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is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/hep-ex?searchtype=author&query=Ahyoune%2C+S">S. Ahyoune</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmueller%2C+K">K. Altenmueller</a>, <a href="/search/hep-ex?searchtype=author&query=Antolin%2C+I">I. Antolin</a>, <a href="/search/hep-ex?searchtype=author&query=Basso%2C+S">S. Basso</a>, <a href="/search/hep-ex?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/hep-ex?searchtype=author&query=Candon%2C+F+R">F. R. Candon</a>, <a href="/search/hep-ex?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/hep-ex?searchtype=author&query=Chouhan%2C+D">D. Chouhan</a>, <a href="/search/hep-ex?searchtype=author&query=Della+Ceca%2C+R">R. Della Ceca</a>, <a href="/search/hep-ex?searchtype=author&query=Cervera-Cortes%2C+M">M. Cervera-Cortes</a>, <a href="/search/hep-ex?searchtype=author&query=Chernov%2C+V">V. Chernov</a>, <a href="/search/hep-ex?searchtype=author&query=Civitani%2C+M+M">M. M. Civitani</a>, <a href="/search/hep-ex?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/hep-ex?searchtype=author&query=Costa%2C+E">E. Costa</a>, <a href="/search/hep-ex?searchtype=author&query=Cotroneo%2C+V">V. Cotroneo</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?searchtype=author&query=Diaz-Martin%2C+M+C">M. C. Diaz-Martin</a>, <a href="/search/hep-ex?searchtype=author&query=Diaz-Morcillo%2C+A">A. Diaz-Morcillo</a>, <a href="/search/hep-ex?searchtype=author&query=Diez-Ibanez%2C+D">D. Diez-Ibanez</a>, <a href="/search/hep-ex?searchtype=author&query=Pardos%2C+C+D">C. Diez Pardos</a>, <a href="/search/hep-ex?searchtype=author&query=Dinter%2C+M">M. Dinter</a>, <a href="/search/hep-ex?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/2406.16840">arXiv:2406.16840</a> <span> [<a href="https://arxiv.org/pdf/2406.16840">pdf</a>, <a href="https://arxiv.org/format/2406.16840">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> </div> </div> <p class="title is-5 mathjax"> A new upper limit on the axion-photon coupling with an extended CAST run with a Xe-based Micromegas detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=CAST+Collaboration"> CAST Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Anastassopoulos%2C+V">V. Anastassopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Arguedas-Cuendis%2C+S">S. Arguedas-Cuendis</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ex?searchtype=author&query=Baier%2C+J">J. Baier</a>, <a href="/search/hep-ex?searchtype=author&query=Barth%2C+K">K. Barth</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A4uninger%2C+H">H. Br盲uninger</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</a>, <a href="/search/hep-ex?searchtype=author&query=Caspers%2C+F">F. Caspers</a>, <a href="/search/hep-ex?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%87etin%2C+S+A">S. A. 脟etin</a>, <a href="/search/hep-ex?searchtype=author&query=Christensen%2C+F">F. Christensen</a>, <a href="/search/hep-ex?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Davenport%2C+M">M. Davenport</a>, <a href="/search/hep-ex?searchtype=author&query=Decker%2C+T+A">T. A. Decker</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=D%C3%B6brich%2C+B">B. D枚brich</a>, <a href="/search/hep-ex?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a>, <a href="/search/hep-ex?searchtype=author&query=Fischer%2C+H">H. Fischer</a>, <a href="/search/hep-ex?searchtype=author&query=Funk%2C+W">W. Funk</a>, <a href="/search/hep-ex?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a> , et al. (40 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="2406.16840v1-abstract-short" style="display: inline;"> Hypothetical axions provide a compelling explanation for dark matter and could be emitted from the hot solar interior. The CERN Axion Solar Telescope (CAST) has been searching for solar axions via their back conversion to X-ray photons in a 9-T 10-m long magnet directed towards the Sun. We report on an extended run with the IAXO (International Axion Observatory) pathfinder detector, doubling the p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16840v1-abstract-full').style.display = 'inline'; document.getElementById('2406.16840v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.16840v1-abstract-full" style="display: none;"> Hypothetical axions provide a compelling explanation for dark matter and could be emitted from the hot solar interior. The CERN Axion Solar Telescope (CAST) has been searching for solar axions via their back conversion to X-ray photons in a 9-T 10-m long magnet directed towards the Sun. We report on an extended run with the IAXO (International Axion Observatory) pathfinder detector, doubling the previous exposure time. The detector was operated with a xenon-based gas mixture for part of the new run, providing technical insights for future detector configurations in IAXO. No counts are detected in the 95\% signal-encircling region during the new run, while one is expected. The new data improve the axion-photon coupling limit to 5.7$\times 10^{-11}\,$GeV$^{-1}$ at 95\% C.L., the most restrictive experimental limit to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16840v1-abstract-full').style.display = 'none'; document.getElementById('2406.16840v1-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> 24 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">8 pages, 4 figures (plus 6 pages, 10 figures of supplemental material) Corresponding authors: C. Margalejo (cmargalejo@unizar.es) and J. Ruz (Jaime.Ruz@cern.ch)</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/hep-ex?searchtype=author&query=Adair%2C+C+M">C. M. Adair</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Anastassopoulos%2C+V">V. Anastassopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Cuendis%2C+S+A">S. Arguedas Cuendis</a>, <a href="/search/hep-ex?searchtype=author&query=Baier%2C+J">J. Baier</a>, <a href="/search/hep-ex?searchtype=author&query=Barth%2C+K">K. Barth</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+A">A. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bozicevic%2C+D">D. Bozicevic</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A4uninger%2C+H">H. Br盲uninger</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</a>, <a href="/search/hep-ex?searchtype=author&query=Caspers%2C+F">F. Caspers</a>, <a href="/search/hep-ex?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%87etin%2C+S+A">S. A. 脟etin</a>, <a href="/search/hep-ex?searchtype=author&query=Chung%2C+W">W. Chung</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+H">H. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+J">J. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Davenport%2C+M">M. Davenport</a>, <a href="/search/hep-ex?searchtype=author&query=Dermenev%2C+A">A. Dermenev</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%B6brich%2C+B">B. D枚brich</a>, <a href="/search/hep-ex?searchtype=author&query=Fischer%2C+H">H. Fischer</a>, <a href="/search/hep-ex?searchtype=author&query=Funk%2C+W">W. Funk</a>, <a href="/search/hep-ex?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Biasuzzi%2C+B">B. Biasuzzi</a>, <a href="/search/hep-ex?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%ADez-Iba%C3%B1ez%2C+D">D. D铆ez-Iba帽ez</a>, <a href="/search/hep-ex?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Galindo%2C+J">J. Galindo</a>, <a href="/search/hep-ex?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/hep-ex?searchtype=author&query=Giganon%2C+A">A. Giganon</a>, <a href="/search/hep-ex?searchtype=author&query=Goblin%2C+C">C. Goblin</a>, <a href="/search/hep-ex?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/hep-ex?searchtype=author&query=Kaminski%2C+J">J. Kaminski</a>, <a href="/search/hep-ex?searchtype=author&query=Luz%C3%B3n%2C+G">G. Luz贸n</a>, <a href="/search/hep-ex?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/hep-ex?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/hep-ex?searchtype=author&query=Navick%2C+X+F">X. F. Navick</a>, <a href="/search/hep-ex?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/hep-ex?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A. Ortiz de Sol贸rzano</a>, <a href="/search/hep-ex?searchtype=author&query=von+Oy%2C+J">J. von Oy</a>, <a href="/search/hep-ex?searchtype=author&query=Papaevangelou%2C+T">T. Papaevangelou</a>, <a href="/search/hep-ex?searchtype=author&query=P%C3%A9rez%2C+O">O. P茅rez</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=K."> K.</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller"> Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Dafn%C3%AD%2C+T">T. Dafn铆</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Galindo%2C+J">J. Galindo</a>, <a href="/search/hep-ex?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/hep-ex?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/hep-ex?searchtype=author&query=Katsioulas%2C+I">I. Katsioulas</a>, <a href="/search/hep-ex?searchtype=author&query=Knights%2C+P">P. Knights</a>, <a href="/search/hep-ex?searchtype=author&query=Luz%C3%B3n%2C+G">G. Luz贸n</a>, <a href="/search/hep-ex?searchtype=author&query=Manthos%2C+I">I. Manthos</a>, <a href="/search/hep-ex?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/hep-ex?searchtype=author&query=Matthews%2C+J">J. Matthews</a>, <a href="/search/hep-ex?searchtype=author&query=Mavrokoridis%2C+K">K. Mavrokoridis</a>, <a href="/search/hep-ex?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/hep-ex?searchtype=author&query=Neep%2C+T">T. Neep</a>, <a href="/search/hep-ex?searchtype=author&query=Nikolopoulos%2C+K">K. Nikolopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/hep-ex?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A. Ortiz de Sol贸rzano</a>, <a href="/search/hep-ex?searchtype=author&query=P%C3%A9rez%2C+O">O. P茅rez</a>, <a href="/search/hep-ex?searchtype=author&query=Philippou%2C+B">B. Philippou</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Adair%2C+C+M">C. M. Adair</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Anastassopoulos%2C+V">V. Anastassopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Cuendis%2C+S+A">S. Arguedas Cuendis</a>, <a href="/search/hep-ex?searchtype=author&query=Baier%2C+J">J. Baier</a>, <a href="/search/hep-ex?searchtype=author&query=Barth%2C+K">K. Barth</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+A">A. Belov</a>, <a href="/search/hep-ex?searchtype=author&query=Bozicevic%2C+D">D. Bozicevic</a>, <a href="/search/hep-ex?searchtype=author&query=Br%C3%A4uninger%2C+H">H. Br盲uninger</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</a>, <a href="/search/hep-ex?searchtype=author&query=Caspers%2C+F">F. Caspers</a>, <a href="/search/hep-ex?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%87etin%2C+S+A">S. A. 脟etin</a>, <a href="/search/hep-ex?searchtype=author&query=Chung%2C+W">W. Chung</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+H">H. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+J">J. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Davenport%2C+M">M. Davenport</a>, <a href="/search/hep-ex?searchtype=author&query=Dermenev%2C+A">A. Dermenev</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%B6brich%2C+B">B. D枚brich</a>, <a href="/search/hep-ex?searchtype=author&query=Fischer%2C+H">H. Fischer</a>, <a href="/search/hep-ex?searchtype=author&query=Funk%2C+W">W. Funk</a>, <a href="/search/hep-ex?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=O%27Hare%2C+C+A+J">C. A. J. O'Hare</a>, <a href="/search/hep-ex?searchtype=author&query=Loomba%2C+D">D. Loomba</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%81lvarez-Pol%2C+H">H. 脕lvarez-Pol</a>, <a href="/search/hep-ex?searchtype=author&query=Amaro%2C+F+D">F. D. Amaro</a>, <a href="/search/hep-ex?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/hep-ex?searchtype=author&query=Sierra%2C+D+A">D. Aristizabal Sierra</a>, <a href="/search/hep-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/hep-ex?searchtype=author&query=Atti%C3%A9%2C+D">D. Atti茅</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ex?searchtype=author&query=Awe%2C+C">C. Awe</a>, <a href="/search/hep-ex?searchtype=author&query=Ayyad%2C+Y">Y. Ayyad</a>, <a href="/search/hep-ex?searchtype=author&query=Baracchini%2C+E">E. Baracchini</a>, <a href="/search/hep-ex?searchtype=author&query=Barbeau%2C+P">P. Barbeau</a>, <a href="/search/hep-ex?searchtype=author&query=Battat%2C+J+B+R">J. B. R. Battat</a>, <a href="/search/hep-ex?searchtype=author&query=Bell%2C+N+F">N. F. Bell</a>, <a href="/search/hep-ex?searchtype=author&query=Biasuzzi%2C+B">B. Biasuzzi</a>, <a href="/search/hep-ex?searchtype=author&query=Bignell%2C+L+J">L. J. Bignell</a>, <a href="/search/hep-ex?searchtype=author&query=Boehm%2C+C">C. Boehm</a>, <a href="/search/hep-ex?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/hep-ex?searchtype=author&query=Brunbauer%2C+F+M">F. M. Brunbauer</a>, <a href="/search/hep-ex?searchtype=author&query=Caama%C3%B1o%2C+M">M. Caama帽o</a>, <a href="/search/hep-ex?searchtype=author&query=Cabo%2C+C">C. Cabo</a>, <a href="/search/hep-ex?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Abeln%2C+A">A. Abeln</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Cuendis%2C+S+A">S. Arguedas Cuendis</a>, <a href="/search/hep-ex?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/hep-ex?searchtype=author&query=Atti%C3%A9%2C+D">D. Atti茅</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ex?searchtype=author&query=Basso%2C+S">S. Basso</a>, <a href="/search/hep-ex?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/hep-ex?searchtype=author&query=Biasuzzi%2C+B">B. Biasuzzi</a>, <a href="/search/hep-ex?searchtype=author&query=De+Sousa%2C+P+T+C+B">P. T. C. Borges De Sousa</a>, <a href="/search/hep-ex?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/hep-ex?searchtype=author&query=Bykovskiy%2C+N">N. Bykovskiy</a>, <a href="/search/hep-ex?searchtype=author&query=Calvet%2C+D">D. Calvet</a>, <a href="/search/hep-ex?searchtype=author&query=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/hep-ex?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Chernov%2C+V">V. Chernov</a>, <a href="/search/hep-ex?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/hep-ex?searchtype=author&query=Civitani%2C+M+M">M. M. Civitani</a>, <a href="/search/hep-ex?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/hep-ex?searchtype=author&query=Dafn%C3%AD%2C+T">T. Dafn铆</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%ADez%2C+D">D. D铆ez</a>, <a href="/search/hep-ex?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> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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