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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.19016">arXiv:2410.19016</a> <span> [<a href="https://arxiv.org/pdf/2410.19016">pdf</a>, <a href="https://arxiv.org/format/2410.19016">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Neutrinoless Double Beta Decay Sensitivity of the XLZD Rare Event Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/physics?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/physics?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/physics?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a> , et al. (419 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.19016v1-abstract-short" style="display: inline;"> The XLZD collaboration is developing a two-phase xenon time projection chamber with an active mass of 60 to 80 t capable of probing the remaining WIMP-nucleon interaction parameter space down to the so-called neutrino fog. In this work we show that, based on the performance of currently operating detectors using the same technology and a realistic reduction of radioactivity in detector materials,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19016v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19016v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19016v1-abstract-full" style="display: none;"> The XLZD collaboration is developing a two-phase xenon time projection chamber with an active mass of 60 to 80 t capable of probing the remaining WIMP-nucleon interaction parameter space down to the so-called neutrino fog. In this work we show that, based on the performance of currently operating detectors using the same technology and a realistic reduction of radioactivity in detector materials, such an experiment will also be able to competitively search for neutrinoless double beta decay in $^{136}$Xe using a natural-abundance xenon target. XLZD can reach a 3$蟽$ discovery potential half-life of 5.7$\times$10$^{27}$ yr (and a 90% CL exclusion of 1.3$\times$10$^{28}$ yr) with 10 years of data taking, corresponding to a Majorana mass range of 7.3-31.3 meV (4.8-20.5 meV). XLZD will thus exclude the inverted neutrino mass ordering parameter space and will start to probe the normal ordering region for most of the nuclear matrix elements commonly considered by the community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19016v1-abstract-full').style.display = 'none'; document.getElementById('2410.19016v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 7 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.17137">arXiv:2410.17137</a> <span> [<a href="https://arxiv.org/pdf/2410.17137">pdf</a>, <a href="https://arxiv.org/format/2410.17137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> The XLZD Design Book: Towards the Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/physics?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/physics?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/physics?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a> , et al. (419 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.17137v1-abstract-short" style="display: inline;"> This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60-80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17137v1-abstract-full').style.display = 'inline'; document.getElementById('2410.17137v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.17137v1-abstract-full" style="display: none;"> This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60-80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generation experiments, LZ and XENONnT. A baseline design and opportunities for further optimization of the individual detector components are discussed. The experiment envisaged here has the capability to explore parameter space for Weakly Interacting Massive Particle (WIMP) dark matter down to the neutrino fog, with a 3$蟽$ evidence potential for the spin-independent WIMP-nucleon cross sections as low as $3\times10^{-49}\rm cm^2$ (at 40 GeV/c$^2$ WIMP mass). The observatory is also projected to have a 3$蟽$ observation potential of neutrinoless double-beta decay of $^{136}$Xe at a half-life of up to $5.7\times 10^{27}$ years. Additionally, it is sensitive to astrophysical neutrinos from the atmosphere, sun, and galactic supernovae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17137v1-abstract-full').style.display = 'none'; document.getElementById('2410.17137v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 14 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.17391">arXiv:2408.17391</a> <span> [<a href="https://arxiv.org/pdf/2408.17391">pdf</a>, <a href="https://arxiv.org/format/2408.17391">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="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Two-neutrino double electron capture of $^{124}$Xe in the first LUX-ZEPLIN exposure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/physics?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/physics?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/physics?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/physics?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/physics?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/physics?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/physics?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/physics?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/physics?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/physics?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/physics?searchtype=author&query=Brew%2C+C+A+J">C. A. J. Brew</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="2408.17391v1-abstract-short" style="display: inline;"> The broad physics reach of the LUX-ZEPLIN (LZ) experiment covers rare phenomena beyond the direct detection of dark matter. We report precise measurements of the extremely rare decay of $^{124}$Xe through the process of two-neutrino double electron capture (2$谓$2EC), utilizing a $1.39\,\mathrm{kg} \times \mathrm{yr}$ isotopic exposure from the first LZ science run. A half-life of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.17391v1-abstract-full').style.display = 'inline'; document.getElementById('2408.17391v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.17391v1-abstract-full" style="display: none;"> The broad physics reach of the LUX-ZEPLIN (LZ) experiment covers rare phenomena beyond the direct detection of dark matter. We report precise measurements of the extremely rare decay of $^{124}$Xe through the process of two-neutrino double electron capture (2$谓$2EC), utilizing a $1.39\,\mathrm{kg} \times \mathrm{yr}$ isotopic exposure from the first LZ science run. A half-life of $T_{1/2}^{2\nu2\mathrm{EC}} = (1.09 \pm 0.14_{\text{stat}} \pm 0.05_{\text{sys}}) \times 10^{22}\,\mathrm{yr}$ is observed with a statistical significance of $8.3\,蟽$, in agreement with literature. First empirical measurements of the KK capture fraction relative to other K-shell modes were conducted, and demonstrate consistency with respect to recent signal models at the $1.4\,蟽$ level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.17391v1-abstract-full').style.display = 'none'; document.getElementById('2408.17391v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/physics?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/physics?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/physics?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/physics?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/physics?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/physics?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/physics?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/physics?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/physics?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/physics?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/physics?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/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/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/physics?searchtype=author&query=Barillier%2C+E+E">E. E. Barillier</a>, <a href="/search/physics?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/physics?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/physics?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/physics?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/physics?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/physics?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/physics?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/physics?searchtype=author&query=Bishop%2C+E">E. Bishop</a>, <a href="/search/physics?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/physics?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/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/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/physics?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/physics?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/physics?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/physics?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/physics?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/physics?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/physics?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/physics?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/physics?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a>, <a href="/search/physics?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/2203.02309">arXiv:2203.02309</a> <span> [<a href="https://arxiv.org/pdf/2203.02309">pdf</a>, <a href="https://arxiv.org/format/2203.02309">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1361-6471/ac841a">10.1088/1361-6471/ac841a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/physics?searchtype=author&query=Aerne%2C+V">V. Aerne</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+F">F. Agostini</a>, <a href="/search/physics?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/physics?searchtype=author&query=Akshat%2C+J">J. Akshat</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/physics?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Amaro%2C+F+D">F. D. Amaro</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/physics?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/physics?searchtype=author&query=Angevaare%2C+J">J. Angevaare</a>, <a href="/search/physics?searchtype=author&query=Antochi%2C+V+C">V. C. Antochi</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/physics?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/physics?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a> , et al. (572 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.02309v1-abstract-short" style="display: inline;"> The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for Weakly Interacting Massive Particles (WIMPs), while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neut… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02309v1-abstract-full').style.display = 'inline'; document.getElementById('2203.02309v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.02309v1-abstract-full" style="display: none;"> The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for Weakly Interacting Massive Particles (WIMPs), while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neutrinos through neutrinoless double-beta decay and through a variety of astrophysical sources. A next-generation xenon-based detector will therefore be a true multi-purpose observatory to significantly advance particle physics, nuclear physics, astrophysics, solar physics, and cosmology. This review article presents the science cases for such a detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02309v1-abstract-full').style.display = 'none'; document.getElementById('2203.02309v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">77 pages, 40 figures, 1262 references</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> INT-PUB-22-003 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Phys. G: Nucl. Part. Phys. 50 (2023) 013001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.13374">arXiv:2104.13374</a> <span> [<a href="https://arxiv.org/pdf/2104.13374">pdf</a>, <a href="https://arxiv.org/format/2104.13374">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="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.104.065501">10.1103/PhysRevC.104.065501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Projected sensitivity of the LUX-ZEPLIN (LZ) experiment to the two-neutrino and neutrinoless double beta decays of $^{134}$Xe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=LUX-ZEPLIN%2C+T">The LUX-ZEPLIN</a>, <a href="/search/physics?searchtype=author&query=Collaboration"> Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Araujo%2C+H+M">H. M. Araujo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/physics?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/physics?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/physics?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/physics?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/physics?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/physics?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/physics?searchtype=author&query=Biekert%2C+A">A. Biekert</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="2104.13374v3-abstract-short" style="display: inline;"> The projected sensitivity of the LUX-ZEPLIN (LZ) experiment to two-neutrino and neutrinoless double beta decay of $^{134}$Xe is presented. LZ is a 10-tonne xenon time projection chamber optimized for the detection of dark matter particles, that is expected to start operating in 2021 at Sanford Underground Research Facility, USA. Its large mass of natural xenon provides an exceptional opportunity t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.13374v3-abstract-full').style.display = 'inline'; document.getElementById('2104.13374v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.13374v3-abstract-full" style="display: none;"> The projected sensitivity of the LUX-ZEPLIN (LZ) experiment to two-neutrino and neutrinoless double beta decay of $^{134}$Xe is presented. LZ is a 10-tonne xenon time projection chamber optimized for the detection of dark matter particles, that is expected to start operating in 2021 at Sanford Underground Research Facility, USA. Its large mass of natural xenon provides an exceptional opportunity to search for the double beta decay of $^{134}$Xe, for which xenon detectors enriched in $^{136}$Xe are less effective. For the two-neutrino decay mode, LZ is predicted to exclude values of the half-life up to 1.7$\times$10$^{24}$ years at 90% confidence level (CL), and has a three-sigma observation potential of 8.7$\times$10$^{23}$ years, approaching the predictions of nuclear models. For the neutrinoless decay mode LZ, is projected to exclude values of the half-life up to 7.3$\times$10$^{24}$ years at 90% CL. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.13374v3-abstract-full').style.display = 'none'; document.getElementById('2104.13374v3-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Version accepted for publication in Phys. Rev. C</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.08753">arXiv:2101.08753</a> <span> [<a href="https://arxiv.org/pdf/2101.08753">pdf</a>, <a href="https://arxiv.org/format/2101.08753">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Enhancing the sensitivity of the LUX-ZEPLIN (LZ) dark matter experiment to low energy signals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/physics?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/physics?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/physics?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/physics?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/physics?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/physics?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/physics?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/physics?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/physics?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/physics?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/physics?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/physics?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/physics?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/physics?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a>, <a href="/search/physics?searchtype=author&query=Blockinger%2C+G+M">G. M. Blockinger</a> , et al. (162 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.08753v1-abstract-short" style="display: inline;"> Two-phase xenon detectors, such as that at the core of the forthcoming LZ dark matter experiment, use photomultiplier tubes to sense the primary (S1) and secondary (S2) scintillation signals resulting from particle interactions in their liquid xenon target. This paper describes a simulation study exploring two techniques to lower the energy threshold of LZ to gain sensitivity to low-mass dark matt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.08753v1-abstract-full').style.display = 'inline'; document.getElementById('2101.08753v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.08753v1-abstract-full" style="display: none;"> Two-phase xenon detectors, such as that at the core of the forthcoming LZ dark matter experiment, use photomultiplier tubes to sense the primary (S1) and secondary (S2) scintillation signals resulting from particle interactions in their liquid xenon target. This paper describes a simulation study exploring two techniques to lower the energy threshold of LZ to gain sensitivity to low-mass dark matter and astrophysical neutrinos, which will be applicable to other liquid xenon detectors. The energy threshold is determined by the number of detected S1 photons; typically, these must be recorded in three or more photomultiplier channels to avoid dark count coincidences that mimic real signals. To lower this threshold: a) we take advantage of the double photoelectron emission effect, whereby a single vacuum ultraviolet photon has a $\sim20\%$ probability of ejecting two photoelectrons from a photomultiplier tube photocathode; and b) we drop the requirement of an S1 signal altogether, and use only the ionization signal, which can be detected more efficiently. For both techniques we develop signal and background models for the nominal exposure, and explore accompanying systematic effects, including the dependence on the free electron lifetime in the liquid xenon. When incorporating double photoelectron signals, we predict a factor of $\sim 4$ sensitivity improvement to the dark matter-nucleon scattering cross-section at $2.5$ GeV/c$^2$, and a factor of $\sim1.6$ increase in the solar $^8$B neutrino detection rate. Dropping the S1 requirement may allow sensitivity gains of two orders of magnitude in both cases. Finally, we apply these techniques to even lower masses by taking into account the atomic Migdal effect; this could lower the dark matter particle mass threshold to $80$ MeV/c$^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.08753v1-abstract-full').style.display = 'none'; document.getElementById('2101.08753v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 6 figures</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 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