on WIMP-nucleus interactions from its initial science run, down to $9.2\times10^{-48}$ cm$^2$ for the spin-independent interaction of a 36 GeV/c$^2$ WIMP at 90% confidence level. In this paper, we present a comprehensive analysis of the backgrounds important for this result and for other upcoming physics analyses, including neutrinoless double-bet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.17120v2-abstract-full').style.display = 'inline'; document.getElementById('2211.17120v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.17120v2-abstract-full" style="display: none;"> The LUX-ZEPLIN experiment recently reported limits on WIMP-nucleus interactions from its initial science run, down to $9.2\times10^{-48}$ cm$^2$ for the spin-independent interaction of a 36 GeV/c$^2$ WIMP at 90% confidence level. In this paper, we present a comprehensive analysis of the backgrounds important for this result and for other upcoming physics analyses, including neutrinoless double-beta decay searches and effective field theory interpretations of LUX-ZEPLIN data. We confirm that the in-situ determinations of bulk and fixed radioactive backgrounds are consistent with expectations from the ex-situ assays. The observed background rate after WIMP search criteria were applied was $(6.3\pm0.5)\times10^{-5}$ events/keV$_{ee}$/kg/day in the low-energy region, approximately 60 times lower than the equivalent rate reported by the LUX experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.17120v2-abstract-full').style.display = 'none'; document.getElementById('2211.17120v2-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 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">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 15 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 108, 012010 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.03764">arXiv:2207.03764</a> <span> [<a href="https://arxiv.org/pdf/2207.03764">pdf</a>, <a href="https://arxiv.org/format/2207.03764">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> </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.131.041002">10.1103/PhysRevLett.131.041002 <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 Results from the LUX-ZEPLIN (LZ) Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Alqahtani%2C+A">A. Alqahtani</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Azadi%2C+S">S. Azadi</a>, <a href="/search/hep-ex?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Barthel%2C+J">J. Barthel</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a> , et al. (322 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="2207.03764v4-abstract-short" style="display: inline;"> The LUX-ZEPLIN experiment is a dark matter detector centered on a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility in Lead, South Dakota, USA. This Letter reports results from LUX-ZEPLIN's first search for weakly interacting massive particles (WIMPs) with an exposure of 60~live days using a fiducial mass of 5.5 t. A profile-likelihood ratio analysis s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03764v4-abstract-full').style.display = 'inline'; document.getElementById('2207.03764v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.03764v4-abstract-full" style="display: none;"> The LUX-ZEPLIN experiment is a dark matter detector centered on a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility in Lead, South Dakota, USA. This Letter reports results from LUX-ZEPLIN's first search for weakly interacting massive particles (WIMPs) with an exposure of 60~live days using a fiducial mass of 5.5 t. A profile-likelihood ratio analysis shows the data to be consistent with a background-only hypothesis, setting new limits on spin-independent WIMP-nucleon, spin-dependent WIMP-neutron, and spin-dependent WIMP-proton cross sections for WIMP masses above 9 GeV/c$^2$. The most stringent limit is set for spin-independent scattering at 36 GeV/c$^2$, rejecting cross sections above 9.2$\times 10^{-48}$ cm$^2$ at the 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03764v4-abstract-full').style.display = 'none'; document.getElementById('2207.03764v4-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">9 pages, 8 figures. See https://doi.org/10.1103/PhysRevLett.131.041002 for a data release related to this paper</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, 041002 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.00897">arXiv:2207.00897</a> <span> [<a href="https://arxiv.org/pdf/2207.00897">pdf</a>, <a href="https://arxiv.org/format/2207.00897">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.107.012007">10.1103/PhysRevD.107.012007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for MeV Electron Recoils from Dark Matter in EXO-200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+E">EXO-200 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Kharusi%2C+S+A">S. Al Kharusi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Darroch%2C+L">L. Darroch</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Dilling%2C+J">J. Dilling</a> , et al. (83 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="2207.00897v3-abstract-short" style="display: inline;"> We present a search for electron-recoil signatures from the charged-current absorption of fermionic dark matter using the EXO-200 detector. We report an average electron recoil background rate of $6.8 \times 10^{-4}\, \mathrm{cts}\,\mathrm{kg}^{-1}\mathrm{yr}^{-1}\mathrm{keV}^{-1}$ above $4\,\mathrm{MeV}$ and find no statistically significant excess over our background projection. Using a total… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.00897v3-abstract-full').style.display = 'inline'; document.getElementById('2207.00897v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.00897v3-abstract-full" style="display: none;"> We present a search for electron-recoil signatures from the charged-current absorption of fermionic dark matter using the EXO-200 detector. We report an average electron recoil background rate of $6.8 \times 10^{-4}\, \mathrm{cts}\,\mathrm{kg}^{-1}\mathrm{yr}^{-1}\mathrm{keV}^{-1}$ above $4\,\mathrm{MeV}$ and find no statistically significant excess over our background projection. Using a total ${}^{136}\mathrm{Xe}$ exposure of $234.1\,\mathrm{kg}\,\mathrm{yr}$ we exclude new parameter space for the charged-current absorption cross-section for dark matter masses between $m_蠂= 2.6\,\mathrm{MeV} - 11.6\,\mathrm{MeV}$ with a minimum of $6\times 10^{-51}\,\mathrm{cm}^2$ at $8.3\,\mathrm{MeV}$ at the $90\%$ confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.00897v3-abstract-full').style.display = 'none'; document.getElementById('2207.00897v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">9 pages, 6 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 107, 012007 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07623">arXiv:2203.07623</a> <span> [<a href="https://arxiv.org/pdf/2203.07623">pdf</a>, <a href="https://arxiv.org/format/2203.07623">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Snowmass2021 Cosmic Frontier White Paper: Calibrations and backgrounds for dark matter direct detection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+D">Daniel Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Bunker%2C+R">Raymond Bunker</a>, <a href="/search/hep-ex?searchtype=author&query=Shaw%2C+S">Sally Shaw</a>, <a href="/search/hep-ex?searchtype=author&query=Westerdale%2C+S">Shawn Westerdale</a>, <a href="/search/hep-ex?searchtype=author&query=Arnquist%2C+I">Isaac Arnquist</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">Daniel S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Calkins%2C+R">Rob Calkins</a>, <a href="/search/hep-ex?searchtype=author&query=Cebri%C3%A1n%2C+S">Susana Cebri谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Dent%2C+J+B">James B. Dent</a>, <a href="/search/hep-ex?searchtype=author&query=di+Vacri%2C+M+L">Maria Laura di Vacri</a>, <a href="/search/hep-ex?searchtype=author&query=Dobson%2C+J">Jim Dobson</a>, <a href="/search/hep-ex?searchtype=author&query=Egana-Ugrinovic%2C+D">Daniel Egana-Ugrinovic</a>, <a href="/search/hep-ex?searchtype=author&query=Erlandson%2C+A">Andrew Erlandson</a>, <a href="/search/hep-ex?searchtype=author&query=Ghag%2C+C">Chamkaur Ghag</a>, <a href="/search/hep-ex?searchtype=author&query=Hall%2C+C">Carter Hall</a>, <a href="/search/hep-ex?searchtype=author&query=Hall%2C+J">Jeter Hall</a>, <a href="/search/hep-ex?searchtype=author&query=Haselschwardt%2C+S">Scott Haselschwardt</a>, <a href="/search/hep-ex?searchtype=author&query=Hoppe%2C+E">Eric Hoppe</a>, <a href="/search/hep-ex?searchtype=author&query=Jackson%2C+C+M">Chris M. Jackson</a>, <a href="/search/hep-ex?searchtype=author&query=Kahn%2C+Y">Yonatan Kahn</a>, <a href="/search/hep-ex?searchtype=author&query=Kamaha%2C+A">Alvine Kamaha</a>, <a href="/search/hep-ex?searchtype=author&query=Kelsey%2C+M">Mike Kelsey</a>, <a href="/search/hep-ex?searchtype=author&query=Kish%2C+A">Alexander Kish</a>, <a href="/search/hep-ex?searchtype=author&query=Kurinsky%2C+N">Noah Kurinsky</a>, <a href="/search/hep-ex?searchtype=author&query=Laubenstein%2C+M">Matthias Laubenstein</a> , et al. (26 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="2203.07623v2-abstract-short" style="display: inline;"> Future dark matter direct detection experiments will reach unprecedented levels of sensitivity. Achieving this sensitivity will require more precise models of signal and background rates in future detectors. Improving the precision of signal and background modeling goes hand-in-hand with novel calibration techniques that can probe rare processes and lower threshold detector response. The goal of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07623v2-abstract-full').style.display = 'inline'; document.getElementById('2203.07623v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07623v2-abstract-full" style="display: none;"> Future dark matter direct detection experiments will reach unprecedented levels of sensitivity. Achieving this sensitivity will require more precise models of signal and background rates in future detectors. Improving the precision of signal and background modeling goes hand-in-hand with novel calibration techniques that can probe rare processes and lower threshold detector response. The goal of this white paper is to outline community needs to meet the background and calibration requirements of next-generation dark matter direct detection experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07623v2-abstract-full').style.display = 'none'; document.getElementById('2203.07623v2-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">Solicited community whitepaper for the Snowmass2021 process (Cosmic frontier, particle dark matter working group)</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/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Aerne%2C+V">V. Aerne</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/hep-ex?searchtype=author&query=Akshat%2C+J">J. Akshat</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Amaro%2C+F+D">F. D. Amaro</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/hep-ex?searchtype=author&query=Angevaare%2C+J">J. Angevaare</a>, <a href="/search/hep-ex?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/hep-ex?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/hep-ex?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/hep-ex?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/hep-ex?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/2201.02858">arXiv:2201.02858</a> <span> [<a href="https://arxiv.org/pdf/2201.02858">pdf</a>, <a href="https://arxiv.org/format/2201.02858">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> </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.105.082004">10.1103/PhysRevD.105.082004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmogenic production of $^{37}$Ar in the context of the LUX-ZEPLIN experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a> , et al. (183 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="2201.02858v2-abstract-short" style="display: inline;"> We estimate the amount of $^{37}$Ar produced in natural xenon via cosmic ray-induced spallation, an inevitable consequence of the transportation and storage of xenon on the Earth's surface. We then calculate the resulting $^{37}$Ar concentration in a 10-tonne payload~(similar to that of the LUX-ZEPLIN experiment) assuming a representative schedule of xenon purification, storage and delivery to the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.02858v2-abstract-full').style.display = 'inline'; document.getElementById('2201.02858v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.02858v2-abstract-full" style="display: none;"> We estimate the amount of $^{37}$Ar produced in natural xenon via cosmic ray-induced spallation, an inevitable consequence of the transportation and storage of xenon on the Earth's surface. We then calculate the resulting $^{37}$Ar concentration in a 10-tonne payload~(similar to that of the LUX-ZEPLIN experiment) assuming a representative schedule of xenon purification, storage and delivery to the underground facility. Using the spallation model by Silberberg and Tsao, the sea level production rate of $^{37}$Ar in natural xenon is estimated to be 0.024~atoms/kg/day. Assuming the xenon is successively purified to remove radioactive contaminants in 1-tonne batches at a rate of 1~tonne/month, the average $^{37}$Ar activity after 10~tonnes are purified and transported underground is 0.058--0.090~$渭$Bq/kg, depending on the degree of argon removal during above-ground purification. Such cosmogenic $^{37}$Ar will appear as a noticeable background in the early science data, while decaying with a 35~day half-life. This newly-noticed production mechanism of $^{37}$Ar should be considered when planning for future liquid xenon-based experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.02858v2-abstract-full').style.display = 'none'; document.getElementById('2201.02858v2-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.00699">arXiv:2201.00699</a> <span> [<a href="https://arxiv.org/pdf/2201.00699">pdf</a>, <a href="https://arxiv.org/format/2201.00699">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/10.1088/1748-0221/17/10/P10035">10.1088/1748-0221/17/10/P10035 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radon Emanation from Dust of Varying Composition and Size </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Meng%2C+Y">Yue Meng</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">Jerry Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Piepke%2C+A">Andreas Piepke</a>, <a href="/search/hep-ex?searchtype=author&query=Tsang%2C+R">Raymond Tsang</a>, <a href="/search/hep-ex?searchtype=author&query=Wu%2C+M">Mengmeng Wu</a>, <a href="/search/hep-ex?searchtype=author&query=Yao%2C+Y">Yukun Yao</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="2201.00699v5-abstract-short" style="display: inline;"> $^{222}Rn$ emanating from environmental dust constitutes an important background component for many low-energy, low-rate experiments. Radon emanation rates from dust and rock, thus, are important for experiment planning. In this paper, we report measured radon emanation fractions for five types of dry dust differing in grain size and composition. These data were obtained by a novel technique in $纬… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.00699v5-abstract-full').style.display = 'inline'; document.getElementById('2201.00699v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.00699v5-abstract-full" style="display: none;"> $^{222}Rn$ emanating from environmental dust constitutes an important background component for many low-energy, low-rate experiments. Radon emanation rates from dust and rock, thus, are important for experiment planning. In this paper, we report measured radon emanation fractions for five types of dry dust differing in grain size and composition. These data were obtained by a novel technique in $纬$-spectroscopy, measuring emanated and non-emanated $^{222}Rn$ progeny activities as well as the the parent $^{226}$Ra activity in a time series. The range of observed radon emanation fractions is $(3.7 \pm 2.0)\%$ to $(16.2 \pm 0.9)\%$. Four of the five samples are standardized samples available commercially, so additional investigations of these samples may be readily carried out. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.00699v5-abstract-full').style.display = 'none'; document.getElementById('2201.00699v5-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">11 pages, 5 figures, 3 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/2109.01327">arXiv:2109.01327</a> <span> [<a href="https://arxiv.org/pdf/2109.01327">pdf</a>, <a href="https://arxiv.org/format/2109.01327">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.112002">10.1103/PhysRevD.104.112002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Majoron-emitting modes of $^{136}$Xe double beta decay with the complete EXO-200 dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Kharusi%2C+S+A">S. Al Kharusi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Darroch%2C+L">L. Darroch</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Dilling%2C+J">J. Dilling</a>, <a href="/search/hep-ex?searchtype=author&query=Dolgolenko%2C+A">A. Dolgolenko</a>, <a href="/search/hep-ex?searchtype=author&query=Dolinski%2C+M+J">M. J. Dolinski</a> , et al. (81 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="2109.01327v2-abstract-short" style="display: inline;"> A search for Majoron-emitting modes of the neutrinoless double-beta decay of $^{136}$Xe is performed with the full EXO-200 dataset. This dataset consists of a total $^{136}$Xe exposure of 234.1 kg$\cdot$yr, and includes data with detector upgrades that have improved the energy threshold relative to previous searches. A lower limit of T$_{1/2}^{\rm{^{136}Xe}}>$4.3$\cdot$10$^{24}$ yr at 90\% C.L. on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.01327v2-abstract-full').style.display = 'inline'; document.getElementById('2109.01327v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.01327v2-abstract-full" style="display: none;"> A search for Majoron-emitting modes of the neutrinoless double-beta decay of $^{136}$Xe is performed with the full EXO-200 dataset. This dataset consists of a total $^{136}$Xe exposure of 234.1 kg$\cdot$yr, and includes data with detector upgrades that have improved the energy threshold relative to previous searches. A lower limit of T$_{1/2}^{\rm{^{136}Xe}}>$4.3$\cdot$10$^{24}$ yr at 90\% C.L. on the half-life of the spectral index $n=1$ Majoron decay was obtained, a factor of 3.6 more stringent than the previous limit from EXO-200, corresponding to a constraint on the Majoron-neutrino coupling constant of $|\langle g_{ee}^{M}\rangle|$$<(0.4$-$0.9)\cdot10^{-5}$. The lower threshold and the additional data taken resulted in a factor 8.4 improvement for the $n=7$ mode compared to the previous EXO search. This search provides the most stringent limits to-date on the Majoron-emitting decays of $^{136}$Xe with spectral indices $n=1,2,3,$ and 7. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.01327v2-abstract-full').style.display = 'none'; document.getElementById('2109.01327v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.06007">arXiv:2107.06007</a> <span> [<a href="https://arxiv.org/pdf/2107.06007">pdf</a>, <a href="https://arxiv.org/format/2107.06007">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/17/02/P02015">10.1088/1748-0221/17/02/P02015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The EXO-200 detector, part II: Auxiliary Systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Ackerman%2C+N">N. Ackerman</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J">J. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Auger%2C+M">M. Auger</a>, <a href="/search/hep-ex?searchtype=author&query=Auty%2C+D+J">D. J. Auty</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Bartoszek%2C+L">L. Bartoszek</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Benitez-Medina%2C+C">C. Benitez-Medina</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Conley%2C+R">R. Conley</a>, <a href="/search/hep-ex?searchtype=author&query=Cook%2C+S">S. Cook</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craddock%2C+W">W. Craddock</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Cree%2C+W">W. Cree</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Darroch%2C+L">L. Darroch</a> , et al. (135 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="2107.06007v3-abstract-short" style="display: inline;"> The EXO-200 experiment searched for neutrinoless double-beta decay of $^{136}$Xe with a single-phase liquid xenon detector. It used an active mass of 110 kg of 80.6%-enriched liquid xenon in an ultra-low background time projection chamber with ionization and scintillation detection and readout. This paper describes the design and performance of the various support systems necessary for detector op… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.06007v3-abstract-full').style.display = 'inline'; document.getElementById('2107.06007v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.06007v3-abstract-full" style="display: none;"> The EXO-200 experiment searched for neutrinoless double-beta decay of $^{136}$Xe with a single-phase liquid xenon detector. It used an active mass of 110 kg of 80.6%-enriched liquid xenon in an ultra-low background time projection chamber with ionization and scintillation detection and readout. This paper describes the design and performance of the various support systems necessary for detector operation, including cryogenics, xenon handling, and controls. Novel features of the system were driven by the need to protect the thin-walled detector chamber containing the liquid xenon, to achieve high chemical purity of the Xe, and to maintain thermal uniformity across the detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.06007v3-abstract-full').style.display = 'none'; document.getElementById('2107.06007v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Manuscript updated in response to JINST reviewer comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.11740">arXiv:2102.11740</a> <span> [<a href="https://arxiv.org/pdf/2102.11740">pdf</a>, <a href="https://arxiv.org/format/2102.11740">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="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.092009">10.1103/PhysRevD.104.092009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Projected sensitivities of the LUX-ZEPLIN (LZ) experiment to new physics via low-energy electron recoils </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ex?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a> , et al. (172 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="2102.11740v2-abstract-short" style="display: inline;"> LUX-ZEPLIN (LZ) is a dark matter detector expected to obtain world-leading sensitivity to weakly interacting massive particles (WIMPs) interacting via nuclear recoils with a ~7-tonne xenon target mass. This manuscript presents sensitivity projections to several low-energy signals of the complementary electron recoil signal type: 1) an effective neutrino magnetic moment and 2) an effective neutrino… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11740v2-abstract-full').style.display = 'inline'; document.getElementById('2102.11740v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.11740v2-abstract-full" style="display: none;"> LUX-ZEPLIN (LZ) is a dark matter detector expected to obtain world-leading sensitivity to weakly interacting massive particles (WIMPs) interacting via nuclear recoils with a ~7-tonne xenon target mass. This manuscript presents sensitivity projections to several low-energy signals of the complementary electron recoil signal type: 1) an effective neutrino magnetic moment and 2) an effective neutrino millicharge, both for pp-chain solar neutrinos, 3) an axion flux generated by the Sun, 4) axion-like particles forming the galactic dark matter, 5) hidden photons, 6) mirror dark matter, and 7) leptophilic dark matter. World-leading sensitivities are expected in each case, a result of the large 5.6t 1000d exposure and low expected rate of electron recoil backgrounds in the $<$100keV energy regime. A consistent signal generation, background model and profile-likelihood analysis framework is used throughout. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11740v2-abstract-full').style.display = 'none'; document.getElementById('2102.11740v2-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">v2 updates exclusion sensitivities from single-sided to two-sided</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.02506">arXiv:2006.02506</a> <span> [<a href="https://arxiv.org/pdf/2006.02506">pdf</a>, <a href="https://arxiv.org/format/2006.02506">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/s10052-020-8420-x">10.1140/epjc/s10052-020-8420-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The LUX-ZEPLIN (LZ) radioactivity and cleanliness control programs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/hep-ex?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/hep-ex?searchtype=author&query=Alquahtani%2C+A">A. Alquahtani</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Arbuckle%2C+A">A. Arbuckle</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Auyeung%2C+H">H. Auyeung</a>, <a href="/search/hep-ex?searchtype=author&query=Aviles%2C+S">S. Aviles</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Bensinger%2C+J">J. Bensinger</a> , et al. (365 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="2006.02506v3-abstract-short" style="display: inline;"> LUX-ZEPLIN (LZ) is a second-generation direct dark matter experiment with spin-independent WIMP-nucleon scattering sensitivity above $1.4 \times 10^{-48}$ cm$^{2}$ for a WIMP mass of 40 GeV/c$^{2}$ and a 1000 d exposure. LZ achieves this sensitivity through a combination of a large 5.6 t fiducial volume, active inner and outer veto systems, and radio-pure construction using materials with inherent… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.02506v3-abstract-full').style.display = 'inline'; document.getElementById('2006.02506v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.02506v3-abstract-full" style="display: none;"> LUX-ZEPLIN (LZ) is a second-generation direct dark matter experiment with spin-independent WIMP-nucleon scattering sensitivity above $1.4 \times 10^{-48}$ cm$^{2}$ for a WIMP mass of 40 GeV/c$^{2}$ and a 1000 d exposure. LZ achieves this sensitivity through a combination of a large 5.6 t fiducial volume, active inner and outer veto systems, and radio-pure construction using materials with inherently low radioactivity content. The LZ collaboration performed an extensive radioassay campaign over a period of six years to inform material selection for construction and provide an input to the experimental background model against which any possible signal excess may be evaluated. The campaign and its results are described in this paper. We present assays of dust and radon daughters depositing on the surface of components as well as cleanliness controls necessary to maintain background expectations through detector construction and assembly. Finally, examples from the campaign to highlight fixed contaminant radioassays for the LZ photomultiplier tubes, quality control and quality assurance procedures through fabrication, radon emanation measurements of major sub-systems, and bespoke detector systems to assay scintillator are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.02506v3-abstract-full').style.display = 'none'; document.getElementById('2006.02506v3-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> 28 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">45 pages (79 inc. tables), 7 figures, 9 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The European Physical Journal C, Volume 80, Article number: 1044 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.09363">arXiv:2001.09363</a> <span> [<a href="https://arxiv.org/pdf/2001.09363">pdf</a>, <a href="https://arxiv.org/format/2001.09363">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/10.1016/j.astropartphys.2020.102480">10.1016/j.astropartphys.2020.102480 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simulations of Events for the LUX-ZEPLIN (LZ) Dark Matter Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+L">The LUX-ZEPLIN Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/hep-ex?searchtype=author&query=Alqahtani%2C+A">A. Alqahtani</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Bensinger%2C+J">J. Bensinger</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/hep-ex?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a> , et al. (173 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="2001.09363v2-abstract-short" style="display: inline;"> The LUX-ZEPLIN dark matter search aims to achieve a sensitivity to the WIMP-nucleon spin-independent cross-section down to (1--2)$\times10^{-12}$\,pb at a WIMP mass of 40 GeV/$c^2$. This paper describes the simulations framework that, along with radioactivity measurements, was used to support this projection, and also to provide mock data for validating reconstruction and analysis software. Of par… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.09363v2-abstract-full').style.display = 'inline'; document.getElementById('2001.09363v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.09363v2-abstract-full" style="display: none;"> The LUX-ZEPLIN dark matter search aims to achieve a sensitivity to the WIMP-nucleon spin-independent cross-section down to (1--2)$\times10^{-12}$\,pb at a WIMP mass of 40 GeV/$c^2$. This paper describes the simulations framework that, along with radioactivity measurements, was used to support this projection, and also to provide mock data for validating reconstruction and analysis software. Of particular note are the event generators, which allow us to model the background radiation, and the detector response physics used in the production of raw signals, which can be converted into digitized waveforms similar to data from the operational detector. Inclusion of the detector response allows us to process simulated data using the same analysis routines as developed to process the experimental data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.09363v2-abstract-full').style.display = 'none'; document.getElementById('2001.09363v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">24 pages, 19 figures; Corresponding Authors: A. Cottle, V. Kudryavtsev, D. Woodward</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.01841">arXiv:1912.01841</a> <span> [<a href="https://arxiv.org/pdf/1912.01841">pdf</a>, <a href="https://arxiv.org/format/1912.01841">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/10.1109/TNS.2020.3035172">10.1109/TNS.2020.3035172 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reflectance of Silicon Photomultipliers at Vacuum Ultraviolet Wavelengths </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Lv%2C+P">P. Lv</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Wen%2C+L+J">L. J. Wen</a>, <a href="/search/hep-ex?searchtype=author&query=Kharusi%2C+S+A">S. Al Kharusi</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Breur%2C+P+A">P. A. Breur</a>, <a href="/search/hep-ex?searchtype=author&query=Brodsky%2C+J+P">J. P. Brodsky</a>, <a href="/search/hep-ex?searchtype=author&query=Brown%2C+E">E. Brown</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Mamahit%2C+S+B">S. Byrne Mamahit</a>, <a href="/search/hep-ex?searchtype=author&query=Caden%2C+E">E. Caden</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+L">L. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Chana%2C+B">B. Chana</a>, <a href="/search/hep-ex?searchtype=author&query=Charlebois%2C+S+A">S. A. Charlebois</a>, <a href="/search/hep-ex?searchtype=author&query=Chiu%2C+M">M. Chiu</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a> , et al. (126 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="1912.01841v1-abstract-short" style="display: inline;"> Characterization of the vacuum ultraviolet (VUV) reflectance of silicon photomultipliers (SiPMs) is important for large-scale SiPM-based photodetector systems. We report the angular dependence of the specular reflectance in a vacuum of SiPMs manufactured by Fondazionc Bruno Kessler (FBK) and Hamamatsu Photonics K.K. (HPK) over wavelengths ranging from 120 nm to 280 nm. Refractive index and extinct… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.01841v1-abstract-full').style.display = 'inline'; document.getElementById('1912.01841v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.01841v1-abstract-full" style="display: none;"> Characterization of the vacuum ultraviolet (VUV) reflectance of silicon photomultipliers (SiPMs) is important for large-scale SiPM-based photodetector systems. We report the angular dependence of the specular reflectance in a vacuum of SiPMs manufactured by Fondazionc Bruno Kessler (FBK) and Hamamatsu Photonics K.K. (HPK) over wavelengths ranging from 120 nm to 280 nm. Refractive index and extinction coefficient of the thin silicon-dioxide film deposited on the surface of the FBK SiPMs are derived from reflectance data of a FBK silicon wafer with the same deposited oxide film as SiPMs. The diffuse reflectance of SiPMs is also measured at 193 nm. We use the VUV spectral dependence of the optical constants to predict the reflectance of the FBK silicon wafer and FBK SiPMs in liquid xenon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.01841v1-abstract-full').style.display = 'none'; document.getElementById('1912.01841v1-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.09124">arXiv:1910.09124</a> <span> [<a href="https://arxiv.org/pdf/1910.09124">pdf</a>, <a href="https://arxiv.org/format/1910.09124">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 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.2019.163047">10.1016/j.nima.2019.163047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The LUX-ZEPLIN (LZ) Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/hep-ex?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/hep-ex?searchtype=author&query=Alquahtani%2C+A">A. Alquahtani</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Arbuckle%2C+A">A. Arbuckle</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Auyeung%2C+H">H. Auyeung</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Barthel%2C+J">J. Barthel</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a> , et al. (357 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="1910.09124v2-abstract-short" style="display: inline;"> We describe the design and assembly of the LUX-ZEPLIN experiment, a direct detection search for cosmic WIMP dark matter particles. The centerpiece of the experiment is a large liquid xenon time projection chamber sensitive to low energy nuclear recoils. Rejection of backgrounds is enhanced by a Xe skin veto detector and by a liquid scintillator Outer Detector loaded with gadolinium for efficient n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.09124v2-abstract-full').style.display = 'inline'; document.getElementById('1910.09124v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.09124v2-abstract-full" style="display: none;"> We describe the design and assembly of the LUX-ZEPLIN experiment, a direct detection search for cosmic WIMP dark matter particles. The centerpiece of the experiment is a large liquid xenon time projection chamber sensitive to low energy nuclear recoils. Rejection of backgrounds is enhanced by a Xe skin veto detector and by a liquid scintillator Outer Detector loaded with gadolinium for efficient neutron capture and tagging. LZ is located in the Davis Cavern at the 4850' level of the Sanford Underground Research Facility in Lead, South Dakota, USA. We describe the major subsystems of the experiment and its key design features and requirements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.09124v2-abstract-full').style.display = 'none'; document.getElementById('1910.09124v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.06438">arXiv:1910.06438</a> <span> [<a href="https://arxiv.org/pdf/1910.06438">pdf</a>, <a href="https://arxiv.org/format/1910.06438">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/10.1088/1748-0221/15/01/P01019">10.1088/1748-0221/15/01/P01019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reflectivity and PDE of VUV4 Hamamatsu SiPMs in Liquid Xenon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Nakarmi%2C+P">P. Nakarmi</a>, <a href="/search/hep-ex?searchtype=author&query=Ostrovskiy%2C+I">I. Ostrovskiy</a>, <a href="/search/hep-ex?searchtype=author&query=Soma%2C+A+K">A. K. Soma</a>, <a href="/search/hep-ex?searchtype=author&query=Retiere%2C+F">F. Retiere</a>, <a href="/search/hep-ex?searchtype=author&query=Kharusi%2C+S+A">S. Al Kharusi</a>, <a href="/search/hep-ex?searchtype=author&query=Alfaris%2C+M">M. Alfaris</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Blatchford%2C+J">J. Blatchford</a>, <a href="/search/hep-ex?searchtype=author&query=Breur%2C+P+A">P. A. Breur</a>, <a href="/search/hep-ex?searchtype=author&query=Brodsky%2C+J+P">J. P. Brodsky</a>, <a href="/search/hep-ex?searchtype=author&query=Brown%2C+E">E. Brown</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Mamahit%2C+S+B">S. Byrne Mamahit</a>, <a href="/search/hep-ex?searchtype=author&query=Caden%2C+E">E. Caden</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+L">L. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Chana%2C+B">B. Chana</a>, <a href="/search/hep-ex?searchtype=author&query=Charlebois%2C+S+A">S. A. Charlebois</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="1910.06438v2-abstract-short" style="display: inline;"> Understanding reflective properties of materials and photodetection efficiency (PDE) of photodetectors is important for optimizing energy resolution and sensitivity of the next generation neutrinoless double beta decay, direct detection dark matter, and neutrino oscillation experiments that will use noble liquid gases, such as nEXO, DARWIN, DarkSide-20k, and DUNE. Little information is currently a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.06438v2-abstract-full').style.display = 'inline'; document.getElementById('1910.06438v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.06438v2-abstract-full" style="display: none;"> Understanding reflective properties of materials and photodetection efficiency (PDE) of photodetectors is important for optimizing energy resolution and sensitivity of the next generation neutrinoless double beta decay, direct detection dark matter, and neutrino oscillation experiments that will use noble liquid gases, such as nEXO, DARWIN, DarkSide-20k, and DUNE. Little information is currently available about reflectivity and PDE in liquid noble gases, because such measurements are difficult to conduct in a cryogenic environment and at short enough wavelengths. Here we report a measurement of specular reflectivity and relative PDE of Hamamatsu VUV4 silicon photomultipliers (SiPMs) with 50 micrometer micro-cells conducted with xenon scintillation light (~175 nm) in liquid xenon. The specular reflectivity at 15 deg. incidence of three samples of VUV4 SiPMs is found to be 30.4+/-1.4%, 28.6+/-1.3%, and 28.0+/-1.3%, respectively. The PDE at normal incidence differs by +/-8% (standard deviation) among the three devices. The angular dependence of the reflectivity and PDE was also measured for one of the SiPMs. Both the reflectivity and PDE decrease as the angle of incidence increases. This is the first measurement of an angular dependence of PDE and reflectivity of a SiPM in liquid xenon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.06438v2-abstract-full').style.display = 'none'; document.getElementById('1910.06438v2-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </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, 15 figures, 6 tables. As accepted by 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/1908.04128">arXiv:1908.04128</a> <span> [<a href="https://arxiv.org/pdf/1908.04128">pdf</a>, <a href="https://arxiv.org/format/1908.04128">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/10.1103/PhysRevC.101.065501">10.1103/PhysRevC.101.065501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the scintillation and ionization response of liquid xenon at MeV energies in the EXO-200 experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+E">EXO-200 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Darroch%2C+L">L. Darroch</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Dilling%2C+J">J. Dilling</a>, <a href="/search/hep-ex?searchtype=author&query=Dolgolenko%2C+A">A. Dolgolenko</a> , et al. (78 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="1908.04128v2-abstract-short" style="display: inline;"> Liquid xenon (LXe) is employed in a number of current and future detectors for rare event searches. We use the EXO-200 experimental data to measure the absolute scintillation and ionization yields generated by $纬$ interactions from $^{228}$Th (2615~keV), $^{226}$Ra (1764~keV) and $^{60}$Co (1332~keV and 1173~keV) calibration sources, over a range of electric fields. The $W$-value that defines the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.04128v2-abstract-full').style.display = 'inline'; document.getElementById('1908.04128v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.04128v2-abstract-full" style="display: none;"> Liquid xenon (LXe) is employed in a number of current and future detectors for rare event searches. We use the EXO-200 experimental data to measure the absolute scintillation and ionization yields generated by $纬$ interactions from $^{228}$Th (2615~keV), $^{226}$Ra (1764~keV) and $^{60}$Co (1332~keV and 1173~keV) calibration sources, over a range of electric fields. The $W$-value that defines the recombination-independent energy scale is measured to be $11.5~\pm~0.5$~(syst.)~$\pm~0.1$~(stat.) eV. These data are also used to measure the recombination fluctuations in the number of electrons and photons produced by the calibration sources at the MeV-scale, which deviate from extrapolations of lower-energy data. Additionally, a semi-empirical model for the energy resolution of the detector is developed, which is used to constrain the recombination efficiency, i.e., the fraction of recombined electrons that result in the emission of a detectable photon. Detailed measurements of the absolute charge and light yields for MeV-scale electron recoils are important for predicting the performance of future neutrinoless double beta decay detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.04128v2-abstract-full').style.display = 'none'; document.getElementById('1908.04128v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 101, 065501 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.02723">arXiv:1906.02723</a> <span> [<a href="https://arxiv.org/pdf/1906.02723">pdf</a>, <a href="https://arxiv.org/format/1906.02723">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.123.161802">10.1103/PhysRevLett.123.161802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Neutrinoless Double-Beta Decay with the Complete EXO-200 Dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Darroch%2C+L">L. Darroch</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Dilling%2C+J">J. Dilling</a>, <a href="/search/hep-ex?searchtype=author&query=Dolgolenko%2C+A">A. Dolgolenko</a>, <a href="/search/hep-ex?searchtype=author&query=Dolinski%2C+M+J">M. J. Dolinski</a> , et al. (77 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="1906.02723v3-abstract-short" style="display: inline;"> A search for neutrinoless double-beta decay ($0谓尾尾$) in $^{136}$Xe is performed with the full EXO-200 dataset using a deep neural network to discriminate between $0谓尾尾$ and background events. Relative to previous analyses, the signal detection efficiency has been raised from 80.8% to 96.4$\pm$3.0% and the energy resolution of the detector at the Q-value of $^{136}$Xe $0谓尾尾$ has been improved from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.02723v3-abstract-full').style.display = 'inline'; document.getElementById('1906.02723v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.02723v3-abstract-full" style="display: none;"> A search for neutrinoless double-beta decay ($0谓尾尾$) in $^{136}$Xe is performed with the full EXO-200 dataset using a deep neural network to discriminate between $0谓尾尾$ and background events. Relative to previous analyses, the signal detection efficiency has been raised from 80.8% to 96.4$\pm$3.0% and the energy resolution of the detector at the Q-value of $^{136}$Xe $0谓尾尾$ has been improved from $蟽/E=1.23\%$ to $1.15\pm0.02\%$ with the upgraded detector. Accounting for the new data, the median 90% confidence level $0谓尾尾$ half-life sensitivity for this analysis is $5.0 \cdot 10^{25}$ yr with a total $^{136}$Xe exposure of 234.1 kg$\cdot$yr. No statistically significant evidence for $0谓尾尾$ is observed, leading to a lower limit on the $0谓尾尾$ half-life of $3.5\cdot10^{25}$ yr at the 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.02723v3-abstract-full').style.display = 'none'; document.getElementById('1906.02723v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </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">v1, 7 pages, 5 figures; v2, fix references; v3, update to accepted version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 123, 161802 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.02112">arXiv:1904.02112</a> <span> [<a href="https://arxiv.org/pdf/1904.02112">pdf</a>, <a href="https://arxiv.org/format/1904.02112">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/10.1016/j.astropartphys.2019.102391">10.1016/j.astropartphys.2019.102391 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the Gamma Ray Background in the Davis Cavern at the Sanford Underground Research Facility </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/hep-ex?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/hep-ex?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a>, <a href="/search/hep-ex?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J+K">J. K. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Carels%2C+C">C. Carels</a>, <a href="/search/hep-ex?searchtype=author&query=Carlsmith%2C+D+L">D. L. Carlsmith</a>, <a href="/search/hep-ex?searchtype=author&query=Carmona-Benitez%2C+M+C">M. C. Carmona-Benitez</a>, <a href="/search/hep-ex?searchtype=author&query=Cascella%2C+M">M. Cascella</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="1904.02112v2-abstract-short" style="display: inline;"> Deep underground environments are ideal for low background searches due to the attenuation of cosmic rays by passage through the earth. However, they are affected by backgrounds from $纬$-rays emitted by $^{40}$K and the $^{238}$U and $^{232}$Th decay chains in the surrounding rock. The LUX-ZEPLIN (LZ) experiment will search for dark matter particle interactions with a liquid xenon TPC located with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.02112v2-abstract-full').style.display = 'inline'; document.getElementById('1904.02112v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.02112v2-abstract-full" style="display: none;"> Deep underground environments are ideal for low background searches due to the attenuation of cosmic rays by passage through the earth. However, they are affected by backgrounds from $纬$-rays emitted by $^{40}$K and the $^{238}$U and $^{232}$Th decay chains in the surrounding rock. The LUX-ZEPLIN (LZ) experiment will search for dark matter particle interactions with a liquid xenon TPC located within the Davis campus at the Sanford Underground Research Facility, Lead, South Dakota, at the 4,850-foot level. In order to characterise the cavern background, in-situ $纬$-ray measurements were taken with a sodium iodide detector in various locations and with lead shielding. The integral count rates (0--3300~keV) varied from 596~Hz to 1355~Hz for unshielded measurements, corresponding to a total flux in the cavern of $1.9\pm0.4$~$纬~$cm$^{-2}$s$^{-1}$. The resulting activity in the walls of the cavern can be characterised as $220\pm60$~Bq/kg of $^{40}$K, $29\pm15$~Bq/kg of $^{238}$U, and $13\pm3$~Bq/kg of $^{232}$Th. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.02112v2-abstract-full').style.display = 'none'; document.getElementById('1904.02112v2-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics, Volume 116, Pages 102391 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.09641">arXiv:1804.09641</a> <span> [<a href="https://arxiv.org/pdf/1804.09641">pdf</a>, <a href="https://arxiv.org/format/1804.09641">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/13/08/P08023">10.1088/1748-0221/13/08/P08023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep Neural Networks for Energy and Position Reconstruction in EXO-200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Jewell%2C+M+J">M. J. Jewell</a>, <a href="/search/hep-ex?searchtype=author&query=Ostrovskiy%2C+I">I. Ostrovskiy</a>, <a href="/search/hep-ex?searchtype=author&query=Weber%2C+M">M. Weber</a>, <a href="/search/hep-ex?searchtype=author&query=Ziegler%2C+T">T. Ziegler</a>, <a href="/search/hep-ex?searchtype=author&query=Dalmasson%2C+J">J. Dalmasson</a>, <a href="/search/hep-ex?searchtype=author&query=Kaufman%2C+L+J">L. J. Kaufman</a>, <a href="/search/hep-ex?searchtype=author&query=Richards%2C+T">T. Richards</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Bayerlein%2C+R">R. Bayerlein</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Cree%2C+W">W. Cree</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a> , et al. (69 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="1804.09641v2-abstract-short" style="display: inline;"> We apply deep neural networks (DNN) to data from the EXO-200 experiment. In the studied cases, the DNN is able to reconstruct the relevant parameters - total energy and position - directly from raw digitized waveforms, with minimal exceptions. For the first time, the developed algorithms are evaluated on real detector calibration data. The accuracy of reconstruction either reaches or exceeds what… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09641v2-abstract-full').style.display = 'inline'; document.getElementById('1804.09641v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.09641v2-abstract-full" style="display: none;"> We apply deep neural networks (DNN) to data from the EXO-200 experiment. In the studied cases, the DNN is able to reconstruct the relevant parameters - total energy and position - directly from raw digitized waveforms, with minimal exceptions. For the first time, the developed algorithms are evaluated on real detector calibration data. The accuracy of reconstruction either reaches or exceeds what was achieved by the conventional approaches developed by EXO-200 over the course of the experiment. Most existing DNN approaches to event reconstruction and classification in particle physics are trained on Monte Carlo simulated events. Such algorithms are inherently limited by the accuracy of the simulation. We describe a unique approach that, in an experiment such as EXO-200, allows to successfully perform certain reconstruction and analysis tasks by training the network on waveforms from experimental data, either reducing or eliminating the reliance on the Monte Carlo. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09641v2-abstract-full').style.display = 'none'; document.getElementById('1804.09641v2-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 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </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 version. 33 pages, 28 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2018 JINST 13 P08023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.06039">arXiv:1802.06039</a> <span> [<a href="https://arxiv.org/pdf/1802.06039">pdf</a>, <a href="https://arxiv.org/format/1802.06039">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="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="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.101.052002">10.1103/PhysRevD.101.052002 <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 LUX-ZEPLIN (LZ) dark matter experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/hep-ex?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/hep-ex?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a>, <a href="/search/hep-ex?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J+K">J. K. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Carels%2C+C">C. Carels</a>, <a href="/search/hep-ex?searchtype=author&query=Carlsmith%2C+D+L">D. L. Carlsmith</a>, <a href="/search/hep-ex?searchtype=author&query=Carlson%2C+B">B. Carlson</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="1802.06039v2-abstract-short" style="display: inline;"> LUX-ZEPLIN (LZ) is a next generation dark matter direct detection experiment that will operate 4850 feet underground at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, USA. Using a two-phase xenon detector with an active mass of 7~tonnes, LZ will search primarily for low-energy interactions with Weakly Interacting Massive Particles (WIMPs), which are hypothesized to make up… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.06039v2-abstract-full').style.display = 'inline'; document.getElementById('1802.06039v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.06039v2-abstract-full" style="display: none;"> LUX-ZEPLIN (LZ) is a next generation dark matter direct detection experiment that will operate 4850 feet underground at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, USA. Using a two-phase xenon detector with an active mass of 7~tonnes, LZ will search primarily for low-energy interactions with Weakly Interacting Massive Particles (WIMPs), which are hypothesized to make up the dark matter in our galactic halo. In this paper, the projected WIMP sensitivity of LZ is presented based on the latest background estimates and simulations of the detector. For a 1000~live day run using a 5.6~tonne fiducial mass, LZ is projected to exclude at 90\% confidence level spin-independent WIMP-nucleon cross sections above $1.4 \times 10^{-48}$~cm$^{2}$ for a 40~$\mathrm{GeV}/c^{2}$ mass WIMP. Additionally, a $5蟽$ discovery potential is projected reaching cross sections below the exclusion limits of recent experiments. For spin-dependent WIMP-neutron(-proton) scattering, a sensitivity of $2.3 \times 10^{-43}$~cm$^{2}$ ($7.1 \times 10^{-42}$~cm$^{2}$) for a 40~$\mathrm{GeV}/c^{2}$ mass WIMP is expected. With underground installation well underway, LZ is on track for commissioning at SURF in 2020. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.06039v2-abstract-full').style.display = 'none'; document.getElementById('1802.06039v2-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </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, 11 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 101, 052002 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.07670">arXiv:1710.07670</a> <span> [<a href="https://arxiv.org/pdf/1710.07670">pdf</a>, <a href="https://arxiv.org/ps/1710.07670">ps</a>, <a href="https://arxiv.org/format/1710.07670">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div 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.97.072007">10.1103/PhysRevD.97.072007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for nucleon decays with EXO-200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Bayerlein%2C+R">R. Bayerlein</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Cree%2C+W">W. Cree</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Daughhetee%2C+J">J. Daughhetee</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Didberidze%2C+T">T. Didberidze</a> , et al. (70 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1710.07670v5-abstract-short" style="display: inline;"> A search for instability of nucleons bound in $^{136}$Xe nuclei is reported with 223 kg$\cdot$yr exposure of $^{136}$Xe in the EXO-200 experiment. Lifetime limits of 3.3$\times 10^{23}$ and 1.9$\times 10^{23}$ yrs are established for nucleon decay to $^{133}$Sb and $^{133}$Te, respectively. These are the most stringent to date, exceeding the prior decay limits by a factor of 9 and 7, respectively. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.07670v5-abstract-full" style="display: none;"> A search for instability of nucleons bound in $^{136}$Xe nuclei is reported with 223 kg$\cdot$yr exposure of $^{136}$Xe in the EXO-200 experiment. Lifetime limits of 3.3$\times 10^{23}$ and 1.9$\times 10^{23}$ yrs are established for nucleon decay to $^{133}$Sb and $^{133}$Te, respectively. These are the most stringent to date, exceeding the prior decay limits by a factor of 9 and 7, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.07670v5-abstract-full').style.display = 'none'; document.getElementById('1710.07670v5-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 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 97, 072007 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.08707">arXiv:1707.08707</a> <span> [<a href="https://arxiv.org/pdf/1707.08707">pdf</a>, <a href="https://arxiv.org/format/1707.08707">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.120.072701">10.1103/PhysRevLett.120.072701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Neutrinoless Double-Beta Decay with the Upgraded EXO-200 Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Bayerlein%2C+R">R. Bayerlein</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Cree%2C+W">W. Cree</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Daughhetee%2C+J">J. Daughhetee</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Didberidze%2C+T">T. Didberidze</a> , et al. (68 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="1707.08707v2-abstract-short" style="display: inline;"> Results from a search for neutrinoless double-beta decay $0谓尾尾$ of $^{136}$Xe are presented using the first year of data taken with the upgraded EXO-200 detector. Relative to previous searches by EXO-200, the energy resolution of the detector has been improved to $蟽/E$=1.23%, the electric field in the drift region has been raised by 50%, and a system to suppress radon in the volume between the cry… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.08707v2-abstract-full').style.display = 'inline'; document.getElementById('1707.08707v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.08707v2-abstract-full" style="display: none;"> Results from a search for neutrinoless double-beta decay $0谓尾尾$ of $^{136}$Xe are presented using the first year of data taken with the upgraded EXO-200 detector. Relative to previous searches by EXO-200, the energy resolution of the detector has been improved to $蟽/E$=1.23%, the electric field in the drift region has been raised by 50%, and a system to suppress radon in the volume between the cryostat and lead shielding has been implemented. In addition, analysis techniques that improve topological discrimination between $0谓尾尾$ and background events have been developed. Incorporating these hardware and analysis improvements, the median 90% confidence level $0谓尾尾$ half-life sensitivity after combining with the full data set acquired before the upgrade has increased 2-fold to $3.7 \times 10^{25}$ yr. No statistically significant evidence for $0谓尾尾$ is observed, leading to a lower limit on the $0谓尾尾$ half-life of $1.8\times10^{25}$ yr at the 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.08707v2-abstract-full').style.display = 'none'; document.getElementById('1707.08707v2-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 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </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, 4 figures, final version submitted to PRL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 120, 072701 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1704.05042">arXiv:1704.05042</a> <span> [<a href="https://arxiv.org/pdf/1704.05042">pdf</a>, <a href="https://arxiv.org/format/1704.05042">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.96.092001">10.1103/PhysRevD.96.092001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searches for Double Beta Decay of $^{134}$Xe with EXO-200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+E">EXO-200 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ex?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Bayerlein%2C+R">R. Bayerlein</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Cree%2C+W">W. Cree</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Daughhetee%2C+J">J. Daughhetee</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a> , et al. (69 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="1704.05042v2-abstract-short" style="display: inline;"> Searches for double beta decay of $^{134}$Xe were performed with EXO-200, a single-phase liquid xenon detector designed to search for neutrinoless double beta decay of $^{136}$Xe. Using an exposure of $29.6\text{ kg}\!\cdot\!\text{yr}$, the lower limits of $\text{T}_{1/2}^{2谓尾\!尾}>8.7\cdot10^{20}\text{ yr}$ and $\text{T}_{1/2}^{0谓尾\!尾}>1.1\cdot10^{23}\text{ yr}$ at 90% confidence level were derive… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.05042v2-abstract-full').style.display = 'inline'; document.getElementById('1704.05042v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.05042v2-abstract-full" style="display: none;"> Searches for double beta decay of $^{134}$Xe were performed with EXO-200, a single-phase liquid xenon detector designed to search for neutrinoless double beta decay of $^{136}$Xe. Using an exposure of $29.6\text{ kg}\!\cdot\!\text{yr}$, the lower limits of $\text{T}_{1/2}^{2谓尾\!尾}>8.7\cdot10^{20}\text{ yr}$ and $\text{T}_{1/2}^{0谓尾\!尾}>1.1\cdot10^{23}\text{ yr}$ at 90% confidence level were derived, with corresponding half-life sensitivities of $1.2\cdot10^{21}\text{ yr}$ and $1.9\cdot10^{23}\text{ yr}$. These limits exceed those in the literature for $^{134}$Xe, improving by factors of nearly $10^{5}$ and 2 for the two antineutrino and neutrinoless modes, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.05042v2-abstract-full').style.display = 'none'; document.getElementById('1704.05042v2-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 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2017. </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, 4 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 96, 092001 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.09144">arXiv:1703.09144</a> <span> [<a href="https://arxiv.org/pdf/1703.09144">pdf</a>, <a href="https://arxiv.org/format/1703.09144">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"> LUX-ZEPLIN (LZ) Technical Design Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Mount%2C+B+J">B. J. Mount</a>, <a href="/search/hep-ex?searchtype=author&query=Hans%2C+S">S. Hans</a>, <a href="/search/hep-ex?searchtype=author&query=Rosero%2C+R">R. Rosero</a>, <a href="/search/hep-ex?searchtype=author&query=Yeh%2C+M">M. Yeh</a>, <a href="/search/hep-ex?searchtype=author&query=Chan%2C+C">C. Chan</a>, <a href="/search/hep-ex?searchtype=author&query=Gaitskell%2C+R+J">R. J. Gaitskell</a>, <a href="/search/hep-ex?searchtype=author&query=Huang%2C+D+Q">D. Q. Huang</a>, <a href="/search/hep-ex?searchtype=author&query=Makkinje%2C+J">J. Makkinje</a>, <a href="/search/hep-ex?searchtype=author&query=Malling%2C+D+C">D. C. Malling</a>, <a href="/search/hep-ex?searchtype=author&query=Pangilinan%2C+M">M. Pangilinan</a>, <a href="/search/hep-ex?searchtype=author&query=Rhyne%2C+C+A">C. A. Rhyne</a>, <a href="/search/hep-ex?searchtype=author&query=Taylor%2C+W+C">W. C. Taylor</a>, <a href="/search/hep-ex?searchtype=author&query=Verbus%2C+J+R">J. R. Verbus</a>, <a href="/search/hep-ex?searchtype=author&query=Kim%2C+Y+D">Y. D. Kim</a>, <a href="/search/hep-ex?searchtype=author&query=Lee%2C+H+S">H. S. Lee</a>, <a href="/search/hep-ex?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/hep-ex?searchtype=author&query=Leonard%2C+D+S">D. S. Leonard</a>, <a href="/search/hep-ex?searchtype=author&query=Li%2C+J">J. Li</a>, <a href="/search/hep-ex?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/hep-ex?searchtype=author&query=Cottle%2C+A">A. Cottle</a>, <a href="/search/hep-ex?searchtype=author&query=Lippincott%2C+W+H">W. H. Lippincott</a>, <a href="/search/hep-ex?searchtype=author&query=Markley%2C+D+J">D. J. Markley</a>, <a href="/search/hep-ex?searchtype=author&query=Martin%2C+T+J">T. J. Martin</a>, <a href="/search/hep-ex?searchtype=author&query=Sarychev%2C+M">M. Sarychev</a>, <a href="/search/hep-ex?searchtype=author&query=Tope%2C+T+E">T. E. Tope</a> , et al. (237 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="1703.09144v1-abstract-short" style="display: inline;"> In this Technical Design Report (TDR) we describe the LZ detector to be built at the Sanford Underground Research Facility (SURF). The LZ dark matter experiment is designed to achieve sensitivity to a WIMP-nucleon spin-independent cross section of three times ten to the negative forty-eighth square centimeters. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.09144v1-abstract-full" style="display: none;"> In this Technical Design Report (TDR) we describe the LZ detector to be built at the Sanford Underground Research Facility (SURF). The LZ dark matter experiment is designed to achieve sensitivity to a WIMP-nucleon spin-independent cross section of three times ten to the negative forty-eighth square centimeters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.09144v1-abstract-full').style.display = 'none'; document.getElementById('1703.09144v1-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 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </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">392 pages. Submitted to the Department of Energy as part of the documentation for the Critical Decision Numbers Two and Three (CD-2 and CD-3) management processes. Report also available by chapter at <a href="http://hep.ucsb.edu/LZ/TDR/">this URL</a></span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LBNL-1007256 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1702.02646">arXiv:1702.02646</a> <span> [<a href="https://arxiv.org/pdf/1702.02646">pdf</a>, <a href="https://arxiv.org/format/1702.02646">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/10.1016/j.astropartphys.2017.09.002">10.1016/j.astropartphys.2017.09.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Identification of Radiopure Titanium for the LZ Dark Matter Experiment and Future Rare Event Searches </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/hep-ex?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/hep-ex?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/hep-ex?searchtype=author&query=Bolozdynya%2C+A">A. Bolozdynya</a>, <a href="/search/hep-ex?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/hep-ex?searchtype=author&query=Bramante%2C+R">R. Bramante</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/hep-ex?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/hep-ex?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a> , et al. (180 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="1702.02646v5-abstract-short" style="display: inline;"> The LUX-ZEPLIN (LZ) experiment will search for dark matter particle interactions with a detector containing a total of 10 tonnes of liquid xenon within a double-vessel cryostat. The large mass and proximity of the cryostat to the active detector volume demand the use of material with extremely low intrinsic radioactivity. We report on the radioassay campaign conducted to identify suitable metals,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.02646v5-abstract-full').style.display = 'inline'; document.getElementById('1702.02646v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.02646v5-abstract-full" style="display: none;"> The LUX-ZEPLIN (LZ) experiment will search for dark matter particle interactions with a detector containing a total of 10 tonnes of liquid xenon within a double-vessel cryostat. The large mass and proximity of the cryostat to the active detector volume demand the use of material with extremely low intrinsic radioactivity. We report on the radioassay campaign conducted to identify suitable metals, the determination of factors limiting radiopure production, and the selection of titanium for construction of the LZ cryostat and other detector components. This titanium has been measured with activities of $^{238}$U$_{e}$~$<$1.6~mBq/kg, $^{238}$U$_{l}$~$<$0.09~mBq/kg, $^{232}$Th$_{e}$~$=0.28\pm 0.03$~mBq/kg, $^{232}$Th$_{l}$~$=0.25\pm 0.02$~mBq/kg, $^{40}$K~$<$0.54~mBq/kg, and $^{60}$Co~$<$0.02~mBq/kg (68\% CL). Such low intrinsic activities, which are some of the lowest ever reported for titanium, enable its use for future dark matter and other rare event searches. Monte Carlo simulations have been performed to assess the expected background contribution from the LZ cryostat with this radioactivity. In 1,000 days of WIMP search exposure of a 5.6-tonne fiducial mass, the cryostat will contribute only a mean background of $0.160\pm0.001$(stat)$\pm0.030$(sys) counts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.02646v5-abstract-full').style.display = 'none'; document.getElementById('1702.02646v5-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 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 3 figures, accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.04467">arXiv:1609.04467</a> <span> [<a href="https://arxiv.org/pdf/1609.04467">pdf</a>, <a href="https://arxiv.org/format/1609.04467">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/10.1103/PhysRevC.95.025502">10.1103/PhysRevC.95.025502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the Drift Velocity and Transverse Diffusion of Electrons in Liquid Xenon with the EXO-200 Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+E">EXO-200 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Burenkov%2C+A">A. Burenkov</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Daughhetee%2C+J">J. Daughhetee</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Didberidze%2C+T">T. Didberidze</a>, <a href="/search/hep-ex?searchtype=author&query=Dilling%2C+J">J. Dilling</a> , et al. (63 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="1609.04467v2-abstract-short" style="display: inline;"> The EXO-200 Collaboration is searching for neutrinoless double beta decay using a liquid xenon (LXe) time projection chamber. This measurement relies on modeling the transport of charge deposits produced by interactions in the LXe to allow discrimination between signal and background events. Here we present measurements of the transverse diffusion constant and drift velocity of electrons at drift… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.04467v2-abstract-full').style.display = 'inline'; document.getElementById('1609.04467v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.04467v2-abstract-full" style="display: none;"> The EXO-200 Collaboration is searching for neutrinoless double beta decay using a liquid xenon (LXe) time projection chamber. This measurement relies on modeling the transport of charge deposits produced by interactions in the LXe to allow discrimination between signal and background events. Here we present measurements of the transverse diffusion constant and drift velocity of electrons at drift fields between 20~V/cm and 615~V/cm using EXO-200 data. At the operating field of 380~V/cm EXO-200 measures a drift velocity of 1.705$_{-0.010}^{+0.014}$~mm/$渭$s and a transverse diffusion coefficient of 55$\pm$4~cm$^2$/s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.04467v2-abstract-full').style.display = 'none'; document.getElementById('1609.04467v2-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 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 7 figures, added minor clarifications recommended by the reviewer on E-field non-uniformities, minor edits to formatting of figures to conform with journal requirements</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.07155">arXiv:1606.07155</a> <span> [<a href="https://arxiv.org/pdf/1606.07155">pdf</a>, <a href="https://arxiv.org/ps/1606.07155">ps</a>, <a href="https://arxiv.org/format/1606.07155">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8205/829/2/L34">10.3847/2041-8205/829/2/L34 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for electron antineutrinos associated with gravitational wave events GW150914 and GW151226 using KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashi%2C+A">A. Hayashi</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Karino%2C+Y">Y. Karino</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/hep-ex?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/hep-ex?searchtype=author&query=Ozaki%2C+H">H. Ozaki</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/hep-ex?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/hep-ex?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/hep-ex?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/hep-ex?searchtype=author&query=Takai%2C+T">T. Takai</a>, <a href="/search/hep-ex?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/hep-ex?searchtype=author&query=Teraoka%2C+Y">Y. Teraoka</a>, <a href="/search/hep-ex?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1606.07155v2-abstract-short" style="display: inline;"> We present a search for low energy antineutrino events coincident with the gravitational wave events GW150914 and GW151226, and the candidate event LVT151012 using KamLAND, a kiloton-scale antineutrino detector. We find no inverse beta-decay neutrino events within $\pm 500$ seconds of either gravitational wave signal. This non-detection is used to constrain the electron antineutrino fluence and th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.07155v2-abstract-full').style.display = 'inline'; document.getElementById('1606.07155v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.07155v2-abstract-full" style="display: none;"> We present a search for low energy antineutrino events coincident with the gravitational wave events GW150914 and GW151226, and the candidate event LVT151012 using KamLAND, a kiloton-scale antineutrino detector. We find no inverse beta-decay neutrino events within $\pm 500$ seconds of either gravitational wave signal. This non-detection is used to constrain the electron antineutrino fluence and the luminosity of the astrophysical sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.07155v2-abstract-full').style.display = 'none'; document.getElementById('1606.07155v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 4 figures, as published in ApJL. Updated to replace power law spectrum with Fermi Dirac spectrum</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.829, L34, 2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.06552">arXiv:1605.06552</a> <span> [<a href="https://arxiv.org/pdf/1605.06552">pdf</a>, <a href="https://arxiv.org/format/1605.06552">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/11/07/P07015">10.1088/1748-0221/11/07/P07015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Optimal Energy Estimator to Reduce Correlated Noise for the EXO-200 Light Readout </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+E">EXO-200 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+C+G">C. G. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Hall%2C+C">C. Hall</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Burenkov%2C+A">A. Burenkov</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cen%2C+W+R">W. R. Cen</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Didberidze%2C+T">T. Didberidze</a> , et al. (63 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="1605.06552v2-abstract-short" style="display: inline;"> The energy resolution of the EXO-200 detector is limited by electronics noise in the measurement of the scintillation response. Here we present a new technique to extract optimal scintillation energy measurements for signals split across multiple channels in the presence of correlated noise. The implementation of these techniques improves the energy resolution of the detector at the neutrinoless d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.06552v2-abstract-full').style.display = 'inline'; document.getElementById('1605.06552v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.06552v2-abstract-full" style="display: none;"> The energy resolution of the EXO-200 detector is limited by electronics noise in the measurement of the scintillation response. Here we present a new technique to extract optimal scintillation energy measurements for signals split across multiple channels in the presence of correlated noise. The implementation of these techniques improves the energy resolution of the detector at the neutrinoless double beta decay Q-value from $\left[1.9641\pm 0.0039\right]\%$ to $\left[1.5820\pm 0.0044\right]\%$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.06552v2-abstract-full').style.display = 'none'; document.getElementById('1605.06552v2-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 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 8 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 11 P07015 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.06835">arXiv:1512.06835</a> <span> [<a href="https://arxiv.org/pdf/1512.06835">pdf</a>, <a href="https://arxiv.org/format/1512.06835">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/10.1088/1475-7516/2016/04/029">10.1088/1475-7516/2016/04/029 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmogenic Backgrounds to 0谓尾尾 in EXO-200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+E">EXO-200 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Auty%2C+D+J">D. J. Auty</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Burenkov%2C+A">A. Burenkov</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Didberidze%2C+T">T. Didberidze</a>, <a href="/search/hep-ex?searchtype=author&query=Dilling%2C+J">J. Dilling</a>, <a href="/search/hep-ex?searchtype=author&query=Dolgolenko%2C+A">A. Dolgolenko</a> , et al. (63 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="1512.06835v2-abstract-short" style="display: inline;"> As neutrinoless double-beta decay experiments become more sensitive and intrinsic radioactivity in detector materials is reduced, previously minor contributions to the background must be understood and eliminated. With this in mind, cosmogenic backgrounds have been studied with the EXO-200 experiment. Using the EXO-200 TPC, the muon flux (through a flat horizontal surface) underground at the Waste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.06835v2-abstract-full').style.display = 'inline'; document.getElementById('1512.06835v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.06835v2-abstract-full" style="display: none;"> As neutrinoless double-beta decay experiments become more sensitive and intrinsic radioactivity in detector materials is reduced, previously minor contributions to the background must be understood and eliminated. With this in mind, cosmogenic backgrounds have been studied with the EXO-200 experiment. Using the EXO-200 TPC, the muon flux (through a flat horizontal surface) underground at the Waste Isolation Pilot Plant (WIPP) has been measured to be 桅 = 4.07 $\pm$ 0.14 (sys) $\pm$ 0.03 (stat) $\times$ $10^{-7}$cm$^{-2}$ s$^{-1}$, with a vertical intensity of $I_{v}$ = 2.97$^{+0.14}_{-0.13}$ (sys) $\pm$ 0.02 (stat) $\times$ $10^{-7}$cm$^{-2}$ s$^{-1}$ sr$^{-1}$. Simulations of muon-induced backgrounds identified several potential cosmogenic radionuclides, though only 137Xe is a significant background for the 136Xe 0谓尾尾 search with EXO-200. Muon-induced neutron backgrounds were measured using 纬-rays from neutron capture on the detector materials. This provided a measurement of 137Xe yield, and a test of the accuracy of the neutron production and transport simulations. The independently measured rates of 136Xe neutron capture and of 137Xe decay agree within uncertainties. Geant4 and FLUKA simulations were performed to estimate neutron capture rates, and these estimates agreed to within ~40% or better with measurements. The ability to identify 136Xe(n,纬) events will allow for rejection of 137Xe backgrounds in future 0谓尾尾 analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.06835v2-abstract-full').style.display = 'none'; document.getElementById('1512.06835v2-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 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in JCAP, 29 pages, 13 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/1511.04770">arXiv:1511.04770</a> <span> [<a href="https://arxiv.org/pdf/1511.04770">pdf</a>, <a href="https://arxiv.org/format/1511.04770">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.93.035501">10.1103/PhysRevC.93.035501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for $2谓尾尾$ decay of $^{136}$Xe to the 0$_1^+$ excited state of $^{136}$Ba with EXO-200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+E">EXO-200 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Auty%2C+D+J">D. J. Auty</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Burenkov%2C+A">A. Burenkov</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Chaves%2C+J">J. Chaves</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Didberidze%2C+T">T. Didberidze</a>, <a href="/search/hep-ex?searchtype=author&query=Dilling%2C+J">J. Dilling</a> , et al. (67 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="1511.04770v2-abstract-short" style="display: inline;"> EXO-200 is a single phase liquid xenon detector designed to search for neutrinoless double-beta decay of $^{136}$Xe to the ground state of $^{136}$Ba. We report here on a search for the two-neutrino double-beta decay of $^{136}$Xe to the first $0^+$ excited state, $0^+_1$, of $^{136}$Ba based on a 100 kg$\cdot$yr exposure of $^{136}$Xe. Using a specialized analysis employing a machine learning alg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.04770v2-abstract-full').style.display = 'inline'; document.getElementById('1511.04770v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.04770v2-abstract-full" style="display: none;"> EXO-200 is a single phase liquid xenon detector designed to search for neutrinoless double-beta decay of $^{136}$Xe to the ground state of $^{136}$Ba. We report here on a search for the two-neutrino double-beta decay of $^{136}$Xe to the first $0^+$ excited state, $0^+_1$, of $^{136}$Ba based on a 100 kg$\cdot$yr exposure of $^{136}$Xe. Using a specialized analysis employing a machine learning algorithm, we obtain a 90% CL half-life sensitivity of $1.7 \times 10^{24}$ yr. We find no statistically significant evidence for the $2谓尾尾$ decay to the excited state resulting in a lower limit of $T^{2谓}_{1/2}$ ($0^+ \rightarrow 0^+_1$) $> 6.9 \times 10^{23}$ yr at 90% CL. This observed limit is consistent with the estimated half-life of $2.5\times10^{25}$ yr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.04770v2-abstract-full').style.display = 'none'; document.getElementById('1511.04770v2-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 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 93, 035501 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.02910">arXiv:1509.02910</a> <span> [<a href="https://arxiv.org/pdf/1509.02910">pdf</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"> LUX-ZEPLIN (LZ) Conceptual Design Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ex?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/hep-ex?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/hep-ex?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/hep-ex?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/hep-ex?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ex?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/hep-ex?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ex?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/hep-ex?searchtype=author&query=Bolozdynya%2C+A+I">A. I. Bolozdynya</a>, <a href="/search/hep-ex?searchtype=author&query=Boulton%2C+E+M">E. M. Boulton</a>, <a href="/search/hep-ex?searchtype=author&query=Bramante%2C+R">R. Bramante</a>, <a href="/search/hep-ex?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/hep-ex?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a>, <a href="/search/hep-ex?searchtype=author&query=Bunker%2C+R">R. Bunker</a>, <a href="/search/hep-ex?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J+K">J. K. Busenitz</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="1509.02910v2-abstract-short" style="display: inline;"> The design and performance of the LUX-ZEPLIN (LZ) detector is described as of March 2015 in this Conceptual Design Report. LZ is a second-generation dark-matter detector with the potential for unprecedented sensitivity to weakly interacting massive particles (WIMPs) of masses from a few GeV/c2 to hundreds of TeV/c2. With total liquid xenon mass of about 10 tonnes, LZ will be the most sensitive exp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02910v2-abstract-full').style.display = 'inline'; document.getElementById('1509.02910v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.02910v2-abstract-full" style="display: none;"> The design and performance of the LUX-ZEPLIN (LZ) detector is described as of March 2015 in this Conceptual Design Report. LZ is a second-generation dark-matter detector with the potential for unprecedented sensitivity to weakly interacting massive particles (WIMPs) of masses from a few GeV/c2 to hundreds of TeV/c2. With total liquid xenon mass of about 10 tonnes, LZ will be the most sensitive experiment for WIMPs in this mass region by the end of the decade. This report describes in detail the design of the LZ technical systems. Expected backgrounds are quantified and the performance of the experiment is presented. The LZ detector will be located at the Sanford Underground Research Facility in South Dakota. The organization of the LZ Project and a summary of the expected cost and current schedule are given. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02910v2-abstract-full').style.display = 'none'; document.getElementById('1509.02910v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">278 pages. Submitted to the Department of Energy as part of the documentation for the Critical Decision Number One (CD-1) management process. Report also available by chapter at http://hep.ucsb.edu/LZ/CDR. This version includes corrections of minor typographic errors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LBNL-190005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1506.01175">arXiv:1506.01175</a> <span> [<a href="https://arxiv.org/pdf/1506.01175">pdf</a>, <a href="https://arxiv.org/ps/1506.01175">ps</a>, <a href="https://arxiv.org/format/1506.01175">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0004-637X/818/1/91">10.3847/0004-637X/818/1/91 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Asakura%2C+K">K. Asakura</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Ishikawa%2C+T">T. Ishikawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ishio%2C+S">S. Ishio</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/hep-ex?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/hep-ex?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/hep-ex?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/hep-ex?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/hep-ex?searchtype=author&query=Tachibana%2C+H">H. Tachibana</a>, <a href="/search/hep-ex?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/hep-ex?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/hep-ex?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1506.01175v4-abstract-short" style="display: inline;"> In the late stages of nuclear burning for massive stars ($M>8~M_{\sun}$), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01175v4-abstract-full').style.display = 'inline'; document.getElementById('1506.01175v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.01175v4-abstract-full" style="display: none;"> In the late stages of nuclear burning for massive stars ($M>8~M_{\sun}$), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta decay on free hydrogen. This is the golden channel for liquid scintillator detectors because the coincidence signature allows for significant reductions in background signals. We find that the kiloton-scale liquid scintillator detector KamLAND can detect these pre-supernova neutrinos from a star with a mass of $25~M_{\sun}$ at a distance less than 690~pc with 3$蟽$ significance before the supernova. This limit is dependent on the neutrino mass ordering and background levels. KamLAND takes data continuously and can provide a supernova alert to the community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01175v4-abstract-full').style.display = 'none'; document.getElementById('1506.01175v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 6 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.06241">arXiv:1503.06241</a> <span> [<a href="https://arxiv.org/pdf/1503.06241">pdf</a>, <a href="https://arxiv.org/format/1503.06241">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.92.015503">10.1103/PhysRevC.92.015503 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigation of radioactivity-induced backgrounds in EXO-200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albert%2C+J+B">J. B. Albert</a>, <a href="/search/hep-ex?searchtype=author&query=Auty%2C+D+J">D. J. Auty</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P+S">P. S. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Benitez-Medina%2C+C">C. Benitez-Medina</a>, <a href="/search/hep-ex?searchtype=author&query=Breidenbach%2C+M">M. Breidenbach</a>, <a href="/search/hep-ex?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ex?searchtype=author&query=Burenkov%2C+A">A. Burenkov</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Chambers%2C+C">C. Chambers</a>, <a href="/search/hep-ex?searchtype=author&query=Cleveland%2C+B">B. Cleveland</a>, <a href="/search/hep-ex?searchtype=author&query=Coon%2C+M">M. Coon</a>, <a href="/search/hep-ex?searchtype=author&query=Craycraft%2C+A">A. Craycraft</a>, <a href="/search/hep-ex?searchtype=author&query=Daniels%2C+T">T. Daniels</a>, <a href="/search/hep-ex?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/hep-ex?searchtype=author&query=Daugherty%2C+S+J">S. J. Daugherty</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+C+G">C. G. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Davis%2C+J">J. Davis</a>, <a href="/search/hep-ex?searchtype=author&query=Delaquis%2C+S">S. Delaquis</a>, <a href="/search/hep-ex?searchtype=author&query=Der+Mesrobian-Kabakian%2C+A">A. Der Mesrobian-Kabakian</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Didberidze%2C+T">T. Didberidze</a>, <a href="/search/hep-ex?searchtype=author&query=Dolgolenko%2C+A">A. Dolgolenko</a>, <a href="/search/hep-ex?searchtype=author&query=Dolinski%2C+M+J">M. J. Dolinski</a> , et al. (61 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1503.06241v2-abstract-short" style="display: inline;"> The search for neutrinoless double-beta decay (0谓尾尾) requires extremely low background and a good understanding of their sources and their influence on the rate in the region of parameter space relevant to the 0谓尾尾 signal. We report on studies of various 尾- and 纬-backgrounds in the liquid- xenon-based EXO-200 0谓尾尾 experiment. With this work we try to better understand the location and strength of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06241v2-abstract-full').style.display = 'inline'; document.getElementById('1503.06241v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.06241v2-abstract-full" style="display: none;"> The search for neutrinoless double-beta decay (0谓尾尾) requires extremely low background and a good understanding of their sources and their influence on the rate in the region of parameter space relevant to the 0谓尾尾 signal. We report on studies of various 尾- and 纬-backgrounds in the liquid- xenon-based EXO-200 0谓尾尾 experiment. With this work we try to better understand the location and strength of specific background sources and compare the conclusions to radioassay results taken before and during detector construction. Finally, we discuss the implications of these studies for EXO-200 as well as for the next-generation, tonne-scale nEXO detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06241v2-abstract-full').style.display = 'none'; document.getElementById('1503.06241v2-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 7 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 92 015503 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.02137">arXiv:1503.02137</a> <span> [<a href="https://arxiv.org/pdf/1503.02137">pdf</a>, <a href="https://arxiv.org/ps/1503.02137">ps</a>, <a href="https://arxiv.org/format/1503.02137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/806/1/87">10.1088/0004-637X/806/1/87 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of electron anti-neutrinos associated with gamma-ray bursts using KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Asakura%2C+K">K. Asakura</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/hep-ex?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/hep-ex?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/hep-ex?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/hep-ex?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/hep-ex?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/hep-ex?searchtype=author&query=Ishikawa%2C+T">T. Ishikawa</a>, <a href="/search/hep-ex?searchtype=author&query=Ishio%2C+S">S. Ishio</a>, <a href="/search/hep-ex?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/hep-ex?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/hep-ex?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/hep-ex?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/hep-ex?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/hep-ex?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/hep-ex?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/hep-ex?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/hep-ex?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/hep-ex?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/hep-ex?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/hep-ex?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/hep-ex?searchtype=author&query=Tachibana%2C+H">H. Tachibana</a>, <a href="/search/hep-ex?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/hep-ex?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1503.02137v2-abstract-short" style="display: inline;"> We search for electron anti-neutrinos ($\overline谓_e$) from long and short-duration gamma-ray bursts~(GRBs) using data taken by the KamLAND detector from August 2002 to June 2013. No statistically significant excess over the background level is found. We place the tightest upper limits on $\overline谓_e$ fluence from GRBs below 7 MeV and place first constraints on the relation between… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02137v2-abstract-full').style.display = 'inline'; document.getElementById('1503.02137v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.02137v2-abstract-full" style="display: none;"> We search for electron anti-neutrinos ($\overline谓_e$) from long and short-duration gamma-ray bursts~(GRBs) using data taken by the KamLAND detector from August 2002 to June 2013. No statistically significant excess over the background level is found. We place the tightest upper limits on $\overline谓_e$ fluence from GRBs below 7 MeV and place first constraints on the relation between $\overline谓_e$ luminosity and effective temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02137v2-abstract-full').style.display = 'none'; document.getElementById('1503.02137v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages and 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 806 87 2015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1502.07837">arXiv:1502.07837</a> <span> [<a href="https://arxiv.org/pdf/1502.07837">pdf</a>, <a href="https://arxiv.org/format/1502.07837">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1109/TNS.2015.2453932">10.1109/TNS.2015.2453932 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of Silicon Photomultipliers for nEXO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Ostrovskiy%2C+I">I. Ostrovskiy</a>, <a href="/search/hep-ex?searchtype=author&query=Retiere%2C+F">F. Retiere</a>, <a href="/search/hep-ex?searchtype=author&query=Auty%2C+D">D. Auty</a>, <a href="/search/hep-ex?searchtype=author&query=Dalmasson%2C+J">J. Dalmasson</a>, <a href="/search/hep-ex?searchtype=author&query=Didberidze%2C+T">T. Didberidze</a>, <a href="/search/hep-ex?searchtype=author&query=DeVoe%2C+R">R. DeVoe</a>, <a href="/search/hep-ex?searchtype=author&query=Gratta%2C+G">G. Gratta</a>, <a href="/search/hep-ex?searchtype=author&query=Huth%2C+L">L. Huth</a>, <a href="/search/hep-ex?searchtype=author&query=James%2C+L">L. James</a>, <a href="/search/hep-ex?searchtype=author&query=Lupin-Jimenez%2C+L">L. Lupin-Jimenez</a>, <a href="/search/hep-ex?searchtype=author&query=Ohmert%2C+N">N. Ohmert</a>, <a href="/search/hep-ex?searchtype=author&query=Piepke%2C+A">A. Piepke</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="1502.07837v2-abstract-short" style="display: inline;"> Silicon Photomultipliers (SiPMs) are attractive candidates for light detectors for next generation liquid xenon double-beta decay experiments, like nEXO. In this paper we discuss the requirements that the SiPMs must satisfy in order to be suitable for nEXO and similar experiments, describe the two test setups operated by the nEXO collaboration, and present the results of characterization of SiPMs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.07837v2-abstract-full').style.display = 'inline'; document.getElementById('1502.07837v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1502.07837v2-abstract-full" style="display: none;"> Silicon Photomultipliers (SiPMs) are attractive candidates for light detectors for next generation liquid xenon double-beta decay experiments, like nEXO. In this paper we discuss the requirements that the SiPMs must satisfy in order to be suitable for nEXO and similar experiments, describe the two test setups operated by the nEXO collaboration, and present the results of characterization of SiPMs from several vendors. In particular, we find that the photon detection efficiency at the peak of xenon scintillation light emission (175-178 nm) approaches the nEXO requirements for tested FBK and Hamamatsu devices. Additionally, the nEXO collaboration performed radioassay of several grams of bare FBK devices using neutron activation analysis, indicating levels of 40K, 232Th, and 238U of the order of <0.15, (6.9e10-4 - 1.3e10-2), and <0.11 mBq/kg, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.07837v2-abstract-full').style.display = 'none'; document.getElementById('1502.07837v2-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 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Version as accepted to Transaction of Nuclear Science. 12 pages, 15 figures (one figure removed following peer review), 8 tables (1 table added following peer review)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Science, IEEE Transactions on , vol.62, no.4, pp.1825,1836, Aug. 2015 </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=Piepke%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Piepke%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Piepke%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" 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