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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/2411.09384">arXiv:2411.09384</a> <span> [<a href="https://arxiv.org/pdf/2411.09384">pdf</a>, <a href="https://arxiv.org/format/2411.09384">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Radon emanation rate measurements using liquid scintillation counting </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Sazzad%2C+A+B+M+R">A. B. M. R. Sazzad</a>, <a href="/search/physics?searchtype=author&query=Acharya%2C+P">P. Acharya</a>, <a href="/search/physics?searchtype=author&query=Back%2C+P">P. Back</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Chernyak%2C+D">D. Chernyak</a>, <a href="/search/physics?searchtype=author&query=Meng%2C+Y">Y. Meng</a>, <a href="/search/physics?searchtype=author&query=Piepke%2C+A">A. Piepke</a>, <a href="/search/physics?searchtype=author&query=Rhyne%2C+C+A">C. A. Rhyne</a>, <a href="/search/physics?searchtype=author&query=Tsang%2C+R">R. Tsang</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="2411.09384v1-abstract-short" style="display: inline;"> This article describes a radon emanation measurement technique using liquid scintillator counting. A model for radon loading and transport is described, along with its calibration. Detector background and blank have been studied and quantified. The Minimal detectable activity has been determined for the counting setup using a toy Monte Carlo simulation. The measurement technique is validated using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09384v1-abstract-full').style.display = 'inline'; document.getElementById('2411.09384v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.09384v1-abstract-full" style="display: none;"> This article describes a radon emanation measurement technique using liquid scintillator counting. A model for radon loading and transport is described, along with its calibration. Detector background and blank have been studied and quantified. The Minimal detectable activity has been determined for the counting setup using a toy Monte Carlo simulation. The measurement technique is validated using a butyl rubber sample previously used for cross-calibration between different radon counting facilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09384v1-abstract-full').style.display = 'none'; document.getElementById('2411.09384v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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, 6 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/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/physics?searchtype=author&query=Sazzad%2C+A+B+M+R">A. B. M. R. Sazzad</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Piepke%2C+A">A. Piepke</a>, <a href="/search/physics?searchtype=author&query=Poudel%2C+S">S. Poudel</a>, <a href="/search/physics?searchtype=author&query=Trewin%2C+H">H. Trewin</a>, <a href="/search/physics?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/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/2201.13285">arXiv:2201.13285</a> <span> [<a href="https://arxiv.org/pdf/2201.13285">pdf</a>, <a href="https://arxiv.org/format/2201.13285">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-022-10726-x">10.1140/epjc/s10052-022-10726-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Double Chooz antineutrino detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Double+Chooz+Collaboration"> Double Chooz Collaboration</a>, <a href="/search/physics?searchtype=author&query=de+Kerret%2C+H">H. de Kerret</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/physics?searchtype=author&query=Aberle%2C+C">C. Aberle</a>, <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Ahijado%2C+J+M">J. M. Ahijado</a>, <a href="/search/physics?searchtype=author&query=Akiri%2C+T">T. Akiri</a>, <a href="/search/physics?searchtype=author&query=Alarc%C3%B3n%2C+J+M">J. M. Alarc贸n</a>, <a href="/search/physics?searchtype=author&query=Alba%2C+J">J. Alba</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Ardellier%2C+F">F. Ardellier</a>, <a href="/search/physics?searchtype=author&query=Barabanov%2C+I">I. Barabanov</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/physics?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/physics?searchtype=author&query=Bertoli%2C+W">W. Bertoli</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blanco%2C+C">C. Blanco</a>, <a href="/search/physics?searchtype=author&query=Bleurvacq%2C+N">N. Bleurvacq</a> , et al. (226 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="2201.13285v2-abstract-short" style="display: inline;"> This article describes the setup and performance of the near and far detectors in the Double Chooz experiment. The electron antineutrinos of the Chooz nuclear power plant were measured in two identically designed detectors with different average baselines of about 400 m and 1050 m from the two reactor cores. Over many years of data taking the neutrino signals were extracted from interactions in th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.13285v2-abstract-full').style.display = 'inline'; document.getElementById('2201.13285v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.13285v2-abstract-full" style="display: none;"> This article describes the setup and performance of the near and far detectors in the Double Chooz experiment. The electron antineutrinos of the Chooz nuclear power plant were measured in two identically designed detectors with different average baselines of about 400 m and 1050 m from the two reactor cores. Over many years of data taking the neutrino signals were extracted from interactions in the detectors with the goal of measuring a fundamental parameter in the context of neutrino oscillation, the mixing angle 胃13. The central part of the Double Chooz detectors was a main detector comprising four cylindrical volumes filled with organic liquids. From the inside towards the outside there were volumes containing gadolinium-loaded scintillator, gadolinium-free scintillator, a buffer oil and, optically separated, another liquid scintillator acting as veto system. Above this main detector an additional outer veto system using plastic scintillator strips was installed. The technologies developed in Double Chooz were inspiration for several other antineutrino detectors in the field. The detector design allowed implementation of efficient background rejection techniques including use of pulse shape information provided by the data acquisition system. The Double Chooz detectors featured remarkable stability, in particular for the detected photons, as well as high radiopurity of the detector components. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.13285v2-abstract-full').style.display = 'none'; document.getElementById('2201.13285v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 January, 2022; <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">49 pages, 29 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur.Phys.J. C (2022) 82:804 </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/physics?searchtype=author&query=Meng%2C+Y">Yue Meng</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">Jerry Busenitz</a>, <a href="/search/physics?searchtype=author&query=Piepke%2C+A">Andreas Piepke</a>, <a href="/search/physics?searchtype=author&query=Tsang%2C+R">Raymond Tsang</a>, <a href="/search/physics?searchtype=author&query=Wu%2C+M">Mengmeng Wu</a>, <a href="/search/physics?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/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> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.05515">arXiv:2009.05515</a> <span> [<a href="https://arxiv.org/pdf/2009.05515">pdf</a>, <a href="https://arxiv.org/format/2009.05515">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-021-09459-0">10.1140/epjc/s10052-021-09459-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Signatures of Sterile Neutrinos with Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+Double+Chooz+Collaboration"> The Double Chooz Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Corpace%2C+O">O. Corpace</a>, <a href="/search/physics?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/physics?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Furuta%2C+H">H. Furuta</a>, <a href="/search/physics?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</a>, <a href="/search/physics?searchtype=author&query=Givaudan%2C+A">A. Givaudan</a>, <a href="/search/physics?searchtype=author&query=Gomez%2C+H">H. Gomez</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="2009.05515v3-abstract-short" style="display: inline;"> We present a search for signatures of neutrino mixing of electron anti-neutrinos with additional hypothetical sterile neutrino flavors using the Double Chooz experiment. The search is based on data from 5 years of operation of Double Chooz, including 2 years in the two-detector configuration. The analysis is based on a profile likelihood, i.e.\ comparing the data to the model prediction of disappe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05515v3-abstract-full').style.display = 'inline'; document.getElementById('2009.05515v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.05515v3-abstract-full" style="display: none;"> We present a search for signatures of neutrino mixing of electron anti-neutrinos with additional hypothetical sterile neutrino flavors using the Double Chooz experiment. The search is based on data from 5 years of operation of Double Chooz, including 2 years in the two-detector configuration. The analysis is based on a profile likelihood, i.e.\ comparing the data to the model prediction of disappearance in a data-to-data comparison of the two respective detectors. The analysis is optimized for a model of three active and one sterile neutrino. It is sensitive in the typical mass range $5 \cdot 10^{-3} $ eV$^2 \lesssim 螖m^2_{41} \lesssim 3\cdot 10^{-1} $ eV$^2$ for mixing angles down to $\sin^2 2胃_{14} \gtrsim 0.02$. No significant disappearance additionally to the conventional disappearance related to $胃_{13} $ is observed and correspondingly exclusion bounds on the sterile mixing parameter $胃_{14} $ as function of $ 螖m^2_{41} $ are obtained. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05515v3-abstract-full').style.display = 'none'; document.getElementById('2009.05515v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication by EPJC</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 62F03 (Primary); 62P35; 65C60 (Secondary) </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 81, 775 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.13431">arXiv:2007.13431</a> <span> [<a href="https://arxiv.org/pdf/2007.13431">pdf</a>, <a href="https://arxiv.org/format/2007.13431">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/10.1007/JHEP01(2021)190">10.1007/JHEP01(2021)190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reactor Rate Modulation oscillation analysis with two detectors in Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Double+Chooz+Collaboration"> Double Chooz Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/physics?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Furuta%2C+H">H. Furuta</a>, <a href="/search/physics?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</a>, <a href="/search/physics?searchtype=author&query=Gonzalez%2C+L+F+G">L. F. G. Gonzalez</a>, <a href="/search/physics?searchtype=author&query=Goodman%2C+M+C">M. C. Goodman</a>, <a href="/search/physics?searchtype=author&query=Hara%2C+T">T. Hara</a>, <a href="/search/physics?searchtype=author&query=Hellwig%2C+D">D. Hellwig</a> , et al. (62 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.13431v2-abstract-short" style="display: inline;"> A $胃_{13}$ oscillation analysis based on the observed antineutrino rates at the Double Chooz far and near detectors for different reactor power conditions is presented. This approach provides a so far unique simultaneous determination of $胃_{13}$ and the total background rates without relying on any assumptions on the specific background contributions. The analysis comprises 865 days of data colle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.13431v2-abstract-full').style.display = 'inline'; document.getElementById('2007.13431v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.13431v2-abstract-full" style="display: none;"> A $胃_{13}$ oscillation analysis based on the observed antineutrino rates at the Double Chooz far and near detectors for different reactor power conditions is presented. This approach provides a so far unique simultaneous determination of $胃_{13}$ and the total background rates without relying on any assumptions on the specific background contributions. The analysis comprises 865 days of data collected in both detectors with at least one reactor in operation. The oscillation results are enhanced by the use of 24.06 days (12.74 days) of reactor-off data in the far (near) detector. The analysis considers the \nue interactions up to a visible energy of 8.5 MeV, using the events at higher energies to build a cosmogenic background model considering fast-neutrons interactions and $^{9}$Li decays. The background-model-independent determination of the mixing angle yields sin$^2(2胃_{13})=0.094\pm0.017$, being the best-fit total background rates fully consistent with the cosmogenic background model. A second oscillation analysis is also performed constraining the total background rates to the cosmogenic background estimates. While the central value is not significantly modified due to the consistency between the reactor-off data and the background estimates, the addition of the background model reduces the uncertainty on $胃_{13}$ to 0.015. Along with the oscillation results, the normalization of the anti-neutrino rate is measured with a precision of 0.86\%, reducing the 1.43\% uncertainty associated to the expectation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.13431v2-abstract-full').style.display = 'none'; document.getElementById('2007.13431v2-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 01 (2021) 190 </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/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/physics?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/physics?searchtype=author&query=Alquahtani%2C+A">A. Alquahtani</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</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=Arbuckle%2C+A">A. Arbuckle</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=Auyeung%2C+H">H. Auyeung</a>, <a href="/search/physics?searchtype=author&query=Aviles%2C+S">S. Aviles</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/physics?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</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=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/physics?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/physics?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/physics?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/physics?searchtype=author&query=Collaboration%2C+T+L">The LUX-ZEPLIN 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=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/physics?searchtype=author&query=Alqahtani%2C+A">A. Alqahtani</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</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=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=Bensinger%2C+J">J. Bensinger</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=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/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/physics?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/physics?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/physics?searchtype=author&query=Alquahtani%2C+A">A. Alquahtani</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</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=Arbuckle%2C+A">A. Arbuckle</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=Auyeung%2C+H">H. Auyeung</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/physics?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</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=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/physics?searchtype=author&query=Barthel%2C+J">J. Barthel</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/physics?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/physics?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/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/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</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=Baxter%2C+A">A. Baxter</a>, <a href="/search/physics?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</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=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/physics?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/physics?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/physics?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/physics?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a>, <a href="/search/physics?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J+K">J. K. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Carels%2C+C">C. Carels</a>, <a href="/search/physics?searchtype=author&query=Carlsmith%2C+D+L">D. L. Carlsmith</a>, <a href="/search/physics?searchtype=author&query=Carmona-Benitez%2C+M+C">M. C. Carmona-Benitez</a>, <a href="/search/physics?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/1903.02643">arXiv:1903.02643</a> <span> [<a href="https://arxiv.org/pdf/1903.02643">pdf</a>, <a href="https://arxiv.org/format/1903.02643">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.apradiso.2019.108963">10.1016/j.apradiso.2019.108963 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A New Method for Evaluating the Effectiveness of Plastic Packaging Against Radon Penetration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Meng%2C+Y">Yue Meng</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">Jerry Busenitz</a>, <a href="/search/physics?searchtype=author&query=Piepke%2C+A">Andreas 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="1903.02643v2-abstract-short" style="display: inline;"> Deposition of $^{222}Rn$ daughters onto detector materials pose a risk to ultra-low background experiments. To mitigate this risk, a common approach is to enclose detector components in sealed plastic bags made of films known to be effective barriers against radon. We describe a new method to evaluate radon barriers which is unique in that (a) it gauges not only the intrinsic resistance to radon p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.02643v2-abstract-full').style.display = 'inline'; document.getElementById('1903.02643v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.02643v2-abstract-full" style="display: none;"> Deposition of $^{222}Rn$ daughters onto detector materials pose a risk to ultra-low background experiments. To mitigate this risk, a common approach is to enclose detector components in sealed plastic bags made of films known to be effective barriers against radon. We describe a new method to evaluate radon barriers which is unique in that (a) it gauges not only the intrinsic resistance to radon penetration of a plastic film but also the integrity of bags fabricated from the film and sealed following some protocol, and (b) it employs gamma spectroscopy rather than alpha spectroscopy. We report the results of applying this method to sealed bags fabricated from polypropylene, Nylon, Mylar, metallized Mylar, FEP, and PFA. Evaluation of the fluoropolymers FEP and PFA as radon barriers are the first such measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.02643v2-abstract-full').style.display = 'none'; document.getElementById('1903.02643v2-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 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">16 pages, 5 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Applied Radiation and Isotopes Volume 156, February 2020, 108963 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.08048">arXiv:1802.08048</a> <span> [<a href="https://arxiv.org/pdf/1802.08048">pdf</a>, <a href="https://arxiv.org/format/1802.08048">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/10.1007/JHEP11(2018)053">10.1007/JHEP11(2018)053 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Yields and production rates of cosmogenic $^9$Li and $^8$He measured with the Double Chooz near and far detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=de+Kerret%2C+H">H. de Kerret</a>, <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Corpace%2C+O">O. Corpace</a>, <a href="/search/physics?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/physics?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Furuta%2C+H">H. Furuta</a>, <a href="/search/physics?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</a>, <a href="/search/physics?searchtype=author&query=Givaudan%2C+A">A. Givaudan</a> , et al. (73 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="1802.08048v3-abstract-short" style="display: inline;"> The yields and production rates of the radioisotopes $^9$Li and $^8$He created by cosmic muon spallation on $^{12}$C, have been measured by the two detectors of the Double Chooz experiment. The identical detectors are located at separate sites and depths, which means they are subject to different muon spectra. The near (far) detector has an overburden of $\sim$120 m.w.e. ($\sim$300 m.w.e.) corresp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.08048v3-abstract-full').style.display = 'inline'; document.getElementById('1802.08048v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.08048v3-abstract-full" style="display: none;"> The yields and production rates of the radioisotopes $^9$Li and $^8$He created by cosmic muon spallation on $^{12}$C, have been measured by the two detectors of the Double Chooz experiment. The identical detectors are located at separate sites and depths, which means they are subject to different muon spectra. The near (far) detector has an overburden of $\sim$120 m.w.e. ($\sim$300 m.w.e.) corresponding to a mean muon energy of $32.1\pm2.0\,\mathrm{GeV}$ ($63.7\pm5.5\,\mathrm{GeV}$). Comparing the data to a detailed simulation of the $^9$Li and $^8$He decays, the contribution of the $^8$He radioisotope at both detectors is found to be compatible with zero. The observed $^9$Li yields in the near and far detectors are $5.51\pm0.51$ and $7.90\pm0.51$, respectively, in units of $10^{-8}渭^{-1} \mathrm{g^{-1} cm^{2} }$. The shallow overburdens of the near and far detectors give a unique insight when combined with measurements by KamLAND and Borexino to give the first multi--experiment, data driven relationship between the $^9$Li yield and the mean muon energy according to the power law $Y = Y_0( <E_渭 >/ 1\,\mathrm{GeV})^{\overline伪}$, giving $\overline伪=0.72\pm0.06$ and $Y_0=(0.43\pm0.11)\times 10^{-8}渭^{-1} \mathrm{g^{-1} cm^{2}}$. This relationship gives future liquid scintillator based experiments the ability to predict their cosmogenic $^9$Li background rates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.08048v3-abstract-full').style.display = 'none'; document.getElementById('1802.08048v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">15 pages, 5 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/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/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</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=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=Bailey%2C+A+J">A. J. Bailey</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=Bauer%2C+D">D. Bauer</a>, <a href="/search/physics?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/physics?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/physics?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/physics?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/physics?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/physics?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/physics?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/physics?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/physics?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/physics?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a>, <a href="/search/physics?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J+K">J. K. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Carels%2C+C">C. Carels</a>, <a href="/search/physics?searchtype=author&query=Carlsmith%2C+D+L">D. L. Carlsmith</a>, <a href="/search/physics?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/1710.04315">arXiv:1710.04315</a> <span> [<a href="https://arxiv.org/pdf/1710.04315">pdf</a>, <a href="https://arxiv.org/format/1710.04315">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/10.1088/1748-0221/13/01/P01031">10.1088/1748-0221/13/01/P01031 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Novel event classification based on spectral analysis of scintillation waveforms in Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Corpace%2C+O">O. Corpace</a>, <a href="/search/physics?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</a>, <a href="/search/physics?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/physics?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fallot%2C+M">M. Fallot</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Furuta%2C+H">H. Furuta</a>, <a href="/search/physics?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</a> , et al. (72 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="1710.04315v3-abstract-short" style="display: inline;"> Liquid scintillators are a common choice for neutrino physics experiments, but their capabilities to perform background rejection by scintillation pulse shape discrimination is generally limited in large detectors. This paper describes a novel approach for a pulse shape based event classification developed in the context of the Double Chooz reactor antineutrino experiment. Unlike previous implemen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.04315v3-abstract-full').style.display = 'inline'; document.getElementById('1710.04315v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.04315v3-abstract-full" style="display: none;"> Liquid scintillators are a common choice for neutrino physics experiments, but their capabilities to perform background rejection by scintillation pulse shape discrimination is generally limited in large detectors. This paper describes a novel approach for a pulse shape based event classification developed in the context of the Double Chooz reactor antineutrino experiment. Unlike previous implementations, this method uses the Fourier power spectra of the scintillation pulse shapes to obtain event-wise information. A classification variable built from spectral information was able to achieve an unprecedented performance, despite the lack of optimization at the detector design level. Several examples of event classification are provided, ranging from differentiation between the detector volumes and an efficient rejection of instrumental light noise, to some sensitivity to the particle type, such as stopping muons, ortho-positronium formation, alpha particles as well as electrons and positrons. In combination with other techniques the method is expected to allow for a versatile and more efficient background rejection in the future, especially if detector optimization is taken into account at the design level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.04315v3-abstract-full').style.display = 'none'; document.getElementById('1710.04315v3-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 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation, Volume 13, Number 01 (2018) P01031 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.08533">arXiv:1708.08533</a> <span> [<a href="https://arxiv.org/pdf/1708.08533">pdf</a>, <a href="https://arxiv.org/format/1708.08533">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1063/1.5018996">10.1063/1.5018996 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining Radon Backgrounds in LZ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Miller%2C+E+H">E. H. Miller</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Edberg%2C+T+K">T. K. Edberg</a>, <a href="/search/physics?searchtype=author&query=Ghag%2C+C">C. Ghag</a>, <a href="/search/physics?searchtype=author&query=Hall%2C+C">C. Hall</a>, <a href="/search/physics?searchtype=author&query=Leonard%2C+R">R. Leonard</a>, <a href="/search/physics?searchtype=author&query=Lesko%2C+K">K. Lesko</a>, <a href="/search/physics?searchtype=author&query=Liu%2C+X">X. Liu</a>, <a href="/search/physics?searchtype=author&query=Meng%2C+Y">Yue Meng</a>, <a href="/search/physics?searchtype=author&query=Piepke%2C+A">A. Piepke</a>, <a href="/search/physics?searchtype=author&query=Schnee%2C+R+W">R. W. Schnee</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="1708.08533v1-abstract-short" style="display: inline;"> The LZ dark matter detector, like many other rare-event searches, will suffer from backgrounds due to the radioactive decay of radon daughters. In order to achieve its science goals, the concentration of radon within the xenon should not exceed $2渭$Bq/kg, or 20 mBq total within its 10 tonnes. The LZ collaboration is in the midst of a program to screen all significant components in contact with the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.08533v1-abstract-full').style.display = 'inline'; document.getElementById('1708.08533v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.08533v1-abstract-full" style="display: none;"> The LZ dark matter detector, like many other rare-event searches, will suffer from backgrounds due to the radioactive decay of radon daughters. In order to achieve its science goals, the concentration of radon within the xenon should not exceed $2渭$Bq/kg, or 20 mBq total within its 10 tonnes. The LZ collaboration is in the midst of a program to screen all significant components in contact with the xenon. The four institutions involved in this effort have begun sharing two cross-calibration sources to ensure consistent measurement results across multiple distinct devices. We present here five preliminary screening results, some mitigation strategies that will reduce the amount of radon produced by the most problematic components, and a summary of the current estimate of radon emanation throughout the detector. This best estimate totals $<17.3$ mBq, sufficiently low to meet the detector's science goals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.08533v1-abstract-full').style.display = 'none'; document.getElementById('1708.08533v1-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 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Low Radioactivity Techniques (LRT) 2017 Workshop Proceedings. 6 pages; 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/physics?searchtype=author&query=Mount%2C+B+J">B. J. Mount</a>, <a href="/search/physics?searchtype=author&query=Hans%2C+S">S. Hans</a>, <a href="/search/physics?searchtype=author&query=Rosero%2C+R">R. Rosero</a>, <a href="/search/physics?searchtype=author&query=Yeh%2C+M">M. Yeh</a>, <a href="/search/physics?searchtype=author&query=Chan%2C+C">C. Chan</a>, <a href="/search/physics?searchtype=author&query=Gaitskell%2C+R+J">R. J. Gaitskell</a>, <a href="/search/physics?searchtype=author&query=Huang%2C+D+Q">D. Q. Huang</a>, <a href="/search/physics?searchtype=author&query=Makkinje%2C+J">J. Makkinje</a>, <a href="/search/physics?searchtype=author&query=Malling%2C+D+C">D. C. Malling</a>, <a href="/search/physics?searchtype=author&query=Pangilinan%2C+M">M. Pangilinan</a>, <a href="/search/physics?searchtype=author&query=Rhyne%2C+C+A">C. A. Rhyne</a>, <a href="/search/physics?searchtype=author&query=Taylor%2C+W+C">W. C. Taylor</a>, <a href="/search/physics?searchtype=author&query=Verbus%2C+J+R">J. R. Verbus</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+Y+D">Y. D. Kim</a>, <a href="/search/physics?searchtype=author&query=Lee%2C+H+S">H. S. Lee</a>, <a href="/search/physics?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/physics?searchtype=author&query=Leonard%2C+D+S">D. S. Leonard</a>, <a href="/search/physics?searchtype=author&query=Li%2C+J">J. Li</a>, <a href="/search/physics?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/physics?searchtype=author&query=Cottle%2C+A">A. Cottle</a>, <a href="/search/physics?searchtype=author&query=Lippincott%2C+W+H">W. H. Lippincott</a>, <a href="/search/physics?searchtype=author&query=Markley%2C+D+J">D. J. Markley</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+T+J">T. J. Martin</a>, <a href="/search/physics?searchtype=author&query=Sarychev%2C+M">M. Sarychev</a>, <a href="/search/physics?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/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/physics?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</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=Arnquist%2C+I+J">I. J. Arnquist</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=Bailey%2C+A+J">A. J. Bailey</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=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/physics?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/physics?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/physics?searchtype=author&query=Benson%2C+T">T. Benson</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=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/physics?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/physics?searchtype=author&query=Bolozdynya%2C+A">A. Bolozdynya</a>, <a href="/search/physics?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/physics?searchtype=author&query=Bramante%2C+R">R. Bramante</a>, <a href="/search/physics?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/physics?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/physics?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/1611.07845">arXiv:1611.07845</a> <span> [<a href="https://arxiv.org/pdf/1611.07845">pdf</a>, <a href="https://arxiv.org/format/1611.07845">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/10.1088/1475-7516/2017/02/017">10.1088/1475-7516/2017/02/017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic-muon characterization and annual modulation measurement with Double Chooz detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Corpace%2C+O">O. Corpace</a>, <a href="/search/physics?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</a>, <a href="/search/physics?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/physics?searchtype=author&query=Dhooghe%2C+J">J. Dhooghe</a>, <a href="/search/physics?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/physics?searchtype=author&query=Dracos%2C+M">M. Dracos</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a> , et al. (85 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="1611.07845v4-abstract-short" style="display: inline;"> A study on cosmic muons has been performed for the two identical near and far neutrino detectors of the Double Chooz experiment, placed at $\sim$120 and $\sim$300 m.w.e. underground respectively, including the corresponding simulations using the MUSIC simulation package. This characterization has allowed to measure the muon flux reaching both detectors to be (3.64 $\pm$ 0.04) $\times$ 10$^{-4}$ cm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.07845v4-abstract-full').style.display = 'inline'; document.getElementById('1611.07845v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.07845v4-abstract-full" style="display: none;"> A study on cosmic muons has been performed for the two identical near and far neutrino detectors of the Double Chooz experiment, placed at $\sim$120 and $\sim$300 m.w.e. underground respectively, including the corresponding simulations using the MUSIC simulation package. This characterization has allowed to measure the muon flux reaching both detectors to be (3.64 $\pm$ 0.04) $\times$ 10$^{-4}$ cm$^{-2}$s$^{-1}$ for the near detector and (7.00 $\pm$ 0.05) $\times$ 10$^{-5}$ cm$^{-2}$s$^{-1}$ for the far one. The seasonal modulation of the signal has also been studied observing a positive correlation with the atmospheric temperature, leading to an effective temperature coefficient of $伪_{T}$ = 0.212 $\pm$ 0.024 and 0.355 $\pm$ 0.019 for the near and far detectors respectively. These measurements, in good agreement with expectations based on theoretical models, represent one of the first measurements of this coefficient in shallow depth installations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.07845v4-abstract-full').style.display = 'none'; document.getElementById('1611.07845v4-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">20 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Cosmology and Astroparticle Physics 02 (2017) 017 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.06895">arXiv:1604.06895</a> <span> [<a href="https://arxiv.org/pdf/1604.06895">pdf</a>, <a href="https://arxiv.org/format/1604.06895">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/10.1088/1748-0221/11/08/P08001">10.1088/1748-0221/11/08/P08001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the Spontaneous Light Emission of the PMTs used in the Double Chooz Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Double+Chooz+collaboration"> Double Chooz collaboration</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Calvo%2C+E">E. Calvo</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/physics?searchtype=author&query=Conover%2C+E">E. Conover</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a> , et al. (124 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="1604.06895v2-abstract-short" style="display: inline;"> During the commissioning of the first of the two detectors of the Double Chooz experiment, an unexpected and dominant background caused by the emission of light inside the optical volume has been observed. A specific study of the ensemble of phenomena called "Light Noise" has been carried out in-situ, and in an external laboratory, in order to characterize the signals and to identify the possible… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06895v2-abstract-full').style.display = 'inline'; document.getElementById('1604.06895v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.06895v2-abstract-full" style="display: none;"> During the commissioning of the first of the two detectors of the Double Chooz experiment, an unexpected and dominant background caused by the emission of light inside the optical volume has been observed. A specific study of the ensemble of phenomena called "Light Noise" has been carried out in-situ, and in an external laboratory, in order to characterize the signals and to identify the possible processes underlying the effect. Some mechanisms of instrumental noise originating from the PMTs were identified and it has been found that the leading one arises from the light emission localized on the photomultiplier base and produced by the combined effect of heat and high voltage across the transparent epoxy resin covering the electric components. The correlation of the rate and the amplitude of the signal with the temperature has been observed. For the first detector in operation the induced background has been mitigated using online and offline analysis selections based on timing and light pattern of the signals, while a modification of the photomultiplier assembly has been implemented for the second detector in order to blacken the PMT bases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06895v2-abstract-full').style.display = 'none'; document.getElementById('1604.06895v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">24 pages, 24 figures. Minor revision to be published in the Journal of Instrumentation (JINST), Corresponding author: R. Santorelli</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 11 (2016) no.08, P08001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.07562">arXiv:1512.07562</a> <span> [<a href="https://arxiv.org/pdf/1512.07562">pdf</a>, <a href="https://arxiv.org/ps/1512.07562">ps</a>, <a href="https://arxiv.org/format/1512.07562">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/10.1103/PhysRevC.93.054608">10.1103/PhysRevC.93.054608 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Muon capture on light isotopes in Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Double+Chooz+collaboration"> Double Chooz collaboration</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/physics?searchtype=author&query=Conover%2C+E">E. Conover</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</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="1512.07562v2-abstract-short" style="display: inline;"> Using the Double Chooz detector, designed to measure the neutrino mixing angle $胃_{13}$, the products of $渭^-$ capture on $^{12}$C, $^{13}$C, $^{14}$N and $^{16}$O have been measured. Over a period of 489.5 days, $2.3\times10^6$ stopping cosmic $渭^-$ have been collected, of which $1.8\times10^5$ captured on carbon, nitrogen, or oxygen nuclei in the inner detector scintillator or acrylic vessels. T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.07562v2-abstract-full').style.display = 'inline'; document.getElementById('1512.07562v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.07562v2-abstract-full" style="display: none;"> Using the Double Chooz detector, designed to measure the neutrino mixing angle $胃_{13}$, the products of $渭^-$ capture on $^{12}$C, $^{13}$C, $^{14}$N and $^{16}$O have been measured. Over a period of 489.5 days, $2.3\times10^6$ stopping cosmic $渭^-$ have been collected, of which $1.8\times10^5$ captured on carbon, nitrogen, or oxygen nuclei in the inner detector scintillator or acrylic vessels. The resulting isotopes were tagged using prompt neutron emission (when applicable), the subsequent beta decays, and, in some cases, $尾$-delayed neutrons. The most precise measurement of the rate of $^{12}\mathrm C(渭^-,谓)^{12}\mathrm B$ to date is reported: $6.57^{+0.11}_{-0.21}\times10^{3}\,\mathrm s^{-1}$, or $(17.35^{+0.35}_{-0.59})\%$ of nuclear captures. By tagging excited states emitting gammas, the ground state transition rate to $^{12}$B has been determined to be $5.68^{+0.14}_{-0.23}\times10^3\,\mathrm s^{-1}$. The heretofore unobserved reactions $^{12}\mathrm C(渭^-,谓伪)^{8}\mathrm{Li}$, $^{13}\mathrm C(渭^-,谓\mathrm n伪)^{8}\mathrm{Li}$, and $^{13}\mathrm C(渭^-,谓\mathrm n)^{12}\mathrm B$ are measured. Further, a population of $尾$n decays following stopping muons is identified with $5.5蟽$ significance. Statistics limit our ability to identify these decays definitively. Assuming negligible production of $^{8}$He, the reaction $^{13}\mathrm C(渭^-,谓伪)^{9}\mathrm{Li}$ is found to be present at the $2.7蟽$ level. Limits are set on a variety of other processes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.07562v2-abstract-full').style.display = 'none'; document.getElementById('1512.07562v2-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 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">21 pages, 14 figures. Minor revisions. Corresponding author: M. Strait</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, 054608 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.08937">arXiv:1510.08937</a> <span> [<a href="https://arxiv.org/pdf/1510.08937">pdf</a>, <a href="https://arxiv.org/ps/1510.08937">ps</a>, <a href="https://arxiv.org/format/1510.08937">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/10.1007/JHEP01(2016)163">10.1007/JHEP01(2016)163 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of $胃_{13}$ in Double Chooz using neutron captures on hydrogen with novel background rejection techniques </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/physics?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/physics?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a>, <a href="/search/physics?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</a> , et al. (120 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="1510.08937v2-abstract-short" style="display: inline;"> The Double Chooz collaboration presents a measurement of the neutrino mixing angle $胃_{13}$ using reactor $\overline谓_{e}$ observed via the inverse beta decay reaction in which the neutron is captured on hydrogen. This measurement is based on 462.72 live days data, approximately twice as much data as in the previous such analysis, collected with a detector positioned at an average distance of 1050… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.08937v2-abstract-full').style.display = 'inline'; document.getElementById('1510.08937v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.08937v2-abstract-full" style="display: none;"> The Double Chooz collaboration presents a measurement of the neutrino mixing angle $胃_{13}$ using reactor $\overline谓_{e}$ observed via the inverse beta decay reaction in which the neutron is captured on hydrogen. This measurement is based on 462.72 live days data, approximately twice as much data as in the previous such analysis, collected with a detector positioned at an average distance of 1050m from two reactor cores. Several novel techniques have been developed to achieve significant reductions of the backgrounds and systematic uncertainties. Accidental coincidences, the dominant background in this analysis, are suppressed by more than an order of magnitude with respect to our previous publication by a multi-variate analysis. These improvements demonstrate the capability of precise measurement of reactor $\overline谓_{e}$ without gadolinium loading. Spectral distortions from the $\overline谓_{e}$ reactor flux predictions previously reported with the neutron capture on gadolinium events are confirmed in the independent data sample presented here. A value of $\sin^{2}2胃_{13} = 0.095^{+0.038}_{-0.039}$(stat+syst) is obtained from a fit to the observed event rate as a function of the reactor power, a method insensitive to the energy spectrum shape. A simultaneous fit of the hydrogen capture events and of the gadolinium capture events yields a measurement of $\sin^{2}2胃_{13} = 0.088\pm0.033$(stat+syst). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.08937v2-abstract-full').style.display = 'none'; document.getElementById('1510.08937v2-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 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 01 (2016) 163 </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/physics?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/physics?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/physics?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/physics?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/physics?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</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=Bai%2C+X">X. Bai</a>, <a href="/search/physics?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</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=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+P">P. Bauer</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=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/physics?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/physics?searchtype=author&query=Bolozdynya%2C+A+I">A. I. Bolozdynya</a>, <a href="/search/physics?searchtype=author&query=Boulton%2C+E+M">E. M. Boulton</a>, <a href="/search/physics?searchtype=author&query=Bramante%2C+R">R. Bramante</a>, <a href="/search/physics?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/physics?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a>, <a href="/search/physics?searchtype=author&query=Bunker%2C+R">R. Bunker</a>, <a href="/search/physics?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/physics?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/1407.6913">arXiv:1407.6913</a> <span> [<a href="https://arxiv.org/pdf/1407.6913">pdf</a>, <a href="https://arxiv.org/ps/1407.6913">ps</a>, <a href="https://arxiv.org/format/1407.6913">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/10.1007/JHEP10(2014)032">10.1007/JHEP10(2014)032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ortho-positronium observation in the Double Chooz Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Caden%2C+E">E. Caden</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chang%2C+P+-">P. -J. Chang</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/physics?searchtype=author&query=Conover%2C+E">E. Conover</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a>, <a href="/search/physics?searchtype=author&query=Crespo-Anadon%2C+J+I">J. I. Crespo-Anadon</a>, <a href="/search/physics?searchtype=author&query=Crum%2C+K">K. Crum</a>, <a href="/search/physics?searchtype=author&query=Cucoanes%2C+A+S">A. S. Cucoanes</a> , et al. (121 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="1407.6913v2-abstract-short" style="display: inline;"> The Double Chooz experiment measures the neutrino mixing angle $胃_{13}$ by detecting reactor $\bar谓_e$ via inverse beta decay. The positron-neutron space and time coincidence allows for a sizable background rejection, nonetheless liquid scintillator detectors would profit from a positron/electron discrimination, if feasible in large detector, to suppress the remaining background. Standard particle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.6913v2-abstract-full').style.display = 'inline'; document.getElementById('1407.6913v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.6913v2-abstract-full" style="display: none;"> The Double Chooz experiment measures the neutrino mixing angle $胃_{13}$ by detecting reactor $\bar谓_e$ via inverse beta decay. The positron-neutron space and time coincidence allows for a sizable background rejection, nonetheless liquid scintillator detectors would profit from a positron/electron discrimination, if feasible in large detector, to suppress the remaining background. Standard particle identification, based on particle dependent time profile of photon emission in liquid scintillator, can not be used given the identical mass of the two particles. However, the positron annihilation is sometimes delayed by the ortho-positronium (o-Ps) metastable state formation, which induces a pulse shape distortion that could be used for positron identification. In this paper we report on the first observation of positronium formation in a large liquid scintillator detector based on pulse shape analysis of single events. The o-Ps formation fraction and its lifetime were measured, finding the values of 44$\%$ $\pm$ 12$\%$ (sys.) $\pm$ 5$\%$ (stat.) and $3.68$ns $\pm$ 0.17ns (sys.) $\pm$ 0.15ns (stat.) respectively, in agreement with the results obtained with a dedicated positron annihilation lifetime spectroscopy setup. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.6913v2-abstract-full').style.display = 'none'; document.getElementById('1407.6913v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </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, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 1410 (2014) 032 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.7763">arXiv:1406.7763</a> <span> [<a href="https://arxiv.org/pdf/1406.7763">pdf</a>, <a href="https://arxiv.org/ps/1406.7763">ps</a>, <a href="https://arxiv.org/format/1406.7763">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/10.1007/JHEP10(2014)086">10.1007/JHEP10(2014)086 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved measurements of the neutrino mixing angle $胃_{13}$ with the Double Chooz detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Caden%2C+E">E. Caden</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chang%2C+P+-">P. -J. Chang</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/physics?searchtype=author&query=Conover%2C+E">E. Conover</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a>, <a href="/search/physics?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</a>, <a href="/search/physics?searchtype=author&query=Crum%2C+K">K. Crum</a>, <a href="/search/physics?searchtype=author&query=Cucoanes%2C+A+S">A. S. Cucoanes</a> , et al. (121 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="1406.7763v4-abstract-short" style="display: inline;"> The Double Chooz experiment presents improved measurements of the neutrino mixing angle $胃_{13}$ using the data collected in 467.90 live days from a detector positioned at an average distance of 1050 m from two reactor cores at the Chooz nuclear power plant. Several novel techniques have been developed to achieve significant reductions of the backgrounds and systematic uncertainties with respect t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.7763v4-abstract-full').style.display = 'inline'; document.getElementById('1406.7763v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.7763v4-abstract-full" style="display: none;"> The Double Chooz experiment presents improved measurements of the neutrino mixing angle $胃_{13}$ using the data collected in 467.90 live days from a detector positioned at an average distance of 1050 m from two reactor cores at the Chooz nuclear power plant. Several novel techniques have been developed to achieve significant reductions of the backgrounds and systematic uncertainties with respect to previous publications, whereas the efficiency of the $\bar谓_{e}$ signal has increased. The value of $胃_{13}$ is measured to be $\sin^{2}2胃_{13} = 0.090 ^{+0.032}_{-0.029}$ from a fit to the observed energy spectrum. Deviations from the reactor $\bar谓_{e}$ prediction observed above a prompt signal energy of 4 MeV and possible explanations are also reported. A consistent value of $胃_{13}$ is obtained from a fit to the observed rate as a function of the reactor power independently of the spectrum shape and background estimation, demonstrating the robustness of the $胃_{13}$ measurement despite the observed distortion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.7763v4-abstract-full').style.display = 'none'; document.getElementById('1406.7763v4-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2014. </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">44 pages, 25 figures. Figures 21 and 22 have been replaced (statistical error bars for bins above 8 MeV have become smaller). No other changes in the results of the paper; an Erratum submitted to JHEP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 10 (2014) 086 [Erratum ibid. 02 (2015) 074] </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.6227">arXiv:1405.6227</a> <span> [<a href="https://arxiv.org/pdf/1405.6227">pdf</a>, <a href="https://arxiv.org/format/1405.6227">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.nima.2014.07.058">10.1016/j.nima.2014.07.058 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precision Muon Reconstruction in Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Double+Chooz+collaboration"> Double Chooz collaboration</a>, <a href="/search/physics?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/physics?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Caden%2C+E">E. Caden</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chang%2C+P+-">P. -J. Chang</a>, <a href="/search/physics?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/physics?searchtype=author&query=Conover%2C+E">E. Conover</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a>, <a href="/search/physics?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</a>, <a href="/search/physics?searchtype=author&query=Crum%2C+K">K. Crum</a> , et al. (119 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="1405.6227v2-abstract-short" style="display: inline;"> We describe a muon track reconstruction algorithm for the reactor anti-neutrino experiment Double Chooz. The Double Chooz detector consists of two optically isolated volumes of liquid scintillator viewed by PMTs, and an Outer Veto above these made of crossed scintillator strips. Muons are reconstructed by their Outer Veto hit positions along with timing information from the other two detector volu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.6227v2-abstract-full').style.display = 'inline'; document.getElementById('1405.6227v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.6227v2-abstract-full" style="display: none;"> We describe a muon track reconstruction algorithm for the reactor anti-neutrino experiment Double Chooz. The Double Chooz detector consists of two optically isolated volumes of liquid scintillator viewed by PMTs, and an Outer Veto above these made of crossed scintillator strips. Muons are reconstructed by their Outer Veto hit positions along with timing information from the other two detector volumes. All muons are fit under the hypothesis that they are through-going and ultrarelativistic. If the energy depositions suggest that the muon may have stopped, the reconstruction fits also for this hypothesis and chooses between the two via the relative goodness-of-fit. In the ideal case of a through-going muon intersecting the center of the detector, the resolution is ~40 mm in each transverse dimension. High quality muon reconstruction is an important tool for reducing the impact of the cosmogenic isotope background in Double Chooz. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.6227v2-abstract-full').style.display = 'none'; document.getElementById('1405.6227v2-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 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </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">12 pages, 8 figures, submitted to Nuclear Instrumentation and Methods A. Author list corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Instrum.Meth.A 764 (2014) 330-339 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.7335">arXiv:1307.7335</a> <span> [<a href="https://arxiv.org/pdf/1307.7335">pdf</a>, <a href="https://arxiv.org/format/1307.7335">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="Accelerator Physics">physics.acc-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 Long-Baseline Neutrino Experiment: Exploring Fundamental Symmetries of the Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=LBNE+Collaboration"> LBNE Collaboration</a>, <a href="/search/physics?searchtype=author&query=Adams%2C+C">Corey Adams</a>, <a href="/search/physics?searchtype=author&query=Adams%2C+D">David Adams</a>, <a href="/search/physics?searchtype=author&query=Akiri%2C+T">Tarek Akiri</a>, <a href="/search/physics?searchtype=author&query=Alion%2C+T">Tyler Alion</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+K">Kris Anderson</a>, <a href="/search/physics?searchtype=author&query=Andreopoulos%2C+C">Costas Andreopoulos</a>, <a href="/search/physics?searchtype=author&query=Andrews%2C+M">Mike Andrews</a>, <a href="/search/physics?searchtype=author&query=Anghel%2C+I">Ioana Anghel</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+C+d">Jo茫o Carlos Costa dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Antonello%2C+M">Maddalena Antonello</a>, <a href="/search/physics?searchtype=author&query=Arrieta-Diaz%2C+E">Enrique Arrieta-Diaz</a>, <a href="/search/physics?searchtype=author&query=Artuso%2C+M">Marina Artuso</a>, <a href="/search/physics?searchtype=author&query=Asaadi%2C+J">Jonathan Asaadi</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+X">Xinhua Bai</a>, <a href="/search/physics?searchtype=author&query=Baibussinov%2C+B">Bagdat Baibussinov</a>, <a href="/search/physics?searchtype=author&query=Baird%2C+M">Michael Baird</a>, <a href="/search/physics?searchtype=author&query=Balantekin%2C+B">Baha Balantekin</a>, <a href="/search/physics?searchtype=author&query=Baller%2C+B">Bruce Baller</a>, <a href="/search/physics?searchtype=author&query=Baptista%2C+B">Brian Baptista</a>, <a href="/search/physics?searchtype=author&query=Barker%2C+D">D'Ann Barker</a>, <a href="/search/physics?searchtype=author&query=Barker%2C+G">Gary Barker</a>, <a href="/search/physics?searchtype=author&query=Barletta%2C+W+A">William A. Barletta</a>, <a href="/search/physics?searchtype=author&query=Barr%2C+G">Giles Barr</a>, <a href="/search/physics?searchtype=author&query=Bartoszek%2C+L">Larry Bartoszek</a> , et al. (461 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="1307.7335v3-abstract-short" style="display: inline;"> The preponderance of matter over antimatter in the early Universe, the dynamics of the supernova bursts that produced the heavy elements necessary for life and whether protons eventually decay --- these mysteries at the forefront of particle physics and astrophysics are key to understanding the early evolution of our Universe, its current state and its eventual fate. The Long-Baseline Neutrino Exp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.7335v3-abstract-full').style.display = 'inline'; document.getElementById('1307.7335v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.7335v3-abstract-full" style="display: none;"> The preponderance of matter over antimatter in the early Universe, the dynamics of the supernova bursts that produced the heavy elements necessary for life and whether protons eventually decay --- these mysteries at the forefront of particle physics and astrophysics are key to understanding the early evolution of our Universe, its current state and its eventual fate. The Long-Baseline Neutrino Experiment (LBNE) represents an extensively developed plan for a world-class experiment dedicated to addressing these questions. LBNE is conceived around three central components: (1) a new, high-intensity neutrino source generated from a megawatt-class proton accelerator at Fermi National Accelerator Laboratory, (2) a near neutrino detector just downstream of the source, and (3) a massive liquid argon time-projection chamber deployed as a far detector deep underground at the Sanford Underground Research Facility. This facility, located at the site of the former Homestake Mine in Lead, South Dakota, is approximately 1,300 km from the neutrino source at Fermilab -- a distance (baseline) that delivers optimal sensitivity to neutrino charge-parity symmetry violation and mass ordering effects. This ambitious yet cost-effective design incorporates scalability and flexibility and can accommodate a variety of upgrades and contributions. With its exceptional combination of experimental configuration, technical capabilities, and potential for transformative discoveries, LBNE promises to be a vital facility for the field of particle physics worldwide, providing physicists from around the globe with opportunities to collaborate in a twenty to thirty year program of exciting science. In this document we provide a comprehensive overview of LBNE's scientific objectives, its place in the landscape of neutrino physics worldwide, the technologies it will incorporate and the capabilities it will possess. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.7335v3-abstract-full').style.display = 'none'; document.getElementById('1307.7335v3-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 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Major update of previous version. This is the reference document for LBNE science program and current status. Chapters 1, 3, and 9 provide a comprehensive overview of LBNE's scientific objectives, its place in the landscape of neutrino physics worldwide, the technologies it will incorporate and the capabilities it will possess. 288 pages, 116 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> BNL-101354-2014-JA, FERMILAB-PUB-14-022, LA-UR-14-20881 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.6632">arXiv:1207.6632</a> <span> [<a href="https://arxiv.org/pdf/1207.6632">pdf</a>, <a href="https://arxiv.org/ps/1207.6632">ps</a>, <a href="https://arxiv.org/format/1207.6632">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.86.052008">10.1103/PhysRevD.86.052008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reactor electron antineutrino disappearance in the Double Chooz experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/physics?searchtype=author&query=Aberle%2C+C">C. Aberle</a>, <a href="/search/physics?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/physics?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/physics?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/physics?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/physics?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/physics?searchtype=author&query=Bezrukhov%2C+L">L. Bezrukhov</a>, <a href="/search/physics?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/physics?searchtype=author&query=Bowden%2C+N+S">N. S. Bowden</a>, <a href="/search/physics?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Caden%2C+E">E. Caden</a>, <a href="/search/physics?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/physics?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/physics?searchtype=author&query=Chang%2C+P+-">P. -J. Chang</a>, <a href="/search/physics?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/physics?searchtype=author&query=Classen%2C+T">T. Classen</a>, <a href="/search/physics?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/physics?searchtype=author&query=Conover%2C+E">E. Conover</a>, <a href="/search/physics?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a>, <a href="/search/physics?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</a>, <a href="/search/physics?searchtype=author&query=Crum%2C+K">K. Crum</a> , et al. (140 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1207.6632v4-abstract-short" style="display: inline;"> The Double Chooz experiment has observed 8,249 candidate electron antineutrino events in 227.93 live days with 33.71 GW-ton-years (reactor power x detector mass x livetime) exposure using a 10.3 cubic meter fiducial volume detector located at 1050 m from the reactor cores of the Chooz nuclear power plant in France. The expectation in case of theta13 = 0 is 8,937 events. The deficit is interpreted… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.6632v4-abstract-full').style.display = 'inline'; document.getElementById('1207.6632v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.6632v4-abstract-full" style="display: none;"> The Double Chooz experiment has observed 8,249 candidate electron antineutrino events in 227.93 live days with 33.71 GW-ton-years (reactor power x detector mass x livetime) exposure using a 10.3 cubic meter fiducial volume detector located at 1050 m from the reactor cores of the Chooz nuclear power plant in France. The expectation in case of theta13 = 0 is 8,937 events. The deficit is interpreted as evidence of electron antineutrino disappearance. From a rate plus spectral shape analysis we find sin^2 2胃13 = 0.109 \pm 0.030(stat) \pm 0.025(syst). The data exclude the no-oscillation hypothesis at 99.8% CL (2.9蟽). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.6632v4-abstract-full').style.display = 'none'; document.getElementById('1207.6632v4-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, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </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">Modified for PRD referees</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 86, 052008 (2012) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0711.3624">arXiv:0711.3624</a> <span> [<a href="https://arxiv.org/pdf/0711.3624">pdf</a>, <a href="https://arxiv.org/ps/0711.3624">ps</a>, <a href="https://arxiv.org/format/0711.3624">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2007.12.002">10.1016/j.nima.2007.12.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A C-13(alpha,n)O-16 calibration source for KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=McKee%2C+D+W">David W. McKee</a>, <a href="/search/physics?searchtype=author&query=Busenitz%2C+J+K">Jerome K. Busenitz</a>, <a href="/search/physics?searchtype=author&query=Ostrovskiy%2C+I">Igor Ostrovskiy</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="0711.3624v3-abstract-short" style="display: inline;"> We report on the construction and performance of a calibration source for KamLAND using the reaction C-13(alpha,n)O-16 with Po-210 as the alpha progenitor. The source provides a direct measurement of this background reaction in our detector, high energy calibration points for the detector energy scale, and data on quenching of the neutron visible energy in KamLAND scintillator. We also discuss t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0711.3624v3-abstract-full').style.display = 'inline'; document.getElementById('0711.3624v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0711.3624v3-abstract-full" style="display: none;"> We report on the construction and performance of a calibration source for KamLAND using the reaction C-13(alpha,n)O-16 with Po-210 as the alpha progenitor. The source provides a direct measurement of this background reaction in our detector, high energy calibration points for the detector energy scale, and data on quenching of the neutron visible energy in KamLAND scintillator. We also discuss the possibility of using the reaction C-13(alpha,n)O-16 as a source of tagged slow neutrons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0711.3624v3-abstract-full').style.display = 'none'; document.getElementById('0711.3624v3-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 March, 2008; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 November, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2007. </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. Revised to agree with the published text</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Instrum.Meth. A, vol. 527, pp. 272-276 2008 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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