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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/2405.19419">arXiv:2405.19419</a> <span> [<a href="https://arxiv.org/pdf/2405.19419">pdf</a>, <a href="https://arxiv.org/format/2405.19419">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.110.093002">10.1103/PhysRevD.110.093002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supernova electron-neutrino interactions with xenon in the nEXO detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=nEXO+Collaboration"> nEXO Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Hedges%2C+S">S. Hedges</a>, <a href="/search/hep-ph?searchtype=author&query=Kharusi%2C+S+A">S. Al Kharusi</a>, <a href="/search/hep-ph?searchtype=author&query=Angelico%2C+E">E. Angelico</a>, <a href="/search/hep-ph?searchtype=author&query=Brodsky%2C+J+P">J. P. Brodsky</a>, <a href="/search/hep-ph?searchtype=author&query=Richardson%2C+G">G. Richardson</a>, <a href="/search/hep-ph?searchtype=author&query=Wilde%2C+S">S. Wilde</a>, <a href="/search/hep-ph?searchtype=author&query=Amy%2C+A">A. Amy</a>, <a href="/search/hep-ph?searchtype=author&query=Anker%2C+A">A. Anker</a>, <a href="/search/hep-ph?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/hep-ph?searchtype=author&query=Arsenault%2C+P">P. Arsenault</a>, <a href="/search/hep-ph?searchtype=author&query=Atencio%2C+A">A. Atencio</a>, <a href="/search/hep-ph?searchtype=author&query=Badhrees%2C+I">I. Badhrees</a>, <a href="/search/hep-ph?searchtype=author&query=Bane%2C+J">J. Bane</a>, <a href="/search/hep-ph?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/hep-ph?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ph?searchtype=author&query=Bhatta%2C+T">T. Bhatta</a>, <a href="/search/hep-ph?searchtype=author&query=Bolotnikov%2C+A">A. Bolotnikov</a>, <a href="/search/hep-ph?searchtype=author&query=Breslin%2C+J">J. Breslin</a>, <a href="/search/hep-ph?searchtype=author&query=Breur%2C+P+A">P. A. Breur</a>, <a href="/search/hep-ph?searchtype=author&query=Brown%2C+E">E. Brown</a>, <a href="/search/hep-ph?searchtype=author&query=Brunner%2C+T">T. Brunner</a>, <a href="/search/hep-ph?searchtype=author&query=Caden%2C+E">E. Caden</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+L+Q">L. Q. Cao</a> , et al. (122 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.19419v2-abstract-short" style="display: inline;"> Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-$尾$ decay detector (~5 metric ton, 90% ${}^{136}$Xe, 10% ${}^{134}$Xe) to evaluate its sensitivity to supernova neutrinos. Predictions for event rates and detectable signatures were modeled using the Model of Argon Reaction Low Energy Yields (MARLEY) event generator. We find good agreement… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19419v2-abstract-full').style.display = 'inline'; document.getElementById('2405.19419v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.19419v2-abstract-full" style="display: none;"> Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-$尾$ decay detector (~5 metric ton, 90% ${}^{136}$Xe, 10% ${}^{134}$Xe) to evaluate its sensitivity to supernova neutrinos. Predictions for event rates and detectable signatures were modeled using the Model of Argon Reaction Low Energy Yields (MARLEY) event generator. We find good agreement between MARLEY's predictions and existing theoretical calculations of the inclusive cross sections at supernova neutrino energies. The interactions modeled by MARLEY were simulated within the nEXO simulation framework and were run through an example reconstruction algorithm to determine the detector's efficiency for reconstructing these events. The simulated data, incorporating the detector response, were used to study the ability of nEXO to reconstruct the incident electron-neutrino spectrum and these results were extended to a larger xenon detector of the same isotope enrichment. We estimate that nEXO will be able to observe electron-neutrino interactions with xenon from supernovae as far as 5-8 kpc from Earth, while the ability to reconstruct incident electron-neutrino spectrum parameters from observed interactions in nEXO is limited to closer supernovae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19419v2-abstract-full').style.display = 'none'; document.getElementById('2405.19419v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LLNL-JRNL-864783 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 110, 093002 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.02858">arXiv:2201.02858</a> <span> [<a href="https://arxiv.org/pdf/2201.02858">pdf</a>, <a href="https://arxiv.org/format/2201.02858">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.105.082004">10.1103/PhysRevD.105.082004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmogenic production of $^{37}$Ar in the context of the LUX-ZEPLIN experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ph?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ph?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/hep-ph?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ph?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ph?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ph?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ph?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ph?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ph?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ph?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ph?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ph?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ph?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ph?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ph?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/hep-ph?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ph?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ph?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ph?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a> , et al. (183 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.02858v2-abstract-short" style="display: inline;"> We estimate the amount of $^{37}$Ar produced in natural xenon via cosmic ray-induced spallation, an inevitable consequence of the transportation and storage of xenon on the Earth's surface. We then calculate the resulting $^{37}$Ar concentration in a 10-tonne payload~(similar to that of the LUX-ZEPLIN experiment) assuming a representative schedule of xenon purification, storage and delivery to the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.02858v2-abstract-full').style.display = 'inline'; document.getElementById('2201.02858v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.02858v2-abstract-full" style="display: none;"> We estimate the amount of $^{37}$Ar produced in natural xenon via cosmic ray-induced spallation, an inevitable consequence of the transportation and storage of xenon on the Earth's surface. We then calculate the resulting $^{37}$Ar concentration in a 10-tonne payload~(similar to that of the LUX-ZEPLIN experiment) assuming a representative schedule of xenon purification, storage and delivery to the underground facility. Using the spallation model by Silberberg and Tsao, the sea level production rate of $^{37}$Ar in natural xenon is estimated to be 0.024~atoms/kg/day. Assuming the xenon is successively purified to remove radioactive contaminants in 1-tonne batches at a rate of 1~tonne/month, the average $^{37}$Ar activity after 10~tonnes are purified and transported underground is 0.058--0.090~$渭$Bq/kg, depending on the degree of argon removal during above-ground purification. Such cosmogenic $^{37}$Ar will appear as a noticeable background in the early science data, while decaying with a 35~day half-life. This newly-noticed production mechanism of $^{37}$Ar should be considered when planning for future liquid xenon-based experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.02858v2-abstract-full').style.display = 'none'; document.getElementById('2201.02858v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.11740">arXiv:2102.11740</a> <span> [<a href="https://arxiv.org/pdf/2102.11740">pdf</a>, <a href="https://arxiv.org/format/2102.11740">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.092009">10.1103/PhysRevD.104.092009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Projected sensitivities of the LUX-ZEPLIN (LZ) experiment to new physics via low-energy electron recoils </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ph?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/hep-ph?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/hep-ph?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/hep-ph?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/hep-ph?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/hep-ph?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ph?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/hep-ph?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ph?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/hep-ph?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/hep-ph?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/hep-ph?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/hep-ph?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ph?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ph?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ph?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/hep-ph?searchtype=author&query=Bhatti%2C+A">A. Bhatti</a>, <a href="/search/hep-ph?searchtype=author&query=Biekert%2C+A">A. Biekert</a>, <a href="/search/hep-ph?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ph?searchtype=author&query=Birch%2C+H+J">H. J. Birch</a> , et al. (172 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.11740v2-abstract-short" style="display: inline;"> LUX-ZEPLIN (LZ) is a dark matter detector expected to obtain world-leading sensitivity to weakly interacting massive particles (WIMPs) interacting via nuclear recoils with a ~7-tonne xenon target mass. This manuscript presents sensitivity projections to several low-energy signals of the complementary electron recoil signal type: 1) an effective neutrino magnetic moment and 2) an effective neutrino… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11740v2-abstract-full').style.display = 'inline'; document.getElementById('2102.11740v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.11740v2-abstract-full" style="display: none;"> LUX-ZEPLIN (LZ) is a dark matter detector expected to obtain world-leading sensitivity to weakly interacting massive particles (WIMPs) interacting via nuclear recoils with a ~7-tonne xenon target mass. This manuscript presents sensitivity projections to several low-energy signals of the complementary electron recoil signal type: 1) an effective neutrino magnetic moment and 2) an effective neutrino millicharge, both for pp-chain solar neutrinos, 3) an axion flux generated by the Sun, 4) axion-like particles forming the galactic dark matter, 5) hidden photons, 6) mirror dark matter, and 7) leptophilic dark matter. World-leading sensitivities are expected in each case, a result of the large 5.6t 1000d exposure and low expected rate of electron recoil backgrounds in the $<$100keV energy regime. A consistent signal generation, background model and profile-likelihood analysis framework is used throughout. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11740v2-abstract-full').style.display = 'none'; document.getElementById('2102.11740v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">v2 updates exclusion sensitivities from single-sided to two-sided</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.03479">arXiv:1908.03479</a> <span> [<a href="https://arxiv.org/pdf/1908.03479">pdf</a>, <a href="https://arxiv.org/format/1908.03479">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> </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.101.012003">10.1103/PhysRevD.101.012003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First direct detection constraint on mirror dark matter kinetic mixing using LUX 2013 data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=LUX+Collaboration"> LUX Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ph?searchtype=author&query=Alsum%2C+S">S. Alsum</a>, <a href="/search/hep-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ph?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/hep-ph?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ph?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/hep-ph?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ph?searchtype=author&query=Boulton%2C+E+M">E. M. Boulton</a>, <a href="/search/hep-ph?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/hep-ph?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/hep-ph?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/hep-ph?searchtype=author&query=Byram%2C+D">D. Byram</a>, <a href="/search/hep-ph?searchtype=author&query=Carmona-Benitez%2C+M+C">M. C. Carmona-Benitez</a>, <a href="/search/hep-ph?searchtype=author&query=Chan%2C+C">C. Chan</a>, <a href="/search/hep-ph?searchtype=author&query=Cutter%2C+J+E">J. E. Cutter</a>, <a href="/search/hep-ph?searchtype=author&query=de+Viveiros%2C+L">L. de Viveiros</a>, <a href="/search/hep-ph?searchtype=author&query=Druszkiewicz%2C+E">E. Druszkiewicz</a>, <a href="/search/hep-ph?searchtype=author&query=Fan%2C+A">A. Fan</a>, <a href="/search/hep-ph?searchtype=author&query=Fiorucci%2C+S">S. Fiorucci</a>, <a href="/search/hep-ph?searchtype=author&query=Gaitskell%2C+R+J">R. J. Gaitskell</a>, <a href="/search/hep-ph?searchtype=author&query=Ghag%2C+C">C. Ghag</a>, <a href="/search/hep-ph?searchtype=author&query=Gilchriese%2C+M+G+D">M. G. D. Gilchriese</a> , et al. (75 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1908.03479v2-abstract-short" style="display: inline;"> We present the results of a direct detection search for mirror dark matter interactions, using data collected from the Large Underground Xenon experiment during 2013, with an exposure of 95 live-days $\times$ 118 kg. Here, the calculations of the mirror electron scattering rate in liquid xenon take into account the shielding effects from mirror dark matter captured within the Earth. Annual and diu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.03479v2-abstract-full').style.display = 'inline'; document.getElementById('1908.03479v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.03479v2-abstract-full" style="display: none;"> We present the results of a direct detection search for mirror dark matter interactions, using data collected from the Large Underground Xenon experiment during 2013, with an exposure of 95 live-days $\times$ 118 kg. Here, the calculations of the mirror electron scattering rate in liquid xenon take into account the shielding effects from mirror dark matter captured within the Earth. Annual and diurnal modulation of the dark matter flux and atomic shell effects in xenon are also accounted for. Having found no evidence for an electron recoil signal induced by mirror dark matter interactions we place an upper limit on the kinetic mixing parameter over a range of local mirror electron temperatures between 0.1 and 0.6 keV. This limit shows significant improvement over the previous experimental constraint from orthopositronium decays and significantly reduces the allowed parameter space for the model. We exclude mirror electron temperatures above 0.3 keV at a 90% confidence level, for this model, and constrain the kinetic mixing below this temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.03479v2-abstract-full').style.display = 'none'; document.getElementById('1908.03479v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 012003 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1704.02297">arXiv:1704.02297</a> <span> [<a href="https://arxiv.org/pdf/1704.02297">pdf</a>, <a href="https://arxiv.org/format/1704.02297">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.118.261301">10.1103/PhysRevLett.118.261301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Searches for Axions and Axion-Like Particles with the LUX Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ph?searchtype=author&query=Alsum%2C+S">S. Alsum</a>, <a href="/search/hep-ph?searchtype=author&query=Aquino%2C+C">C. Aquino</a>, <a href="/search/hep-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/hep-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ph?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ph?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ph?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/hep-ph?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ph?searchtype=author&query=Boulton%2C+E+M">E. M. Boulton</a>, <a href="/search/hep-ph?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/hep-ph?searchtype=author&query=Byram%2C+D">D. Byram</a>, <a href="/search/hep-ph?searchtype=author&query=Cahn%2C+S+B">S. B. Cahn</a>, <a href="/search/hep-ph?searchtype=author&query=Carmona-Benitez%2C+M+C">M. C. Carmona-Benitez</a>, <a href="/search/hep-ph?searchtype=author&query=Chan%2C+C">C. Chan</a>, <a href="/search/hep-ph?searchtype=author&query=Chiller%2C+A+A">A. A. Chiller</a>, <a href="/search/hep-ph?searchtype=author&query=Chiller%2C+C">C. Chiller</a>, <a href="/search/hep-ph?searchtype=author&query=Currie%2C+A">A. Currie</a>, <a href="/search/hep-ph?searchtype=author&query=Cutter%2C+J+E">J. E. Cutter</a>, <a href="/search/hep-ph?searchtype=author&query=Davison%2C+T+J+R">T. J. R. Davison</a>, <a href="/search/hep-ph?searchtype=author&query=Dobi%2C+A">A. Dobi</a>, <a href="/search/hep-ph?searchtype=author&query=Dobson%2C+J+E+Y">J. E. Y. Dobson</a>, <a href="/search/hep-ph?searchtype=author&query=Druszkiewicz%2C+E">E. Druszkiewicz</a> , et al. (76 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1704.02297v2-abstract-short" style="display: inline;"> The first searches for axions and axion-like particles with the Large Underground Xenon (LUX) experiment are presented. Under the assumption of an axio-electric interaction in xenon, the coupling constant between axions and electrons, gAe is tested, using data collected in 2013 with an exposure totalling 95 live-days $\times$ 118 kg. A double-sided, profile likelihood ratio statistic test excludes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.02297v2-abstract-full').style.display = 'inline'; document.getElementById('1704.02297v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.02297v2-abstract-full" style="display: none;"> The first searches for axions and axion-like particles with the Large Underground Xenon (LUX) experiment are presented. Under the assumption of an axio-electric interaction in xenon, the coupling constant between axions and electrons, gAe is tested, using data collected in 2013 with an exposure totalling 95 live-days $\times$ 118 kg. A double-sided, profile likelihood ratio statistic test excludes gAe larger than 3.5 $\times$ 10$^{-12}$ (90% C.L.) for solar axions. Assuming the DFSZ theoretical description, the upper limit in coupling corresponds to an upper limit on axion mass of 0.12 eV/c$^{2}$, while for the KSVZ description masses above 36.6 eV/c$^{2}$ are excluded. For galactic axion-like particles, values of gAe larger than 4.2 $\times$ 10$^{-13}$ are excluded for particle masses in the range 1-16 keV/c$^{2}$. These are the most stringent constraints to date for these interactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.02297v2-abstract-full').style.display = 'none'; document.getElementById('1704.02297v2-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 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 118, 261301 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.03489">arXiv:1602.03489</a> <span> [<a href="https://arxiv.org/pdf/1602.03489">pdf</a>, <a href="https://arxiv.org/format/1602.03489">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.116.161302">10.1103/PhysRevLett.116.161302 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Results on the Spin-Dependent Scattering of Weakly Interacting Massive Particles on Nucleons from the Run 3 Data of the LUX Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=LUX+Collaboration"> LUX Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/hep-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/hep-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/hep-ph?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ph?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/hep-ph?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/hep-ph?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/hep-ph?searchtype=author&query=Boulton%2C+E+M">E. M. Boulton</a>, <a href="/search/hep-ph?searchtype=author&query=Bradley%2C+A">A. Bradley</a>, <a href="/search/hep-ph?searchtype=author&query=Bramante%2C+R">R. Bramante</a>, <a href="/search/hep-ph?searchtype=author&query=Cahn%2C+S+B">S. B. Cahn</a>, <a href="/search/hep-ph?searchtype=author&query=Carmona-Benitez%2C+M+C">M. C. Carmona-Benitez</a>, <a href="/search/hep-ph?searchtype=author&query=Chan%2C+C">C. Chan</a>, <a href="/search/hep-ph?searchtype=author&query=Chapman%2C+J+J">J. J. Chapman</a>, <a href="/search/hep-ph?searchtype=author&query=Chiller%2C+A+A">A. A. Chiller</a>, <a href="/search/hep-ph?searchtype=author&query=Chiller%2C+C">C. Chiller</a>, <a href="/search/hep-ph?searchtype=author&query=Currie%2C+A">A. Currie</a>, <a href="/search/hep-ph?searchtype=author&query=Cutter%2C+J+E">J. E. Cutter</a>, <a href="/search/hep-ph?searchtype=author&query=Davison%2C+T+J+R">T. J. R. Davison</a>, <a href="/search/hep-ph?searchtype=author&query=de+Viveiros%2C+L">L. de Viveiros</a>, <a href="/search/hep-ph?searchtype=author&query=Dobi%2C+A">A. Dobi</a>, <a href="/search/hep-ph?searchtype=author&query=Dobson%2C+J+E+Y">J. E. Y. Dobson</a> , et al. (77 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1602.03489v3-abstract-short" style="display: inline;"> We present the first experimental constraints on the spin-dependent WIMP-nucleon elastic cross sections from LUX data acquired in 2013. LUX is a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility (Lead, South Dakota), which is designed to observe the recoil signature of galactic WIMPs scattering from xenon nuclei. A profile likelihood ratio analysis of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.03489v3-abstract-full').style.display = 'inline'; document.getElementById('1602.03489v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.03489v3-abstract-full" style="display: none;"> We present the first experimental constraints on the spin-dependent WIMP-nucleon elastic cross sections from LUX data acquired in 2013. LUX is a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility (Lead, South Dakota), which is designed to observe the recoil signature of galactic WIMPs scattering from xenon nuclei. A profile likelihood ratio analysis of $1.4~\times~10^{4}~\text{kg}\cdot~\text{days}$ of fiducial exposure allows 90% CL upper limits to be set on the WIMP-neutron (WIMP-proton) cross section of $蟽_n~=~9.4~\times~10^{-41}~\text{cm}^2$ ($蟽_p~=~2.9~\times~10^{-39}~\text{cm}^2$) at 33 GeV/c$^2$. The spin-dependent WIMP-neutron limit is the most sensitive constraint to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.03489v3-abstract-full').style.display = 'none'; document.getElementById('1602.03489v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">6 pages, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 116, 161302 (2016) </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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