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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/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> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.01084">arXiv:1906.01084</a> <span> [<a href="https://arxiv.org/pdf/1906.01084">pdf</a>, <a href="https://arxiv.org/format/1906.01084">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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"> First Results on the Search for Chameleons with the KWISP Detector at CAST </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Baum%2C+S">S. Baum</a>, <a href="/search/hep-ex?searchtype=author&query=Bayirli%2C+A">A. Bayirli</a>, <a href="/search/hep-ex?searchtype=author&query=Belov%2C+A">A. Belov</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=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=Cetin%2C+S+A">S. A. Cetin</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=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/hep-ex?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a>, <a href="/search/hep-ex?searchtype=author&query=Garza%2C+J+G">J. G. Garza</a>, <a href="/search/hep-ex?searchtype=author&query=Gninenko%2C+S">S. Gninenko</a>, <a href="/search/hep-ex?searchtype=author&query=Hasinoff%2C+M+D">M. D. Hasinoff</a>, <a href="/search/hep-ex?searchtype=author&query=Hoffmann%2C+D+H+H">D. H. H. Hoffmann</a>, <a href="/search/hep-ex?searchtype=author&query=Iguaz%2C+F+J">F. J. Iguaz</a> , et al. (28 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="1906.01084v1-abstract-short" style="display: inline;"> We report on a first measurement with a sensitive opto-mechanical force sensor designed for the direct detection of coupling of real chameleons to matter. These dark energy candidates could be produced in the Sun and stream unimpeded to Earth. The KWISP detector installed on the CAST axion search experiment at CERN looks for tiny displacements of a thin membrane caused by the mechanical effect of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.01084v1-abstract-full').style.display = 'inline'; document.getElementById('1906.01084v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.01084v1-abstract-full" style="display: none;"> We report on a first measurement with a sensitive opto-mechanical force sensor designed for the direct detection of coupling of real chameleons to matter. These dark energy candidates could be produced in the Sun and stream unimpeded to Earth. The KWISP detector installed on the CAST axion search experiment at CERN looks for tiny displacements of a thin membrane caused by the mechanical effect of solar chameleons. The displacements are detected by a Michelson interferometer with a homodyne readout scheme. The sensor benefits from the focusing action of the ABRIXAS X-ray telescope installed at CAST, which increases the chameleon flux on the membrane. A mechanical chopper placed between the telescope output and the detector modulates the incoming chameleon stream. We present the results of the solar chameleon measurements taken at CAST in July 2017, setting an upper bound on the force acting on the membrane of $80$~pN at 95\% confidence level. The detector is sensitive for direct coupling to matter $10^4 \leq尾_m \leq 10^8$, where the coupling to photons is locally bound to $尾_纬\leq 10^{11}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.01084v1-abstract-full').style.display = 'none'; document.getElementById('1906.01084v1-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> 3 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">21 pages, 12 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/1904.09155">arXiv:1904.09155</a> <span> [<a href="https://arxiv.org/pdf/1904.09155">pdf</a>, <a href="https://arxiv.org/format/1904.09155">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1088/1475-7516/2019/06/047">10.1088/1475-7516/2019/06/047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Physics potential of the International Axion Observatory (IAXO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/hep-ex?searchtype=author&query=Attie%2C+D">D. Attie</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=Bykovskiy%2C+N">N. Bykovskiy</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=Cicoli%2C+M">M. Cicoli</a>, <a href="/search/hep-ex?searchtype=author&query=Civitani%2C+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=Conlon%2C+J+P">J. P. Conlon</a>, <a href="/search/hep-ex?searchtype=author&query=Costa%2C+D">D. Costa</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Daido%2C+R">R. Daido</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A+V">A. V. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Descalle%2C+M+A">M. A. Descalle</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?searchtype=author&query=Dratchnev%2C+I+S">I. S. Dratchnev</a>, <a href="/search/hep-ex?searchtype=author&query=D%7F%C3%B6brich%2C+B">B. D枚brich</a>, <a href="/search/hep-ex?searchtype=author&query=Dudarev%2C+A">A. Dudarev</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=Fleck%2C+I">I. Fleck</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=Galanti%2C+G">G. Galanti</a> , et al. (66 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="1904.09155v3-abstract-short" style="display: inline;"> We review the physics potential of a next generation search for solar axions: the International Axion Observatory (IAXO). Endowed with a sensitivity to discover axion-like particles (ALPs) with a coupling to photons as small as $g_{a纬}\sim 10^{-12}$ GeV$^{-1}$, or to electrons $g_{ae}\sim$10$^{-13}$, IAXO has the potential to find the QCD axion in the 1 meV$\sim$1 eV mass range where it solves the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.09155v3-abstract-full').style.display = 'inline'; document.getElementById('1904.09155v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.09155v3-abstract-full" style="display: none;"> We review the physics potential of a next generation search for solar axions: the International Axion Observatory (IAXO). Endowed with a sensitivity to discover axion-like particles (ALPs) with a coupling to photons as small as $g_{a纬}\sim 10^{-12}$ GeV$^{-1}$, or to electrons $g_{ae}\sim$10$^{-13}$, IAXO has the potential to find the QCD axion in the 1 meV$\sim$1 eV mass range where it solves the strong CP problem, can account for the cold dark matter of the Universe and be responsible for the anomalous cooling observed in a number of stellar systems. At the same time, IAXO will have enough sensitivity to detect lower mass axions invoked to explain: 1) the origin of the anomalous "transparency" of the Universe to gamma-rays, 2) the observed soft X-ray excess from galaxy clusters or 3) some inflationary models. In addition, we review string theory axions with parameters accessible by IAXO and discuss their potential role in cosmology as Dark Matter and Dark Radiation as well as their connections to the above mentioned conundrums. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.09155v3-abstract-full').style.display = 'none'; document.getElementById('1904.09155v3-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> 6 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">Prepared for submission to JCAP; new version with very minor corrections after referee review</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.08167">arXiv:1809.08167</a> <span> [<a href="https://arxiv.org/pdf/1809.08167">pdf</a>, <a href="https://arxiv.org/format/1809.08167">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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/10.3390/sym10100432">10.3390/sym10100432 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Twin Peaks: A possible signal in the production of resonances beyond special relativity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Albalate%2C+G">G. Albalate</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=Cortes%2C+J+L">J. L. Cortes</a>, <a href="/search/hep-ex?searchtype=author&query=Relancio%2C+J+J">J. J. Relancio</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="1809.08167v1-abstract-short" style="display: inline;"> It is usually expected that quantum gravity corrections will modify somehow the symmetries of special relativity. In this paper we point out that the possibility of very low-energy (with respect to the Planck energy) modifications to special relativity in the framework of a deformed relativistic theory is not ruled out, and that, depending on the value of that scale, such a possibility could be te… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.08167v1-abstract-full').style.display = 'inline'; document.getElementById('1809.08167v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.08167v1-abstract-full" style="display: none;"> It is usually expected that quantum gravity corrections will modify somehow the symmetries of special relativity. In this paper we point out that the possibility of very low-energy (with respect to the Planck energy) modifications to special relativity in the framework of a deformed relativistic theory is not ruled out, and that, depending on the value of that scale, such a possibility could be tested in accelerator physics. In particular, we take a simple example of a relativistic kinematics beyond special relativity from the literature, and obtain a remarkable effect: two correlated peaks ("twin peaks") associated to a single resonance. We analyze this phenomenology in detail, use LEP data to put constraints of the order of TeV on the scale of corrections to special relativity, and note that such an effect might be observable in a future very high-energy proton collider. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.08167v1-abstract-full').style.display = 'none'; document.getElementById('1809.08167v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, accepted for publication in Symmetry</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Symmetry 2018, 10, 432 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.00066">arXiv:1808.00066</a> <span> [<a href="https://arxiv.org/pdf/1808.00066">pdf</a>, <a href="https://arxiv.org/format/1808.00066">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/10.1088/1475-7516/2019/01/032">10.1088/1475-7516/2019/01/032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved Search for Solar Chameleons with a GridPix Detector at CAST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Anastassopoulos%2C+V">V. Anastassopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</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=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=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=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Christensen%2C+F">F. Christensen</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=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/hep-ex?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a>, <a href="/search/hep-ex?searchtype=author&query=Garza%2C+J+G">J. G. Garza</a>, <a href="/search/hep-ex?searchtype=author&query=Gazis%2C+E+N">E. N. Gazis</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a> , et al. (44 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="1808.00066v2-abstract-short" style="display: inline;"> We report on a new search for solar chameleons with the CERN Axion Solar Telescope (CAST). A GridPix detector was used to search for soft X-ray photons in the energy range from 200 eV to 10 keV from converted solar chameleons. No signiffcant excess over the expected background has been observed in the data taken in 2014 and 2015. We set an improved limit on the chameleon photon coupling,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.00066v2-abstract-full').style.display = 'inline'; document.getElementById('1808.00066v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.00066v2-abstract-full" style="display: none;"> We report on a new search for solar chameleons with the CERN Axion Solar Telescope (CAST). A GridPix detector was used to search for soft X-ray photons in the energy range from 200 eV to 10 keV from converted solar chameleons. No signiffcant excess over the expected background has been observed in the data taken in 2014 and 2015. We set an improved limit on the chameleon photon coupling, $尾_纬< 5.7\times10^{10}$ for $1<尾_\mathrm{m}<10^6$ at 95% C.L. improving our previous results by a factor two and for the first time reaching sensitivity below the solar luminosity bound for tachocline magnetic fields up to $12.5\,\mathrm{T}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.00066v2-abstract-full').style.display = 'none'; document.getElementById('1808.00066v2-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> 8 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 12 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.02290">arXiv:1705.02290</a> <span> [<a href="https://arxiv.org/pdf/1705.02290">pdf</a>, <a href="https://arxiv.org/format/1705.02290">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/nphys4109">10.1038/nphys4109 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New CAST Limit on the Axion-Photon Interaction </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=Anastassopoulos%2C+V">V. Anastassopoulos</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</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=Br%7Fauninger%2C+H">H. Brauninger</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</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=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Christensen%2C+F">F. Christensen</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</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=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=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Garcia%2C+J+A">J. A. Garcia</a>, <a href="/search/hep-ex?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a>, <a href="/search/hep-ex?searchtype=author&query=Garza%2C+J+G">J. G. Garza</a>, <a href="/search/hep-ex?searchtype=author&query=Gazis%2C+E+N">E. N. Gazis</a> , et al. (42 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="1705.02290v2-abstract-short" style="display: inline;"> During 2003--2015, the CERN Axion Solar Telescope (CAST) has searched for $a\to纬$ conversion in the 9 T magnetic field of a refurbished LHC test magnet that can be directed toward the Sun. In its final phase of solar axion searches (2013--2015), CAST has returned to evacuated magnet pipes, which is optimal for small axion masses. The absence of a significant signal above background provides a worl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.02290v2-abstract-full').style.display = 'inline'; document.getElementById('1705.02290v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.02290v2-abstract-full" style="display: none;"> During 2003--2015, the CERN Axion Solar Telescope (CAST) has searched for $a\to纬$ conversion in the 9 T magnetic field of a refurbished LHC test magnet that can be directed toward the Sun. In its final phase of solar axion searches (2013--2015), CAST has returned to evacuated magnet pipes, which is optimal for small axion masses. The absence of a significant signal above background provides a world leading limit of $g_{a纬} < 0.66 \times 10^{-10} {\rm GeV}^{-1}$ (95% C.L.) on the axion-photon coupling strength for $m_a \lesssim 0.02$ eV. Compared with the first vacuum phase (2003--2004), the sensitivity was vastly increased with low-background x-ray detectors and a new x-ray telescope. These innovations also serve as pathfinders for a possible next-generation axion helioscope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.02290v2-abstract-full').style.display = 'none'; document.getElementById('1705.02290v2-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 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </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">Second version after referees comments (post-print). Published version available Open Access at https://www.nature.com/articles/nphys4109</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Phys. 13 (2017) 584-590 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.00610">arXiv:1503.00610</a> <span> [<a href="https://arxiv.org/pdf/1503.00610">pdf</a>, <a href="https://arxiv.org/ps/1503.00610">ps</a>, <a href="https://arxiv.org/format/1503.00610">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/10.1103/PhysRevD.92.021101">10.1103/PhysRevD.92.021101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New solar axion search in CAST with $^4$He filling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Arik%2C+M">M. Arik</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</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=Br%7F%C3%A4uninger%2C+H">H. Br盲uninger</a>, <a href="/search/hep-ex?searchtype=author&query=Bremer%2C+J">J. Bremer</a>, <a href="/search/hep-ex?searchtype=author&query=Burwitz%2C+V">V. Burwitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</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=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</a>, <a href="/search/hep-ex?searchtype=author&query=Da+Riva%2C+E">E. Da Riva</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=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Elias%2C+N">N. Elias</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=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>, <a href="/search/hep-ex?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a>, <a href="/search/hep-ex?searchtype=author&query=Garza%2C+J+G">J. G. Garza</a>, <a href="/search/hep-ex?searchtype=author&query=Gazis%2C+E+N">E. N. Gazis</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</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="1503.00610v2-abstract-short" style="display: inline;"> The CERN Axion Solar Telescope (CAST) searches for $a\to纬$ conversion in the 9 T magnetic field of a refurbished LHC test magnet that can be directed toward the Sun. Two parallel magnet bores can be filled with helium of adjustable pressure to match the X-ray refractive mass $m_纬$ to the axion search mass $m_a$. After the vacuum phase (2003--2004), which is optimal for $m_a\lesssim0.02$ eV, we use… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.00610v2-abstract-full').style.display = 'inline'; document.getElementById('1503.00610v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.00610v2-abstract-full" style="display: none;"> The CERN Axion Solar Telescope (CAST) searches for $a\to纬$ conversion in the 9 T magnetic field of a refurbished LHC test magnet that can be directed toward the Sun. Two parallel magnet bores can be filled with helium of adjustable pressure to match the X-ray refractive mass $m_纬$ to the axion search mass $m_a$. After the vacuum phase (2003--2004), which is optimal for $m_a\lesssim0.02$ eV, we used $^4$He in 2005--2007 to cover the mass range of 0.02--0.39 eV and $^3$He in 2009--2011 to scan from 0.39--1.17 eV. After improving the detectors and shielding, we returned to $^4$He in 2012 to investigate a narrow $m_a$ range around 0.2 eV ("candidate setting" of our earlier search) and 0.39--0.42 eV, the upper axion mass range reachable with $^4$He, to "cross the axion line" for the KSVZ model. We have improved the limit on the axion-photon coupling to $g_{a纬}< 1.47\times10^{-10} {\rm GeV}^{-1}$ (95% C.L.), depending on the pressure settings. Since 2013, we have returned to vacuum and aim for a significant increase in sensitivity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.00610v2-abstract-full').style.display = 'none'; document.getElementById('1503.00610v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </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">CAST Collaboration 6 pages 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 92, 021101 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.3233">arXiv:1401.3233</a> <span> [<a href="https://arxiv.org/pdf/1401.3233">pdf</a>, <a href="https://arxiv.org/format/1401.3233">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/10.1088/1748-0221/9/05/T05002">10.1088/1748-0221/9/05/T05002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Conceptual Design of the International Axion Observatory (IAXO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/hep-ex?searchtype=author&query=Avignone%2C+F+T">F. T. Avignone</a>, <a href="/search/hep-ex?searchtype=author&query=Betz%2C+M">M. Betz</a>, <a href="/search/hep-ex?searchtype=author&query=Brax%2C+P">P. Brax</a>, <a href="/search/hep-ex?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</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=Carosi%2C+G+P">G. P. Carosi</a>, <a href="/search/hep-ex?searchtype=author&query=Caspers%2C+F">F. Caspers</a>, <a href="/search/hep-ex?searchtype=author&query=Caspi%2C+S">S. Caspi</a>, <a href="/search/hep-ex?searchtype=author&query=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Chelouche%2C+D">D. Chelouche</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=Dael%2C+A">A. Dael</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=Derbin%2C+A+V">A. V. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?searchtype=author&query=Diago%2C+A">A. Diago</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=Dratchnev%2C+I">I. Dratchnev</a>, <a href="/search/hep-ex?searchtype=author&query=Dudarev%2C+A">A. Dudarev</a>, <a href="/search/hep-ex?searchtype=author&query=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</a>, <a href="/search/hep-ex?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a> , et al. (63 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="1401.3233v1-abstract-short" style="display: inline;"> The International Axion Observatory (IAXO) will be a forth generation axion helioscope. As its primary physics goal, IAXO will look for axions or axion-like particles (ALPs) originating in the Sun via the Primakoff conversion of the solar plasma photons. In terms of signal-to-noise ratio, IAXO will be about 4-5 orders of magnitude more sensitive than CAST, currently the most powerful axion heliosc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.3233v1-abstract-full').style.display = 'inline'; document.getElementById('1401.3233v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.3233v1-abstract-full" style="display: none;"> The International Axion Observatory (IAXO) will be a forth generation axion helioscope. As its primary physics goal, IAXO will look for axions or axion-like particles (ALPs) originating in the Sun via the Primakoff conversion of the solar plasma photons. In terms of signal-to-noise ratio, IAXO will be about 4-5 orders of magnitude more sensitive than CAST, currently the most powerful axion helioscope, reaching sensitivity to axion-photon couplings down to a few $\times 10^{-12}$ GeV$^{-1}$ and thus probing a large fraction of the currently unexplored axion and ALP parameter space. IAXO will also be sensitive to solar axions produced by mechanisms mediated by the axion-electron coupling $g_{ae}$ with sensitivity $-$for the first time$-$ to values of $g_{ae}$ not previously excluded by astrophysics. With several other possible physics cases, IAXO has the potential to serve as a multi-purpose facility for generic axion and ALP research in the next decade. In this paper we present the conceptual design of IAXO, which follows the layout of an enhanced axion helioscope, based on a purpose-built 20m-long 8-coils toroidal superconducting magnet. All the eight 60cm-diameter magnet bores are equipped with focusing x-ray optics, able to focus the signal photons into $\sim 0.2$ cm$^2$ spots that are imaged by ultra-low-background Micromegas x-ray detectors. The magnet is built into a structure with elevation and azimuth drives that will allow for solar tracking for $\sim$12 h each day. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.3233v1-abstract-full').style.display = 'none'; document.getElementById('1401.3233v1-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> 14 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">47 pages, submitted to JINST</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 9 (2014) T05002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.1985">arXiv:1307.1985</a> <span> [<a href="https://arxiv.org/pdf/1307.1985">pdf</a>, <a href="https://arxiv.org/ps/1307.1985">ps</a>, <a href="https://arxiv.org/format/1307.1985">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="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/10.1103/PhysRevLett.112.091302">10.1103/PhysRevLett.112.091302 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CAST solar axion search with 3^He buffer gas: Closing the hot dark matter gap </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Arik%2C+M">M. Arik</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</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=Borghi%2C+S">S. Borghi</a>, <a href="/search/hep-ex?searchtype=author&query=Brauninger%2C+H">H. Brauninger</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</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=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</a>, <a href="/search/hep-ex?searchtype=author&query=Da+Riva%2C+E">E. Da Riva</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=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Elias%2C+N">N. Elias</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Friedrich%2C+P">P. Friedrich</a>, <a href="/search/hep-ex?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/hep-ex?searchtype=author&query=Garcia%2C+J+A">J. A. Garcia</a>, <a href="/search/hep-ex?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a>, <a href="/search/hep-ex?searchtype=author&query=Garza%2C+J+G">J. G. Garza</a>, <a href="/search/hep-ex?searchtype=author&query=Gazis%2C+E+N">E. N. Gazis</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a>, <a href="/search/hep-ex?searchtype=author&query=Georgiopoulou%2C+E">E. Georgiopoulou</a> , et al. (50 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1307.1985v2-abstract-short" style="display: inline;"> The CERN Axion Solar Telescope (CAST) has finished its search for solar axions with 3^He buffer gas, covering the search range 0.64 eV < m_a <1.17 eV. This closes the gap to the cosmological hot dark matter limit and actually overlaps with it. From the absence of excess X-rays when the magnet was pointing to the Sun we set a typical upper limit on the axion-photon coupling of g_ag < 3.3 x 10^{-10}… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.1985v2-abstract-full').style.display = 'inline'; document.getElementById('1307.1985v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.1985v2-abstract-full" style="display: none;"> The CERN Axion Solar Telescope (CAST) has finished its search for solar axions with 3^He buffer gas, covering the search range 0.64 eV < m_a <1.17 eV. This closes the gap to the cosmological hot dark matter limit and actually overlaps with it. From the absence of excess X-rays when the magnet was pointing to the Sun we set a typical upper limit on the axion-photon coupling of g_ag < 3.3 x 10^{-10} GeV^{-1} at 95% CL, with the exact value depending on the pressure setting. Future direct solar axion searches will focus on increasing the sensitivity to smaller values of g_a, for example by the currently discussed next generation helioscope IAXO. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.1985v2-abstract-full').style.display = 'none'; document.getElementById('1307.1985v2-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 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures. Last version uploaded</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 112, 091302 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1302.3273">arXiv:1302.3273</a> <span> [<a href="https://arxiv.org/pdf/1302.3273">pdf</a>, <a href="https://arxiv.org/ps/1302.3273">ps</a>, <a href="https://arxiv.org/format/1302.3273">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> <p class="title is-5 mathjax"> IAXO - The International Axion Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Vogel%2C+J+K">J. K. Vogel</a>, <a href="/search/hep-ex?searchtype=author&query=Avignone%2C+F+T">F. T. Avignone</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</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=Caspi%2C+S">S. Caspi</a>, <a href="/search/hep-ex?searchtype=author&query=Cetin%2C+S+A">S. A. Cetin</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=Dael%2C+A">A. Dael</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=Derbin%2C+A+V">A. V. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/hep-ex?searchtype=author&query=Diago%2C+A">A. Diago</a>, <a href="/search/hep-ex?searchtype=author&query=Dudarev%2C+A">A. Dudarev</a>, <a href="/search/hep-ex?searchtype=author&query=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Galan%2C+J">J. Galan</a>, <a href="/search/hep-ex?searchtype=author&query=Garcia%2C+J+A">J. A. Garcia</a>, <a href="/search/hep-ex?searchtype=author&query=Garza%2C+J+G">J. G. Garza</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a>, <a href="/search/hep-ex?searchtype=author&query=Gimeno%2C+B">B. Gimeno</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</a>, <a href="/search/hep-ex?searchtype=author&query=Gninenko%2C+S">S. Gninenko</a>, <a href="/search/hep-ex?searchtype=author&query=Gomez%2C+H">H. Gomez</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="1302.3273v1-abstract-short" style="display: inline;"> The International Axion Observatory (IAXO) is a next generation axion helioscope aiming at a sensitivity to the axion-photon coupling of a few 10^{-12} GeV^{-1}, i.e. 1-1.5 orders of magnitude beyond sensitivities achieved by the currently most sensitive axion helioscope, the CERN Axion Solar Telescope (CAST). Crucial factors in improving the sensitivity for IAXO are the increase of the magnetic f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1302.3273v1-abstract-full').style.display = 'inline'; document.getElementById('1302.3273v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1302.3273v1-abstract-full" style="display: none;"> The International Axion Observatory (IAXO) is a next generation axion helioscope aiming at a sensitivity to the axion-photon coupling of a few 10^{-12} GeV^{-1}, i.e. 1-1.5 orders of magnitude beyond sensitivities achieved by the currently most sensitive axion helioscope, the CERN Axion Solar Telescope (CAST). Crucial factors in improving the sensitivity for IAXO are the increase of the magnetic field volume together with the extensive use of x-ray focusing optics and low background detectors, innovations already successfully tested at CAST. Electron-coupled axions invoked to explain the white dwarf cooling, relic axions, and a large variety of more generic axion-like particles (ALPs) along with other novel excitations at the low-energy frontier of elementary particle physics could provide additional physics motivation for IAXO. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1302.3273v1-abstract-full').style.display = 'none'; document.getElementById('1302.3273v1-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> 13 February, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2013. </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">6 pages, 1 figure, Contribution to the 8th Patras Workshop on Axions, WIMPs and WISPs, Chicago, IL, USA, 2012</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1209.6347">arXiv:1209.6347</a> <span> [<a href="https://arxiv.org/pdf/1209.6347">pdf</a>, <a href="https://arxiv.org/format/1209.6347">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Results and perspectives of the solar axion search with the CAST experiment </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=Arik%2C+M">M. Arik</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</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=Borghi%2C+S">S. Borghi</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=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/hep-ex?searchtype=author&query=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</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=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Elias%2C+N">N. Elias</a>, <a href="/search/hep-ex?searchtype=author&query=Ezer%2C+C">C. Ezer</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</a>, <a href="/search/hep-ex?searchtype=author&query=Friedrich%2C+P">P. Friedrich</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>, <a href="/search/hep-ex?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a>, <a href="/search/hep-ex?searchtype=author&query=Garza%2C+J+G">J. G. Garza</a>, <a href="/search/hep-ex?searchtype=author&query=Gazis%2C+E+N">E. N. Gazis</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</a> , et al. (47 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="1209.6347v3-abstract-short" style="display: inline;"> The status of the solar axion search with the CERN Axion Solar Telescope (CAST) will be presented. Recent results obtained by the use of $^3$He as a buffer gas has allowed us to extend our sensitivity to higher axion masses than our previous measurements with $^4$He. With about 1 h of data taking at each of 252 different pressure settings we have scanned the axion mass range 0.39 eV… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.6347v3-abstract-full').style.display = 'inline'; document.getElementById('1209.6347v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1209.6347v3-abstract-full" style="display: none;"> The status of the solar axion search with the CERN Axion Solar Telescope (CAST) will be presented. Recent results obtained by the use of $^3$He as a buffer gas has allowed us to extend our sensitivity to higher axion masses than our previous measurements with $^4$He. With about 1 h of data taking at each of 252 different pressure settings we have scanned the axion mass range 0.39 eV$ \le m_{a} \le $ 0.64 eV. From the absence of an excess of x rays when the magnet was pointing to the Sun we set a typical upper limit on the axion-photon coupling of g$_{a纬} \le 2.3\times 10^{-10}$ GeV$^{-1}$ at 95% C.L., the exact value depending on the pressure setting. CAST published results represent the best experimental limit on the photon couplings to axions and other similar exotic particles dubbed WISPs (Weakly Interacting Slim Particles) in the considered mass range and for the first time the limit enters the region favored by QCD axion models. Preliminary sensitivities for axion masses up to 1.16 eV will also be shown reaching mean upper limits on the axion-photon coupling of g$_{a纬} \le 3.5\times 10^{-10}$ GeV$^{-1}$ at 95% C.L. Expected sensibilities for the extension of the CAST program up to 2014 will be presented. Moreover long term options for a new helioscope experiment will be evoked. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.6347v3-abstract-full').style.display = 'none'; document.getElementById('1209.6347v3-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> 30 October, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 September, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2012. </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 pages, to appear in the proceedings of the 24th Rencontres de Blois V2 A few affiliations were not corrected in previous version V3 Author added</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1206.6199">arXiv:1206.6199</a> <span> [<a href="https://arxiv.org/pdf/1206.6199">pdf</a>, <a href="https://arxiv.org/format/1206.6199">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> <p class="title is-5 mathjax"> Design and characterization of the SiPM tracking system of NEXT-DEMO, a demonstrator prototype of the NEXT-100 experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=NEXT+Collaboration"> NEXT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%81lvarez%2C+V">V. 脕lvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Ball%2C+M">M. Ball</a>, <a href="/search/hep-ex?searchtype=author&query=Borges%2C+F+I+G+M">F. I. G. M. Borges</a>, <a href="/search/hep-ex?searchtype=author&query=C%C3%A1rcel%2C+S">S. C谩rcel</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">J. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=Catal%C3%A1%2C+J+M">J. M. Catal谩</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=Cervera%2C+A">A. Cervera</a>, <a href="/search/hep-ex?searchtype=author&query=Chan%2C+D">D. Chan</a>, <a href="/search/hep-ex?searchtype=author&query=Conde%2C+C+A+N">C. A. N. Conde</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Dias%2C+T+H+V+T">T. H. V. T. Dias</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%ADaz%2C+J">J. D铆az</a>, <a href="/search/hep-ex?searchtype=author&query=Egorov%2C+M">M. Egorov</a>, <a href="/search/hep-ex?searchtype=author&query=Esteve%2C+R">R. Esteve</a>, <a href="/search/hep-ex?searchtype=author&query=Evtoukhovitch%2C+P">P. Evtoukhovitch</a>, <a href="/search/hep-ex?searchtype=author&query=Fernandes%2C+L+M+P">L. M. P. Fernandes</a>, <a href="/search/hep-ex?searchtype=author&query=Ferrario%2C+P">P. Ferrario</a>, <a href="/search/hep-ex?searchtype=author&query=Ferreira%2C+A+L">A. L. Ferreira</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=Freitas%2C+E+D+C">E. D. C. Freitas</a>, <a href="/search/hep-ex?searchtype=author&query=Garcia%2C+A+N+C">A. N. C. Garcia</a>, <a href="/search/hep-ex?searchtype=author&query=Gehman%2C+V+M">V. M. Gehman</a> , et al. (64 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="1206.6199v2-abstract-short" style="display: inline;"> NEXT-100 experiment aims at searching the neutrinoless double-beta decay of the Xe-136 isotope using a TPC filled with a 100 kg of high-pressure gaseous xenon, with 90% isotopic enrichment. The experiment will take place at the Laboratorio Subterr谩neo de Canfranc (LSC), Spain. NEXT-100 uses electroluminescence (EL) technology for energy measurement with a resolution better than 1% FWHM. The gaseou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.6199v2-abstract-full').style.display = 'inline'; document.getElementById('1206.6199v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1206.6199v2-abstract-full" style="display: none;"> NEXT-100 experiment aims at searching the neutrinoless double-beta decay of the Xe-136 isotope using a TPC filled with a 100 kg of high-pressure gaseous xenon, with 90% isotopic enrichment. The experiment will take place at the Laboratorio Subterr谩neo de Canfranc (LSC), Spain. NEXT-100 uses electroluminescence (EL) technology for energy measurement with a resolution better than 1% FWHM. The gaseous xenon in the TPC additionally allows the tracks of the two beta particles to be recorded, which are expected to have a length of up to 30 cm at 10 bar pressure. The ability to record the topological signature of the neutrinoless double-beta events provides a powerful background rejection factor for the double-beta experiment. In this paper, we present a novel 3D imaging concept using SiPMs coated with tetraphenyl butadiene (TPB) for the EL read out and its first implementation in NEXT-DEMO, a large-scale prototype of the NEXT-100 experiment. The design and the first characterization measurements of the NEXT-DEMO SiPM tracking system are presented. The SiPM response uniformity over the tracking plane drawn from its gain map is shown to be better than 4%. An automated active control system for the stabilization of the SiPMs gain was developed, based on the voltage supply compensation of the gain drifts. The gain is shown to be stabilized within 0.2% relative variation around its nominal value, provided by Hamamatsu, in a temperature range of 10 degree C. The noise level from the electronics and the SiPM dark noise is shown to lay typically below the level of 10 photoelectrons (pe) in the ADC. Hence, a detection threshold at 10 pe is set for the acquisition of the tracking signals. The ADC full dynamic range (4096 channels) is shown to be adequate for signal levels of up to 200 pe/microsecond, which enables recording most of the tracking signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.6199v2-abstract-full').style.display = 'none'; document.getElementById('1206.6199v2-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 February, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 June, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to 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/1202.0721">arXiv:1202.0721</a> <span> [<a href="https://arxiv.org/pdf/1202.0721">pdf</a>, <a href="https://arxiv.org/format/1202.0721">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/10.1088/1748-0221/7/06/T06001">10.1088/1748-0221/7/06/T06001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NEXT-100 Technical Design Report (TDR). Executive Summary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=NEXT+Collaboration"> NEXT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%81lvarez%2C+V">V. 脕lvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Borges%2C+F+I+G+M">F. I. G. M. Borges</a>, <a href="/search/hep-ex?searchtype=author&query=C%C3%A1rcel%2C+S">S. C谩rcel</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">J. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=Catal%C3%A1%2C+J+M">J. M. Catal谩</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=Cervera%2C+A">A. Cervera</a>, <a href="/search/hep-ex?searchtype=author&query=Chan%2C+D">D. Chan</a>, <a href="/search/hep-ex?searchtype=author&query=Conde%2C+C+A+N">C. A. N. Conde</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Dias%2C+T+H+V+T">T. H. V. T. Dias</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%ADaz%2C+J">J. D铆az</a>, <a href="/search/hep-ex?searchtype=author&query=Egorov%2C+M">M. Egorov</a>, <a href="/search/hep-ex?searchtype=author&query=Esteve%2C+R">R. Esteve</a>, <a href="/search/hep-ex?searchtype=author&query=Evtoukhovitch%2C+P">P. Evtoukhovitch</a>, <a href="/search/hep-ex?searchtype=author&query=Fernandes%2C+L+M+P">L. M. P. Fernandes</a>, <a href="/search/hep-ex?searchtype=author&query=Ferrario%2C+P">P. Ferrario</a>, <a href="/search/hep-ex?searchtype=author&query=Ferreira%2C+A+L">A. L. Ferreira</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=Freitas%2C+E+D+C">E. D. C. Freitas</a>, <a href="/search/hep-ex?searchtype=author&query=Gehman%2C+V+M">V. M. Gehman</a>, <a href="/search/hep-ex?searchtype=author&query=Gil%2C+A">A. Gil</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</a> , et al. (62 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="1202.0721v2-abstract-short" style="display: inline;"> In this Technical Design Report (TDR) we describe the NEXT-100 detector that will search for neutrinoless double beta decay (bbonu) in Xe-136 at the Laboratorio Subterraneo de Canfranc (LSC), in Spain. The document formalizes the design presented in our Conceptual Design Report (CDR): an electroluminescence time projection chamber, with separate readout planes for calorimetry and tracking, located… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.0721v2-abstract-full').style.display = 'inline'; document.getElementById('1202.0721v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.0721v2-abstract-full" style="display: none;"> In this Technical Design Report (TDR) we describe the NEXT-100 detector that will search for neutrinoless double beta decay (bbonu) in Xe-136 at the Laboratorio Subterraneo de Canfranc (LSC), in Spain. The document formalizes the design presented in our Conceptual Design Report (CDR): an electroluminescence time projection chamber, with separate readout planes for calorimetry and tracking, located, respectively, behind cathode and anode. The detector is designed to hold a maximum of about 150 kg of xenon at 15 bar, or 100 kg at 10 bar. This option builds in the capability to increase the total isotope mass by 50% while keeping the operating pressure at a manageable level. The readout plane performing the energy measurement is composed of Hamamatsu R11410-10 photomultipliers, specially designed for operation in low-background, xenon-based detectors. Each individual PMT will be isolated from the gas by an individual, pressure resistant enclosure and will be coupled to the sensitive volume through a sapphire window. The tracking plane consists in an array of Hamamatsu S10362-11-050P MPPCs used as tracking pixels. They will be arranged in square boards holding 64 sensors (8 times8) with a 1-cm pitch. The inner walls of the TPC, the sapphire windows and the boards holding the MPPCs will be coated with tetraphenyl butadiene (TPB), a wavelength shifter, to improve the light collection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.0721v2-abstract-full').style.display = 'none'; document.getElementById('1202.0721v2-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> 16 April, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 22 figures, 5 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 7 (2012) T06001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.3849">arXiv:1201.3849</a> <span> [<a href="https://arxiv.org/pdf/1201.3849">pdf</a>, <a href="https://arxiv.org/ps/1201.3849">ps</a>, <a href="https://arxiv.org/format/1201.3849">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"> The International Axion Observatory (IAXO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/hep-ex?searchtype=author&query=Avignone%2C+F+T">F. T. Avignone</a>, <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">G. Cantatore</a>, <a href="/search/hep-ex?searchtype=author&query=Caspi%2C+S">S. Caspi</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=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=Dudarev%2C+A">A. Dudarev</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Galan%2C+J">J. Galan</a>, <a href="/search/hep-ex?searchtype=author&query=Garcia%2C+J+A">J. A. Garcia</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</a>, <a href="/search/hep-ex?searchtype=author&query=Gninenko%2C+S">S. Gninenko</a>, <a href="/search/hep-ex?searchtype=author&query=Gomez%2C+H">H. Gomez</a>, <a href="/search/hep-ex?searchtype=author&query=Hoffmann%2C+D+H+H">D. H. H. Hoffmann</a>, <a href="/search/hep-ex?searchtype=author&query=Iguaz%2C+F+J">F. J. Iguaz</a>, <a href="/search/hep-ex?searchtype=author&query=Jakovcic%2C+K">K. Jakovcic</a>, <a href="/search/hep-ex?searchtype=author&query=Krcmar%2C+M">M. Krcmar</a>, <a href="/search/hep-ex?searchtype=author&query=Lakic%2C+B">B. Lakic</a>, <a href="/search/hep-ex?searchtype=author&query=Luzon%2C+G">G. Luzon</a>, <a href="/search/hep-ex?searchtype=author&query=Lindner%2C+A">A. Lindner</a>, <a href="/search/hep-ex?searchtype=author&query=Pivovaroff%2C+M">M. Pivovaroff</a>, <a href="/search/hep-ex?searchtype=author&query=Papaevangelou%2C+T">T. Papaevangelou</a> , et al. (14 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="1201.3849v1-abstract-short" style="display: inline;"> The International Axion Observatory (IAXO) is a new generation axion helioscope aiming at a sensitivity to the axion-photon coupling of a few 10$^{12}$ GeV$^{-1}$, i.e. 1 - 1.5 orders of magnitude beyond the one currently achieved by CAST. The project relies on improvements in magnetic field volume together with extensive use of x-ray focusing optics and low background detectors, innovations alrea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.3849v1-abstract-full').style.display = 'inline'; document.getElementById('1201.3849v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.3849v1-abstract-full" style="display: none;"> The International Axion Observatory (IAXO) is a new generation axion helioscope aiming at a sensitivity to the axion-photon coupling of a few 10$^{12}$ GeV$^{-1}$, i.e. 1 - 1.5 orders of magnitude beyond the one currently achieved by CAST. The project relies on improvements in magnetic field volume together with extensive use of x-ray focusing optics and low background detectors, innovations already successfully tested in CAST. Additional physics cases of IAXO could include the detection of electron-coupled axions invoked to solve the white dwarfs anomaly, relic axions, and a large variety of more generic axion-like particles (ALPs) and other novel excitations at the low-energy frontier of elementary particle physics. This contribution is a summary of our paper [1] to which we refer for further details. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.3849v1-abstract-full').style.display = 'none'; document.getElementById('1201.3849v1-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 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2012. </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. To appear in the proceedings of the 7th Patras Workshop on Axions, WIMPs and WISPs, Mykonos, Greece, 2011</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.2018">arXiv:1201.2018</a> <span> [<a href="https://arxiv.org/pdf/1201.2018">pdf</a>, <a href="https://arxiv.org/format/1201.2018">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/10.1088/1748-0221/7/02/P02010">10.1088/1748-0221/7/02/P02010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SiPMs coated with TPB : coating protocol and characterization for NEXT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=%C3%81lvarez%2C+V">V. 脕lvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Agramunt%2C+J">J. Agramunt</a>, <a href="/search/hep-ex?searchtype=author&query=Ball%2C+M">M. Ball</a>, <a href="/search/hep-ex?searchtype=author&query=Batall%C3%A9%2C+M">M. Batall茅</a>, <a href="/search/hep-ex?searchtype=author&query=Bayarri%2C+J">J. Bayarri</a>, <a href="/search/hep-ex?searchtype=author&query=Borges%2C+F+I+G">F. I. G. Borges</a>, <a href="/search/hep-ex?searchtype=author&query=Bolink%2C+H">H. Bolink</a>, <a href="/search/hep-ex?searchtype=author&query=Brine%2C+H">H. Brine</a>, <a href="/search/hep-ex?searchtype=author&query=C%C3%A1rcel%2C+S">S. C谩rcel</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">J. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=Catal%C3%A1%2C+J+M">J. M. Catal谩</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=Cervera%2C+A">A. Cervera</a>, <a href="/search/hep-ex?searchtype=author&query=Chan%2C+D">D. Chan</a>, <a href="/search/hep-ex?searchtype=author&query=Conde%2C+C+A+N">C. A. N. Conde</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Dias%2C+T+H+V+T">T. H. V. T. Dias</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%ADaz%2C+J">J. D铆az</a>, <a href="/search/hep-ex?searchtype=author&query=Esteve%2C+R">R. Esteve</a>, <a href="/search/hep-ex?searchtype=author&query=Evtoukhovitch%2C+P">P. Evtoukhovitch</a>, <a href="/search/hep-ex?searchtype=author&query=Ferrando%2C+J">J. Ferrando</a>, <a href="/search/hep-ex?searchtype=author&query=Fernandes%2C+L+M+P">L. M. P. Fernandes</a>, <a href="/search/hep-ex?searchtype=author&query=Ferrario%2C+P">P. Ferrario</a>, <a href="/search/hep-ex?searchtype=author&query=Ferreira%2C+A+L">A. L. Ferreira</a> , et al. (69 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="1201.2018v1-abstract-short" style="display: inline;"> Silicon photomultipliers (SiPM) are the photon detectors chosen for the tracking readout in NEXT, a neutrinoless 尾尾 decay experiment which uses a high pressure gaseous xenon time projection chamber (TPC). The reconstruction of event track and topology in this gaseous detector is a key handle for background rejection. Among the commercially available sensors that can be used for tracking, SiPMs off… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.2018v1-abstract-full').style.display = 'inline'; document.getElementById('1201.2018v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.2018v1-abstract-full" style="display: none;"> Silicon photomultipliers (SiPM) are the photon detectors chosen for the tracking readout in NEXT, a neutrinoless 尾尾 decay experiment which uses a high pressure gaseous xenon time projection chamber (TPC). The reconstruction of event track and topology in this gaseous detector is a key handle for background rejection. Among the commercially available sensors that can be used for tracking, SiPMs offer important advantages, mainly high gain, ruggedness, cost-effectiveness and radio-purity. Their main drawback, however, is their non sensitivity in the emission spectrum of the xenon scintillation (peak at 175 nm). This is overcome by coating these sensors with the organic wavelength shifter tetraphenyl butadienne (TPB). In this paper we describe the protocol developed for coating the SiPMs with TPB and the measurements performed for characterizing the coatings as well as the performance of the coated sensors in the UV-VUV range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.2018v1-abstract-full').style.display = 'none'; document.getElementById('1201.2018v1-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 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to the Journal of Instrumentation on december 26th 2011</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 7 (2012) P02010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1106.3919">arXiv:1106.3919</a> <span> [<a href="https://arxiv.org/pdf/1106.3919">pdf</a>, <a href="https://arxiv.org/ps/1106.3919">ps</a>, <a href="https://arxiv.org/format/1106.3919">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 class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.107.261302">10.1103/PhysRevLett.107.261302 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CAST search for sub-eV mass solar axions with 3He buffer gas </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Arik%2C+M">M. Arik</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</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=Borghi%2C+S">S. Borghi</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=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/hep-ex?searchtype=author&query=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</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=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Elias%2C+N">N. Elias</a>, <a href="/search/hep-ex?searchtype=author&query=Ezer%2C+C">C. Ezer</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Friedrich%2C+P">P. Friedrich</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>, <a href="/search/hep-ex?searchtype=author&query=Gardikiotis%2C+A">A. Gardikiotis</a>, <a href="/search/hep-ex?searchtype=author&query=Gazis%2C+E+N">E. N. Gazis</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</a>, <a href="/search/hep-ex?searchtype=author&query=Gninenko%2C+S">S. Gninenko</a> , et al. (46 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="1106.3919v2-abstract-short" style="display: inline;"> The CERN Axion Solar Telescope (CAST) has extended its search for solar axions by using 3He as a buffer gas. At T=1.8 K this allows for larger pressure settings and hence sensitivity to higher axion masses than our previous measurements with 4He. With about 1 h of data taking at each of 252 different pressure settings we have scanned the axion mass range 0.39 eV < m_a < 0.64 eV. From the absence o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.3919v2-abstract-full').style.display = 'inline'; document.getElementById('1106.3919v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1106.3919v2-abstract-full" style="display: none;"> The CERN Axion Solar Telescope (CAST) has extended its search for solar axions by using 3He as a buffer gas. At T=1.8 K this allows for larger pressure settings and hence sensitivity to higher axion masses than our previous measurements with 4He. With about 1 h of data taking at each of 252 different pressure settings we have scanned the axion mass range 0.39 eV < m_a < 0.64 eV. From the absence of excess X-rays when the magnet was pointing to the Sun we set a typical upper limit on the axion-photon coupling of g_ag < 2.3 x 10^{-10} GeV^{-1} at 95% CL, the exact value depending on the pressure setting. KSVZ axions are excluded at the upper end of our mass range, the first time ever for any solar axion search. In future we will extend our search to m_a < 1.15 eV, comfortably overlapping with cosmological hot dark matter bounds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.3919v2-abstract-full').style.display = 'none'; document.getElementById('1106.3919v2-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 October, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures, updated author list, revised arguments, results unchanged</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 107 (2011) 261302 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1106.3630">arXiv:1106.3630</a> <span> [<a href="https://arxiv.org/pdf/1106.3630">pdf</a>, <a href="https://arxiv.org/format/1106.3630">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> <p class="title is-5 mathjax"> The NEXT-100 experiment for neutrinoless double beta decay searches (Conceptual Design Report) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=NEXT+Collaboration"> NEXT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%C3%81lvarez%2C+V">V. 脕lvarez</a>, <a href="/search/hep-ex?searchtype=author&query=Ball%2C+M">M. Ball</a>, <a href="/search/hep-ex?searchtype=author&query=Batall%C3%A9%2C+M">M. Batall茅</a>, <a href="/search/hep-ex?searchtype=author&query=Bayarri%2C+J">J. Bayarri</a>, <a href="/search/hep-ex?searchtype=author&query=Borges%2C+F+I+G">F. I. G. Borges</a>, <a href="/search/hep-ex?searchtype=author&query=C%C3%A1rcel%2C+S">S. C谩rcel</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">J. Castel</a>, <a href="/search/hep-ex?searchtype=author&query=Catal%C3%A1%2C+J+M">J. M. Catal谩</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=Cervera-Villanueva%2C+A">A. Cervera-Villanueva</a>, <a href="/search/hep-ex?searchtype=author&query=Chan%2C+D">D. Chan</a>, <a href="/search/hep-ex?searchtype=author&query=Conde%2C+C+A+N">C. A. N. Conde</a>, <a href="/search/hep-ex?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/hep-ex?searchtype=author&query=Dias%2C+T+H+V+T">T. H. V. T. Dias</a>, <a href="/search/hep-ex?searchtype=author&query=D%C3%ADaz%2C+J">J. D铆az</a>, <a href="/search/hep-ex?searchtype=author&query=Esteve%2C+R">R. Esteve</a>, <a href="/search/hep-ex?searchtype=author&query=Evtoukhovitch%2C+P">P. Evtoukhovitch</a>, <a href="/search/hep-ex?searchtype=author&query=Fernandes%2C+L+M+P">L. M. P. Fernandes</a>, <a href="/search/hep-ex?searchtype=author&query=Ferrario%2C+P">P. Ferrario</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=Ferreira%2C+A+L">A. L. Ferreira</a>, <a href="/search/hep-ex?searchtype=author&query=Freitas%2C+E+D+C">E. D. C. Freitas</a>, <a href="/search/hep-ex?searchtype=author&query=Gil%2C+A">A. Gil</a> , et al. (58 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="1106.3630v1-abstract-short" style="display: inline;"> We propose an EASY (Electroluminescent ApparatuS of high Yield) and SOFT (Separated Optimized FuncTion) time-projection chamber for the NEXT experiment, that will search for neutrinoless double beta decay (bb0nu) in Xe-136. Our experiment must be competitive with the new generation of bb0nu searches already in operation or in construction. This requires a detector with very good energy resolution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.3630v1-abstract-full').style.display = 'inline'; document.getElementById('1106.3630v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1106.3630v1-abstract-full" style="display: none;"> We propose an EASY (Electroluminescent ApparatuS of high Yield) and SOFT (Separated Optimized FuncTion) time-projection chamber for the NEXT experiment, that will search for neutrinoless double beta decay (bb0nu) in Xe-136. Our experiment must be competitive with the new generation of bb0nu searches already in operation or in construction. This requires a detector with very good energy resolution (<1%), very low background con- tamination (1E-4 counts/(keV \bullet kg \bullet y)) and large target mass. In addition, it needs to be operational as soon as possible. The design described here optimizes energy resolution thanks to the use of proportional electroluminescent amplification (EL); it is compact, as the Xe gas is under high pressure; and it allows the measurement of the topological signature of the event to further reduce the background contamination. The SOFT design uses different sensors for tracking and calorimetry. We propose the use of SiPMs (MPPCs) coated with a suitable wavelength shifter for the tracking, and the use of radiopure photomultipliers for the measurement of the energy and the primary scintillation needed to estimate the t0. This design provides the best possible energy resolution compared with other NEXT designs based on avalanche gain devices. The baseline design is an Asymmetric Neutrino Gas EL apparatus (ANGEL), which was already outlined in the NEXT LOI. ANGEL is conceived to be easy to fabricate. It requires very little R&D and most of the proposed solutions have already been tested in the NEXT-1 prototypes. Therefore, the detector can be ready by 2013. In this Conceptual Design Report (CDR) we discuss first the physics case, present a full design of the detector, describe the NEXT-1 EL prototypes and their initial results, and outline a project to build a detector with 100 kg of enriched xenon to be installed in the Canfranc Underground Laboratory in 2013. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.3630v1-abstract-full').style.display = 'none'; document.getElementById('1106.3630v1-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 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2011. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1103.5334">arXiv:1103.5334</a> <span> [<a href="https://arxiv.org/pdf/1103.5334">pdf</a>, <a href="https://arxiv.org/ps/1103.5334">ps</a>, <a href="https://arxiv.org/format/1103.5334">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 class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2011/06/013">10.1088/1475-7516/2011/06/013 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Towards a new generation axion helioscope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/hep-ex?searchtype=author&query=Avignone%2C+F+T">F. T. Avignone</a>, <a href="/search/hep-ex?searchtype=author&query=Caspi%2C+S">S. Caspi</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=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=Dudarev%2C+A">A. Dudarev</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Galan%2C+J">J. Galan</a>, <a href="/search/hep-ex?searchtype=author&query=Garcia%2C+J+A">J. A. Garcia</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</a>, <a href="/search/hep-ex?searchtype=author&query=Gomez%2C+H">H. Gomez</a>, <a href="/search/hep-ex?searchtype=author&query=Hoffmann%2C+D+H+H">D. H. H. Hoffmann</a>, <a href="/search/hep-ex?searchtype=author&query=Iguaz%2C+F+J">F. J. Iguaz</a>, <a href="/search/hep-ex?searchtype=author&query=Jakovcic%2C+K">K. Jakovcic</a>, <a href="/search/hep-ex?searchtype=author&query=Krcmar%2C+M">M. Krcmar</a>, <a href="/search/hep-ex?searchtype=author&query=Lakic%2C+B">B. Lakic</a>, <a href="/search/hep-ex?searchtype=author&query=Luzon%2C+G">G. Luzon</a>, <a href="/search/hep-ex?searchtype=author&query=Pivovaroff%2C+M">M. Pivovaroff</a>, <a href="/search/hep-ex?searchtype=author&query=Papaevangelou%2C+T">T. Papaevangelou</a>, <a href="/search/hep-ex?searchtype=author&query=Raffelt%2C+G">G. Raffelt</a>, <a href="/search/hep-ex?searchtype=author&query=Redondo%2C+J">J. Redondo</a>, <a href="/search/hep-ex?searchtype=author&query=Rodriguez%2C+A">A. Rodriguez</a> , et al. (11 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="1103.5334v3-abstract-short" style="display: inline;"> We study the feasibility of a new generation axion helioscope, the most ambitious and promising detector of solar axions to date. We show that large improvements in magnetic field volume, x-ray focusing optics and detector backgrounds are possible beyond those achieved in the CERN Axion Solar Telescope (CAST). For hadronic models, a sensitivity to the axion-photon coupling of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.5334v3-abstract-full').style.display = 'inline'; document.getElementById('1103.5334v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1103.5334v3-abstract-full" style="display: none;"> We study the feasibility of a new generation axion helioscope, the most ambitious and promising detector of solar axions to date. We show that large improvements in magnetic field volume, x-ray focusing optics and detector backgrounds are possible beyond those achieved in the CERN Axion Solar Telescope (CAST). For hadronic models, a sensitivity to the axion-photon coupling of $\gagamma\gtrsim {\rm few} \times 10^{-12}$ GeV$^{-1}$ is conceivable, 1--1.5 orders of magnitude beyond the CAST sensitivity. If axions also couple to electrons, the Sun produces a larger flux for the same value of the Peccei-Quinn scale, allowing one to probe a broader class of models. Except for the axion dark matter searches, this experiment will be the most sensitive axion search ever, reaching or surpassing the stringent bounds from SN1987A and possibly testing the axion interpretation of anomalous white-dwarf cooling that predicts $m_a$ of a few meV. Beyond axions, this new instrument will probe entirely unexplored ranges of parameters for a large variety of axion-like particles (ALPs) and other novel excitations at the low-energy frontier of elementary particle physics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.5334v3-abstract-full').style.display = 'none'; document.getElementById('1103.5334v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 March, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 11 figures, accepted for publication in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 1106 (2011) 013 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0907.4054">arXiv:0907.4054</a> <span> [<a href="https://arxiv.org/pdf/0907.4054">pdf</a>, <a href="https://arxiv.org/format/0907.4054">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="Nuclear Experiment">nucl-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"> NEXT, a HPGXe TPC for neutrinoless double beta decay searches </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+NEXT+Collaboration"> The NEXT Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Granena%2C+F">F. Granena</a>, <a href="/search/hep-ex?searchtype=author&query=Lux%2C+T">T. Lux</a>, <a href="/search/hep-ex?searchtype=author&query=Nova%2C+F">F. Nova</a>, <a href="/search/hep-ex?searchtype=author&query=Rico%2C+J">J. Rico</a>, <a href="/search/hep-ex?searchtype=author&query=Sanchez%2C+F">F. Sanchez</a>, <a href="/search/hep-ex?searchtype=author&query=Nygren%2C+D+R">D. R. Nygren</a>, <a href="/search/hep-ex?searchtype=author&query=Barata%2C+J+A+S">J. A. S. Barata</a>, <a href="/search/hep-ex?searchtype=author&query=Borges%2C+F+I+G+M">F. I. G. M. Borges</a>, <a href="/search/hep-ex?searchtype=author&query=Conde%2C+C+A+N">C. A. N. Conde</a>, <a href="/search/hep-ex?searchtype=author&query=Dias%2C+T+H+V+T">T. H. V. T. Dias</a>, <a href="/search/hep-ex?searchtype=author&query=Fernandes%2C+L+M+P">L. M. P. Fernandes</a>, <a href="/search/hep-ex?searchtype=author&query=Freitas%2C+E+D+C">E. D. C. Freitas</a>, <a href="/search/hep-ex?searchtype=author&query=Lopes%2C+J+A+M">J. A. M. Lopes</a>, <a href="/search/hep-ex?searchtype=author&query=Monteiro%2C+C+M+B">C. M. B. Monteiro</a>, <a href="/search/hep-ex?searchtype=author&query=Santos%2C+J+M+F+d">J. M. F. dos Santos</a>, <a href="/search/hep-ex?searchtype=author&query=Santos%2C+F+P">F. P. Santos</a>, <a href="/search/hep-ex?searchtype=author&query=Tavora%2C+L+M+N">L. M. N. Tavora</a>, <a href="/search/hep-ex?searchtype=author&query=Veloso%2C+J+F+C+A">J. F. C. A. Veloso</a>, <a href="/search/hep-ex?searchtype=author&query=Calvo%2C+E">E. Calvo</a>, <a href="/search/hep-ex?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</a>, <a href="/search/hep-ex?searchtype=author&query=Novella%2C+P">P. Novella</a>, <a href="/search/hep-ex?searchtype=author&query=Palomares%2C+C">C. Palomares</a>, <a href="/search/hep-ex?searchtype=author&query=Verdugo%2C+A">A. Verdugo</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</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="0907.4054v1-abstract-short" style="display: inline;"> We propose a novel detection concept for neutrinoless double-beta decay searches. This concept is based on a Time Projection Chamber (TPC) filled with high-pressure gaseous xenon, and with separated-function capabilities for calorimetry and tracking. Thanks to its excellent energy resolution, together with its powerful background rejection provided by the distinct double-beta decay topological s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.4054v1-abstract-full').style.display = 'inline'; document.getElementById('0907.4054v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.4054v1-abstract-full" style="display: none;"> We propose a novel detection concept for neutrinoless double-beta decay searches. This concept is based on a Time Projection Chamber (TPC) filled with high-pressure gaseous xenon, and with separated-function capabilities for calorimetry and tracking. Thanks to its excellent energy resolution, together with its powerful background rejection provided by the distinct double-beta decay topological signature, the design discussed in this Letter Of Intent promises to be competitive and possibly out-perform existing proposals for next-generation neutrinoless double-beta decay experiments. We discuss the detection principles, design specifications, physics potential and R&D plans to construct a detector with 100 kg fiducial mass in the double-beta decay emitting isotope Xe(136), to be installed in the Canfranc Underground Laboratory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.4054v1-abstract-full').style.display = 'none'; document.getElementById('0907.4054v1-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 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2009. </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">Letter of Intent to the LSC Scientific Committee 115 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0906.4488">arXiv:0906.4488</a> <span> [<a href="https://arxiv.org/pdf/0906.4488">pdf</a>, <a href="https://arxiv.org/ps/0906.4488">ps</a>, <a href="https://arxiv.org/format/0906.4488">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 class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2009/12/002">10.1088/1475-7516/2009/12/002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for 14.4 keV solar axions emitted in the M1-transition of 57Fe nuclei with CAST </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=Andriamonje%2C+S">S. Andriamonje</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ex?searchtype=author&query=Autiero%2C+D">D. Autiero</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=Beltr%C3%A1n%2C+B">B. Beltr谩n</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=Carmona%2C+J+M">J. M. Carmona</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=Collar%2C+J+I">J. I. Collar</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=Di+Lella%2C+L">L. Di Lella</a>, <a href="/search/hep-ex?searchtype=author&query=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Englhauser%2C+J">J. Englhauser</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Franz%2C+J">J. Franz</a>, <a href="/search/hep-ex?searchtype=author&query=Friedrich%2C+P">P. Friedrich</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</a>, <a href="/search/hep-ex?searchtype=author&query=Gninenko%2C+S">S. Gninenko</a>, <a href="/search/hep-ex?searchtype=author&query=G%C3%B3mez%2C+H">H. G贸mez</a> , et al. (36 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="0906.4488v2-abstract-short" style="display: inline;"> We have searched for 14.4 keV solar axions or more general axion-like particles (ALPs), that may be emitted in the M1 nuclear transition of 57Fe, by using the axion-to-photon conversion in the CERN Axion Solar Telescope (CAST) with evacuated magnet bores (Phase I). From the absence of excess of the monoenergetic X-rays when the magnet was pointing to the Sun, we set model-independent constraints… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0906.4488v2-abstract-full').style.display = 'inline'; document.getElementById('0906.4488v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0906.4488v2-abstract-full" style="display: none;"> We have searched for 14.4 keV solar axions or more general axion-like particles (ALPs), that may be emitted in the M1 nuclear transition of 57Fe, by using the axion-to-photon conversion in the CERN Axion Solar Telescope (CAST) with evacuated magnet bores (Phase I). From the absence of excess of the monoenergetic X-rays when the magnet was pointing to the Sun, we set model-independent constraints on the coupling constants of pseudoscalar particles that couple to two photons and to a nucleon g_{a纬} |-1.19 g_{aN}^{0}+g_{aN}^{3}|<1.36\times 10^{-16} GeV^{-1} for m_{a}<0.03 eV at the 95% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0906.4488v2-abstract-full').style.display = 'none'; document.getElementById('0906.4488v2-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 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 June, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2009. </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">23 pages, 5 figures. Revised version of the paper after referee`s comments. Main changes in the Measurement and data analysis section</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 0912:002,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0904.2103">arXiv:0904.2103</a> <span> [<a href="https://arxiv.org/pdf/0904.2103">pdf</a>, <a href="https://arxiv.org/ps/0904.2103">ps</a>, <a href="https://arxiv.org/format/0904.2103">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 class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2010/03/032">10.1088/1475-7516/2010/03/032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for solar axion emission from 7Li and D(p,gamma)3He nuclear decays with the CAST gamma-ray calorimeter </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=Andriamonje%2C+S">S. Andriamonje</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ex?searchtype=author&query=Autiero%2C+D">D. Autiero</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=Beltran%2C+B">B. Beltran</a>, <a href="/search/hep-ex?searchtype=author&query=Brauninger%2C+H">H. Brauninger</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=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</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=Lella%2C+L+D">L. Di. Lella</a>, <a href="/search/hep-ex?searchtype=author&query=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Englhauser%2C+J">J. Englhauser</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</a>, <a href="/search/hep-ex?searchtype=author&query=Ribas%2C+E+F">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=Franz%2C+J">J. Franz</a>, <a href="/search/hep-ex?searchtype=author&query=Friedrich%2C+P">P. Friedrich</a>, <a href="/search/hep-ex?searchtype=author&query=Geralis%2C+T">T. Geralis</a>, <a href="/search/hep-ex?searchtype=author&query=Giomataris%2C+I">I. Giomataris</a>, <a href="/search/hep-ex?searchtype=author&query=Gninenko%2C+S">S. Gninenko</a>, <a href="/search/hep-ex?searchtype=author&query=Gomez%2C+H">H. Gomez</a> , et al. (36 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="0904.2103v4-abstract-short" style="display: inline;"> We present the results of a search for a high-energy axion emission signal from 7Li (0.478 MeV) and D(p,gamma)3He (5.5 MeV) nuclear transitions using a low-background gamma-ray calorimeter during Phase I of the CAST experiment. These so-called "hadronic axions" could provide a solution to the long-standing strong-CP problem and can be emitted from the solar core from nuclear M1 transitions. This… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0904.2103v4-abstract-full').style.display = 'inline'; document.getElementById('0904.2103v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0904.2103v4-abstract-full" style="display: none;"> We present the results of a search for a high-energy axion emission signal from 7Li (0.478 MeV) and D(p,gamma)3He (5.5 MeV) nuclear transitions using a low-background gamma-ray calorimeter during Phase I of the CAST experiment. These so-called "hadronic axions" could provide a solution to the long-standing strong-CP problem and can be emitted from the solar core from nuclear M1 transitions. This is the first such search for high-energy pseudoscalar bosons with couplings to nucleons conducted using a helioscope approach. No excess signal above background was found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0904.2103v4-abstract-full').style.display = 'none'; document.getElementById('0904.2103v4-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> 6 March, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 April, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2009. </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">20 pages, 8 figures, final version to be published in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 1003:032,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0810.4482">arXiv:0810.4482</a> <span> [<a href="https://arxiv.org/pdf/0810.4482">pdf</a>, <a href="https://arxiv.org/ps/0810.4482">ps</a>, <a href="https://arxiv.org/format/0810.4482">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 class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2009/02/008">10.1088/1475-7516/2009/02/008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing eV-scale axions with CAST </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=Arik%2C+E">E. Arik</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ex?searchtype=author&query=Autiero%2C+D">D. Autiero</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=Beltr%C3%A1n%2C+B">B. Beltr谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Borghi%2C+S">S. Borghi</a>, <a href="/search/hep-ex?searchtype=author&query=Bourlis%2C+G">G. Bourlis</a>, <a href="/search/hep-ex?searchtype=author&query=Boydag%2C+F+S">F. S. Boydag</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=Carmona%2C+J+M">J. M. Carmona</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=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</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=Di+Lella%2C+L">L. Di Lella</a>, <a href="/search/hep-ex?searchtype=author&query=Dogan%2C+O+B">O. B. Dogan</a>, <a href="/search/hep-ex?searchtype=author&query=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Elias%2C+N">N. Elias</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Friedrich%2C+P">P. Friedrich</a> , et al. (48 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="0810.4482v2-abstract-short" style="display: inline;"> We have searched for solar axions or other pseudoscalar particles that couple to two photons by using the CERN Axion Solar Telescope (CAST) setup. Whereas we previously have reported results from CAST with evacuated magnet bores (Phase I), setting limits on lower mass axions, here we report results from CAST where the magnet bores were filled with \hefour gas (Phase II) of variable pressure. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0810.4482v2-abstract-full').style.display = 'inline'; document.getElementById('0810.4482v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0810.4482v2-abstract-full" style="display: none;"> We have searched for solar axions or other pseudoscalar particles that couple to two photons by using the CERN Axion Solar Telescope (CAST) setup. Whereas we previously have reported results from CAST with evacuated magnet bores (Phase I), setting limits on lower mass axions, here we report results from CAST where the magnet bores were filled with \hefour gas (Phase II) of variable pressure. The introduction of gas generated a refractive photon mass $m_纬$, thereby achieving the maximum possible conversion rate for those axion masses \ma that match $m_纬$. With 160 different pressure settings we have scanned \ma up to about 0.4 eV, taking approximately 2 h of data for each setting. From the absence of excess X-rays when the magnet was pointing to the Sun, we set a typical upper limit on the axion-photon coupling of $\gag\lesssim 2.17\times 10^{-10} {\rm GeV}^{-1}$ at 95% CL for $\ma \lesssim 0.4$ eV, the exact result depending on the pressure setting. The excluded parameter range covers realistic axion models with a Peccei-Quinn scale in the neighborhood of $f_{\rm a}\sim10^{7}$ GeV. Currently in the second part of CAST Phase II, we are searching for axions with masses up to about 1.2 eV using \hethree as a buffer gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0810.4482v2-abstract-full').style.display = 'none'; document.getElementById('0810.4482v2-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 January, 2009; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 October, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2008. </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, 7 figures. Revised version of the paper after referee's comments. Main changes on the gas section</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 0902:008,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0810.1874">arXiv:0810.1874</a> <span> [<a href="https://arxiv.org/pdf/0810.1874">pdf</a>, <a href="https://arxiv.org/ps/0810.1874">ps</a>, <a href="https://arxiv.org/format/0810.1874">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"> Solar axion search with the CAST experiment </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=Arik%2C+E">E. Arik</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ex?searchtype=author&query=Autiero%2C+D">D. Autiero</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=Beltr%C3%A1n%2C+B">B. Beltr谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Borghi%2C+S">S. Borghi</a>, <a href="/search/hep-ex?searchtype=author&query=Boydag%2C+F+S">F. S. Boydag</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=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/hep-ex?searchtype=author&query=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</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=Di+Lella%2C+L">L. Di Lella</a>, <a href="/search/hep-ex?searchtype=author&query=Dogan%2C+O+B">O. B. Dogan</a>, <a href="/search/hep-ex?searchtype=author&query=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Elias%2C+N">N. Elias</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Franz%2C+J">J. Franz</a>, <a href="/search/hep-ex?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a> , et al. (52 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="0810.1874v1-abstract-short" style="display: inline;"> The CAST (CERN Axion Solar Telescope) experiment is searching for solar axions by their conversion into photons inside the magnet pipe of an LHC dipole. The analysis of the data recorded during the first phase of the experiment with vacuum in the magnet pipes has resulted in the most restrictive experimental limit on the coupling constant of axions to photons. In the second phase, CAST is operat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0810.1874v1-abstract-full').style.display = 'inline'; document.getElementById('0810.1874v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0810.1874v1-abstract-full" style="display: none;"> The CAST (CERN Axion Solar Telescope) experiment is searching for solar axions by their conversion into photons inside the magnet pipe of an LHC dipole. The analysis of the data recorded during the first phase of the experiment with vacuum in the magnet pipes has resulted in the most restrictive experimental limit on the coupling constant of axions to photons. In the second phase, CAST is operating with a buffer gas inside the magnet pipes in order to extent the sensitivity of the experiment to higher axion masses. We will present the first results on the $^{4}{\rm He}$ data taking as well as the system upgrades that have been operated in the last year in order to adapt the experiment for the $^{3}{\rm He}$ data taking. Expected sensitivities on the coupling constant of axions to photons will be given for the recent $^{3}{\rm He}$ run just started in March 2008. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0810.1874v1-abstract-full').style.display = 'none'; document.getElementById('0810.1874v1-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 October, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2008. </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">Proceedings of the ICHEP 2008 conference</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0809.4581">arXiv:0809.4581</a> <span> [<a href="https://arxiv.org/pdf/0809.4581">pdf</a>, <a href="https://arxiv.org/ps/0809.4581">ps</a>, <a href="https://arxiv.org/format/0809.4581">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"> Search for low Energy solar Axions with CAST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Cantatore%2C+G">Giovanni Cantatore</a>, <a href="/search/hep-ex?searchtype=author&query=Arik%2C+E">E. Arik</a>, <a href="/search/hep-ex?searchtype=author&query=Aune%2C+S">S. Aune</a>, <a href="/search/hep-ex?searchtype=author&query=Autiero%2C+D">D. Autiero</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=Beltr%C3%A1n%2C+B">B. Beltr谩n</a>, <a href="/search/hep-ex?searchtype=author&query=Borghi%2C+S">S. Borghi</a>, <a href="/search/hep-ex?searchtype=author&query=Boydag%2C+F+S">F. S. Boydag</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=Carmona%2C+J+M">J. M. Carmona</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=Cetin%2C+S+A">S. A. Cetin</a>, <a href="/search/hep-ex?searchtype=author&query=Collar%2C+J+I">J. I. Collar</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=Di+Lella%2C+L">L. Di Lella</a>, <a href="/search/hep-ex?searchtype=author&query=Dogan%2C+O+B">O. B. Dogan</a>, <a href="/search/hep-ex?searchtype=author&query=Eleftheriadis%2C+C">C. Eleftheriadis</a>, <a href="/search/hep-ex?searchtype=author&query=Elias%2C+N">N. Elias</a>, <a href="/search/hep-ex?searchtype=author&query=Fanourakis%2C+G">G. Fanourakis</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=Franz%2C+J">J. Franz</a> , et al. (55 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="0809.4581v2-abstract-short" style="display: inline;"> We have started the development of a detector system, sensitive to single photons in the eV energy range, to be suitably coupled to one of the CAST magnet ports. This system should open to CAST a window on possible detection of low energy Axion Like Particles emitted by the sun. Preliminary tests have involved a cooled photomultiplier tube coupled to the CAST magnet via a Galileian telescope and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0809.4581v2-abstract-full').style.display = 'inline'; document.getElementById('0809.4581v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0809.4581v2-abstract-full" style="display: none;"> We have started the development of a detector system, sensitive to single photons in the eV energy range, to be suitably coupled to one of the CAST magnet ports. This system should open to CAST a window on possible detection of low energy Axion Like Particles emitted by the sun. Preliminary tests have involved a cooled photomultiplier tube coupled to the CAST magnet via a Galileian telescope and a switched 40 m long optical fiber. This system has reached the limit background level of the detector alone in ideal conditions, and two solar tracking runs have been performed with it at CAST. Such a measurement has never been done before with an axion helioscope. We will present results from these runs and briefly discuss future detector developments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0809.4581v2-abstract-full').style.display = 'none'; document.getElementById('0809.4581v2-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 September, 2008; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 September, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2008. </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">Paper submitted to the proceedings of the "4th Patras Workshop on Axions, WIMPs and WISPs", DESY, Hamburg Site - Germany, 18-21 June 2008. Author affiliations are reported on the title page of the paper. In version 2: 1 affiliation change, 3 references added</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ex/0403009">arXiv:hep-ex/0403009</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0403009">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0403009">ps</a>, <a href="https://arxiv.org/format/hep-ex/0403009">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 class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2004.04.002">10.1016/j.astropartphys.2004.04.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron background at the Canfranc Underground Laboratory and its contribution to the IGEX-DM dark matter experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/hep-ex?searchtype=author&query=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/hep-ex?searchtype=author&query=Garcia%2C+E">E. Garcia</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=Luzon%2C+G">G. Luzon</a>, <a href="/search/hep-ex?searchtype=author&query=Morales%2C+A">A. Morales</a>, <a href="/search/hep-ex?searchtype=author&query=Morales%2C+J">J. Morales</a>, <a href="/search/hep-ex?searchtype=author&query=de+Solorzano%2C+A+O">A. Ortiz de Solorzano</a>, <a href="/search/hep-ex?searchtype=author&query=Puimedon%2C+J">J. Puimedon</a>, <a href="/search/hep-ex?searchtype=author&query=Sarsa%2C+M+L">M. L. Sarsa</a>, <a href="/search/hep-ex?searchtype=author&query=Villar%2C+J+A">J. A. Villar</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="hep-ex/0403009v2-abstract-short" style="display: inline;"> A quantitative study of the neutron environment in the Canfranc Underground Laboratory has been performed. The analysis is based on a complete set of simulations and, particularly, it is focused on the IGEX-DM dark matter experiment. The simulations are compared to the IGEX-DM low energy data obtained with different shielding conditions. The results of the study allow us to conclude, with respec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0403009v2-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0403009v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0403009v2-abstract-full" style="display: none;"> A quantitative study of the neutron environment in the Canfranc Underground Laboratory has been performed. The analysis is based on a complete set of simulations and, particularly, it is focused on the IGEX-DM dark matter experiment. The simulations are compared to the IGEX-DM low energy data obtained with different shielding conditions. The results of the study allow us to conclude, with respect to the IGEX-DM background, that the main neutron population, coming from radioactivity from the surrounding rock, is practically eliminated after the implementation of a suitable neutron shielding. The remaining neutron background (muon-induced neutrons in the shielding and in the rock) is substantially below the present background level thanks to the muon veto system. In addition, the present analysis gives us a further insight on the effect of neutrons in other current and future experiments at the Canfranc Underground Laboratory. The comparison of simulations with the body of data available has allowed to set the flux of neutrons from radioactivity of the Canfranc rock, (3.82 +- 0.44) x 10^{-6} cm^{-2} s^{-1}, as well as the flux of muon-induced neutrons in the rock, (1.73 +- 0.22(stat) \+- 0.69(syst)) x 10^{-9} cm^{-2} s^{-1}, or the rate of neutron production by muons in the lead shielding, (4.8 +- 0.6 (stat) +- 1.9 (syst)) x 10^{-9} cm^{-3} s^{-1}. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0403009v2-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0403009v2-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> 7 April, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 March, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2004. </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">17 pages, 8 figures, elsart document class; final version to appear in Astroparticle Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart.Phys.21:523-533,2004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ex/0211050">arXiv:hep-ex/0211050</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0211050">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0211050">ps</a>, <a href="https://arxiv.org/format/hep-ex/0211050">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 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/S0920-5632(02)01898-4">10.1016/S0920-5632(02)01898-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Status of the ANAIS experiment at Canfranc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/hep-ex?searchtype=author&query=Amare%2C+J">J. Amare</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=Garcia%2C+E">E. Garcia</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=Luzon%2C+G">G. Luzon</a>, <a href="/search/hep-ex?searchtype=author&query=Morales%2C+A">A. Morales</a>, <a href="/search/hep-ex?searchtype=author&query=Morales%2C+J">J. Morales</a>, <a href="/search/hep-ex?searchtype=author&query=de+Solorzano%2C+A+O">A. Ortiz de Solorzano</a>, <a href="/search/hep-ex?searchtype=author&query=Puimedon%2C+J">J. Puimedon</a>, <a href="/search/hep-ex?searchtype=author&query=Sarsa%2C+M+L">M. L. Sarsa</a>, <a href="/search/hep-ex?searchtype=author&query=Villar%2C+J+A">J. A. Villar</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="hep-ex/0211050v1-abstract-short" style="display: inline;"> The present status of the ANAIS experiment (Annual Modulation with NaI's) is shown. ANAIS is intended to use more than 100 kg of NaI(Tl) in the Canfranc Underground Laboratory (Spain) searching for seasonal modulation effects in the WIMP signal; in a first stage, a prototype (one single 10.7 kg crystal) has been developed in order to obtain the best conditions regarding the energy threshold and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0211050v1-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0211050v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0211050v1-abstract-full" style="display: none;"> The present status of the ANAIS experiment (Annual Modulation with NaI's) is shown. ANAIS is intended to use more than 100 kg of NaI(Tl) in the Canfranc Underground Laboratory (Spain) searching for seasonal modulation effects in the WIMP signal; in a first stage, a prototype (one single 10.7 kg crystal) has been developed in order to obtain the best conditions regarding the energy threshold and the radioactive background in the low energy region as well as to check the stability of the environmental conditions. The first results corresponding to an exposure of 2069.85 kg day show an average background level of 1.2 counts/(keV kg day) from threshold ($E_{thr} \sim 4$ keV, even using one single photomultiplier) up to 10 keV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0211050v1-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0211050v1-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 November, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2002. </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">5 pages, 4 figures, Submitted contribution XXX International Meeting on Fundamental Physics, IMFP2002, February 2002, Jaca, Spain. To appear in Nucl. Phys. B (Proc. Suppl)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Phys.Proc.Suppl. 114 (2003) 111-115 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0211535">arXiv:astro-ph/0211535</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0211535">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0211535">ps</a>, <a href="https://arxiv.org/format/astro-ph/0211535">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1142/9789812791313_0043">10.1142/9789812791313_0043 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Status of IGEX dark matter search at Canfranc Underground Laboratory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/hep-ex?searchtype=author&query=Morales%2C+A">A. Morales</a>, <a href="/search/hep-ex?searchtype=author&query=Aalseth%2C+C+E">C. E. Aalseth</a>, <a href="/search/hep-ex?searchtype=author&query=Avignone%2C+F+T">F. T. Avignone III</a>, <a href="/search/hep-ex?searchtype=author&query=Brodzinski%2C+R+L">R. L. Brodzinski</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=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/hep-ex?searchtype=author&query=Garcia%2C+E">E. Garcia</a>, <a href="/search/hep-ex?searchtype=author&query=Kirpichnikov%2C+I+V">I. V. Kirpichnikov</a>, <a href="/search/hep-ex?searchtype=author&query=Klimenko%2C+A+A">A. A. Klimenko</a>, <a href="/search/hep-ex?searchtype=author&query=Luzon%2C+G">G. Luzon</a>, <a href="/search/hep-ex?searchtype=author&query=Miley%2C+H+S">H. S. Miley</a>, <a href="/search/hep-ex?searchtype=author&query=Morales%2C+J">J. Morales</a>, <a href="/search/hep-ex?searchtype=author&query=de+Solorzano%2C+A+O">A. Ortiz de Solorzano</a>, <a href="/search/hep-ex?searchtype=author&query=Osetrov%2C+S+B">S. B. Osetrov</a>, <a href="/search/hep-ex?searchtype=author&query=Pogosov%2C+V+S">V. S. Pogosov</a>, <a href="/search/hep-ex?searchtype=author&query=Puimedon%2C+J">J. Puimedon</a>, <a href="/search/hep-ex?searchtype=author&query=Reeves%2C+J+H">J. H. Reeves</a>, <a href="/search/hep-ex?searchtype=author&query=Sarsa%2C+M+L">M. L. Sarsa</a>, <a href="/search/hep-ex?searchtype=author&query=Smolnikov%2C+A+A">A. A. Smolnikov</a>, <a href="/search/hep-ex?searchtype=author&query=Tamanyan%2C+A+G">A. G. Tamanyan</a>, <a href="/search/hep-ex?searchtype=author&query=Vasenko%2C+A+A">A. A. Vasenko</a>, <a href="/search/hep-ex?searchtype=author&query=Vasiliev%2C+S+I">S. I. Vasiliev</a>, <a href="/search/hep-ex?searchtype=author&query=Villar%2C+J+A">J. A. Villar</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="astro-ph/0211535v1-abstract-short" style="display: inline;"> One IGEX 76Ge double-beta decay detector is currently operating in the Canfranc Underground Laboratory in a search for dark matter WIMPs, through the Ge nuclear recoil produced by the WIMP elastic scattering. In this talk we report on the on-going efforts to understand and eventually reject the background at low energy. These efforts have led to the improvement of the neutron shielding and to pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0211535v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0211535v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0211535v1-abstract-full" style="display: none;"> One IGEX 76Ge double-beta decay detector is currently operating in the Canfranc Underground Laboratory in a search for dark matter WIMPs, through the Ge nuclear recoil produced by the WIMP elastic scattering. In this talk we report on the on-going efforts to understand and eventually reject the background at low energy. These efforts have led to the improvement of the neutron shielding and to partial reduction of the background, but still the remaining events are not totally identified. A tritium contamination or muon-induced neutrons are considered as possible sources, simulations and experimental test being still under progress. According to the success of this study we comment the prospects of the experiment as well as those of its future extension, the GEDEON dark matter experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0211535v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0211535v1-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> 25 November, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2002. </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">6 pages, 3 figures, talk given at 4th International Workshop on the Identification of Dark Matter, York, September 2002</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ex/0111075">arXiv:hep-ex/0111075</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/0111075">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/0111075">ps</a>, <a href="https://arxiv.org/format/hep-ex/0111075">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 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/S0920-5632(02)01462-7">10.1016/S0920-5632(02)01462-7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Status and preliminary results of the ANAIS experiment at Canfranc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/hep-ex?searchtype=author&query=Amare%2C+J">J. Amare</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=Garcia%2C+E">E. Garcia</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=Luzon%2C+G">G. Luzon</a>, <a href="/search/hep-ex?searchtype=author&query=Morales%2C+A">A. Morales</a>, <a href="/search/hep-ex?searchtype=author&query=Morales%2C+J">J. Morales</a>, <a href="/search/hep-ex?searchtype=author&query=de+Solorzano%2C+A+O">A. Ortiz de Solorzano</a>, <a href="/search/hep-ex?searchtype=author&query=Puimedon%2C+J">J. Puimedon</a>, <a href="/search/hep-ex?searchtype=author&query=Sarsa%2C+M+L">M. L. Sarsa</a>, <a href="/search/hep-ex?searchtype=author&query=Villar%2C+J+A">J. A. Villar</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="hep-ex/0111075v1-abstract-short" style="display: inline;"> ANAIS (Annual Modulation with NaI's) is an experiment planned to investigate seasonal modulation effects in the signal of galactic WIMPs using up to 107 kg of NaI(Tl) in the Canfranc Underground Laboratory (Spain). A prototype using one single crystal (10.7 kg) is being developed before the installation of the complete experiment; the first results presented here show an average background level… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0111075v1-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/0111075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/0111075v1-abstract-full" style="display: none;"> ANAIS (Annual Modulation with NaI's) is an experiment planned to investigate seasonal modulation effects in the signal of galactic WIMPs using up to 107 kg of NaI(Tl) in the Canfranc Underground Laboratory (Spain). A prototype using one single crystal (10.7 kg) is being developed before the installation of the complete experiment; the first results presented here show an average background level of 1.2 counts/(keV kg day) from threshold (Ethr~4 keV) up to 10 keV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/0111075v1-abstract-full').style.display = 'none'; document.getElementById('hep-ex/0111075v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 November, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2001. </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, 2 figures, talk delivered at the 7th International Workshop on Topics in Astroparticle and Underground Physics (TAUP 2001), September 2001, Laboratori Nazionali del Gran Sasso, Italy (to appear in the Conference Proceedings, Nucl. Phys. B (Proc. Suppl.))</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Phys.Proc.Suppl. 110 (2002) 94-96 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ph/0007057">arXiv:hep-ph/0007057</a> <span> [<a href="https://arxiv.org/pdf/hep-ph/0007057">pdf</a>, <a href="https://arxiv.org/ps/hep-ph/0007057">ps</a>, <a href="https://arxiv.org/format/hep-ph/0007057">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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 - Theory">hep-th</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/S0370-2693(00)01182-5">10.1016/S0370-2693(00)01182-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing Lorentz invariance violations in the tritium beta-decay anomaly </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Carmona%2C+J+M">J. M. Carmona</a>, <a href="/search/hep-ex?searchtype=author&query=Cortes%2C+J+L">J. L. Cortes</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="hep-ph/0007057v2-abstract-short" style="display: inline;"> We consider a Lorentz non-invariant dispersion relation for the neutrino, which would produce unexpected effects with neutrinos of few eV, exactly where the tritium beta-decay anomaly is found. We use this anomaly to put bounds on the violation of Lorentz invariance. We discuss other consequences of this non-invariant dispersion relation in neutrino experiments and high-energy cosmic-ray physics… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ph/0007057v2-abstract-full').style.display = 'inline'; document.getElementById('hep-ph/0007057v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ph/0007057v2-abstract-full" style="display: none;"> We consider a Lorentz non-invariant dispersion relation for the neutrino, which would produce unexpected effects with neutrinos of few eV, exactly where the tritium beta-decay anomaly is found. We use this anomaly to put bounds on the violation of Lorentz invariance. We discuss other consequences of this non-invariant dispersion relation in neutrino experiments and high-energy cosmic-ray physics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ph/0007057v2-abstract-full').style.display = 'none'; document.getElementById('hep-ph/0007057v2-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 October, 2000; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 July, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2000. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 2 figures, elsart style. Some references added. Final version to appear in Physics Letters B</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DFTUZ 00/05 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett. B494 (2000) 75-80 </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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