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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.19864">arXiv:2412.19864</a> <span> [<a href="https://arxiv.org/pdf/2412.19864">pdf</a>, <a href="https://arxiv.org/format/2412.19864">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"> Micromegas with GEM preamplification for enhanced energy threshold in low-background gaseous time projection chambers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Castel%2C+J">J. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Ib%C3%A1%C3%B1ez%2C+D">D. D铆ez-Ib谩帽ez</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Ezquerro%2C+A">A. Ezquerro</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">I. G Irastorza</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">G. Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A. Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">O. P茅rez</a>, <a href="/search/physics?searchtype=author&query=Porr%C3%B3n%2C+J">J. Porr贸n</a>, <a href="/search/physics?searchtype=author&query=Puyuelo%2C+M+J">M. J. Puyuelo</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="2412.19864v1-abstract-short" style="display: inline;"> Background: we develop the concept of a Micromegas (MICRO-MEsh GAseous Structure) readout plane with an additional GEM (Gas Electron Multiplier) preamplification stage placed a few mm above it, to increase the maximum effective gain of the combined readout. We implement it and test it in realistic conditions for its application to low-background dark matter searches like the TREX-DM experiment. Me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19864v1-abstract-full').style.display = 'inline'; document.getElementById('2412.19864v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.19864v1-abstract-full" style="display: none;"> Background: we develop the concept of a Micromegas (MICRO-MEsh GAseous Structure) readout plane with an additional GEM (Gas Electron Multiplier) preamplification stage placed a few mm above it, to increase the maximum effective gain of the combined readout. We implement it and test it in realistic conditions for its application to low-background dark matter searches like the TREX-DM experiment. Methods: for this, we use a Micromegas of microbulk type, built with radiopure materials. A small test chamber allowing for systematic scanning of voltages and pressures is used. In addition, a TREX-DM full-scale set-up has also been built and tested, featuring a replica of the fully-patterned TREX-DM microbulk readout. Results: we report on GEM effective extra gain factors of about 90, 50 and 20 in 1, 4 and 10 bar of Ar-1%iC$_{4}$H$_{10}$. Conclusions: the results here obtained show promise to lower the threshold of the experiment down to 50 eV$_{ee}$, corresponding to substantially enhanced sensitivity to low-mass WIMPs (Weakly Interacting Massive Particles). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19864v1-abstract-full').style.display = 'none'; document.getElementById('2412.19864v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">14 pages, 8 figures, corresponding authors: 脫scar P茅rez (oscarperlaz@unizar.es), H茅ctor Mirallas (mirallas@unizar.es)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.13915">arXiv:2411.13915</a> <span> [<a href="https://arxiv.org/pdf/2411.13915">pdf</a>, <a href="https://arxiv.org/format/2411.13915">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> An accurate solar axions ray-tracing response of BabyIAXO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ahyoune%2C+S">S. Ahyoune</a>, <a href="/search/physics?searchtype=author&query=Altenmueller%2C+K">K. Altenmueller</a>, <a href="/search/physics?searchtype=author&query=Antolin%2C+I">I. Antolin</a>, <a href="/search/physics?searchtype=author&query=Basso%2C+S">S. Basso</a>, <a href="/search/physics?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/physics?searchtype=author&query=Candon%2C+F+R">F. R. Candon</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/physics?searchtype=author&query=Chouhan%2C+D">D. Chouhan</a>, <a href="/search/physics?searchtype=author&query=Della+Ceca%2C+R">R. Della Ceca</a>, <a href="/search/physics?searchtype=author&query=Cervera-Cortes%2C+M">M. Cervera-Cortes</a>, <a href="/search/physics?searchtype=author&query=Chernov%2C+V">V. Chernov</a>, <a href="/search/physics?searchtype=author&query=Civitani%2C+M+M">M. M. Civitani</a>, <a href="/search/physics?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/physics?searchtype=author&query=Costa%2C+E">E. Costa</a>, <a href="/search/physics?searchtype=author&query=Cotroneo%2C+V">V. Cotroneo</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/physics?searchtype=author&query=Diaz-Martin%2C+M+C">M. C. Diaz-Martin</a>, <a href="/search/physics?searchtype=author&query=Diaz-Morcillo%2C+A">A. Diaz-Morcillo</a>, <a href="/search/physics?searchtype=author&query=Diez-Ibanez%2C+D">D. Diez-Ibanez</a>, <a href="/search/physics?searchtype=author&query=Pardos%2C+C+D">C. Diez Pardos</a>, <a href="/search/physics?searchtype=author&query=Dinter%2C+M">M. Dinter</a>, <a href="/search/physics?searchtype=author&query=Doebrich%2C+B">B. Doebrich</a> , et al. (102 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="2411.13915v2-abstract-short" style="display: inline;"> BabyIAXO is the intermediate stage of the International Axion Observatory (IAXO) to be hosted at DESY. Its primary goal is the detection of solar axions following the axion helioscope technique. Axions are converted into photons in a large magnet that is pointing to the sun. The resulting X-rays are focused by appropriate X-ray optics and detected by sensitive low-background detectors placed at th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13915v2-abstract-full').style.display = 'inline'; document.getElementById('2411.13915v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.13915v2-abstract-full" style="display: none;"> BabyIAXO is the intermediate stage of the International Axion Observatory (IAXO) to be hosted at DESY. Its primary goal is the detection of solar axions following the axion helioscope technique. Axions are converted into photons in a large magnet that is pointing to the sun. The resulting X-rays are focused by appropriate X-ray optics and detected by sensitive low-background detectors placed at the focal spot. The aim of this article is to provide an accurate quantitative description of the different components (such as the magnet, optics, and X-ray detectors) involved in the detection of axions. Our efforts have focused on developing robust and integrated software tools to model these helioscope components, enabling future assessments of modifications or upgrades to any part of the IAXO axion helioscope and evaluating the potential impact on the experiment's sensitivity. In this manuscript, we demonstrate the application of these tools by presenting a precise signal calculation and response analysis of BabyIAXO's sensitivity to the axion-photon coupling. Though focusing on the Primakoff solar flux component, our virtual helioscope model can be used to test different production mechanisms, allowing for direct comparisons within a unified framework. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13915v2-abstract-full').style.display = 'none'; document.getElementById('2411.13915v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 18 figures, 4 tables, Submitted to JHEP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.10972">arXiv:2405.10972</a> <span> [<a href="https://arxiv.org/pdf/2405.10972">pdf</a>, <a href="https://arxiv.org/format/2405.10972">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and 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> <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 daily modulations and broadband strategy in axion searches. An application with CAST-CAPP detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adair%2C+C+M">C. M. Adair</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Anastassopoulos%2C+V">V. Anastassopoulos</a>, <a href="/search/physics?searchtype=author&query=Cuendis%2C+S+A">S. Arguedas Cuendis</a>, <a href="/search/physics?searchtype=author&query=Baier%2C+J">J. Baier</a>, <a href="/search/physics?searchtype=author&query=Barth%2C+K">K. Barth</a>, <a href="/search/physics?searchtype=author&query=Belov%2C+A">A. Belov</a>, <a href="/search/physics?searchtype=author&query=Bozicevic%2C+D">D. Bozicevic</a>, <a href="/search/physics?searchtype=author&query=Br%C3%A4uninger%2C+H">H. Br盲uninger</a>, <a href="/search/physics?searchtype=author&query=Cantatore%2C+G">G. Cantatore</a>, <a href="/search/physics?searchtype=author&query=Caspers%2C+F">F. Caspers</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=%C3%87etin%2C+S+A">S. A. 脟etin</a>, <a href="/search/physics?searchtype=author&query=Chung%2C+W">W. Chung</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+H">H. Choi</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+J">J. Choi</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=Davenport%2C+M">M. Davenport</a>, <a href="/search/physics?searchtype=author&query=Dermenev%2C+A">A. Dermenev</a>, <a href="/search/physics?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/physics?searchtype=author&query=D%C3%B6brich%2C+B">B. D枚brich</a>, <a href="/search/physics?searchtype=author&query=Fischer%2C+H">H. Fischer</a>, <a href="/search/physics?searchtype=author&query=Funk%2C+W">W. Funk</a>, <a href="/search/physics?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/physics?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.10972v1-abstract-short" style="display: inline;"> It has been previously advocated that the presence of the daily and annual modulations of the axion flux on the Earth's surface may dramatically change the strategy of the axion searches. The arguments were based on the so-called Axion Quark Nugget (AQN) dark matter model which was originally put forward to explain the similarity of the dark and visible cosmological matter densities… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.10972v1-abstract-full').style.display = 'inline'; document.getElementById('2405.10972v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.10972v1-abstract-full" style="display: none;"> It has been previously advocated that the presence of the daily and annual modulations of the axion flux on the Earth's surface may dramatically change the strategy of the axion searches. The arguments were based on the so-called Axion Quark Nugget (AQN) dark matter model which was originally put forward to explain the similarity of the dark and visible cosmological matter densities $惟_{\rm dark}\sim 惟_{\rm visible}$. In this framework, the population of galactic axions with mass $ 10^{-6} {\rm eV}\lesssim m_a\lesssim 10^{-3}{\rm eV}$ and velocity $\langle v_a\rangle\sim 10^{-3} c$ will be accompanied by axions with typical velocities $\langle v_a\rangle\sim 0.6 c$ emitted by AQNs. Furthermore, in this framework, it has also been argued that the AQN-induced axion daily modulation (in contrast with the conventional WIMP paradigm) could be as large as $(10-20)\%$, which represents the main motivation for the present investigation. We argue that the daily modulations along with the broadband detection strategy can be very useful tools for the discovery of such relativistic axions. The data from the CAST-CAPP detector have been used following such arguments. Unfortunately, due to the dependence of the amplifier chain on temperature-dependent gain drifts and other factors, we could not conclusively show the presence or absence of a dark sector-originated daily modulation. However, this proof of principle analysis procedure can serve as a reference for future studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.10972v1-abstract-full').style.display = 'none'; document.getElementById('2405.10972v1-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> 9 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 8 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/2404.09727">arXiv:2404.09727</a> <span> [<a href="https://arxiv.org/pdf/2404.09727">pdf</a>, <a href="https://arxiv.org/format/2404.09727">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"> Using Micromegas detectors for direct dark matter searches: challenges and perspectives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Altenmueller%2C+K">K. Altenmueller</a>, <a href="/search/physics?searchtype=author&query=Antolin%2C+.">. Antolin</a>, <a href="/search/physics?searchtype=author&query=Calvet%2C+D">D. Calvet</a>, <a href="/search/physics?searchtype=author&query=Candon%2C+F+R">F. R. Candon</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J">J. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/physics?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=Ibanez%2C+D+D">D. Diez Ibanez</a>, <a href="/search/physics?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a>, <a href="/search/physics?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/physics?searchtype=author&query=Garcia%2C+J+A">J. A. Garcia</a>, <a href="/search/physics?searchtype=author&query=Gomez%2C+H">H. Gomez</a>, <a href="/search/physics?searchtype=author&query=Gu%2C+Y">Y. Gu</a>, <a href="/search/physics?searchtype=author&query=Ezquerro%2C+A">A. Ezquerro</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">I. G Irastorza</a>, <a href="/search/physics?searchtype=author&query=Luzon%2C+G">G. Luzon</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/physics?searchtype=author&query=de+Solorzano%2C+A+O">A. Ortiz de Solorzano</a>, <a href="/search/physics?searchtype=author&query=Papaevangelou%2C+T">T. Papaevangelou</a>, <a href="/search/physics?searchtype=author&query=Perez%2C+O">O. Perez</a>, <a href="/search/physics?searchtype=author&query=Picatoste%2C+E">E. Picatoste</a>, <a href="/search/physics?searchtype=author&query=Porron%2C+J">J. Porron</a> , et al. (5 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="2404.09727v1-abstract-short" style="display: inline;"> Gas time projection chambers (TPCs) with Micromegas pixelated readouts are being used in dark matter searches and other rare event searches, due to their potential in terms of low background levels, energy and spatial resolution, gain, and operational stability. Moreover, these detectors can provide precious features,such as topological information, allowing for event directionality and powerful s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09727v1-abstract-full').style.display = 'inline'; document.getElementById('2404.09727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.09727v1-abstract-full" style="display: none;"> Gas time projection chambers (TPCs) with Micromegas pixelated readouts are being used in dark matter searches and other rare event searches, due to their potential in terms of low background levels, energy and spatial resolution, gain, and operational stability. Moreover, these detectors can provide precious features,such as topological information, allowing for event directionality and powerful signal-background discrimination. The Micromegas technology of the microbulk type is particularly suited to low-background applications and is being exploited by detectors for CAST and IAXO (solar axions) and TREX-DM (low-mass WIMPs) experiments. Challenges for the future include reducing intrinsic background levels, reaching lower energy detection levels, and technical issues such as robustness of detector, new design choices, novel gas mixtures and operation points, scaling up to larger detector sizes, handling large readout granularity, etc. We report on the status and prospects of the development ongoing in the context of IAXO and TREX-DM experiments, pointing to promising perspectives for the use of Micromegas detectors in directdark matter searches <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09727v1-abstract-full').style.display = 'none'; document.getElementById('2404.09727v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.06316">arXiv:2403.06316</a> <span> [<a href="https://arxiv.org/pdf/2403.06316">pdf</a>, <a href="https://arxiv.org/format/2403.06316">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"> Background discrimination with a Micromegas detector prototype and veto system for BabyIAXO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Iba%C3%B1ez%2C+D">D. D铆ez-Iba帽ez</a>, <a href="/search/physics?searchtype=author&query=Ezquerro%2C+A">A. Ezquerro</a>, <a href="/search/physics?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a>, <a href="/search/physics?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/physics?searchtype=author&query=Galindo%2C+J">J. Galindo</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Giganon%2C+A">A. Giganon</a>, <a href="/search/physics?searchtype=author&query=Goblin%2C+C">C. Goblin</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/physics?searchtype=author&query=Loiseau%2C+C">C. Loiseau</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">G. Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Navick%2C+X+F">X. F. Navick</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A. Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=Papaevangelou%2C+T">T. Papaevangelou</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">O. P茅rez</a>, <a href="/search/physics?searchtype=author&query=Quintana%2C+A">A. Quintana</a>, <a href="/search/physics?searchtype=author&query=Ruz%2C+J">J. Ruz</a>, <a href="/search/physics?searchtype=author&query=Vogel%2C+J+K">J. K. Vogel</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="2403.06316v1-abstract-short" style="display: inline;"> In this paper we present measurements performed with a Micromegas X-ray detector setup. The detector is a prototype in the context of the BabyIAXO helioscope, which is under construction to search for an emission of the hypothetical axion particle from the sun. An important component of such a helioscope is a low background X-ray detector with a high efficiency in the 1-10 keV energy range. The go… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.06316v1-abstract-full').style.display = 'inline'; document.getElementById('2403.06316v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.06316v1-abstract-full" style="display: none;"> In this paper we present measurements performed with a Micromegas X-ray detector setup. The detector is a prototype in the context of the BabyIAXO helioscope, which is under construction to search for an emission of the hypothetical axion particle from the sun. An important component of such a helioscope is a low background X-ray detector with a high efficiency in the 1-10 keV energy range. The goal of the measurement was to study techniques for background discrimination. In addition to common techniques we used a multi-layer veto system designed to tag cosmogenic neutron background. Over an effective time of 52 days, a background level of $8.6 \times 10^{-7}\,\text{counts keV}^{-1}\,\text{cm}^{-2} \, \text{s}^{-1}$ was reached in a laboratory at above ground level. This is the lowest background level achieved at surface level. In this paper we present the experimental setup, show simulations of the neutron-induced background, and demonstrate the process to identify background signals in the data. Finally, prospects to reach lower background levels down to $10^{-7} \, \text{counts keV}^{-1} \, \text{cm}^{-2} \, \text{s}^{-1}$ will be discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.06316v1-abstract-full').style.display = 'none'; document.getElementById('2403.06316v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.12622">arXiv:2312.12622</a> <span> [<a href="https://arxiv.org/pdf/2312.12622">pdf</a>, <a href="https://arxiv.org/format/2312.12622">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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Searching for WIMPs with TREX-DM: achievements and challenges </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">Juan F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">Susana Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">Theopisti Dafni</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Ib%C3%A1%C3%B1ez%2C+D">David D铆ez-Ib谩帽ez</a>, <a href="/search/physics?searchtype=author&query=Ezquerro%2C+%C3%81">脕lvaro Ezquerro</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">Javier Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">Juan Antonio Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">Igor G. Irastorza</a>, <a href="/search/physics?searchtype=author&query=Jim%C3%A9nez%2C+M">Mar铆a Jim茅nez</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">Gloria Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">Cristina Margalejo</a>, <a href="/search/physics?searchtype=author&query=de+Mira%2C+%C3%81">脕ngel de Mira</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">Hector Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">Luis Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">Alfonso Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">Oscar P茅rez</a>, <a href="/search/physics?searchtype=author&query=Ruz%2C+J">Jaime Ruz</a>, <a href="/search/physics?searchtype=author&query=Vogel%2C+J">Julia Vogel</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="2312.12622v1-abstract-short" style="display: inline;"> The TREX-DM detector, a low background chamber with microbulk Micromegas readout, was commissioned in the underground laboratory of Canfranc (LSC) in 2018. Since then, data taking campaigns have been carried out with Argon and Neon mixtures, at different pressures from 1 to 4 bar. By achieving a low energy threshold of 1 keV$_{ee}$ and a background level of 80 counts keV$^{-1}$ Kg$^{-1}$ day… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12622v1-abstract-full').style.display = 'inline'; document.getElementById('2312.12622v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.12622v1-abstract-full" style="display: none;"> The TREX-DM detector, a low background chamber with microbulk Micromegas readout, was commissioned in the underground laboratory of Canfranc (LSC) in 2018. Since then, data taking campaigns have been carried out with Argon and Neon mixtures, at different pressures from 1 to 4 bar. By achieving a low energy threshold of 1 keV$_{ee}$ and a background level of 80 counts keV$^{-1}$ Kg$^{-1}$ day$^{-1}$ in the region from 1 to 7 keV$_{ee}$, the experiment demonstrates its potential to search for low-mass WIMPs. Two of the most important challenges currently faced are the reduction of both, background level and energy threshold. With respect to the energy threshold, recently a new readout plane is being developed, based on the combination of Micromegas and GEM technologies, aiming to have a pre-amplification stage that would permit very low energy thresholds, close to the single-electron ionization energy. With respect to the background reduction, apart from studies to identify and minimize contamination population, a high sensitivity alpha detector is being developed in order to allow a proper material selection for the TREX-DM detector components. Both challenges, together with the optimization of the gas mixture used as target for the WIMP detection, will take TREX-DM to explore regions of WIMP's mass below 1 GeV c$^{-2}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12622v1-abstract-full').style.display = 'none'; document.getElementById('2312.12622v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">LIDINE 2023: LIght Detection In Noble Elements</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15028">arXiv:2303.15028</a> <span> [<a href="https://arxiv.org/pdf/2303.15028">pdf</a>, <a href="https://arxiv.org/format/2303.15028">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Ultra low background Micromegas detectors for BabyIAXO solar axion search </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Biasuzzi%2C+B">B. Biasuzzi</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Iba%C3%B1ez%2C+D">D. D铆ez-Iba帽ez</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Galindo%2C+J">J. Galindo</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Giganon%2C+A">A. Giganon</a>, <a href="/search/physics?searchtype=author&query=Goblin%2C+C">C. Goblin</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/physics?searchtype=author&query=Kaminski%2C+J">J. Kaminski</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">G. Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/physics?searchtype=author&query=Navick%2C+X+F">X. F. Navick</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A. Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=von+Oy%2C+J">J. von Oy</a>, <a href="/search/physics?searchtype=author&query=Papaevangelou%2C+T">T. Papaevangelou</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">O. P茅rez</a>, <a href="/search/physics?searchtype=author&query=Picatoste%2C+E">E. Picatoste</a> , et al. (5 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="2303.15028v2-abstract-short" style="display: inline;"> The International AXion Observatory (IAXO) is a large scale axion helioscope that will look for axions and axion-like particles produced in the Sun with unprecedented sensitivity. BabyIAXO is an intermediate experimental stage that will be hosted at DESY (Germany) and that will test all IAXO subsystems serving as a prototype for IAXO but at the same time as a fully-fledged helioscope with potentia… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15028v2-abstract-full').style.display = 'inline'; document.getElementById('2303.15028v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15028v2-abstract-full" style="display: none;"> The International AXion Observatory (IAXO) is a large scale axion helioscope that will look for axions and axion-like particles produced in the Sun with unprecedented sensitivity. BabyIAXO is an intermediate experimental stage that will be hosted at DESY (Germany) and that will test all IAXO subsystems serving as a prototype for IAXO but at the same time as a fully-fledged helioscope with potential for discovery. One of the crucial components of the project is the ultra-low background X-ray detectors that will image the X-ray photons produced by axion conversion in the experiment. The baseline detection technology for this purpose are Micromegas (Microbulk) detectors. We will show the quest and the strategy to attain the very challenging levels of background targeted for BabyIAXO that need a multi-approach strategy coming from ground measurements, screening campaigns of components of the detector, underground measurements, background models, in-situ background measurements as well as powerful rejection algorithms. First results from the commissioning of the BabyIAXO prototype will be shown. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15028v2-abstract-full').style.display = 'none'; document.getElementById('2303.15028v2-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 2 figures, submitted for the proceedings of the International Conference on Micro Pattern Gaseous Detectors, December 2022, Israel</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.10148">arXiv:2211.10148</a> <span> [<a href="https://arxiv.org/pdf/2211.10148">pdf</a>, <a href="https://arxiv.org/format/2211.10148">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1109/NSS/MIC44867.2021.9875870">10.1109/NSS/MIC44867.2021.9875870 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Purification Efficiency and Radon Emanation of Gas Purifiers used with Pure and Binary Gas Mixtures for Gaseous Dark Matter Detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=K."> K.</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller"> Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafn%C3%AD%2C+T">T. Dafn铆</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Ib%C3%A1%C3%B1ez%2C+D">D. D铆ez-Ib谩帽ez</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Galindo%2C+J">J. Galindo</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/physics?searchtype=author&query=Katsioulas%2C+I">I. Katsioulas</a>, <a href="/search/physics?searchtype=author&query=Knights%2C+P">P. Knights</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">G. Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Manthos%2C+I">I. Manthos</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/physics?searchtype=author&query=Matthews%2C+J">J. Matthews</a>, <a href="/search/physics?searchtype=author&query=Mavrokoridis%2C+K">K. Mavrokoridis</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/physics?searchtype=author&query=Neep%2C+T">T. Neep</a>, <a href="/search/physics?searchtype=author&query=Nikolopoulos%2C+K">K. Nikolopoulos</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A. Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">O. P茅rez</a>, <a href="/search/physics?searchtype=author&query=Philippou%2C+B">B. Philippou</a>, <a href="/search/physics?searchtype=author&query=Ward%2C+R">R. Ward</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="2211.10148v1-abstract-short" style="display: inline;"> Rare event searches require extreme radiopurity in all detector components. This includes the active medium, which in the case of gaseous detectors, is the operating gas. The gases used typically include noble gas mixtures with molecular quenchers. Purification of these gases is required to achieve the desired detector performance, however, purifiers are known to emanate 222 Rn, which is a potenti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.10148v1-abstract-full').style.display = 'inline'; document.getElementById('2211.10148v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.10148v1-abstract-full" style="display: none;"> Rare event searches require extreme radiopurity in all detector components. This includes the active medium, which in the case of gaseous detectors, is the operating gas. The gases used typically include noble gas mixtures with molecular quenchers. Purification of these gases is required to achieve the desired detector performance, however, purifiers are known to emanate 222 Rn, which is a potential source of background. Several purifiers are studied for their O 2 and H 2 O purification efficiency and Rn emanation rates, aiming to identify the lowest-Rn options. Furthermore, the absorption of quenchers by the purifiers is assessed when used in a recirculating closed-loop gas system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.10148v1-abstract-full').style.display = 'none'; document.getElementById('2211.10148v1-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">3 pages, 4 figures. Contribution to 2021 IEEE Nuclear Science Symposium and Medical Imaging Conference (NSS/MIC)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2021 IEEE Nuclear Science Symposium and Medical Imaging Conference (NSS/MIC), 2021, pp. 1-3 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.02902">arXiv:2211.02902</a> <span> [<a href="https://arxiv.org/pdf/2211.02902">pdf</a>, <a href="https://arxiv.org/format/2211.02902">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41467-022-33913-6">10.1038/s41467-022-33913-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Dark Matter Axions with CAST-CAPP </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adair%2C+C+M">C. M. Adair</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Anastassopoulos%2C+V">V. Anastassopoulos</a>, <a href="/search/physics?searchtype=author&query=Cuendis%2C+S+A">S. Arguedas Cuendis</a>, <a href="/search/physics?searchtype=author&query=Baier%2C+J">J. Baier</a>, <a href="/search/physics?searchtype=author&query=Barth%2C+K">K. Barth</a>, <a href="/search/physics?searchtype=author&query=Belov%2C+A">A. Belov</a>, <a href="/search/physics?searchtype=author&query=Bozicevic%2C+D">D. Bozicevic</a>, <a href="/search/physics?searchtype=author&query=Br%C3%A4uninger%2C+H">H. Br盲uninger</a>, <a href="/search/physics?searchtype=author&query=Cantatore%2C+G">G. Cantatore</a>, <a href="/search/physics?searchtype=author&query=Caspers%2C+F">F. Caspers</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=%C3%87etin%2C+S+A">S. A. 脟etin</a>, <a href="/search/physics?searchtype=author&query=Chung%2C+W">W. Chung</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+H">H. Choi</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+J">J. Choi</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=Davenport%2C+M">M. Davenport</a>, <a href="/search/physics?searchtype=author&query=Dermenev%2C+A">A. Dermenev</a>, <a href="/search/physics?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/physics?searchtype=author&query=D%C3%B6brich%2C+B">B. D枚brich</a>, <a href="/search/physics?searchtype=author&query=Fischer%2C+H">H. Fischer</a>, <a href="/search/physics?searchtype=author&query=Funk%2C+W">W. Funk</a>, <a href="/search/physics?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/physics?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a> , et al. (39 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="2211.02902v1-abstract-short" style="display: inline;"> The CAST-CAPP axion haloscope, operating at CERN inside the CAST dipole magnet, has searched for axions in the 19.74 $渭$eV to 22.47 $渭$eV mass range. The detection concept follows the Sikivie haloscope principle, where Dark Matter axions convert into photons within a resonator immersed in a magnetic field. The CAST-CAPP resonator is an array of four individual rectangular cavities inserted in a st… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.02902v1-abstract-full').style.display = 'inline'; document.getElementById('2211.02902v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.02902v1-abstract-full" style="display: none;"> The CAST-CAPP axion haloscope, operating at CERN inside the CAST dipole magnet, has searched for axions in the 19.74 $渭$eV to 22.47 $渭$eV mass range. The detection concept follows the Sikivie haloscope principle, where Dark Matter axions convert into photons within a resonator immersed in a magnetic field. The CAST-CAPP resonator is an array of four individual rectangular cavities inserted in a strong dipole magnet, phase-matched to maximize the detection sensitivity. Here we report on the data acquired for 4124 h from 2019 to 2021. Each cavity is equipped with a fast frequency tuning mechanism of 10 MHz/min between 4.774 GHz and 5.434 GHz. In the present work, we exclude axion-photon couplings for virialized galactic axions down to $g_{a纬纬} = 8 \times {10^{-14}}$ $GeV^{-1}$ at the 90% confidence level. The here implemented phase-matching technique also allows for future large-scale upgrades. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.02902v1-abstract-full').style.display = 'none'; document.getElementById('2211.02902v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">24 pages, 5 figures, Published version available with Open Access at https://www.nature.com/articles/s41467-022-33913-6</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Commun. 13, 6180 (2022) </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/physics?searchtype=author&query=O%27Hare%2C+C+A+J">C. A. J. O'Hare</a>, <a href="/search/physics?searchtype=author&query=Loomba%2C+D">D. Loomba</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=%C3%81lvarez-Pol%2C+H">H. 脕lvarez-Pol</a>, <a href="/search/physics?searchtype=author&query=Amaro%2C+F+D">F. D. Amaro</a>, <a href="/search/physics?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/physics?searchtype=author&query=Sierra%2C+D+A">D. Aristizabal Sierra</a>, <a href="/search/physics?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/physics?searchtype=author&query=Atti%C3%A9%2C+D">D. Atti茅</a>, <a href="/search/physics?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/physics?searchtype=author&query=Awe%2C+C">C. Awe</a>, <a href="/search/physics?searchtype=author&query=Ayyad%2C+Y">Y. Ayyad</a>, <a href="/search/physics?searchtype=author&query=Baracchini%2C+E">E. Baracchini</a>, <a href="/search/physics?searchtype=author&query=Barbeau%2C+P">P. Barbeau</a>, <a href="/search/physics?searchtype=author&query=Battat%2C+J+B+R">J. B. R. Battat</a>, <a href="/search/physics?searchtype=author&query=Bell%2C+N+F">N. F. Bell</a>, <a href="/search/physics?searchtype=author&query=Biasuzzi%2C+B">B. Biasuzzi</a>, <a href="/search/physics?searchtype=author&query=Bignell%2C+L+J">L. J. Bignell</a>, <a href="/search/physics?searchtype=author&query=Boehm%2C+C">C. Boehm</a>, <a href="/search/physics?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/physics?searchtype=author&query=Brunbauer%2C+F+M">F. M. Brunbauer</a>, <a href="/search/physics?searchtype=author&query=Caama%C3%B1o%2C+M">M. Caama帽o</a>, <a href="/search/physics?searchtype=author&query=Cabo%2C+C">C. Cabo</a>, <a href="/search/physics?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/physics?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/2201.01859">arXiv:2201.01859</a> <span> [<a href="https://arxiv.org/pdf/2201.01859">pdf</a>, <a href="https://arxiv.org/format/2201.01859">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/10.1088/1748-0221/17/08/P08035">10.1088/1748-0221/17/08/P08035 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> AlphaCAMM, a Micromegas-based camera for high-sensitivity screening of alpha surface contamination </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">Konrad Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">Juan F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">Susana Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">Theopisti Dafni</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Ib%C3%A1%C3%B1ez%2C+D">David D铆ez-Ib谩帽ez</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">Javier Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Galindo%2C+J">Javier Galindo</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">Juan Antonio Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">Igor G. Irastorza</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">Gloria Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">Cristina Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">Hector Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">Luis Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">Alfonso Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">Oscar P茅rez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.01859v4-abstract-short" style="display: inline;"> Surface contamination of $^{222}$Rn progeny from the $^{238}$U natural decay chain is one of the most difficult background contributions to measure in rare event searches experiments. In this work we propose AlphaCAMM, a gaseous chamber read with a segmented Micromegas, for the direct measurement of $^{210}$Pb surface contamination of flat samples. The detection concept exploits the readout capabi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01859v4-abstract-full').style.display = 'inline'; document.getElementById('2201.01859v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.01859v4-abstract-full" style="display: none;"> Surface contamination of $^{222}$Rn progeny from the $^{238}$U natural decay chain is one of the most difficult background contributions to measure in rare event searches experiments. In this work we propose AlphaCAMM, a gaseous chamber read with a segmented Micromegas, for the direct measurement of $^{210}$Pb surface contamination of flat samples. The detection concept exploits the readout capabilities of the Micromegas detectors for the reconstruction of $^{210}$Po alpha tracks to increase the signal-to-background ratio. We report here on the design and realization of a first 26$\times$26 cm$^2$ non-radiopure prototype, with which the detection concept is demonstrated by the use of a new algorithm for the reconstruction of alpha tracks. AlphaCAMM aims for minimum detectable $^{210}$Pb activities of $100$ nBq cm$^{-2}$ and sensitivity upper limits about $60$ nBq cm$^{-2}$ at 95\% of C.L., which requires an intrinsic background level of $5\times10^{-8}$ alphas cm$^{-2}$ s$^{-1}$. We discuss here the prospects to reach these sensitivity goals with a radiopure AlphaCAMM prototype currently under construction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01859v4-abstract-full').style.display = 'none'; document.getElementById('2201.01859v4-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Prepared for submission to JINST</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.05863">arXiv:2109.05863</a> <span> [<a href="https://arxiv.org/pdf/2109.05863">pdf</a>, <a href="https://arxiv.org/format/2109.05863">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</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.cpc.2021.108281">10.1016/j.cpc.2021.108281 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> REST-for-Physics, a ROOT-based framework for event oriented data analysis and combined Monte Carlo response </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">Konrad Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">Susana Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">Theopisti Dafni</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Ib%C3%A1%C3%B1ez%2C+D">David D铆ez-Ib谩帽ez</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">Javier Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Galindo%2C+J">Javier Galindo</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">Juan Antonio Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">Igor G. Irastorza</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">Gloria Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">Cristina Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">Hector Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">Luis Obis</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">Oscar P茅rez</a>, <a href="/search/physics?searchtype=author&query=Han%2C+K">Ke Han</a>, <a href="/search/physics?searchtype=author&query=Ni%2C+K">Kaixiang Ni</a>, <a href="/search/physics?searchtype=author&query=Bedfer%2C+Y">Yann Bedfer</a>, <a href="/search/physics?searchtype=author&query=Biasuzzi%2C+B">Barbara Biasuzzi</a>, <a href="/search/physics?searchtype=author&query=Ferrer-Ribas%2C+E">Esther Ferrer-Ribas</a>, <a href="/search/physics?searchtype=author&query=Neyret%2C+D">Damien Neyret</a>, <a href="/search/physics?searchtype=author&query=Papaevangelou%2C+T">Thomas Papaevangelou</a>, <a href="/search/physics?searchtype=author&query=Cogollos%2C+C">Cristian Cogollos</a>, <a href="/search/physics?searchtype=author&query=Picatoste%2C+E">Eduardo Picatoste</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="2109.05863v2-abstract-short" style="display: inline;"> The REST-for-Physics (Rare Event Searches Toolkit for Physics) framework is a ROOT-based solution providing the means to process and analyze experimental or Monte Carlo event data. Special care has been taken on the traceability of the code and the validation of the results produced within the framework, together with the connectivity between code and data stored registered through specific versio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.05863v2-abstract-full').style.display = 'inline'; document.getElementById('2109.05863v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.05863v2-abstract-full" style="display: none;"> The REST-for-Physics (Rare Event Searches Toolkit for Physics) framework is a ROOT-based solution providing the means to process and analyze experimental or Monte Carlo event data. Special care has been taken on the traceability of the code and the validation of the results produced within the framework, together with the connectivity between code and data stored registered through specific version metadata members. The framework development was originally motivated to cover the needs at Rare Event Searches experiments (experiments looking for phenomena having extremely low occurrence probability like dark matter or neutrino interactions or rare nuclear decays), and its components naturally implement tools to address the challenges in these kinds of experiments; the integration of a detector physics response, the implementation of signal processing routines, or topological algorithms for physical event identification are some examples. Despite this specialization, the framework was conceived thinking in scalability, and other event-oriented applications could benefit from the data processing routines and/or metadata description implemented in REST, being the generic framework tools completely decoupled from dedicated libraries. REST-for-Physics is a consolidated piece of software already serving the needs of different physics experiments - using gaseous Time Projection Chambers (TPCs) as detection technology - for background data analysis and detector characterization, as well as generic detector R\&D. Even though REST has been exploited mainly with gaseous TPCs, the code could be easily applied or adapted to other detection technologies. We present in this work an overview of REST-for-Physics, providing a broad perspective to the infrastructure and organization of the project as a whole. The framework and its different components will be described in the text. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.05863v2-abstract-full').style.display = 'none'; document.getElementById('2109.05863v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">27 pages, 14 figures, prepared for submission to Computer Physics Communications</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.12076">arXiv:2010.12076</a> <span> [<a href="https://arxiv.org/pdf/2010.12076">pdf</a>, <a href="https://arxiv.org/format/2010.12076">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Conceptual Design of BabyIAXO, the intermediate stage towards the International Axion Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abeln%2C+A">A. Abeln</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Cuendis%2C+S+A">S. Arguedas Cuendis</a>, <a href="/search/physics?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/physics?searchtype=author&query=Atti%C3%A9%2C+D">D. Atti茅</a>, <a href="/search/physics?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/physics?searchtype=author&query=Basso%2C+S">S. Basso</a>, <a href="/search/physics?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/physics?searchtype=author&query=Biasuzzi%2C+B">B. Biasuzzi</a>, <a href="/search/physics?searchtype=author&query=De+Sousa%2C+P+T+C+B">P. T. C. Borges De Sousa</a>, <a href="/search/physics?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/physics?searchtype=author&query=Bykovskiy%2C+N">N. Bykovskiy</a>, <a href="/search/physics?searchtype=author&query=Calvet%2C+D">D. Calvet</a>, <a href="/search/physics?searchtype=author&query=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Chernov%2C+V">V. Chernov</a>, <a href="/search/physics?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/physics?searchtype=author&query=Civitani%2C+M+M">M. M. Civitani</a>, <a href="/search/physics?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/physics?searchtype=author&query=Dafn%C3%AD%2C+T">T. Dafn铆</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez%2C+D">D. D铆ez</a>, <a href="/search/physics?searchtype=author&query=Dinter%2C+M">M. Dinter</a> , et al. (101 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="2010.12076v3-abstract-short" style="display: inline;"> This article describes BabyIAXO, an intermediate experimental stage of the International Axion Observatory (IAXO), proposed to be sited at DESY. IAXO is a large-scale axion helioscope that will look for axions and axion-like particles (ALPs), produced in the Sun, with unprecedented sensitivity. BabyIAXO is conceived to test all IAXO subsystems (magnet, optics and detectors) at a relevant scale for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.12076v3-abstract-full').style.display = 'inline'; document.getElementById('2010.12076v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.12076v3-abstract-full" style="display: none;"> This article describes BabyIAXO, an intermediate experimental stage of the International Axion Observatory (IAXO), proposed to be sited at DESY. IAXO is a large-scale axion helioscope that will look for axions and axion-like particles (ALPs), produced in the Sun, with unprecedented sensitivity. BabyIAXO is conceived to test all IAXO subsystems (magnet, optics and detectors) at a relevant scale for the final system and thus serve as prototype for IAXO, but at the same time as a fully-fledged helioscope with relevant physics reach itself, and with potential for discovery. The BabyIAXO magnet will feature two 10 m long, 70 cm diameter bores, and will host two detection lines (optics and detector) of dimensions similar to the final ones foreseen for IAXO. BabyIAXO will detect or reject solar axions or ALPs with axion-photon couplings down to $g_{a纬} \sim 1.5 \times 10^{-11}$ GeV$^{-1}$, and masses up to $m_a\sim 0.25$ eV. BabyIAXO will offer additional opportunities for axion research in view of IAXO, like the development of precision x-ray detectors to identify particular spectral features in the solar axion spectrum, and the implementation of radiofrequency-cavity-based axion dark matter setups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.12076v3-abstract-full').style.display = 'none'; document.getElementById('2010.12076v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">77 pages, 49 figures. Prepared for submission to JHEP. Third version after referees comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.13957">arXiv:1910.13957</a> <span> [<a href="https://arxiv.org/pdf/1910.13957">pdf</a>, <a href="https://arxiv.org/format/1910.13957">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/1468/1/012063">10.1088/1742-6596/1468/1/012063 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TREX-DM experiment at the Canfranc Underground Laboratory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Castel%2C+J">J Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">S Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T Dafni</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">J Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I">IG Irastorza</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">G Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H Mirallas</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=Peir%C3%B3%2C+A">A Peir贸</a>, <a href="/search/physics?searchtype=author&query=Ruiz-Ch%C3%B3liz%2C+E">E Ruiz-Ch贸liz</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="1910.13957v2-abstract-short" style="display: inline;"> TREX-DM (TPC Rare Event eXperiment for Dark Matter) is intended to look for low mass WIMPs in the Canfranc Underground Laboratory (LSC) in Spain, using light elements (Ne, Ar) as target in a high pressure TPC equipped with Micromegas readouts. Here, a description of the detector, the first results from commissioning data and the expected sensitivity from the developed background model are briefly… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.13957v2-abstract-full').style.display = 'inline'; document.getElementById('1910.13957v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.13957v2-abstract-full" style="display: none;"> TREX-DM (TPC Rare Event eXperiment for Dark Matter) is intended to look for low mass WIMPs in the Canfranc Underground Laboratory (LSC) in Spain, using light elements (Ne, Ar) as target in a high pressure TPC equipped with Micromegas readouts. Here, a description of the detector, the first results from commissioning data and the expected sensitivity from the developed background model are briefly presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.13957v2-abstract-full').style.display = 'none'; document.getElementById('1910.13957v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">TAUP2019 proceedings</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J Castel et al 2020 J. Phys.: Conf. 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