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class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.08022">arXiv:2411.08022</a> <span> [<a href="https://arxiv.org/pdf/2411.08022">pdf</a>, <a href="https://arxiv.org/format/2411.08022">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Commissioning of the 2.6 m tall two-phase xenon time projection chamber of Xenoscope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/?searchtype=author&query=Biondi%2C+Y">Y. Biondi</a>, <a href="/search/?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/?searchtype=author&query=Ch%C3%A1vez%2C+A+P+C">A. P. Cimental Ch谩vez</a>, <a href="/search/?searchtype=author&query=Cuenca-Garc%C3%ADa%2C+J+J">J. J. Cuenca-Garc铆a</a>, <a href="/search/?searchtype=author&query=Galloway%2C+M">M. Galloway</a>, <a href="/search/?searchtype=author&query=Girard%2C+F">F. Girard</a>, <a href="/search/?searchtype=author&query=J%C3%B6rg%2C+F">F. J枚rg</a>, <a href="/search/?searchtype=author&query=Ouahada%2C+S">S. Ouahada</a>, <a href="/search/?searchtype=author&query=Peres%2C+R">R. Peres</a>, <a href="/search/?searchtype=author&query=Piastra%2C+F">F. Piastra</a>, <a href="/search/?searchtype=author&query=Silva%2C+M+R">M. Rajado Silva</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa%2C+D+R">D. Ram铆rez Garc铆a</a>, <a href="/search/?searchtype=author&query=Wittweg%2C+C">C. Wittweg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.08022v2-abstract-short" style="display: inline;"> Xenoscope is a demonstrator for a next-generation xenon-based observatory for astroparticle physics, as proposed by the XLZD (XENON-LUX-ZEPLIN-DARWIN) collaboration. It houses a 2.6 m tall, two-phase xenon time projection chamber (TPC), in a cryostat filled with $\sim$ 360 kg of liquid xenon. The main goals of the facility are to demonstrate electron drift in liquid xenon over this distance, to me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08022v2-abstract-full').style.display = 'inline'; document.getElementById('2411.08022v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.08022v2-abstract-full" style="display: none;"> Xenoscope is a demonstrator for a next-generation xenon-based observatory for astroparticle physics, as proposed by the XLZD (XENON-LUX-ZEPLIN-DARWIN) collaboration. It houses a 2.6 m tall, two-phase xenon time projection chamber (TPC), in a cryostat filled with $\sim$ 360 kg of liquid xenon. The main goals of the facility are to demonstrate electron drift in liquid xenon over this distance, to measure the electron cloud transversal and longitudinal diffusion, as well as the optical properties of the medium. In this work, we describe in detail the construction and commissioning of the TPC and report on the observation of light and charge signals with cosmic muons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08022v2-abstract-full').style.display = 'none'; document.getElementById('2411.08022v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.19016">arXiv:2410.19016</a> <span> [<a href="https://arxiv.org/pdf/2410.19016">pdf</a>, <a href="https://arxiv.org/format/2410.19016">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Neutrinoless Double Beta Decay Sensitivity of the XLZD Rare Event Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/?searchtype=author&query=Bang%2C+J">J. Bang</a> , et al. (419 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.19016v1-abstract-short" style="display: inline;"> The XLZD collaboration is developing a two-phase xenon time projection chamber with an active mass of 60 to 80 t capable of probing the remaining WIMP-nucleon interaction parameter space down to the so-called neutrino fog. In this work we show that, based on the performance of currently operating detectors using the same technology and a realistic reduction of radioactivity in detector materials,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19016v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19016v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19016v1-abstract-full" style="display: none;"> The XLZD collaboration is developing a two-phase xenon time projection chamber with an active mass of 60 to 80 t capable of probing the remaining WIMP-nucleon interaction parameter space down to the so-called neutrino fog. In this work we show that, based on the performance of currently operating detectors using the same technology and a realistic reduction of radioactivity in detector materials, such an experiment will also be able to competitively search for neutrinoless double beta decay in $^{136}$Xe using a natural-abundance xenon target. XLZD can reach a 3$蟽$ discovery potential half-life of 5.7$\times$10$^{27}$ yr (and a 90% CL exclusion of 1.3$\times$10$^{28}$ yr) with 10 years of data taking, corresponding to a Majorana mass range of 7.3-31.3 meV (4.8-20.5 meV). XLZD will thus exclude the inverted neutrino mass ordering parameter space and will start to probe the normal ordering region for most of the nuclear matrix elements commonly considered by the community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19016v1-abstract-full').style.display = 'none'; document.getElementById('2410.19016v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 7 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.17137">arXiv:2410.17137</a> <span> [<a href="https://arxiv.org/pdf/2410.17137">pdf</a>, <a href="https://arxiv.org/format/2410.17137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> The XLZD Design Book: Towards the Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=XLZD+Collaboration"> XLZD Collaboration</a>, <a href="/search/?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/?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/2410.00755">arXiv:2410.00755</a> <span> [<a href="https://arxiv.org/pdf/2410.00755">pdf</a>, <a href="https://arxiv.org/format/2410.00755">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Model-independent searches of new physics in DARWIN with a semi-supervised deep learning pipeline </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/?searchtype=author&query=Maouloud%2C+S+A">S. Ahmed Maouloud</a>, <a href="/search/?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/?searchtype=author&query=Amaral%2C+D+W+P">D. W. P. Amaral</a>, <a href="/search/?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/?searchtype=author&query=Martin%2C+D+A">D. Ant贸n Martin</a>, <a href="/search/?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/?searchtype=author&query=Balzer%2C+M">M. Balzer</a>, <a href="/search/?searchtype=author&query=Barberio%2C+E">E. Barberio</a>, <a href="/search/?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/?searchtype=author&query=Bell%2C+N+F">N. F. Bell</a>, <a href="/search/?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/?searchtype=author&query=Biondi%2C+Y">Y. Biondi</a>, <a href="/search/?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/?searchtype=author&query=Boehm%2C+C">C. Boehm</a>, <a href="/search/?searchtype=author&query=Boese%2C+K">K. Boese</a>, <a href="/search/?searchtype=author&query=Braun%2C+R">R. Braun</a> , et al. (209 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="2410.00755v1-abstract-short" style="display: inline;"> We present a novel deep learning pipeline to perform a model-independent, likelihood-free search for anomalous (i.e., non-background) events in the proposed next generation multi-ton scale liquid Xenon-based direct detection experiment, DARWIN. We train an anomaly detector comprising a variational autoencoder and a classifier on extensive, high-dimensional simulated detector response data and cons… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00755v1-abstract-full').style.display = 'inline'; document.getElementById('2410.00755v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.00755v1-abstract-full" style="display: none;"> We present a novel deep learning pipeline to perform a model-independent, likelihood-free search for anomalous (i.e., non-background) events in the proposed next generation multi-ton scale liquid Xenon-based direct detection experiment, DARWIN. We train an anomaly detector comprising a variational autoencoder and a classifier on extensive, high-dimensional simulated detector response data and construct a one-dimensional anomaly score optimised to reject the background only hypothesis in the presence of an excess of non-background-like events. We benchmark the procedure with a sensitivity study that determines its power to reject the background-only hypothesis in the presence of an injected WIMP dark matter signal, outperforming the classical, likelihood-based background rejection test. We show that our neural networks learn relevant energy features of the events from low-level, high-dimensional detector outputs, without the need to compress this data into lower-dimensional observables, thus reducing computational effort and information loss. For the future, our approach lays the foundation for an efficient end-to-end pipeline that eliminates the need for many of the corrections and cuts that are traditionally part of the analysis chain, with the potential of achieving higher accuracy and significant reduction of analysis time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00755v1-abstract-full').style.display = 'none'; document.getElementById('2410.00755v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 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">10 Figures, 3 Tables, 23 Pages (incl. references)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.16340">arXiv:2306.16340</a> <span> [<a href="https://arxiv.org/pdf/2306.16340">pdf</a>, <a href="https://arxiv.org/format/2306.16340">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-023-12298-w">10.1140/epjc/s10052-023-12298-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmogenic background simulations for the DARWIN observatory at different underground locations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Adrover%2C+M">M. Adrover</a>, <a href="/search/?searchtype=author&query=Althueser%2C+L">L. Althueser</a>, <a href="/search/?searchtype=author&query=Andrieu%2C+B">B. Andrieu</a>, <a href="/search/?searchtype=author&query=Angelino%2C+E">E. Angelino</a>, <a href="/search/?searchtype=author&query=Angevaare%2C+J+R">J. R. Angevaare</a>, <a href="/search/?searchtype=author&query=Antunovic%2C+B">B. Antunovic</a>, <a href="/search/?searchtype=author&query=Aprile%2C+E">E. Aprile</a>, <a href="/search/?searchtype=author&query=Babicz%2C+M">M. Babicz</a>, <a href="/search/?searchtype=author&query=Bajpai%2C+D">D. Bajpai</a>, <a href="/search/?searchtype=author&query=Barberio%2C+E">E. Barberio</a>, <a href="/search/?searchtype=author&query=Baudis%2C+L">L. Baudis</a>, <a href="/search/?searchtype=author&query=Bazyk%2C+M">M. Bazyk</a>, <a href="/search/?searchtype=author&query=Bell%2C+N">N. Bell</a>, <a href="/search/?searchtype=author&query=Bellagamba%2C+L">L. Bellagamba</a>, <a href="/search/?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/?searchtype=author&query=Biondi%2C+Y">Y. Biondi</a>, <a href="/search/?searchtype=author&query=Bismark%2C+A">A. Bismark</a>, <a href="/search/?searchtype=author&query=Boehm%2C+C">C. Boehm</a>, <a href="/search/?searchtype=author&query=Breskin%2C+A">A. Breskin</a>, <a href="/search/?searchtype=author&query=Brookes%2C+E+J">E. J. Brookes</a>, <a href="/search/?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/?searchtype=author&query=Budnik%2C+R">R. Budnik</a>, <a href="/search/?searchtype=author&query=Capelli%2C+C">C. Capelli</a>, <a href="/search/?searchtype=author&query=Cardoso%2C+J+M+R">J. M. R. Cardoso</a> , et al. (158 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="2306.16340v1-abstract-short" style="display: inline;"> Xenon dual-phase time projections chambers (TPCs) have proven to be a successful technology in studying physical phenomena that require low-background conditions. With 40t of liquid xenon (LXe) in the TPC baseline design, DARWIN will have a high sensitivity for the detection of particle dark matter, neutrinoless double beta decay ($0谓尾尾$), and axion-like particles (ALPs). Although cosmic muons are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16340v1-abstract-full').style.display = 'inline'; document.getElementById('2306.16340v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.16340v1-abstract-full" style="display: none;"> Xenon dual-phase time projections chambers (TPCs) have proven to be a successful technology in studying physical phenomena that require low-background conditions. With 40t of liquid xenon (LXe) in the TPC baseline design, DARWIN will have a high sensitivity for the detection of particle dark matter, neutrinoless double beta decay ($0谓尾尾$), and axion-like particles (ALPs). Although cosmic muons are a source of background that cannot be entirely eliminated, they may be greatly diminished by placing the detector deep underground. In this study, we used Monte Carlo simulations to model the cosmogenic background expected for the DARWIN observatory at four underground laboratories: Laboratori Nazionali del Gran Sasso (LNGS), Sanford Underground Research Facility (SURF), Laboratoire Souterrain de Modane (LSM) and SNOLAB. We determine the production rates of unstable xenon isotopes and tritium due to muon-included neutron fluxes and muon-induced spallation. These are expected to represent the dominant contributions to cosmogenic backgrounds and thus the most relevant for site selection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16340v1-abstract-full').style.display = 'none'; document.getElementById('2306.16340v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.10032">arXiv:2004.10032</a> <span> [<a href="https://arxiv.org/pdf/2004.10032">pdf</a>, <a href="https://arxiv.org/format/2004.10032">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 Astrophysical Phenomena">astro-ph.HE</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/10.1093/mnras/staa1156">10.1093/mnras/staa1156 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The high-energy emission from HD~93129A near periastron </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=del+Palacio%2C+S">S. del Palacio</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa%2C+F">F. Garc铆a</a>, <a href="/search/?searchtype=author&query=Altamirano%2C+D">D. Altamirano</a>, <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&query=Bosch-Ramon%2C+V">V. Bosch-Ramon</a>, <a href="/search/?searchtype=author&query=Corcoran%2C+M">M. Corcoran</a>, <a href="/search/?searchtype=author&query=De+Becker%2C+M">M. De Becker</a>, <a href="/search/?searchtype=author&query=Hamaguchi%2C+K">K. Hamaguchi</a>, <a href="/search/?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/?searchtype=author&query=Adrover%2C+P+M">P. Munar Adrover</a>, <a href="/search/?searchtype=author&query=Paredes%2C+J+M">J. M. Paredes</a>, <a href="/search/?searchtype=author&query=Romero%2C+G+E">G. E. Romero</a>, <a href="/search/?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/?searchtype=author&query=Tavani%2C+M">M. Tavani</a>, <a href="/search/?searchtype=author&query=ud-Doula%2C+A">A. ud-Doula</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="2004.10032v1-abstract-short" style="display: inline;"> We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD~93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites \textit{Chandra} and \textit{NuSTAR} and the $纬$-ray satellite \textit{AGILE}… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10032v1-abstract-full').style.display = 'inline'; document.getElementById('2004.10032v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.10032v1-abstract-full" style="display: none;"> We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD~93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites \textit{Chandra} and \textit{NuSTAR} and the $纬$-ray satellite \textit{AGILE}. High-energy emission coincident with HD~93129A was detected in the X-ray band up to $\sim$18~keV, whereas in the $纬$-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, $f_\mathrm{NT,e} < 0.02$. In addition, we set a lower limit for the magnetic field in the wind-collision region as $B_\mathrm{WCR} > 0.3$~G. We also argue a putative interpretation of the emission from which we estimate $f_\mathrm{NT,e} \approx 0.006$ and $B_\mathrm{WCR} \approx 0.5$~G. We conclude that multi-wavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterising the relativistic particle content and magnetic field intensity in colliding wind binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10032v1-abstract-full').style.display = 'none'; document.getElementById('2004.10032v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 10 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.09342">arXiv:1909.09342</a> <span> [<a href="https://arxiv.org/pdf/1909.09342">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Raman LIDARs for the atmospheric calibration along the line-of-sight of CTA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ballester%2C+O">Otger Ballester</a>, <a href="/search/?searchtype=author&query=Blanch%2C+O">Oscar Blanch</a>, <a href="/search/?searchtype=author&query=Boix%2C+J">Joan Boix</a>, <a href="/search/?searchtype=author&query=Bregeon%2C+J">Johan Bregeon</a>, <a href="/search/?searchtype=author&query=Brun%2C+P">Patrick Brun</a>, <a href="/search/?searchtype=author&query=Colak%2C+M">Merve Colak</a>, <a href="/search/?searchtype=author&query=Doro%2C+M">Michele Doro</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">Vania Da Deppo</a>, <a href="/search/?searchtype=author&query=Font%2C+L">Lluis Font</a>, <a href="/search/?searchtype=author&query=Gabella%2C+O">Omar Gabella</a>, <a href="/search/?searchtype=author&query=Garcia%2C+R">Rafael Garcia</a>, <a href="/search/?searchtype=author&query=Gaug%2C+M">Markus Gaug</a>, <a href="/search/?searchtype=author&query=Maggio%2C+C">Camilla Maggio</a>, <a href="/search/?searchtype=author&query=Martinez%2C+M">Manel Martinez</a>, <a href="/search/?searchtype=author&query=Martinez%2C+O">Oscar Martinez</a>, <a href="/search/?searchtype=author&query=Adrover%2C+P+M">Pere Munar Adrover</a>, <a href="/search/?searchtype=author&query=Ramos%2C+R">Raul Ramos</a>, <a href="/search/?searchtype=author&query=Rivoire%2C+S">Stephane Rivoire</a>, <a href="/search/?searchtype=author&query=Stanic%2C+S">Samo Stanic</a>, <a href="/search/?searchtype=author&query=Villar%2C+D">David Villar</a>, <a href="/search/?searchtype=author&query=Vasileiadis%2C+G">George Vasileiadis</a>, <a href="/search/?searchtype=author&query=Wang%2C+L">Longlong Wang</a>, <a href="/search/?searchtype=author&query=Zavrtanik%2C+M">Marko Zavrtanik</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="1909.09342v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is the next generation ground based observatory for gamma ray astronomy at very high energies. Employing more than 100 Imaging Atmospheric Cherenkov Telescopes in the northern and southern hemispheres, it was designed to reach unprecedented sensitivity and energy resolution. Understanding and correcting for systematic biases on the absolute energy scale and inst… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.09342v1-abstract-full').style.display = 'inline'; document.getElementById('1909.09342v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.09342v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is the next generation ground based observatory for gamma ray astronomy at very high energies. Employing more than 100 Imaging Atmospheric Cherenkov Telescopes in the northern and southern hemispheres, it was designed to reach unprecedented sensitivity and energy resolution. Understanding and correcting for systematic biases on the absolute energy scale and instrument response functions will be a crucial issue for the performance of CTA. The LUPM group and the Spanish/Italian/Slovenian collaboration are currently building two Raman LIDAR prototypes for the online atmospheric calibration along the line of sight of the CTA. Requirements for such a solution include the ability to characterize aerosol extinction at two wavelengths to distances of 30 km with an accuracy better than 5%, within time scales of about a minute, steering capabilities and close interaction with the CTA array control and data acquisition system as well as other auxiliary instruments. Our Raman LIDARs have design features that make them different from those used in atmospheric science and are characterized by large collecting mirrors (2.5 m2), liquid light guides that collect the light at the focal plane and transport it to the readout system, reduced acquisition time and highly precise Raman spectrometers. The Raman LIDARs will participate in a cross calibration and characterization campaign of the atmosphere at the CTA North site at La Palma, together with other site characterization instruments. After a one year test period there, an in depth evaluation of the solutions adopted by the two projects will lead to a final Raman LIDAR design proposal for both CTA sites. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.09342v1-abstract-full').style.display = 'none'; document.getElementById('1909.09342v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </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 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