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is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.17137">arXiv:2410.17137</a> <span> [<a href="https://arxiv.org/pdf/2410.17137">pdf</a>, <a href="https://arxiv.org/format/2410.17137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> The XLZD Design Book: Towards the Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/hep-ph?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/hep-ph?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/hep-ph?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</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=Althueser%2C+L">L. Althueser</a>, <a href="/search/hep-ph?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</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=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/hep-ph?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/hep-ph?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/hep-ph?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/hep-ph?searchtype=author&query=Aprile%2C+E">E. Aprile</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=Babicz%2C+M">M. Babicz</a>, <a href="/search/hep-ph?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/hep-ph?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/hep-ph?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/hep-ph?searchtype=author&query=Bang%2C+J">J. Bang</a> , et al. (419 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.17137v1-abstract-short" style="display: inline;"> This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60-80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17137v1-abstract-full').style.display = 'inline'; document.getElementById('2410.17137v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.17137v1-abstract-full" style="display: none;"> This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60-80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generation experiments, LZ and XENONnT. A baseline design and opportunities for further optimization of the individual detector components are discussed. The experiment envisaged here has the capability to explore parameter space for Weakly Interacting Massive Particle (WIMP) dark matter down to the neutrino fog, with a 3$蟽$ evidence potential for the spin-independent WIMP-nucleon cross sections as low as $3\times10^{-49}\rm cm^2$ (at 40 GeV/c$^2$ WIMP mass). The observatory is also projected to have a 3$蟽$ observation potential of neutrinoless double-beta decay of $^{136}$Xe at a half-life of up to $5.7\times 10^{27}$ years. Additionally, it is sensitive to astrophysical neutrinos from the atmosphere, sun, and galactic supernovae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17137v1-abstract-full').style.display = 'none'; document.getElementById('2410.17137v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 14 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.05914">arXiv:2203.05914</a> <span> [<a href="https://arxiv.org/pdf/2203.05914">pdf</a>, <a href="https://arxiv.org/format/2203.05914">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="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Recoil imaging for directional detection of dark matter, neutrinos, and physics beyond the Standard Model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=O%27Hare%2C+C+A+J">C. A. J. O'Hare</a>, <a href="/search/hep-ph?searchtype=author&query=Loomba%2C+D">D. Loomba</a>, <a href="/search/hep-ph?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ph?searchtype=author&query=%C3%81lvarez-Pol%2C+H">H. 脕lvarez-Pol</a>, <a href="/search/hep-ph?searchtype=author&query=Amaro%2C+F+D">F. D. Amaro</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=Sierra%2C+D+A">D. Aristizabal Sierra</a>, <a href="/search/hep-ph?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/hep-ph?searchtype=author&query=Atti%C3%A9%2C+D">D. Atti茅</a>, <a href="/search/hep-ph?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ph?searchtype=author&query=Awe%2C+C">C. Awe</a>, <a href="/search/hep-ph?searchtype=author&query=Ayyad%2C+Y">Y. Ayyad</a>, <a href="/search/hep-ph?searchtype=author&query=Baracchini%2C+E">E. Baracchini</a>, <a href="/search/hep-ph?searchtype=author&query=Barbeau%2C+P">P. Barbeau</a>, <a href="/search/hep-ph?searchtype=author&query=Battat%2C+J+B+R">J. B. R. Battat</a>, <a href="/search/hep-ph?searchtype=author&query=Bell%2C+N+F">N. F. Bell</a>, <a href="/search/hep-ph?searchtype=author&query=Biasuzzi%2C+B">B. Biasuzzi</a>, <a href="/search/hep-ph?searchtype=author&query=Bignell%2C+L+J">L. J. Bignell</a>, <a href="/search/hep-ph?searchtype=author&query=Boehm%2C+C">C. Boehm</a>, <a href="/search/hep-ph?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/hep-ph?searchtype=author&query=Brunbauer%2C+F+M">F. M. Brunbauer</a>, <a href="/search/hep-ph?searchtype=author&query=Caama%C3%B1o%2C+M">M. Caama帽o</a>, <a href="/search/hep-ph?searchtype=author&query=Cabo%2C+C">C. Cabo</a>, <a href="/search/hep-ph?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/hep-ph?searchtype=author&query=Carmona%2C+J+M">J. M. Carmona</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="2203.05914v3-abstract-short" style="display: inline;"> Recoil imaging entails the detection of spatially resolved ionization tracks generated by particle interactions. This is a highly sought-after capability in many classes of detector, with broad applications across particle and astroparticle physics. However, at low energies, where ionization signatures are small in size, recoil imaging only seems to be a practical goal for micro-pattern gas detect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.05914v3-abstract-full').style.display = 'inline'; document.getElementById('2203.05914v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.05914v3-abstract-full" style="display: none;"> Recoil imaging entails the detection of spatially resolved ionization tracks generated by particle interactions. This is a highly sought-after capability in many classes of detector, with broad applications across particle and astroparticle physics. However, at low energies, where ionization signatures are small in size, recoil imaging only seems to be a practical goal for micro-pattern gas detectors. This white paper outlines the physics case for recoil imaging, and puts forward a decadal plan to advance towards the directional detection of low-energy recoils with sensitivity and resolution close to fundamental performance limits. The science case covered includes: the discovery of dark matter into the neutrino fog, directional detection of sub-MeV solar neutrinos, the precision study of coherent-elastic neutrino-nucleus scattering, the detection of solar axions, the measurement of the Migdal effect, X-ray polarimetry, and several other applied physics goals. We also outline the R&D programs necessary to test concepts that are crucial to advance detector performance towards their fundamental limit: single primary electron sensitivity with full 3D spatial resolution at the $\sim$100 micron-scale. These advancements include: the use of negative ion drift, electron counting with high-definition electronic readout, time projection chambers with optical readout, and the possibility for nuclear recoil tracking in high-density gases such as argon. We also discuss the readout and electronics systems needed to scale-up such detectors to the ton-scale and beyond. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.05914v3-abstract-full').style.display = 'none'; document.getElementById('2203.05914v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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, 20 figures. Submitted to the Proceedings of the US Community Study on the Future of Particle Physics (Snowmass 2021)</span> </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/1809.03753">arXiv:1809.03753</a> <span> [<a href="https://arxiv.org/pdf/1809.03753">pdf</a>, <a href="https://arxiv.org/format/1809.03753">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> </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/s10052-018-6523-4">10.1140/epjc/s10052-018-6523-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on Dark Matter Effective Field Theory Parameters with CRESST-II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/hep-ph?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/hep-ph?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/hep-ph?searchtype=author&query=Bertoldo%2C+E">E. Bertoldo</a>, <a href="/search/hep-ph?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/hep-ph?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/hep-ph?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/hep-ph?searchtype=author&query=Defay%2C+X">X. Defay</a>, <a href="/search/hep-ph?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/hep-ph?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/hep-ph?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/hep-ph?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/hep-ph?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/hep-ph?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/hep-ph?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/hep-ph?searchtype=author&query=Kiefer%2C+M">M. Kiefer</a>, <a href="/search/hep-ph?searchtype=author&query=Kluck%2C+H">H. Kluck</a>, <a href="/search/hep-ph?searchtype=author&query=Kraus%2C+H">H. Kraus</a>, <a href="/search/hep-ph?searchtype=author&query=Langenk%C3%A4mper%2C+A">A. Langenk盲mper</a>, <a href="/search/hep-ph?searchtype=author&query=Mancuso%2C+M">M. Mancuso</a>, <a href="/search/hep-ph?searchtype=author&query=Mokina%2C+V">V. Mokina</a>, <a href="/search/hep-ph?searchtype=author&query=Mondragon%2C+E">E. Mondragon</a>, <a href="/search/hep-ph?searchtype=author&query=Morgalyuk%2C+V">V. Morgalyuk</a>, <a href="/search/hep-ph?searchtype=author&query=M%C3%BCnster%2C+A">A. M眉nster</a>, <a href="/search/hep-ph?searchtype=author&query=Olmi%2C+M">M. Olmi</a> , et al. (20 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="1809.03753v1-abstract-short" style="display: inline;"> CRESST is a direct dark matter search experiment, aiming for an observation of nuclear recoils induced by the interaction of dark matter particles with cryogenic scintillating calcium tungstate crystals. Instead of confining ourselves to standard spin-independent and spin-dependent searches, we re-analyze data from CRESST-II using a more general effective field theory (EFT) framework. On many of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.03753v1-abstract-full').style.display = 'inline'; document.getElementById('1809.03753v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.03753v1-abstract-full" style="display: none;"> CRESST is a direct dark matter search experiment, aiming for an observation of nuclear recoils induced by the interaction of dark matter particles with cryogenic scintillating calcium tungstate crystals. Instead of confining ourselves to standard spin-independent and spin-dependent searches, we re-analyze data from CRESST-II using a more general effective field theory (EFT) framework. On many of the EFT coupling constants, improved exclusion limits in the low-mass region (< 3-4 GeV) are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.03753v1-abstract-full').style.display = 'none'; document.getElementById('1809.03753v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">7 pages, 9 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/1408.2357">arXiv:1408.2357</a> <span> [<a href="https://arxiv.org/pdf/1408.2357">pdf</a>, <a href="https://arxiv.org/format/1408.2357">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="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.astropartphys.2015.03.010">10.1016/j.astropartphys.2015.03.010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Impact of Coherent Neutrino Nucleus Scattering on Direct Dark Matter Searches based on CaWO$_4$ Crystals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=G%C3%BCtlein%2C+A">A. G眉tlein</a>, <a href="/search/hep-ph?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/hep-ph?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/hep-ph?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/hep-ph?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/hep-ph?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/hep-ph?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/hep-ph?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/hep-ph?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/hep-ph?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/hep-ph?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/hep-ph?searchtype=author&query=Kiefer%2C+M">M. Kiefer</a>, <a href="/search/hep-ph?searchtype=author&query=Kluck%2C+H">H. Kluck</a>, <a href="/search/hep-ph?searchtype=author&query=Kraus%2C+H">H. Kraus</a>, <a href="/search/hep-ph?searchtype=author&query=Lanfranchi%2C+J+-">J. -C. Lanfranchi</a>, <a href="/search/hep-ph?searchtype=author&query=Loebell%2C+J">J. Loebell</a>, <a href="/search/hep-ph?searchtype=author&query=M%C3%BCnster%2C+A">A. M眉nster</a>, <a href="/search/hep-ph?searchtype=author&query=Petricca%2C+F">F. Petricca</a>, <a href="/search/hep-ph?searchtype=author&query=Potzel%2C+W">W. Potzel</a>, <a href="/search/hep-ph?searchtype=author&query=Pr%C3%B6bst%2C+F">F. Pr枚bst</a>, <a href="/search/hep-ph?searchtype=author&query=Reindl%2C+F">F. Reindl</a>, <a href="/search/hep-ph?searchtype=author&query=Roth%2C+S">S. Roth</a>, <a href="/search/hep-ph?searchtype=author&query=Rottler%2C+K">K. Rottler</a>, <a href="/search/hep-ph?searchtype=author&query=Sailer%2C+C">C. Sailer</a>, <a href="/search/hep-ph?searchtype=author&query=Sch%C3%A4ffner%2C+K">K. Sch盲ffner</a> , et al. (15 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="1408.2357v2-abstract-short" style="display: inline;"> Atmospheric and solar neutrinos scattering coherently off target nuclei will be an important background source for the next generation of direct dark matter searches. In this work we focus on calcium tungstate as target material. For comparison with existing works we calculate the neutrino floor indicating which sensitivities can be reached before the neutrino background appears. In addition, we i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.2357v2-abstract-full').style.display = 'inline'; document.getElementById('1408.2357v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.2357v2-abstract-full" style="display: none;"> Atmospheric and solar neutrinos scattering coherently off target nuclei will be an important background source for the next generation of direct dark matter searches. In this work we focus on calcium tungstate as target material. For comparison with existing works we calculate the neutrino floor indicating which sensitivities can be reached before the neutrino background appears. In addition, we investigate the sensitivities of future direct dark matter searches using CRESST-II like detectors. Extending previous works we take into account achievable energy resolutions and thresholds as well as beta and gamma backgrounds for this investigation. We show that an exploration of WIMP-nucleon cross sections below the neutrino floor is possible for exposures of $\gtrsim10$ kg-years or higher. In the third part we show that a first detection of coherent neutrino nucleus scattering of atmospheric and solar neutrinos using the same detectors and the backgrounds is feasible for exposures of $\gtrsim50$ kg-years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.2357v2-abstract-full').style.display = 'none'; document.getElementById('1408.2357v2-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 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">submitted to Astorparticle 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/1307.1488">arXiv:1307.1488</a> <span> [<a href="https://arxiv.org/pdf/1307.1488">pdf</a>, <a href="https://arxiv.org/ps/1307.1488">ps</a>, <a href="https://arxiv.org/format/1307.1488">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/10.1088/1475-7516/2013/11/067">10.1088/1475-7516/2013/11/067 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Axion searches with the EDELWEISS-II experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/hep-ph?searchtype=author&query=Arnaud%2C+Q">Q. Arnaud</a>, <a href="/search/hep-ph?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/hep-ph?searchtype=author&query=Benoit%2C+A">A. Benoit</a>, <a href="/search/hep-ph?searchtype=author&query=Benoit%2C+A">A. Benoit</a>, <a href="/search/hep-ph?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/hep-ph?searchtype=author&query=Bergmann%2C+T">T. Bergmann</a>, <a href="/search/hep-ph?searchtype=author&query=Bl%C3%BCmer%2C+J">J. Bl眉mer</a>, <a href="/search/hep-ph?searchtype=author&query=Broniatowski%2C+A">A. Broniatowski</a>, <a href="/search/hep-ph?searchtype=author&query=Brudanin%2C+V">V. Brudanin</a>, <a href="/search/hep-ph?searchtype=author&query=Camus%2C+P">P. Camus</a>, <a href="/search/hep-ph?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/hep-ph?searchtype=author&query=Censier%2C+B">B. Censier</a>, <a href="/search/hep-ph?searchtype=author&query=Chapellier%2C+M">M. Chapellier</a>, <a href="/search/hep-ph?searchtype=author&query=Charlieux%2C+F">F. Charlieux</a>, <a href="/search/hep-ph?searchtype=author&query=Cou%C3%ABdo%2C+F">F. Cou毛do</a>, <a href="/search/hep-ph?searchtype=author&query=Coulter%2C+P">P. Coulter</a>, <a href="/search/hep-ph?searchtype=author&query=Cox%2C+G+A">G. A. Cox</a>, <a href="/search/hep-ph?searchtype=author&query=de+Boissi%C3%A8re%2C+T">T. de Boissi猫re</a>, <a href="/search/hep-ph?searchtype=author&query=De+Jesus%2C+M">M. De Jesus</a>, <a href="/search/hep-ph?searchtype=author&query=Dolgorouky%2C+Y">Y. Dolgorouky</a>, <a href="/search/hep-ph?searchtype=author&query=Drillien%2C+A+A">A. A. Drillien</a>, <a href="/search/hep-ph?searchtype=author&query=Dumoulin%2C+L">L. Dumoulin</a>, <a href="/search/hep-ph?searchtype=author&query=Eitel%2C+K">K. Eitel</a>, <a href="/search/hep-ph?searchtype=author&query=Filosofov%2C+D">D. Filosofov</a> , et al. (41 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="1307.1488v1-abstract-short" style="display: inline;"> We present new constraints on the couplings of axions and more generic axion-like particles using data from the EDELWEISS-II experiment. The EDELWEISS experiment, located at the Underground Laboratory of Modane, primarily aims at the direct detection of WIMPs using germanium bolometers. It is also sensitive to the low-energy electron recoils that would be induced by solar or dark matter axions. Us… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.1488v1-abstract-full').style.display = 'inline'; document.getElementById('1307.1488v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.1488v1-abstract-full" style="display: none;"> We present new constraints on the couplings of axions and more generic axion-like particles using data from the EDELWEISS-II experiment. The EDELWEISS experiment, located at the Underground Laboratory of Modane, primarily aims at the direct detection of WIMPs using germanium bolometers. It is also sensitive to the low-energy electron recoils that would be induced by solar or dark matter axions. Using a total exposure of up to 448 kg.d, we searched for axion-induced electron recoils down to 2.5 keV within four scenarios involving different hypotheses on the origin and couplings of axions. We set a 95% CL limit on the coupling to photons $g_{A纬}<2.13\times 10^{-9}$ GeV$^{-1}$ in a mass range not fully covered by axion helioscopes. We also constrain the coupling to electrons, $g_{Ae} < 2.56\times 10^{-11}$, similar to the more indirect solar neutrino bound. Finally we place a limit on $g_{Ae}\times g_{AN}^{\rm eff}<4.70 \times 10^{-17}$, where $g_{AN}^{\rm eff}$ is the effective axion-nucleon coupling for $^{57}$Fe. Combining these results we fully exclude the mass range $0.91\,{\rm eV}<m_A<80$ keV for DFSZ axions and $5.73\,{\rm eV}<m_A<40$ keV for KSVZ axions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.1488v1-abstract-full').style.display = 'none'; document.getElementById('1307.1488v1-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 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">Journal ref:</span> JCAP 1311 (2013) 067 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1109.2589">arXiv:1109.2589</a> <span> [<a href="https://arxiv.org/pdf/1109.2589">pdf</a>, <a href="https://arxiv.org/format/1109.2589">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/PhysRevD.85.021301">10.1103/PhysRevD.85.021301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extending the CRESST-II commissioning run limits to lower masses </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Brown%2C+A">Andrew Brown</a>, <a href="/search/hep-ph?searchtype=author&query=Henry%2C+S">Sam Henry</a>, <a href="/search/hep-ph?searchtype=author&query=Kraus%2C+H">Hans Kraus</a>, <a href="/search/hep-ph?searchtype=author&query=McCabe%2C+C">Christopher McCabe</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="1109.2589v2-abstract-short" style="display: inline;"> Motivated by the recent interest in light WIMPs of mass ~O(10 GeV), an extension of the elastic, spin-independent WIMP-nucleon cross-section limits resulting from the CRESST-II commissioning run (2007) are presented. Previously, these data were used to set cross-section limits from 1000 GeV down to ~17 GeV, using tungsten recoils, in 47.9 kg-days of exposure of calcium tungstate. Here, the overlap… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.2589v2-abstract-full').style.display = 'inline'; document.getElementById('1109.2589v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1109.2589v2-abstract-full" style="display: none;"> Motivated by the recent interest in light WIMPs of mass ~O(10 GeV), an extension of the elastic, spin-independent WIMP-nucleon cross-section limits resulting from the CRESST-II commissioning run (2007) are presented. Previously, these data were used to set cross-section limits from 1000 GeV down to ~17 GeV, using tungsten recoils, in 47.9 kg-days of exposure of calcium tungstate. Here, the overlap of the oxygen and calcium bands with the acceptance region of the commissioning run data set is reconstructed using previously published quenching factors. The resulting elastic WIMP cross section limits, accounting for the additional exposure of oxygen and calcium, are presented down to 5 GeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.2589v2-abstract-full').style.display = 'none'; document.getElementById('1109.2589v2-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 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 September, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2011. </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">4 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> OUTP-11-50-P </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D85:021301,2012 </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 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