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<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/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> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a 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