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<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/2410.07257">arXiv:2410.07257</a> <span> [<a href="https://arxiv.org/pdf/2410.07257">pdf</a>, <a href="https://arxiv.org/ps/2410.07257">ps</a>, <a href="https://arxiv.org/format/2410.07257">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/10.3389/fdest.2024.1438902">10.3389/fdest.2024.1438902 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The muon beam monitor for the FAMU experiment: design, simulation, test and operation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Rossini%2C+R">R. Rossini</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Banfi%2C+S">S. Banfi</a>, <a href="/search/physics?searchtype=author&query=Baruzzo%2C+M">M. Baruzzo</a>, <a href="/search/physics?searchtype=author&query=Benocci%2C+R">R. Benocci</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Carsi%2C+S">S. Carsi</a>, <a href="/search/physics?searchtype=author&query=Cirrincione%2C+D">D. Cirrincione</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Colace%2C+L">L. Colace</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=de+Vecchi%2C+C">C. de Vecchi</a>, <a href="/search/physics?searchtype=author&query=Fasci%2C+E">E. Fasci</a>, <a href="/search/physics?searchtype=author&query=Gaigher%2C+R">R. Gaigher</a>, <a href="/search/physics?searchtype=author&query=Gianfrani%2C+L">L. Gianfrani</a>, <a href="/search/physics?searchtype=author&query=Hillier%2C+A+D">A. D. Hillier</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+K">K. Ishida</a>, <a href="/search/physics?searchtype=author&query=King%2C+P+J+C">P. J. C. King</a>, <a href="/search/physics?searchtype=author&query=Lord%2C+J+S">J. S. Lord</a>, <a href="/search/physics?searchtype=author&query=Mazza%2C+R">R. Mazza</a>, <a href="/search/physics?searchtype=author&query=Menegolli%2C+A">A. Menegolli</a>, <a href="/search/physics?searchtype=author&query=Mocchiutti%2C+E">E. Mocchiutti</a>, <a href="/search/physics?searchtype=author&query=Monzani%2C+S">S. Monzani</a>, <a href="/search/physics?searchtype=author&query=Moretti%2C+L">L. Moretti</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.07257v1-abstract-short" style="display: inline;"> FAMU is an INFN-led muonic atom physics experiment based at the RIKEN-RAL muon facility at the ISIS Neutron and Muon Source (United Kingdom). The aim of FAMU is to measure the hyperfine splitting in muonic hydrogen to determine the value of the proton Zemach radius with accuracy better than 1%.The experiment has a scintillating-fibre hodoscope for beam monitoring and data normalisation. In order t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07257v1-abstract-full').style.display = 'inline'; document.getElementById('2410.07257v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.07257v1-abstract-full" style="display: none;"> FAMU is an INFN-led muonic atom physics experiment based at the RIKEN-RAL muon facility at the ISIS Neutron and Muon Source (United Kingdom). The aim of FAMU is to measure the hyperfine splitting in muonic hydrogen to determine the value of the proton Zemach radius with accuracy better than 1%.The experiment has a scintillating-fibre hodoscope for beam monitoring and data normalisation. In order to carry out muon flux estimation, low-rate measurements were performed to extract the single-muon average deposited charge. Then, detector simulation in Geant4 and FLUKA allowed a thorough understanding of the single-muon response function, crucial for determining the muon flux. This work presents the design features of the FAMU beam monitor, along with the simulation and absolute calibration measurements in order to enable flux determination and enable data normalisation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07257v1-abstract-full').style.display = 'none'; document.getElementById('2410.07257v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Front. Detect. Sci. Technol., 05 August 2024 Volume 2 - 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.05145">arXiv:2403.05145</a> <span> [<a href="https://arxiv.org/pdf/2403.05145">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1080/10619127.2023.2198913">10.1080/10619127.2023.2198913 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating the Proton Structure: The FAMU experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">A. Adamczak</a>, <a href="/search/physics?searchtype=author&query=Bakalov%2C+D">D. Bakalov</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Baruzzo%2C+M">M. Baruzzo</a>, <a href="/search/physics?searchtype=author&query=Benocci%2C+R">R. Benocci</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+H">H. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Carsi%2C+S">S. Carsi</a>, <a href="/search/physics?searchtype=author&query=Cirrincione%2C+D">D. Cirrincione</a>, <a href="/search/physics?searchtype=author&query=Chignoli%2C+F">F. Chignoli</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Colace%2C+L">L. Colace</a>, <a href="/search/physics?searchtype=author&query=Danailov%2C+M">M. Danailov</a>, <a href="/search/physics?searchtype=author&query=Danev%2C+P">P. Danev</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=De+Vecchi%2C+C">C. De Vecchi</a>, <a href="/search/physics?searchtype=author&query=De+Vincenzi%2C+M">M. De Vincenzi</a>, <a href="/search/physics?searchtype=author&query=Fasci%2C+E">E. Fasci</a>, <a href="/search/physics?searchtype=author&query=Gadedjisso-Tossou%2C+K+S">K. S. Gadedjisso-Tossou</a>, <a href="/search/physics?searchtype=author&query=Gianfrani%2C+L">L. Gianfrani</a>, <a href="/search/physics?searchtype=author&query=Hillier%2C+A+D">A. D. Hillier</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+K">K. Ishida</a>, <a href="/search/physics?searchtype=author&query=King%2C+P+J+C">P. J. C. King</a> , et al. (24 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="2403.05145v1-abstract-short" style="display: inline;"> The article gives the motivations for the measurement of the hyperfine splitting (hfs) in the ground state of muonic hydrogen to explore the properties of the proton at low momentum transfer. It summarizes these proposed measurement methods and finally describes the FAMU experiment in more detail. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.05145v1-abstract-full" style="display: none;"> The article gives the motivations for the measurement of the hyperfine splitting (hfs) in the ground state of muonic hydrogen to explore the properties of the proton at low momentum transfer. It summarizes these proposed measurement methods and finally describes the FAMU experiment in more detail. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05145v1-abstract-full').style.display = 'none'; document.getElementById('2403.05145v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Physics News 33:4, 9-16, 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.02900">arXiv:2401.02900</a> <span> [<a href="https://arxiv.org/pdf/2401.02900">pdf</a>, <a href="https://arxiv.org/format/2401.02900">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 Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2023.168825">10.1016/j.nima.2023.168825 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New detailed characterization of the residual luminescence emitted by the GAGG:Ce scintillator crystals for the HERMES Pathfinder mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Della+Casa%2C+G">Giovanni Della Casa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">Nicola Zampa</a>, <a href="/search/physics?searchtype=author&query=Cirrincione%2C+D">Daniela Cirrincione</a>, <a href="/search/physics?searchtype=author&query=Monzani%2C+S">Simone Monzani</a>, <a href="/search/physics?searchtype=author&query=Baruzzo%2C+M">Marco Baruzzo</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+R">Riccardo Campana</a>, <a href="/search/physics?searchtype=author&query=Cauz%2C+D">Diego Cauz</a>, <a href="/search/physics?searchtype=author&query=Citossi%2C+M">Marco Citossi</a>, <a href="/search/physics?searchtype=author&query=Crupi%2C+R">Riccardo Crupi</a>, <a href="/search/physics?searchtype=author&query=Dilillo%2C+G">Giuseppe Dilillo</a>, <a href="/search/physics?searchtype=author&query=Pauletta%2C+G">Giovanni Pauletta</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+F">Fabrizio Fiore</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">Andrea Vacchi</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="2401.02900v1-abstract-short" style="display: inline;"> The HERMES (High Energy Rapid Modular Ensemble of Satellites) Pathfinder mission aims to develop a constellation of nanosatellites to study astronomical transient sources, such as gamma-ray bursts, in the X and soft $纬$ energy range, exploiting a novel inorganic scintillator. This study presents the results obtained describing, with an empirical model, the unusually intense and long-lasting residu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02900v1-abstract-full').style.display = 'inline'; document.getElementById('2401.02900v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.02900v1-abstract-full" style="display: none;"> The HERMES (High Energy Rapid Modular Ensemble of Satellites) Pathfinder mission aims to develop a constellation of nanosatellites to study astronomical transient sources, such as gamma-ray bursts, in the X and soft $纬$ energy range, exploiting a novel inorganic scintillator. This study presents the results obtained describing, with an empirical model, the unusually intense and long-lasting residual emission of the GAGG:Ce scintillating crystal after irradiating it with high energy protons (70 MeV) and ultraviolet light ($\sim$ 300 nm). From the model so derived, the consequences of this residual luminescence for the detector performance in operational conditions has been analyzed. It was demonstrated that the current generated by the residual emission peaks at 1-2 pA, thus ascertaining the complete compatibility of this detector with the HERMES Pathfinder nanosatellites. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02900v1-abstract-full').style.display = 'none'; document.getElementById('2401.02900v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Instrum.MethA, 1058 (2024) 168825 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.04987">arXiv:2312.04987</a> <span> [<a href="https://arxiv.org/pdf/2312.04987">pdf</a>, <a href="https://arxiv.org/format/2312.04987">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-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/10.1088/1748-0221/19/02/C02034">10.1088/1748-0221/19/02/C02034 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Status of the detector setup for the FAMU experiment at RIKEN-RAL for a precision measurement of the Zemach radius of the proton in muonic hydrogen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Rossini%2C+R">R. Rossini</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">A. Adamczak</a>, <a href="/search/physics?searchtype=author&query=Bakalov%2C+D">D. Bakalov</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Banfi%2C+S">S. Banfi</a>, <a href="/search/physics?searchtype=author&query=Baruzzo%2C+M">M. Baruzzo</a>, <a href="/search/physics?searchtype=author&query=Benocci%2C+R">R. Benocci</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+H">H. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Carsi%2C+S">S. Carsi</a>, <a href="/search/physics?searchtype=author&query=Cirrincione%2C+D">D. Cirrincione</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Colace%2C+L">L. Colace</a>, <a href="/search/physics?searchtype=author&query=Danailov%2C+M+B">M. B. Danailov</a>, <a href="/search/physics?searchtype=author&query=Danev%2C+P">P. Danev</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=de+Vecchi%2C+C">C. de Vecchi</a>, <a href="/search/physics?searchtype=author&query=Fasci%2C+E">E. Fasci</a>, <a href="/search/physics?searchtype=author&query=Gadedjisso-Tossou%2C+K+S">K. S. Gadedjisso-Tossou</a>, <a href="/search/physics?searchtype=author&query=Gaigher%2C+R">R. Gaigher</a>, <a href="/search/physics?searchtype=author&query=Gianfrani%2C+L">L. Gianfrani</a>, <a href="/search/physics?searchtype=author&query=Hillier%2C+A+D">A. D. Hillier</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+K">K. Ishida</a> , et al. (24 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="2312.04987v1-abstract-short" style="display: inline;"> The FAMU experiment at RIKEN-RAL is a muonic atom experiment with the aim to determine the Zemach radius of the proton by measuring the 1s hyperfine splitting in muonic hydrogen. The activity of the FAMU Collaboration in the years 2015-2023 enabled the final optimisation of the detector-target setup as well as the gas working condition in terms of temperature, pressure and gas mixture composition.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.04987v1-abstract-full').style.display = 'inline'; document.getElementById('2312.04987v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.04987v1-abstract-full" style="display: none;"> The FAMU experiment at RIKEN-RAL is a muonic atom experiment with the aim to determine the Zemach radius of the proton by measuring the 1s hyperfine splitting in muonic hydrogen. The activity of the FAMU Collaboration in the years 2015-2023 enabled the final optimisation of the detector-target setup as well as the gas working condition in terms of temperature, pressure and gas mixture composition. The experiment has started its data taking in July 2023. The status of the detector setup for the 2023 experimental runs, for the beam characterisation and muonic X-ray detection in the 100-200 keV energy range, is presented and discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.04987v1-abstract-full').style.display = 'none'; document.getElementById('2312.04987v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2303.15575">arXiv:2303.15575</a> <span> [<a href="https://arxiv.org/pdf/2303.15575">pdf</a>, <a href="https://arxiv.org/ps/2303.15575">ps</a>, <a href="https://arxiv.org/format/2303.15575">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevA.107.032823">10.1103/PhysRevA.107.032823 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental determination of the energy dependence of the rate of the muon transfer reaction from muonic hydrogen to oxygen for collision energies up to 0.1 eV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Stoilov%2C+M">M. Stoilov</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">A. Adamczak</a>, <a href="/search/physics?searchtype=author&query=Bakalov%2C+D">D. Bakalov</a>, <a href="/search/physics?searchtype=author&query=Danev%2C+P">P. Danev</a>, <a href="/search/physics?searchtype=author&query=Mocchiutti%2C+E">E. Mocchiutti</a>, <a href="/search/physics?searchtype=author&query=Pizzolotto%2C+C">C. Pizzolotto</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Baruzzo%2C+M">M. Baruzzo</a>, <a href="/search/physics?searchtype=author&query=Benocci%2C+R">R. Benocci</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Cirrincione%2C+D">D. Cirrincione</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Fuschino%2C+F">F. Fuschino</a>, <a href="/search/physics?searchtype=author&query=Hillier%2C+A+D">A. D. Hillier</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+K">K. Ishida</a>, <a href="/search/physics?searchtype=author&query=King%2C+P+J+C">P. J. C. King</a>, <a href="/search/physics?searchtype=author&query=Menegolli%2C+A">A. Menegolli</a>, <a href="/search/physics?searchtype=author&query=Monzani%2C+S">S. Monzani</a>, <a href="/search/physics?searchtype=author&query=Ramponi%2C+R">R. Ramponi</a>, <a href="/search/physics?searchtype=author&query=Rignanese%2C+L+P">L. P. Rignanese</a>, <a href="/search/physics?searchtype=author&query=Sarkar%2C+R">R. Sarkar</a>, <a href="/search/physics?searchtype=author&query=Sbrizzi%2C+A">A. Sbrizzi</a>, <a href="/search/physics?searchtype=author&query=Tortora%2C+L">L. Tortora</a>, <a href="/search/physics?searchtype=author&query=Vallazza%2C+E">E. Vallazza</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</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="2303.15575v1-abstract-short" style="display: inline;"> We report the first experimental determination of the collision-energy dependence of the muon transfer rate from the ground state of muonic hydrogen to oxygen at near-thermal energies. A sharp increase by nearly an order of magnitude in the energy range 0 - 70 meV was found that is not observed in other gases. The results set a reliable reference for quantum-mechanical calculations of low-energy p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15575v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15575v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15575v1-abstract-full" style="display: none;"> We report the first experimental determination of the collision-energy dependence of the muon transfer rate from the ground state of muonic hydrogen to oxygen at near-thermal energies. A sharp increase by nearly an order of magnitude in the energy range 0 - 70 meV was found that is not observed in other gases. The results set a reliable reference for quantum-mechanical calculations of low-energy processes with exotic atoms, and provide firm ground for the measurement of the hyperfine splitting in muonic hydrogen and the determination of the Zemach radius of the proton by the FAMU collaboration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15575v1-abstract-full').style.display = 'none'; document.getElementById('2303.15575v1-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> 27 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. A 107, 032823, 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.01698">arXiv:2201.01698</a> <span> [<a href="https://arxiv.org/pdf/2201.01698">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and 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/10.1109/TNS.2015.2513602">10.1109/TNS.2015.2513602 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-Ray Silicon Drift Detector-CMOS Front-End System with High Energy Resolution at Room Temperature </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bertuccio%2C+G">G. Bertuccio</a>, <a href="/search/physics?searchtype=author&query=Ahangarianabhari%2C+M">M. Ahangarianabhari</a>, <a href="/search/physics?searchtype=author&query=Graziani%2C+C">C. Graziani</a>, <a href="/search/physics?searchtype=author&query=Macera%2C+D">D. Macera</a>, <a href="/search/physics?searchtype=author&query=Shi%2C+Y">Y. Shi</a>, <a href="/search/physics?searchtype=author&query=Gandola%2C+M">M. Gandola</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Rashevskaya%2C+I">I. Rashevskaya</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/physics?searchtype=author&query=Bellutti%2C+P">P. Bellutti</a>, <a href="/search/physics?searchtype=author&query=Giacomini%2C+G">G. Giacomini</a>, <a href="/search/physics?searchtype=author&query=Picciotto%2C+A">A. Picciotto</a>, <a href="/search/physics?searchtype=author&query=Piemonte%2C+C">C. Piemonte</a>, <a href="/search/physics?searchtype=author&query=Zorzi%2C+N">N. Zorzi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.01698v1-abstract-short" style="display: inline;"> We present a spectroscopic system constituted by a Silicon Drift Detector (SDD) coupled to a CMOS charge sensitive preamplifier, named SIRIO, specifically designed to reach ultimate low noise levels. The SDD, with an active area of 13 mm , has been manufactured by optimizing the production processes in order to reduce the anode current, successfully reaching current densities between 17 pA/cm and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01698v1-abstract-full').style.display = 'inline'; document.getElementById('2201.01698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.01698v1-abstract-full" style="display: none;"> We present a spectroscopic system constituted by a Silicon Drift Detector (SDD) coupled to a CMOS charge sensitive preamplifier, named SIRIO, specifically designed to reach ultimate low noise levels. The SDD, with an active area of 13 mm , has been manufactured by optimizing the production processes in order to reduce the anode current, successfully reaching current densities between 17 pA/cm and 25 pA/cm at 20 for drift fields ranging from 100 V/cm to 500 V/cm. The preamplifier shows minimum intrinsic noise levels of 1.27 and 1.0 electrons r.m.s. at 20 and 30 , respectively. At room temperature ( ) the 5.9 keV and the pulser lines have 136 eV and 64 eV FWHM, respectively, corresponding to an equivalent noise charge of 7.4 electrons r.m.s.; the noise threshold is at 165 eV. The energy resolution, as measured on the pulser line, ranges from 82 eV FWHM (9.4 electrons r.m.s.) at 30C down to 29 eV FWHM (3.3 electrons r.m.s.) at 30C . <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01698v1-abstract-full').style.display = 'none'; document.getElementById('2201.01698v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> IEEE TRANSACTIONS ON NUCLEAR SCIENCE, VOL. 63, NO. 1, FEBRUARY 2016, pp. 400-406 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.02897">arXiv:2112.02897</a> <span> [<a href="https://arxiv.org/pdf/2112.02897">pdf</a>, <a href="https://arxiv.org/format/2112.02897">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 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/10.1016/j.nimb.2021.12.006">10.1016/j.nimb.2021.12.006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Space applications of GAGG:Ce scintillators: a study of afterglow emission by proton irradiation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Dilillo%2C+G">Giuseppe Dilillo</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">Nicola Zampa</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+R">Riccardo Campana</a>, <a href="/search/physics?searchtype=author&query=Fuschino%2C+F">Fabio Fuschino</a>, <a href="/search/physics?searchtype=author&query=Pauletta%2C+G">Giovanni Pauletta</a>, <a href="/search/physics?searchtype=author&query=Rashevskaya%2C+I">Irina Rashevskaya</a>, <a href="/search/physics?searchtype=author&query=Ambrosino%2C+F">Filippo Ambrosino</a>, <a href="/search/physics?searchtype=author&query=Baruzzo%2C+M">Marco Baruzzo</a>, <a href="/search/physics?searchtype=author&query=Cauz%2C+D">Diego Cauz</a>, <a href="/search/physics?searchtype=author&query=Cirrincione%2C+D">Daniela Cirrincione</a>, <a href="/search/physics?searchtype=author&query=Citossi%2C+M">Marco Citossi</a>, <a href="/search/physics?searchtype=author&query=Della+Casa%2C+G">Giovanni Della Casa</a>, <a href="/search/physics?searchtype=author&query=Di+Ruzza%2C+B">Benedetto Di Ruzza</a>, <a href="/search/physics?searchtype=author&query=Evangelista%2C+Y">Yuri Evangelista</a>, <a href="/search/physics?searchtype=author&query=Galg%C3%B3czi%2C+G">G谩bor Galg贸czi</a>, <a href="/search/physics?searchtype=author&query=Labanti%2C+C">Claudio Labanti</a>, <a href="/search/physics?searchtype=author&query=Ripa%2C+J">Jakub Ripa</a>, <a href="/search/physics?searchtype=author&query=Tommasino%2C+F">Francesco Tommasino</a>, <a href="/search/physics?searchtype=author&query=Verroi%2C+E">Enrico Verroi</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+F">Fabrizio Fiore</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">Andrea Vacchi</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="2112.02897v3-abstract-short" style="display: inline;"> We discuss the results of a proton irradiation campaign of a GAGG:Ce (Cerium-doped Gadolinium Aluminium Gallium Garnet) scintillation crystal, carried out in the framework of the HERMES-TP/SP (High Energy Rapid Modular Ensemble of Satellites -- Technological and Scientific Pathfinder) mission. A scintillator sample was irradiated with 70 MeV protons, at levels equivalent to those expected in equat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02897v3-abstract-full').style.display = 'inline'; document.getElementById('2112.02897v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.02897v3-abstract-full" style="display: none;"> We discuss the results of a proton irradiation campaign of a GAGG:Ce (Cerium-doped Gadolinium Aluminium Gallium Garnet) scintillation crystal, carried out in the framework of the HERMES-TP/SP (High Energy Rapid Modular Ensemble of Satellites -- Technological and Scientific Pathfinder) mission. A scintillator sample was irradiated with 70 MeV protons, at levels equivalent to those expected in equatorial and sun-synchronous low-Earth orbits over orbital periods spanning 6 months to 10 years. The data we acquired are used to introduce an original model of GAGG:Ce afterglow emission. Results from this model are applied to the HERMES-TP/SP scenario, aiming at an upper-bound estimate of the detector performance degradation resulting from afterglow emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02897v3-abstract-full').style.display = 'none'; document.getElementById('2112.02897v3-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Instrum.Meth.B 513 (2022): 33-43 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.06407">arXiv:2108.06407</a> <span> [<a href="https://arxiv.org/pdf/2108.06407">pdf</a>, <a href="https://arxiv.org/ps/2108.06407">ps</a>, <a href="https://arxiv.org/format/2108.06407">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac1a74">10.3847/2041-8213/ac1a74 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solar-Cycle Variations of South-Atlantic Anomaly Proton Intensities Measured With The PAMELA Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Martucci%2C+M">M. Martucci</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F+S">F. S. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Sparvoli%2C+R">R. Sparvoli</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Kvashnin%2C+A+N">A. N. Kvashnin</a>, <a href="/search/physics?searchtype=author&query=Lenni%2C+A">A. Lenni</a>, <a href="/search/physics?searchtype=author&query=Leonov%2C+A+A">A. A. Leonov</a>, <a href="/search/physics?searchtype=author&query=Malakhov%2C+V+V">V. V. Malakhov</a>, <a href="/search/physics?searchtype=author&query=Marcelli%2C+L">L. Marcelli</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="2108.06407v1-abstract-short" style="display: inline;"> We present a study of the solar-cycle variations of >80 MeV proton flux intensities in the lower edge of the inner radiation belt, based on the measurements of the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) mission. The analyzed data sample covers an ~8 year interval from 2006 July to 2014 September, thus spanning from the decaying phase of the 23rd solar cycl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.06407v1-abstract-full').style.display = 'inline'; document.getElementById('2108.06407v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.06407v1-abstract-full" style="display: none;"> We present a study of the solar-cycle variations of >80 MeV proton flux intensities in the lower edge of the inner radiation belt, based on the measurements of the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) mission. The analyzed data sample covers an ~8 year interval from 2006 July to 2014 September, thus spanning from the decaying phase of the 23rd solar cycle to the maximum of the 24th cycle. We explored the intensity temporal variations as a function of drift shell and proton energy, also providing an explicit investigation of the solar-modulation effects at different equatorial pitch angles. PAMELA observations offer new important constraints for the modeling of low-altitude particle radiation environment at the highest trapping energies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.06407v1-abstract-full').style.display = 'none'; document.getElementById('2108.06407v1-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in the Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.06701">arXiv:2105.06701</a> <span> [<a href="https://arxiv.org/pdf/2105.06701">pdf</a>, <a href="https://arxiv.org/format/2105.06701">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physleta.2021.127401">10.1016/j.physleta.2021.127401 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the muon transfer rate from muonic hydrogen to oxygen in the range 70-336 K </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Pizzolotto%2C+C">C. Pizzolotto</a>, <a href="/search/physics?searchtype=author&query=Sbrizzi%2C+A">A. Sbrizzi</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">A. Adamczak</a>, <a href="/search/physics?searchtype=author&query=Bakalov%2C+D">D. Bakalov</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Baruzzo%2C+M">M. Baruzzo</a>, <a href="/search/physics?searchtype=author&query=Benocci%2C+R">R. Benocci</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Cabrera%2C+H">H. Cabrera</a>, <a href="/search/physics?searchtype=author&query=Cirrincione%2C+D">D. Cirrincione</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Colace%2C+L">L. Colace</a>, <a href="/search/physics?searchtype=author&query=Danailov%2C+M">M. Danailov</a>, <a href="/search/physics?searchtype=author&query=Danev%2C+P">P. Danev</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=De+Vecchio%2C+C">C. De Vecchio</a>, <a href="/search/physics?searchtype=author&query=De+Vincenzi%2C+M">M. De Vincenzi</a>, <a href="/search/physics?searchtype=author&query=Fasci%2C+E">E. Fasci</a>, <a href="/search/physics?searchtype=author&query=Fuschino%2C+F">F. Fuschino</a>, <a href="/search/physics?searchtype=author&query=Gadedjisso-Tossou%2C+K+S">K. S. Gadedjisso-Tossou</a>, <a href="/search/physics?searchtype=author&query=Gianfrani%2C+L">L. Gianfrani</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+K">K. Ishida</a>, <a href="/search/physics?searchtype=author&query=Labanti%2C+C">C. Labanti</a>, <a href="/search/physics?searchtype=author&query=Maggi%2C+V">V. Maggi</a> , et al. (17 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="2105.06701v1-abstract-short" style="display: inline;"> The first measurement of the temperature dependence of the muon transfer rate from muonic hydrogen to oxygen was performed by the FAMU collaboration in 2016. The results provide evidence that the transfer rate rises with the temperature in the range 104-300 K. This paper presents the results of the experiment done in 2018 to extend the measurements towards lower (70 K) and higher (336 K) temperatu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06701v1-abstract-full').style.display = 'inline'; document.getElementById('2105.06701v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.06701v1-abstract-full" style="display: none;"> The first measurement of the temperature dependence of the muon transfer rate from muonic hydrogen to oxygen was performed by the FAMU collaboration in 2016. The results provide evidence that the transfer rate rises with the temperature in the range 104-300 K. This paper presents the results of the experiment done in 2018 to extend the measurements towards lower (70 K) and higher (336 K) temperatures. The 2018 results confirm the temperature dependence of the muon transfer rate observed in 2016 and sets firm ground for comparison with the theoretical predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06701v1-abstract-full').style.display = 'none'; document.getElementById('2105.06701v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.03035">arXiv:2101.03035</a> <span> [<a href="https://arxiv.org/pdf/2101.03035">pdf</a>, <a href="https://arxiv.org/format/2101.03035">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 Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1117/12.2561037">10.1117/12.2561037 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An innovative architecture for a wide band transient monitor on board the HERMES nano-satellite constellation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Fuschino%2C+F">F. Fuschino</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+R">R. Campana</a>, <a href="/search/physics?searchtype=author&query=Labanti%2C+C">C. Labanti</a>, <a href="/search/physics?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/physics?searchtype=author&query=Gandola%2C+M">M. Gandola</a>, <a href="/search/physics?searchtype=author&query=Grassi%2C+M">M. Grassi</a>, <a href="/search/physics?searchtype=author&query=Mele%2C+F">F. Mele</a>, <a href="/search/physics?searchtype=author&query=Ambrosino%2C+F">F. Ambrosino</a>, <a href="/search/physics?searchtype=author&query=Ceraudo%2C+F">F. Ceraudo</a>, <a href="/search/physics?searchtype=author&query=Demenev%2C+E">E. Demenev</a>, <a href="/search/physics?searchtype=author&query=Fiorini%2C+M">M. Fiorini</a>, <a href="/search/physics?searchtype=author&query=Morgante%2C+G">G. Morgante</a>, <a href="/search/physics?searchtype=author&query=Piazzolla%2C+R">R. Piazzolla</a>, <a href="/search/physics?searchtype=author&query=Bertuccio%2C+G">G. Bertuccio</a>, <a href="/search/physics?searchtype=author&query=Malcovati%2C+P">P. Malcovati</a>, <a href="/search/physics?searchtype=author&query=Bellutti%2C+P">P. Bellutti</a>, <a href="/search/physics?searchtype=author&query=Borghi%2C+G">G. Borghi</a>, <a href="/search/physics?searchtype=author&query=Dilillo%2C+G">G. Dilillo</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/physics?searchtype=author&query=Ficorella%2C+F">F. Ficorella</a>, <a href="/search/physics?searchtype=author&query=La+Rosa%2C+G">G. La Rosa</a>, <a href="/search/physics?searchtype=author&query=Nogara%2C+P">P. Nogara</a>, <a href="/search/physics?searchtype=author&query=Pauletta%2C+G">G. Pauletta</a>, <a href="/search/physics?searchtype=author&query=Picciotto%2C+A">A. Picciotto</a> , et al. (13 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="2101.03035v1-abstract-short" style="display: inline;"> The HERMES-TP/SP mission, based on a nanosatellite constellation, has very stringent constraints of sensitivity and compactness, and requires an innovative wide energy range instrument. The instrument technology is based on the "siswich" concept, in which custom-designed, low-noise Silicon Drift Detectors are used to simultaneously detect soft X-rays and to readout the optical light produced by th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03035v1-abstract-full').style.display = 'inline'; document.getElementById('2101.03035v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.03035v1-abstract-full" style="display: none;"> The HERMES-TP/SP mission, based on a nanosatellite constellation, has very stringent constraints of sensitivity and compactness, and requires an innovative wide energy range instrument. The instrument technology is based on the "siswich" concept, in which custom-designed, low-noise Silicon Drift Detectors are used to simultaneously detect soft X-rays and to readout the optical light produced by the interaction of higher energy photons in GAGG:Ce scintillators. To preserve the inherent excellent spectroscopic performances of SDDs, advanced readout electronics is necessary. In this paper, the HERMES detector architecture concept will be described in detail, as well as the specifically developed front-end ASICs (LYRA-FE and LYRA-BE) and integration solutions. The experimental performance of the integrated system composed by scintillator+SDD+LYRA ASIC will be discussed, demonstrating that the requirements of a wide energy range sensitivity, from 2 keV up to 2 MeV, are met in a compact instrument. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03035v1-abstract-full').style.display = 'none'; document.getElementById('2101.03035v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures. Proceedings of SPIE "Astronomical Telescopes and Instrumentation" 2020</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> SPIE Proceedings Volume 11444, Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray; 114441S (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.08524">arXiv:2005.08524</a> <span> [<a href="https://arxiv.org/pdf/2005.08524">pdf</a>, <a href="https://arxiv.org/format/2005.08524">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <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="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab80c2">10.3847/1538-4357/ab80c2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Time dependence of the flux of helium nuclei in cosmic rays measured by the PAMELA experiment between July 2006 and December 2009 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Marcelli%2C+N">N. Marcelli</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Lenni%2C+A">A. Lenni</a>, <a href="/search/physics?searchtype=author&query=Menn%2C+W">W. Menn</a>, <a href="/search/physics?searchtype=author&query=Munini%2C+R">R. Munini</a>, <a href="/search/physics?searchtype=author&query=Aslam%2C+O+P+M">O. P. M. Aslam</a>, <a href="/search/physics?searchtype=author&query=Bisschoff%2C+D">D. Bisschoff</a>, <a href="/search/physics?searchtype=author&query=Ngobeni%2C+M+D">M. D. Ngobeni</a>, <a href="/search/physics?searchtype=author&query=Potgieter%2C+M+S">M. S. Potgieter</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a> , et al. (31 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="2005.08524v1-abstract-short" style="display: inline;"> Precise time-dependent measurements of the Z = 2 component in the cosmic radiation provide crucial information about the propagation of charged particles through the heliosphere. The PAMELA experiment, with its long flight duration (15th June 2006 - 23rd January 2016) and the low energy threshold (80 MeV/n) is an ideal detector for cosmic ray solar modulation studies. In this paper, the helium nuc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.08524v1-abstract-full').style.display = 'inline'; document.getElementById('2005.08524v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.08524v1-abstract-full" style="display: none;"> Precise time-dependent measurements of the Z = 2 component in the cosmic radiation provide crucial information about the propagation of charged particles through the heliosphere. The PAMELA experiment, with its long flight duration (15th June 2006 - 23rd January 2016) and the low energy threshold (80 MeV/n) is an ideal detector for cosmic ray solar modulation studies. In this paper, the helium nuclei spectra measured by the PAMELA instrument from July 2006 to December 2009 over a Carrington rotation time basis are presented. A state-of-the-art three-dimensional model for cosmic-ray propagation inside the heliosphere was used to interpret the time-dependent measured fluxes. Proton-to-helium flux ratio time profiles at various rigidities are also presented in order to study any features which could result from the different masses and local interstellar spectra shapes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.08524v1-abstract-full').style.display = 'none'; document.getElementById('2005.08524v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 893, Number 2, 2020 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.02049">arXiv:1905.02049</a> <span> [<a href="https://arxiv.org/pdf/1905.02049">pdf</a>, <a href="https://arxiv.org/ps/1905.02049">ps</a>, <a href="https://arxiv.org/format/1905.02049">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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 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.physleta.2020.126667">10.1016/j.physleta.2020.126667 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First measurement of the temperature dependence of muon transfer rate from muonic hydrogen atoms to oxygen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=FAMU+Collaboration"> FAMU Collaboration</a>, <a href="/search/physics?searchtype=author&query=Mocchiutti%2C+E">E. Mocchiutti</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">A. Adamczak</a>, <a href="/search/physics?searchtype=author&query=Bakalov%2C+D">D. Bakalov</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Benocci%2C+R">R. Benocci</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Morales%2C+H+C">H. Cabrera Morales</a>, <a href="/search/physics?searchtype=author&query=Chignoli%2C+F">F. Chignoli</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Colace%2C+L">L. Colace</a>, <a href="/search/physics?searchtype=author&query=Danailov%2C+M">M. Danailov</a>, <a href="/search/physics?searchtype=author&query=Danev%2C+P">P. Danev</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=De+Vecchi%2C+C">C. De Vecchi</a>, <a href="/search/physics?searchtype=author&query=De+Vincenzi%2C+M">M. De Vincenzi</a>, <a href="/search/physics?searchtype=author&query=Furlanetto%2C+E">E. Furlanetto</a>, <a href="/search/physics?searchtype=author&query=Fuschino%2C+F">F. Fuschino</a>, <a href="/search/physics?searchtype=author&query=Gadedjisso-Tossou%2C+K+S">K. S. Gadedjisso-Tossou</a>, <a href="/search/physics?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+K">K. Ishida</a>, <a href="/search/physics?searchtype=author&query=Labanti%2C+C">C. Labanti</a>, <a href="/search/physics?searchtype=author&query=Maggi%2C+V">V. Maggi</a> , et al. (17 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="1905.02049v3-abstract-short" style="display: inline;"> We report the first measurement of the temperature dependence of muon transfer rate from $渭$p atoms to oxygen between 100 and 300 K. Data were obtained from the X-ray spectra of delayed events in gaseous target H$_2$/O$_2$ exposed to a muon beam. Based on the data, we determined the muon transfer energy dependence up to 0.1 eV, showing an 8-fold increase in contrast with the predictions of constan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.02049v3-abstract-full').style.display = 'inline'; document.getElementById('1905.02049v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.02049v3-abstract-full" style="display: none;"> We report the first measurement of the temperature dependence of muon transfer rate from $渭$p atoms to oxygen between 100 and 300 K. Data were obtained from the X-ray spectra of delayed events in gaseous target H$_2$/O$_2$ exposed to a muon beam. Based on the data, we determined the muon transfer energy dependence up to 0.1 eV, showing an 8-fold increase in contrast with the predictions of constant rate in the low energy limit. This work set constraints on theoretical models of muon transfer, and is of fundamental importance for the measurement of the hyperfine splitting of $渭$p by the FAMU collaboration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.02049v3-abstract-full').style.display = 'none'; document.getElementById('1905.02049v3-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">11 pages, 4 figure</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Lett. A, 384/26 (2020) 126667 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.06380">arXiv:1808.06380</a> <span> [<a href="https://arxiv.org/pdf/1808.06380">pdf</a>, <a href="https://arxiv.org/ps/1808.06380">ps</a>, <a href="https://arxiv.org/format/1808.06380">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/1138/1/012017">10.1088/1742-6596/1138/1/012017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> FAMU: study of the energy dependent transfer rate $螞_{渭p \rightarrow 渭O}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=FAMU+Collaboration"> FAMU Collaboration</a>, <a href="/search/physics?searchtype=author&query=Mocchiutti%2C+E">E. Mocchiutti</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Danailov%2C+M">M. Danailov</a>, <a href="/search/physics?searchtype=author&query=Furlanetto%2C+E">E. Furlanetto</a>, <a href="/search/physics?searchtype=author&query=Gadedjisso-Tossou%2C+K+S">K. S. Gadedjisso-Tossou</a>, <a href="/search/physics?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/physics?searchtype=author&query=Pizzolotto%2C+C">C. Pizzolotto</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Stoychev%2C+L">L. Stoychev</a>, <a href="/search/physics?searchtype=author&query=Vallazza%2C+E">E. Vallazza</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Niemela%2C+J">J. Niemela</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+K">K. Ishida</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">A. Adamczak</a>, <a href="/search/physics?searchtype=author&query=Baccolo%2C+G">G. Baccolo</a>, <a href="/search/physics?searchtype=author&query=Benocci%2C+R">R. Benocci</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Chignoli%2C+F">F. Chignoli</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Curioni%2C+A">A. Curioni</a>, <a href="/search/physics?searchtype=author&query=Maggi%2C+V">V. Maggi</a>, <a href="/search/physics?searchtype=author&query=Mazza%2C+R">R. Mazza</a>, <a href="/search/physics?searchtype=author&query=Moretti%2C+M">M. Moretti</a> , et al. (31 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="1808.06380v2-abstract-short" style="display: inline;"> The main goal of the FAMU experiment is the measurement of the hyperfine splitting (hfs) in the 1S state of muonic hydrogen $螖E_{hfs}(渭^-p)1S$. The physical process behind this experiment is the following: $渭p$ are formed in a mixture of hydrogen and a higher-Z gas. When absorbing a photon at resonance-energy $螖E_{hfs}\approx0.182$~eV, in subsequent collisions with the surrounding $H_2$ molecules,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.06380v2-abstract-full').style.display = 'inline'; document.getElementById('1808.06380v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.06380v2-abstract-full" style="display: none;"> The main goal of the FAMU experiment is the measurement of the hyperfine splitting (hfs) in the 1S state of muonic hydrogen $螖E_{hfs}(渭^-p)1S$. The physical process behind this experiment is the following: $渭p$ are formed in a mixture of hydrogen and a higher-Z gas. When absorbing a photon at resonance-energy $螖E_{hfs}\approx0.182$~eV, in subsequent collisions with the surrounding $H_2$ molecules, the $渭p$ is quickly de-excited and accelerated by $\sim2/3$ of the excitation energy. The observable is the time distribution of the K-lines X-rays emitted from the $渭Z$ formed by muon transfer $(渭p) +Z \rightarrow (渭Z)^*+p$, a reaction whose rate depends on the $渭p$ kinetic energy. The maximal response, to the tuned laser wavelength, of the time distribution of X-ray from K-lines of the $(渭Z)^*$ cascade indicate the resonance. During the preparatory phase of the FAMU experiment, several measurements have been performed both to validate the methodology and to prepare the best configuration of target and detectors for the spectroscopic measurement. We present here the crucial study of the energy dependence of the transfer rate from muonic hydrogen to oxygen ($螞_{渭p \rightarrow 渭O}$), precisely measured for the first time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.06380v2-abstract-full').style.display = 'none'; document.getElementById('1808.06380v2-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 August, 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">11 pages, 4 figures, published on Journal of Physics: Conference Series, proc. of International Conference on Precision Physics of Simple Atomic Systems - PSAS2018. arXiv admin note: text overlap with arXiv:1708.03172</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Phys.: Conf. Ser. 1138 012017 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.10948">arXiv:1806.10948</a> <span> [<a href="https://arxiv.org/pdf/1806.10948">pdf</a>, <a href="https://arxiv.org/ps/1806.10948">ps</a>, <a href="https://arxiv.org/format/1806.10948">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <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/10.3847/1538-4357/aacf89">10.3847/1538-4357/aacf89 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lithium and Beryllium isotopes with the PAMELA experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Menn%2C+W">W. Menn</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Simon%2C+M">M. Simon</a>, <a href="/search/physics?searchtype=author&query=Vasilyev%2C+G">G. Vasilyev</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a> , et al. (34 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="1806.10948v1-abstract-short" style="display: inline;"> The cosmic-ray lithium and beryllium ($^{6}$Li, $^{7}$Li, $^{7}$Be, $^{9}$Be, $^{10}$Be) isotopic composition has been measured with the satellite-borne experiment PAMELA, which was launched into low-Earth orbit on-board the Resurs-DK1 satellite on June 15th 2006. The rare lithium and beryllium isotopes in cosmic rays are believed to originate mainly from the interaction of high energy carbon, nit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.10948v1-abstract-full').style.display = 'inline'; document.getElementById('1806.10948v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.10948v1-abstract-full" style="display: none;"> The cosmic-ray lithium and beryllium ($^{6}$Li, $^{7}$Li, $^{7}$Be, $^{9}$Be, $^{10}$Be) isotopic composition has been measured with the satellite-borne experiment PAMELA, which was launched into low-Earth orbit on-board the Resurs-DK1 satellite on June 15th 2006. The rare lithium and beryllium isotopes in cosmic rays are believed to originate mainly from the interaction of high energy carbon, nitrogen and oxygen nuclei with the interstellar medium (ISM), but also on "tertiary" interactions in the ISM (i.e. produced by further fragmentation of secondary beryllium and boron). In this paper the isotopic ratios $^{7}$Li/$^{6}$Li and $^{7}$Be/($^{9}$Be + $^{10}$Be) measured between 150 and 1100 MeV/n using two different detector systems from July 2006 to September 2014 will be presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.10948v1-abstract-full').style.display = 'none'; document.getElementById('1806.10948v1-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> 27 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">13 pages, 11 figures, accepted for publication in the Astrophysical Journal. arXiv admin note: text overlap with arXiv:1512.06535</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.06166">arXiv:1803.06166</a> <span> [<a href="https://arxiv.org/pdf/1803.06166">pdf</a>, <a href="https://arxiv.org/format/1803.06166">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aaa0c8">10.3847/1538-4357/aaa0c8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence of energy and charge sign dependence of the recovery time for the December 2006 Forbush event measured by the PAMELA experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Munini%2C+R">R. Munini</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Martucci%2C+M">M. Martucci</a>, <a href="/search/physics?searchtype=author&query=Merge%2C+M">M. Merge</a>, <a href="/search/physics?searchtype=author&query=Richardson%2C+I+G">I. G. Richardson</a>, <a href="/search/physics?searchtype=author&query=Ryan%2C+J+M">J. M. Ryan</a>, <a href="/search/physics?searchtype=author&query=Stochaj%2C+S">S. Stochaj</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a> , et al. (33 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="1803.06166v1-abstract-short" style="display: inline;"> New results on the short-term galactic cosmic ray (GCR) intensity variation (Forbush decrease) in December 2006 measured by the PAMELA instrument are presented. Forbush decreases are sudden suppressions of the GCR intensities which are associated with the passage of interplanetary transients such as shocks and interplanetary coronal mass ejections (ICMEs). Most of the past measurements of this phe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.06166v1-abstract-full').style.display = 'inline'; document.getElementById('1803.06166v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.06166v1-abstract-full" style="display: none;"> New results on the short-term galactic cosmic ray (GCR) intensity variation (Forbush decrease) in December 2006 measured by the PAMELA instrument are presented. Forbush decreases are sudden suppressions of the GCR intensities which are associated with the passage of interplanetary transients such as shocks and interplanetary coronal mass ejections (ICMEs). Most of the past measurements of this phenomenon were carried out with ground-based detectors such as neutron monitors or muon telescopes. These techniques allow only the indirect detection of the overall GCR intensity over an integrated energy range. For the first time, thanks to the unique features of the PAMELA magnetic spectrometer, the Forbush decrease commencing on 2006 December 14, following a CME at the Sun on 2006 December 13 was studied in a wide rigidity range (0.4 - 20 GV) and for different species of GCRs detected directly in space. The daily averaged GCR proton intensity was used to investigate the rigidity dependence of the amplitude and the recovery time of the Forbush decrease. Additionally, for the first time, the temporal variations in the helium and electron intensities during a Forbush decrease were studied. Interestingly, the temporal evolutions of the helium and proton intensities during the Forbush decrease were found in good agreement, while the low rigidity electrons (< 2 GV) displayed a faster recovery. This difference in the electron recovery is interpreted as a charge-sign dependence introduced by drift motions experienced by the GCRs during their propagation through the heliosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.06166v1-abstract-full').style.display = 'none'; document.getElementById('1803.06166v1-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 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 853, 76, 2018 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.08717">arXiv:1801.08717</a> <span> [<a href="https://arxiv.org/pdf/1801.08717">pdf</a>, <a href="https://arxiv.org/format/1801.08717">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2018.01.094">10.1016/j.nima.2018.01.094 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EuPRAXIA@SPARC_LAB Design study towards a compact FEL facility at LNF </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ferrario%2C+M">M. Ferrario</a>, <a href="/search/physics?searchtype=author&query=Alesini%2C+D">D. Alesini</a>, <a href="/search/physics?searchtype=author&query=Anania%2C+M+P">M. P. Anania</a>, <a href="/search/physics?searchtype=author&query=Artioli%2C+M">M. Artioli</a>, <a href="/search/physics?searchtype=author&query=Bacci%2C+A">A. Bacci</a>, <a href="/search/physics?searchtype=author&query=Bartocci%2C+S">S. Bartocci</a>, <a href="/search/physics?searchtype=author&query=Bedogni%2C+R">R. Bedogni</a>, <a href="/search/physics?searchtype=author&query=Bellaveglia%2C+M">M. Bellaveglia</a>, <a href="/search/physics?searchtype=author&query=Biagioni%2C+A">A. Biagioni</a>, <a href="/search/physics?searchtype=author&query=Bisesto%2C+F">F. Bisesto</a>, <a href="/search/physics?searchtype=author&query=Brandi%2C+F">F. Brandi</a>, <a href="/search/physics?searchtype=author&query=Brentegani%2C+E">E. Brentegani</a>, <a href="/search/physics?searchtype=author&query=Broggi%2C+F">F. Broggi</a>, <a href="/search/physics?searchtype=author&query=Buonomo%2C+B">B. Buonomo</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+P+L">P. L. Campana</a>, <a href="/search/physics?searchtype=author&query=Campogiani%2C+G">G. Campogiani</a>, <a href="/search/physics?searchtype=author&query=Cannaos%2C+C">C. Cannaos</a>, <a href="/search/physics?searchtype=author&query=Cantarella%2C+S">S. Cantarella</a>, <a href="/search/physics?searchtype=author&query=Cardelli%2C+F">F. Cardelli</a>, <a href="/search/physics?searchtype=author&query=Carpanese%2C+M">M. Carpanese</a>, <a href="/search/physics?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/physics?searchtype=author&query=Castorina%2C+G">G. Castorina</a>, <a href="/search/physics?searchtype=author&query=Lasheras%2C+N+C">N. Catalan Lasheras</a>, <a href="/search/physics?searchtype=author&query=Chiadroni%2C+E">E. Chiadroni</a>, <a href="/search/physics?searchtype=author&query=Cianchi%2C+A">A. Cianchi</a> , et al. (95 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="1801.08717v1-abstract-short" style="display: inline;"> On the wake of the results obtained so far at the SPARC\_LAB test-facility at the Laboratori Nazionali di Frascati (Italy), we are currently investigating the possibility to design and build a new multi-disciplinary user-facility, equipped with a soft X-ray Free Electron Laser (FEL) driven by a $\sim$1 GeV high brightness linac based on plasma accelerator modules. This design study is performed in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08717v1-abstract-full').style.display = 'inline'; document.getElementById('1801.08717v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.08717v1-abstract-full" style="display: none;"> On the wake of the results obtained so far at the SPARC\_LAB test-facility at the Laboratori Nazionali di Frascati (Italy), we are currently investigating the possibility to design and build a new multi-disciplinary user-facility, equipped with a soft X-ray Free Electron Laser (FEL) driven by a $\sim$1 GeV high brightness linac based on plasma accelerator modules. This design study is performed in synergy with the EuPRAXIA design study. In this paper we report about the recent progresses in the on going design study of the new facility. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08717v1-abstract-full').style.display = 'none'; document.getElementById('1801.08717v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.08418">arXiv:1801.08418</a> <span> [<a href="https://arxiv.org/pdf/1801.08418">pdf</a>, <a href="https://arxiv.org/format/1801.08418">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.3847/2041-8213/aaa403">10.3847/2041-8213/aaa403 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unexpected cyclic behavior in cosmic ray protons observed by PAMELA at 1 AU </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Krutkov%2C+S+Y">S. Y. Krutkov</a>, <a href="/search/physics?searchtype=author&query=Kvashnin%2C+A+N">A. N. Kvashnin</a>, <a href="/search/physics?searchtype=author&query=Leonov%2C+A">A. Leonov</a>, <a href="/search/physics?searchtype=author&query=Malakhov%2C+V">V. Malakhov</a>, <a href="/search/physics?searchtype=author&query=Marcelli%2C+L">L. Marcelli</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="1801.08418v1-abstract-short" style="display: inline;"> Protons detected by the PAMELA experiment in the period 2006-2014 have been analyzed in the energy range between 0.40-50 GV to explore possible periodicities besides the well known solar undecennial modulation. An unexpected clear and regular feature has been found at rigidities below 15 GV, with a quasi-periodicity of $\sim$450 days. A possible Jovian origin of this periodicity has been investiga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08418v1-abstract-full').style.display = 'inline'; document.getElementById('1801.08418v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.08418v1-abstract-full" style="display: none;"> Protons detected by the PAMELA experiment in the period 2006-2014 have been analyzed in the energy range between 0.40-50 GV to explore possible periodicities besides the well known solar undecennial modulation. An unexpected clear and regular feature has been found at rigidities below 15 GV, with a quasi-periodicity of $\sim$450 days. A possible Jovian origin of this periodicity has been investigated in different ways. The results seem to favor a small but not negligible contribution to cosmic rays from the Jovian magnetosphere, even if other explanations cannot be excluded. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08418v1-abstract-full').style.display = 'none'; document.getElementById('1801.08418v1-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 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">article 4 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, Volume 852, Number 2, 2018 January </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.07112">arXiv:1801.07112</a> <span> [<a href="https://arxiv.org/pdf/1801.07112">pdf</a>, <a href="https://arxiv.org/format/1801.07112">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aaa9b2">10.3847/2041-8213/aaa9b2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Proton fluxes measured by the PAMELA experiment from the minimum to the maximum solar activity for the 24th solar cycle </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Martucci%2C+M">M. Martucci</a>, <a href="/search/physics?searchtype=author&query=Munini%2C+R">R. Munini</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Krutkov%2C+S+Y">S. Y. Krutkov</a>, <a href="/search/physics?searchtype=author&query=Kvashnin%2C+A+N">A. N. Kvashnin</a>, <a href="/search/physics?searchtype=author&query=Leonov%2C+A">A. Leonov</a> , et al. (29 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="1801.07112v2-abstract-short" style="display: inline;"> Precise measurements of the time-dependent intensity of the low energy ($<50$ GeV) galactic cosmic rays are fundamental to test and improve the models which describe their propagation inside the heliosphere. Especially, data spanning different solar activity periods, i.e. from minimum to maximum, are needed to achieve comprehensive understanding of such physical phenomenon. The minimum phase betwe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.07112v2-abstract-full').style.display = 'inline'; document.getElementById('1801.07112v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.07112v2-abstract-full" style="display: none;"> Precise measurements of the time-dependent intensity of the low energy ($<50$ GeV) galactic cosmic rays are fundamental to test and improve the models which describe their propagation inside the heliosphere. Especially, data spanning different solar activity periods, i.e. from minimum to maximum, are needed to achieve comprehensive understanding of such physical phenomenon. The minimum phase between the 23$^{rd}$ and the 24$^{th}$ solar cycles was peculiarly long, extending up to the beginning of 2010 and followed by the maximum phase, reached during early 2014. In this paper, we present proton differential spectra measured from January 2010 to February 2014 by the PAMELA experiment. For the first time the galactic cosmic ray proton intensity was studied over a wide energy range (0.08-50 GeV) by a single apparatus from a minimum to a maximum period of solar activity. The large statistics allowed the time variation to be investigated on a nearly monthly basis. Data were compared and interpreted in the context of a state-of-the-art three-dimensional model describing the galactic cosmic rays propagation through the heliosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.07112v2-abstract-full').style.display = 'none'; document.getElementById('1801.07112v2-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 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">article, 4 figures. Accepted for publication on The Astrophysical Journal Letters (January 2018)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, Volume 854, Number 1 published 2018 February 5 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.03172">arXiv:1708.03172</a> <span> [<a href="https://arxiv.org/pdf/1708.03172">pdf</a>, <a href="https://arxiv.org/ps/1708.03172">ps</a>, <a href="https://arxiv.org/format/1708.03172">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> First FAMU observation of muon transfer from mu-p atoms to higher-Z elements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=FAMU+Collaboration"> FAMU Collaboration</a>, <a href="/search/physics?searchtype=author&query=Mocchiutti%2C+E">Emiliano Mocchiutti</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">Valter Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">Rita Carbone</a>, <a href="/search/physics?searchtype=author&query=Danailov%2C+M">Miltcho Danailov</a>, <a href="/search/physics?searchtype=author&query=Furlanetto%2C+E">Elena Furlanetto</a>, <a href="/search/physics?searchtype=author&query=Gadedjisso-Tossou%2C+K+S">Komlan Segbeya Gadedjisso-Tossou</a>, <a href="/search/physics?searchtype=author&query=Guffanti%2C+D">Daniele Guffanti</a>, <a href="/search/physics?searchtype=author&query=Pizzolotto%2C+C">Cecilia Pizzolotto</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">Alexandre Rachevski</a>, <a href="/search/physics?searchtype=author&query=Stoychev%2C+L">Lyubomir Stoychev</a>, <a href="/search/physics?searchtype=author&query=Vallazza%2C+E+S">Erik Silvio Vallazza</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">Gianluigi Zampa</a>, <a href="/search/physics?searchtype=author&query=Niemela%2C+J">Joseph Niemela</a>, <a href="/search/physics?searchtype=author&query=Ishida%2C+K">Katsuhiko Ishida</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">Andrzej Adamczak</a>, <a href="/search/physics?searchtype=author&query=Baccolo%2C+G">Giovanni Baccolo</a>, <a href="/search/physics?searchtype=author&query=Benocci%2C+R">Roberto Benocci</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">Roberto Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">Maurizio Bonesini</a>, <a href="/search/physics?searchtype=author&query=Chignoli%2C+F">Francesco Chignoli</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">Massimiliano Clemenza</a>, <a href="/search/physics?searchtype=author&query=Curioni%2C+A">Alessandro Curioni</a>, <a href="/search/physics?searchtype=author&query=Maggi%2C+V">Valter Maggi</a>, <a href="/search/physics?searchtype=author&query=Mazza%2C+R">Roberto Mazza</a> , et al. (32 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="1708.03172v3-abstract-short" style="display: inline;"> The FAMU experiment aims to accurately measure the hyperfine splitting of the ground state of the muonic hydrogen atom. A measurement of the transfer rate of muons from hydrogen to heavier gases is necessary for this purpose. In June 2014, within a preliminary experiment, a pressurized gas-target was exposed to the pulsed low-energy muon beam at the RIKEN RAL muon facility (Rutherford Appleton Lab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.03172v3-abstract-full').style.display = 'inline'; document.getElementById('1708.03172v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.03172v3-abstract-full" style="display: none;"> The FAMU experiment aims to accurately measure the hyperfine splitting of the ground state of the muonic hydrogen atom. A measurement of the transfer rate of muons from hydrogen to heavier gases is necessary for this purpose. In June 2014, within a preliminary experiment, a pressurized gas-target was exposed to the pulsed low-energy muon beam at the RIKEN RAL muon facility (Rutherford Appleton Laboratory, UK). The main goal of the test was the characterization of both the noise induced by the pulsed beam and the X-ray detectors. The apparatus, to some extent rudimental, has served admirably to this task. Technical results have been published that prove the validity of the choices made and pave the way for the next steps. This paper presents the results of physical relevance of measurements of the muon transfer rate to carbon dioxide, oxygen, and argon from non-thermalized excited mu-p atoms. The analysis methodology and the approach to the systematics errors are useful for the subsequent study of the transfer rate as function of the kinetic energy of the mu-p currently under way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.03172v3-abstract-full').style.display = 'none'; document.getElementById('1708.03172v3-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 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">15 pages, 3 figures, 2 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/1704.06122">arXiv:1704.06122</a> <span> [<a href="https://arxiv.org/pdf/1704.06122">pdf</a>, <a href="https://arxiv.org/format/1704.06122">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 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/10.1117/12.2232597">10.1117/12.2232597 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A compact and modular X and gamma-ray detector with a CsI scintillator and double-readout Silicon Drift Detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Campana%2C+R">R. Campana</a>, <a href="/search/physics?searchtype=author&query=Fuschino%2C+F">F. Fuschino</a>, <a href="/search/physics?searchtype=author&query=Labanti%2C+C">C. Labanti</a>, <a href="/search/physics?searchtype=author&query=Marisaldi%2C+M">M. Marisaldi</a>, <a href="/search/physics?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/physics?searchtype=author&query=Fiorini%2C+M">M. Fiorini</a>, <a href="/search/physics?searchtype=author&query=Uslenghi%2C+M">M. Uslenghi</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Bellutti%2C+P">P. Bellutti</a>, <a href="/search/physics?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/physics?searchtype=author&query=Elmi%2C+I">I. Elmi</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/physics?searchtype=author&query=Ficorella%2C+F">F. Ficorella</a>, <a href="/search/physics?searchtype=author&query=Frontera%2C+F">F. Frontera</a>, <a href="/search/physics?searchtype=author&query=Picciotto%2C+A">A. Picciotto</a>, <a href="/search/physics?searchtype=author&query=Piemonte%2C+C">C. Piemonte</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Rashevskaya%2C+I">I. Rashevskaya</a>, <a href="/search/physics?searchtype=author&query=Rignanese%2C+L+P">L. P. Rignanese</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zorzi%2C+N">N. Zorzi</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="1704.06122v1-abstract-short" style="display: inline;"> A future compact and modular X and gamma-ray spectrometer (XGS) has been designed and a series of prototypes have been developed and tested. The experiment envisages the use of CsI scintillator bars read out at both ends by single-cell 25 mm2 Silicon Drift Detectors. Digital algorithms are used to discriminate between events absorbed in the Silicon layer (lower energy X rays) and events absorbed i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.06122v1-abstract-full').style.display = 'inline'; document.getElementById('1704.06122v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.06122v1-abstract-full" style="display: none;"> A future compact and modular X and gamma-ray spectrometer (XGS) has been designed and a series of prototypes have been developed and tested. The experiment envisages the use of CsI scintillator bars read out at both ends by single-cell 25 mm2 Silicon Drift Detectors. Digital algorithms are used to discriminate between events absorbed in the Silicon layer (lower energy X rays) and events absorbed in the scintillator crystal (higher energy X rays and gamma-rays). The prototype characterization is shown and the modular design for future experiments with possible astrophysical applications (e.g. for the THESEUS mission proposed for the ESA M5 call) are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.06122v1-abstract-full').style.display = 'none'; document.getElementById('1704.06122v1-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 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">10 pages, 11 figures. Published in Proceeding of SPIE Astronomical Telescopes and Instrumentation 2016</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings of the SPIE, 9905, 99056I (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.01447">arXiv:1703.01447</a> <span> [<a href="https://arxiv.org/pdf/1703.01447">pdf</a>, <a href="https://arxiv.org/format/1703.01447">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/10.1088/1748-0221/12/03/C03035">10.1088/1748-0221/12/03/C03035 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The construction of the Fiber-SiPM beam monitor system of the R484 and R582 experiments at the RIKEN-RAL muon facility </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Chignoli%2C+F">F. Chignoli</a>, <a href="/search/physics?searchtype=author&query=Mazza%2C+R">R. Mazza</a>, <a href="/search/physics?searchtype=author&query=Cervi%2C+T">T. Cervi</a>, <a href="/search/physics?searchtype=author&query=deBari%2C+A">A. deBari</a>, <a href="/search/physics?searchtype=author&query=Menegolli%2C+A">A. Menegolli</a>, <a href="/search/physics?searchtype=author&query=Prata%2C+M+C">M. C. Prata</a>, <a href="/search/physics?searchtype=author&query=Rossella%2C+M">M. Rossella</a>, <a href="/search/physics?searchtype=author&query=Tortora%2C+L">L. Tortora</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Mocchiutti%2C+E">E. Mocchiutti</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Vallazza%2C+E">E. Vallazza</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</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="1703.01447v1-abstract-short" style="display: inline;"> The scintillating fiber-SiPM beam monitor detectors, designed to deliver beam informations for the R484 and R582 experiments at the high intensity, low energy pulsed muon beam at the RIKEN-RAL facility, have been successfully constructed and operated. Details on their construction and first performances in beam are reported </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.01447v1-abstract-full" style="display: none;"> The scintillating fiber-SiPM beam monitor detectors, designed to deliver beam informations for the R484 and R582 experiments at the high intensity, low energy pulsed muon beam at the RIKEN-RAL facility, have been successfully constructed and operated. Details on their construction and first performances in beam are reported <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.01447v1-abstract-full').style.display = 'none'; document.getElementById('1703.01447v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">14th Topical Seminar on Innovative Particle and Radiation Detectors 3-6 October 2016, Siena to be published on 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/1607.02870">arXiv:1607.02870</a> <span> [<a href="https://arxiv.org/pdf/1607.02870">pdf</a>, <a href="https://arxiv.org/ps/1607.02870">ps</a>, <a href="https://arxiv.org/format/1607.02870">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.asr.2016.06.042">10.1016/j.asr.2016.06.042 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Geomagnetically trapped, albedo and solar energetic particles: trajectory analysis and flux reconstruction with PAMELA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a> , et al. (37 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="1607.02870v1-abstract-short" style="display: inline;"> The PAMELA satellite experiment is providing comprehensive observations of the interplanetary and magnetospheric radiation in the near-Earth environment. Thanks to its identification capabilities and the semi-polar orbit, PAMELA is able to precisely measure the energetic spectra and the angular distributions of the different cosmic-ray populations over a wide latitude region, including geomagnetic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.02870v1-abstract-full').style.display = 'inline'; document.getElementById('1607.02870v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.02870v1-abstract-full" style="display: none;"> The PAMELA satellite experiment is providing comprehensive observations of the interplanetary and magnetospheric radiation in the near-Earth environment. Thanks to its identification capabilities and the semi-polar orbit, PAMELA is able to precisely measure the energetic spectra and the angular distributions of the different cosmic-ray populations over a wide latitude region, including geomagnetically trapped and albedo particles. Its observations comprise the solar energetic particle events between solar cycles 23 and 24, and the geomagnetic cutoff variations during magnetospheric storms. PAMELA's measurements are supported by an accurate analysis of particle trajectories in the Earth's magnetosphere based on a realistic geomagnetic field modeling, which allows the classification of particle populations of different origin and the investigation of the asymptotic directions of arrival. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.02870v1-abstract-full').style.display = 'none'; document.getElementById('1607.02870v1-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 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </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">Accepted for publication in Advances in Space Research, 2016. 21 pages, 7 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.01572">arXiv:1604.01572</a> <span> [<a href="https://arxiv.org/pdf/1604.01572">pdf</a>, <a href="https://arxiv.org/ps/1604.01572">ps</a>, <a href="https://arxiv.org/format/1604.01572">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/11/05/P05007">10.1088/1748-0221/11/05/P05007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Steps towards the hyperfine splitting measurement of the muonic hydrogen ground state: pulsed muon beam and detection system characterization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">A. Adamczak</a>, <a href="/search/physics?searchtype=author&query=Baccolo%2C+G">G. Baccolo</a>, <a href="/search/physics?searchtype=author&query=Bakalov%2C+D">D. Bakalov</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+R">R. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Cervi%2C+T">T. Cervi</a>, <a href="/search/physics?searchtype=author&query=Chignoli%2C+F">F. Chignoli</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Colace%2C+L">L. Colace</a>, <a href="/search/physics?searchtype=author&query=Curioni%2C+A">A. Curioni</a>, <a href="/search/physics?searchtype=author&query=Danailov%2C+M">M. Danailov</a>, <a href="/search/physics?searchtype=author&query=Danev%2C+P">P. Danev</a>, <a href="/search/physics?searchtype=author&query=D%27Antone%2C+I">I. D'Antone</a>, <a href="/search/physics?searchtype=author&query=De%2C+A">A. De</a>, <a href="/search/physics?searchtype=author&query=De%2C+C">C. De</a>, <a href="/search/physics?searchtype=author&query=De%2C+M">M. De</a>, <a href="/search/physics?searchtype=author&query=Furini%2C+M">M. Furini</a>, <a href="/search/physics?searchtype=author&query=Fuschino%2C+F">F. Fuschino</a>, <a href="/search/physics?searchtype=author&query=Gadejisso-Tossou%2C+K">K. Gadejisso-Tossou</a>, <a href="/search/physics?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/physics?searchtype=author&query=Iaciofano%2C+A">A. Iaciofano</a> , et al. (30 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="1604.01572v2-abstract-short" style="display: inline;"> The high precision measurement of the hyperfine splitting of the muonic-hydrogen atom ground state with pulsed and intense muon beam requires careful technological choices both in the construction of a gas target and of the detectors. In June 2014, the pressurized gas target of the FAMU experiment was exposed to the low energy pulsed muon beam at the RIKEN RAL muon facility. The objectives of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.01572v2-abstract-full').style.display = 'inline'; document.getElementById('1604.01572v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.01572v2-abstract-full" style="display: none;"> The high precision measurement of the hyperfine splitting of the muonic-hydrogen atom ground state with pulsed and intense muon beam requires careful technological choices both in the construction of a gas target and of the detectors. In June 2014, the pressurized gas target of the FAMU experiment was exposed to the low energy pulsed muon beam at the RIKEN RAL muon facility. The objectives of the test were the characterization of the target, the hodoscope and the X-ray detectors. The apparatus consisted of a beam hodoscope and X-rays detectors made with high purity Germanium and Lanthanum Bromide crystals. In this paper the experimental setup is described and the results of the detector characterization are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.01572v2-abstract-full').style.display = 'none'; document.getElementById('1604.01572v2-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 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </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">22 pages, 14 figures, published and open access on JINST</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation 11/05, P05007, 2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.05509">arXiv:1602.05509</a> <span> [<a href="https://arxiv.org/pdf/1602.05509">pdf</a>, <a href="https://arxiv.org/ps/1602.05509">ps</a>, <a href="https://arxiv.org/format/1602.05509">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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/10.1002/2016SW001364">10.1002/2016SW001364 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PAMELA's measurements of geomagnetic cutoff variations during the 14 December 2006 storm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Krutkov%2C+S+Y">S. Y. Krutkov</a> , et al. (33 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="1602.05509v2-abstract-short" style="display: inline;"> Data from the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) satellite experiment were used to measure the geomagnetic cutoff for high-energy (>80 MeV) protons during the 14 December 2006 geomagnetic storm. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to spacecraft orbital periods (94 mi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.05509v2-abstract-full').style.display = 'inline'; document.getElementById('1602.05509v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.05509v2-abstract-full" style="display: none;"> Data from the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) satellite experiment were used to measure the geomagnetic cutoff for high-energy (>80 MeV) protons during the 14 December 2006 geomagnetic storm. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to spacecraft orbital periods (94 min). Estimated cutoff values were compared with those obtained by means of a trajectory tracing approach based on a dynamical empirical modeling of the Earth's magnetosphere. We found significant variations in the cutoff latitude, with a maximum suppression of about 7 deg at lowest rigidities during the main phase of the storm. The observed reduction in the geomagnetic shielding and its temporal evolution were related to the changes in the magnetospheric configuration, investigating the role of interplanetary magnetic field, solar wind and geomagnetic parameters. PAMELA's results represent the first direct measurement of geomagnetic cutoffs for protons with kinetic energies in the sub-GeV and GeV region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.05509v2-abstract-full').style.display = 'none'; document.getElementById('1602.05509v2-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 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2016. </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">26 pages, 6 figures and 1 table. Accepted for publication in Space Weather</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.05407">arXiv:1601.05407</a> <span> [<a href="https://arxiv.org/pdf/1601.05407">pdf</a>, <a href="https://arxiv.org/ps/1601.05407">ps</a>, <a href="https://arxiv.org/format/1601.05407">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Solar energetic particle events: trajectory analysis and flux reconstruction with PAMELA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</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="1601.05407v1-abstract-short" style="display: inline;"> The PAMELA satellite experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from about 80 MeV to several GeV in near-Earth space, bridging the low energy data by other space-based instruments and the Ground Level Enhancement (GLE) data by the worldwide network of neutron monitors. Its unique observational capabilities include the possibility of measurin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.05407v1-abstract-full').style.display = 'inline'; document.getElementById('1601.05407v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.05407v1-abstract-full" style="display: none;"> The PAMELA satellite experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from about 80 MeV to several GeV in near-Earth space, bridging the low energy data by other space-based instruments and the Ground Level Enhancement (GLE) data by the worldwide network of neutron monitors. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies. This work reports the analysis methods developed to estimate the SEP energy spectra as a function of the particle pitch-angle with respect to the Interplanetary Magnetic Field (IMF) direction. The crucial ingredient is provided by an accurate simulation of the asymptotic exposition of the PAMELA apparatus, based on a realistic reconstruction of particle trajectories in the Earth's magnetosphere. As case study, the results for the May 17, 2012 event are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.05407v1-abstract-full').style.display = 'none'; document.getElementById('1601.05407v1-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> 2 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2016. </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">Conference: The 34th International Cosmic Ray Conference (ICRC2015), 30 July - 6 August, 2015, The Hague, The Netherlands, Volume: PoS(ICRC2015)085</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.02784">arXiv:1601.02784</a> <span> [<a href="https://arxiv.org/pdf/1601.02784">pdf</a>, <a href="https://arxiv.org/format/1601.02784">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/689/1/012017">10.1088/1742-6596/689/1/012017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Development and tests of a new prototype detector for the XAFS beamline at Elettra Synchrotron in Trieste </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Fabiani%2C+S">S Fabiani</a>, <a href="/search/physics?searchtype=author&query=Ahangarianabhari%2C+M">M Ahangarianabhari</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Bellutti%2C+P">P Bellutti</a>, <a href="/search/physics?searchtype=author&query=Bertuccio%2C+G">G Bertuccio</a>, <a href="/search/physics?searchtype=author&query=Bruschi%2C+M">M Bruschi</a>, <a href="/search/physics?searchtype=author&query=Bufon%2C+J">J Bufon</a>, <a href="/search/physics?searchtype=author&query=Carrato%2C+S">S Carrato</a>, <a href="/search/physics?searchtype=author&query=Castoldi%2C+A">A Castoldi</a>, <a href="/search/physics?searchtype=author&query=Cautero%2C+G">G Cautero</a>, <a href="/search/physics?searchtype=author&query=Ciano%2C+S">S Ciano</a>, <a href="/search/physics?searchtype=author&query=Cicuttin%2C+A">A Cicuttin</a>, <a href="/search/physics?searchtype=author&query=Crespo%2C+M+L">M L Crespo</a>, <a href="/search/physics?searchtype=author&query=Santos%2C+M+D">M Dos Santos</a>, <a href="/search/physics?searchtype=author&query=Gandola%2C+M">M Gandola</a>, <a href="/search/physics?searchtype=author&query=Giacomini%2C+G">G Giacomini</a>, <a href="/search/physics?searchtype=author&query=Giuressi%2C+D">D Giuressi</a>, <a href="/search/physics?searchtype=author&query=Guazzoni%2C+C">C Guazzoni</a>, <a href="/search/physics?searchtype=author&query=Menk%2C+R+H">R H Menk</a>, <a href="/search/physics?searchtype=author&query=Niemela%2C+J">J Niemela</a>, <a href="/search/physics?searchtype=author&query=Olivi%2C+L">L Olivi</a>, <a href="/search/physics?searchtype=author&query=Picciotto%2C+A">A Picciotto</a>, <a href="/search/physics?searchtype=author&query=Piemonte%2C+C">C Piemonte</a>, <a href="/search/physics?searchtype=author&query=Rashevskaya%2C+I">I Rashevskaya</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A Rachevski</a> , et al. (8 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="1601.02784v1-abstract-short" style="display: inline;"> The XAFS beamline at Elettra Synchrotron in Trieste combines X-ray absorption spectroscopy and X-ray diffraction to provide chemically specific structural information of materials. It operates in the energy range 2.4-27 keV by using a silicon double reflection Bragg monochromator. The fluorescence measurement is performed in place of the absorption spectroscopy when the sample transparency is too… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.02784v1-abstract-full').style.display = 'inline'; document.getElementById('1601.02784v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.02784v1-abstract-full" style="display: none;"> The XAFS beamline at Elettra Synchrotron in Trieste combines X-ray absorption spectroscopy and X-ray diffraction to provide chemically specific structural information of materials. It operates in the energy range 2.4-27 keV by using a silicon double reflection Bragg monochromator. The fluorescence measurement is performed in place of the absorption spectroscopy when the sample transparency is too low for transmission measurements or the element to study is too diluted in the sample. We report on the development and on the preliminary tests of a new prototype detector based on Silicon Drift Detectors technology and the SIRIO ultra low noise front-end ASIC. The new system will be able to reduce drastically the time needed to perform fluorescence measurements, while keeping a short dead time and maintaining an adequate energy resolution to perform spectroscopy. The custom-made silicon sensor and the electronics are designed specifically for the beamline requirements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.02784v1-abstract-full').style.display = 'none'; document.getElementById('1601.02784v1-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> 12 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2016. </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">Proceeding of the 6YRM 12th-14th Oct 2015 - L'Aquila (Italy). Accepted for publication on Journal of Physics: Conference Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.05005">arXiv:1511.05005</a> <span> [<a href="https://arxiv.org/pdf/1511.05005">pdf</a>, <a href="https://arxiv.org/ps/1511.05005">ps</a>, <a href="https://arxiv.org/format/1511.05005">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="Atomic Physics">physics.atom-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/11/03/P03019">10.1088/1748-0221/11/03/P03019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-energy negative muon interaction with matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Danev%2C+P">Petar Danev</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">Andrzej Adamczak</a>, <a href="/search/physics?searchtype=author&query=Bakalov%2C+D">Dimitar Bakalov</a>, <a href="/search/physics?searchtype=author&query=Mocchiutti%2C+E">Emiliano Mocchiutti</a>, <a href="/search/physics?searchtype=author&query=Stoilov%2C+M">Mihail Stoilov</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">Andrea Vacchi</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="1511.05005v3-abstract-short" style="display: inline;"> Using simulated data, obtained with the FLUKA code, we derive empirical regularities about the propagation and stopping of low-energy negative muons in hydrogen and selected solid materials. The results are intended to help the preliminary stages of the set-up design for experimental studies of muon capture and muonic atom spectroscopy. Provided are approximate expressions for the parameters of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.05005v3-abstract-full').style.display = 'inline'; document.getElementById('1511.05005v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.05005v3-abstract-full" style="display: none;"> Using simulated data, obtained with the FLUKA code, we derive empirical regularities about the propagation and stopping of low-energy negative muons in hydrogen and selected solid materials. The results are intended to help the preliminary stages of the set-up design for experimental studies of muon capture and muonic atom spectroscopy. Provided are approximate expressions for the parameters of the the momentum, spatial and angular distribution of the propagating muons. In comparison with the available data on the stopping power and range of muons (with which they agree in the considered energy range) these results have the advantage to also describe the statistical spread of the muon characteristics of interest. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.05005v3-abstract-full').style.display = 'none'; document.getElementById('1511.05005v3-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 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">17 pages, 9 figures; Version accepted for publication in JINST</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation, Volume 11, March 2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.00543">arXiv:1511.00543</a> <span> [<a href="https://arxiv.org/pdf/1511.00543">pdf</a>, <a href="https://arxiv.org/ps/1511.00543">ps</a>, <a href="https://arxiv.org/format/1511.00543">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> PAMELA's measurements of geomagnetically trapped and albedo protons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</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="1511.00543v2-abstract-short" style="display: inline;"> Data from the PAMELA satellite experiment were used to perform a detailed measurement of under-cutoff protons at low Earth orbits. On the basis of a trajectory tracing approach using a realistic description of the magnetosphere, protons were classified into geomagnetically trapped and re-entrant albedo. The former include stably-trapped protons in the South Atlantic Anomaly, which were analyzed in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00543v2-abstract-full').style.display = 'inline'; document.getElementById('1511.00543v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00543v2-abstract-full" style="display: none;"> Data from the PAMELA satellite experiment were used to perform a detailed measurement of under-cutoff protons at low Earth orbits. On the basis of a trajectory tracing approach using a realistic description of the magnetosphere, protons were classified into geomagnetically trapped and re-entrant albedo. The former include stably-trapped protons in the South Atlantic Anomaly, which were analyzed in the framework of the adiabatic theory, investigating energy spectra, spatial and angular distributions; results were compared with the predictions of the AP8 and the PSB97 empirical trapped models. The albedo protons were classified into quasi-trapped, concentrating in the magnetic equatorial region, and un-trapped, spreading over all latitudes and including both short-lived (precipitating) and long-lived (pseudo-trapped) components. Features of the penumbra region around the geomagnetic cutoff were investigated as well. PAMELA observations significantly improve the characterization of the high energy proton populations in near Earth orbits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00543v2-abstract-full').style.display = 'none'; document.getElementById('1511.00543v2-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Conference: The 34th International Cosmic Ray Conference (ICRC2015), 30 July - 6 August, 2015, The Hague, The Netherlands, Volume: PoS(ICRC2015)288</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.00530">arXiv:1511.00530</a> <span> [<a href="https://arxiv.org/pdf/1511.00530">pdf</a>, <a href="https://arxiv.org/ps/1511.00530">ps</a>, <a href="https://arxiv.org/format/1511.00530">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> PAMELA's measurements of geomagnetic cutoff variations during solar energetic particle events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</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="1511.00530v1-abstract-short" style="display: inline;"> Data from the PAMELA satellite experiment were used to measure the geomagnetic cutoff for high-energy ($\gtrsim$ 80 MeV) protons during the solar particle events on 2006 December 13 and 14. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to single spacecraft orbits (about 94 minutes). Estimated cutoff values were cross-chec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00530v1-abstract-full').style.display = 'inline'; document.getElementById('1511.00530v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00530v1-abstract-full" style="display: none;"> Data from the PAMELA satellite experiment were used to measure the geomagnetic cutoff for high-energy ($\gtrsim$ 80 MeV) protons during the solar particle events on 2006 December 13 and 14. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to single spacecraft orbits (about 94 minutes). Estimated cutoff values were cross-checked with those obtained by means of a trajectory tracing approach based on dynamical empirical modeling of the Earth's magnetosphere. We find significant variations in the cutoff latitude, with a maximum suppression of about 6 deg for $\sim$80 MeV protons during the main phase of the storm. The observed reduction in the geomagnetic shielding and its temporal evolution were compared with the changes in the magnetosphere configuration, investigating the role of IMF, solar wind and geomagnetic (Kp, Dst and Sym-H indexes) variables and their correlation with PAMELA cutoff results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00530v1-abstract-full').style.display = 'none'; document.getElementById('1511.00530v1-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> 2 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Conference: The 34th International Cosmic Ray Conference (ICRC2015), 30 July - 6 August, 2015, The Hague, The Netherlands, Volume: PoS(ICRC2015)287</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.06253">arXiv:1504.06253</a> <span> [<a href="https://arxiv.org/pdf/1504.06253">pdf</a>, <a href="https://arxiv.org/ps/1504.06253">ps</a>, <a href="https://arxiv.org/format/1504.06253">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Re-Entrant Albedo Proton Fluxes Measured by the PAMELA Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Krutkov%2C+S+Y">S. Y. Krutkov</a> , et al. (34 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="1504.06253v1-abstract-short" style="display: inline;"> We present a precise measurement of downward-going albedo proton fluxes for kinetic energy above $\sim$ 70 MeV performed by the PAMELA experiment at an altitude between 350 and 610 km. On the basis of a trajectory tracing simulation, the analyzed protons were classified into quasi-trapped, concentrating in the magnetic equatorial region, and un-trapped spreading over all latitudes, including both… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.06253v1-abstract-full').style.display = 'inline'; document.getElementById('1504.06253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.06253v1-abstract-full" style="display: none;"> We present a precise measurement of downward-going albedo proton fluxes for kinetic energy above $\sim$ 70 MeV performed by the PAMELA experiment at an altitude between 350 and 610 km. On the basis of a trajectory tracing simulation, the analyzed protons were classified into quasi-trapped, concentrating in the magnetic equatorial region, and un-trapped spreading over all latitudes, including both short-lived (precipitating) and long-lived (pseudo-trapped) components. In addition, features of the penumbra region around the geomagnetic cutoff were investigated in detail. PAMELA results significantly improve the characterization of the high energy albedo proton populations at low Earth orbits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.06253v1-abstract-full').style.display = 'none'; document.getElementById('1504.06253v1-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">28 pages, 8 figures. Accepted for publication in Journal of Geophysical Research - Space Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.07682">arXiv:1503.07682</a> <span> [<a href="https://arxiv.org/pdf/1503.07682">pdf</a>, <a href="https://arxiv.org/ps/1503.07682">ps</a>, <a href="https://arxiv.org/format/1503.07682">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div 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/10.1088/1748-0221/10/05/P05002">10.1088/1748-0221/10/05/P05002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The effect of the displacement damage on the Charge Collection Efficiency in Silicon Drift Detectors for the LOFT satellite </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/physics?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/physics?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/physics?searchtype=author&query=Cadoux%2C+F">F. Cadoux</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/physics?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</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="1503.07682v1-abstract-short" style="display: inline;"> The technology of Silicon Drift Detectors (SDDs) has been selected for the two instruments aboard the Large Observatory For X-ray Timing (LOFT) space mission. LOFT underwent a three year long assessment phase as candidate for the M3 launch opportunity within the "Cosmic Vision 2015 -- 2025" long-term science plan of the European Space Agency. During the LOFT assessment phase, we studied the displa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.07682v1-abstract-full').style.display = 'inline'; document.getElementById('1503.07682v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.07682v1-abstract-full" style="display: none;"> The technology of Silicon Drift Detectors (SDDs) has been selected for the two instruments aboard the Large Observatory For X-ray Timing (LOFT) space mission. LOFT underwent a three year long assessment phase as candidate for the M3 launch opportunity within the "Cosmic Vision 2015 -- 2025" long-term science plan of the European Space Agency. During the LOFT assessment phase, we studied the displacement damage produced in the SDDs by the protons trapped in the Earth's magnetosphere. In a previous paper we discussed the effects of the Non Ionising Energy Losses from protons on the SDD leakage current. In this paper we report the measurement of the variation of Charge Collection Efficiency produced by displacement damage caused by protons and the comparison with the expected damage in orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.07682v1-abstract-full').style.display = 'none'; document.getElementById('1503.07682v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 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">17 pages, 7 figures. Accepted for publication by Journal of Instrumentation</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.06657">arXiv:1503.06657</a> <span> [<a href="https://arxiv.org/pdf/1503.06657">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.asr.2015.06.040">10.1016/j.asr.2015.06.040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A separation of electrons and protons in the GAMMA-400 gamma-ray telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Leonov%2C+A+A">A. A. Leonov</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Topchiev%2C+N+P">N. P. Topchiev</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Aptekar%2C+R+L">R. L. Aptekar</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskaja%2C+I+V">I. V. Arkhangelskaja</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskiy%2C+A+I">A. I. Arkhangelskiy</a>, <a href="/search/physics?searchtype=author&query=Bergstrom%2C+L">L. Bergstrom</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bobkov%2C+S+G">S. G. Bobkov</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+S">S. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/physics?searchtype=author&query=Cumani%2C+P">P. Cumani</a>, <a href="/search/physics?searchtype=author&query=Dedenko%2C+G+L">G. L. Dedenko</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=Dogiel%2C+V+A">V. A. Dogiel</a>, <a href="/search/physics?searchtype=author&query=Gorbunov%2C+M+S">M. S. Gorbunov</a>, <a href="/search/physics?searchtype=author&query=Gusakov%2C+Y+V">Yu. V. Gusakov</a> , et al. (41 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1503.06657v1-abstract-short" style="display: inline;"> The GAMMA-400 gamma-ray telescope is intended to measure the fluxes of gamma rays and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV. Such measurements concern with the following scientific goals: search for signatures of dark matter, investigation of gamma-ray point and extended sources, studies of the energy spectra of Galactic and extragalactic diffuse emissi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06657v1-abstract-full').style.display = 'inline'; document.getElementById('1503.06657v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.06657v1-abstract-full" style="display: none;"> The GAMMA-400 gamma-ray telescope is intended to measure the fluxes of gamma rays and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV. Such measurements concern with the following scientific goals: search for signatures of dark matter, investigation of gamma-ray point and extended sources, studies of the energy spectra of Galactic and extragalactic diffuse emission, studies of gamma-ray bursts and gamma-ray emission from the active Sun, as well as high-precision measurements of spectra of high-energy electrons and positrons, protons, and nuclei up to the knee. The main components of cosmic rays are protons and helium nuclei, whereas the part of lepton component in the total flux is ~10E-3 for high energies. In present paper, the capability of the GAMMA-400 gamma-ray telescope to distinguish electrons and positrons from protons in cosmic rays is investigated. The individual contribution to the proton rejection is studied for each detector system of the GAMMA-400 gamma-ray telescope. Using combined information from all detector systems allow us to provide the proton rejection from electrons with a factor of ~4x10E5 for vertical incident particles and ~3x10E5 for particles with initial inclination of 30 degrees. The calculations were performed for the electron energy range from 50 GeV to 1 TeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06657v1-abstract-full').style.display = 'none'; document.getElementById('1503.06657v1-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 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">19 pages, 10 figures, submitted to Advances and Space Research</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.4239">arXiv:1412.4239</a> <span> [<a href="https://arxiv.org/pdf/1412.4239">pdf</a>, <a href="https://arxiv.org/format/1412.4239">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 Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The GAMMA-400 space observatory: status and perspectives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Topchiev%2C+N+P">N. P. Topchiev</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Aptekar%2C+R+L">R. L. Aptekar</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskaja%2C+I+V">I. V. Arkhangelskaja</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskiy%2C+A+I">A. I. Arkhangelskiy</a>, <a href="/search/physics?searchtype=author&query=Bergstrom%2C+L">L. Bergstrom</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bobkov%2C+S+G">S. G. Bobkov</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+S">S. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Boyarchuk%2C+K+A">K. A. Boyarchuk</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/physics?searchtype=author&query=Cumani%2C+P">P. Cumani</a>, <a href="/search/physics?searchtype=author&query=Dedenko%2C+G+L">G. L. Dedenko</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=Dogiel%2C+V+A">V. A. Dogiel</a>, <a href="/search/physics?searchtype=author&query=Gorbunov%2C+M+S">M. S. Gorbunov</a>, <a href="/search/physics?searchtype=author&query=Gusakov%2C+Y+V">Yu. V. Gusakov</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="1412.4239v1-abstract-short" style="display: inline;"> The present design of the new space observatory GAMMA-400 is presented in this paper. The instrument has been designed for the optimal detection of gamma rays in a broad energy range (from ~100 MeV up to 3 TeV), with excellent angular and energy resolution. The observatory will also allow precise and high statistic studies of the electron component in the cosmic rays up to the multi TeV region, as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4239v1-abstract-full').style.display = 'inline'; document.getElementById('1412.4239v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.4239v1-abstract-full" style="display: none;"> The present design of the new space observatory GAMMA-400 is presented in this paper. The instrument has been designed for the optimal detection of gamma rays in a broad energy range (from ~100 MeV up to 3 TeV), with excellent angular and energy resolution. The observatory will also allow precise and high statistic studies of the electron component in the cosmic rays up to the multi TeV region, as well as protons and nuclei spectra up to the knee region. The GAMMA-400 observatory will allow to address a broad range of science topics, like search for signatures of dark matter, studies of Galactic and extragalactic gamma-ray sources, Galactic and extragalactic diffuse emission, gamma-ray bursts and charged cosmic rays acceleration and diffusion mechanism up to the knee. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4239v1-abstract-full').style.display = 'none'; document.getElementById('1412.4239v1-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 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.1765">arXiv:1412.1765</a> <span> [<a href="https://arxiv.org/pdf/1412.1765">pdf</a>, <a href="https://arxiv.org/ps/1412.1765">ps</a>, <a href="https://arxiv.org/format/1412.1765">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 Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Back-Tracing and Flux Reconstruction for Solar Events with PAMELA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</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="1412.1765v5-abstract-short" style="display: inline;"> The PAMELA satellite-borne experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from $\sim$80 MeV to several GeV in near-Earth space. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies related to SEP events. This paper focuses on the analysis methods dev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1765v5-abstract-full').style.display = 'inline'; document.getElementById('1412.1765v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.1765v5-abstract-full" style="display: none;"> The PAMELA satellite-borne experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from $\sim$80 MeV to several GeV in near-Earth space. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies related to SEP events. This paper focuses on the analysis methods developed to estimate SEP energy spectra as a function of the particle pitch angle with respect to the Interplanetary Magnetic Field (IMF). The crucial ingredient is provided by an accurate simulation of the asymptotic exposition of the PAMELA apparatus, based on a realistic reconstruction of particle trajectories in the Earth's magnetosphere. As case study, the results of the calculation for the May 17, 2012 event are reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1765v5-abstract-full').style.display = 'none'; document.getElementById('1412.1765v5-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> 2 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">25 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.1258">arXiv:1412.1258</a> <span> [<a href="https://arxiv.org/pdf/1412.1258">pdf</a>, <a href="https://arxiv.org/ps/1412.1258">ps</a>, <a href="https://arxiv.org/format/1412.1258">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/799/1/L4">10.1088/2041-8205/799/1/L4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Trapped proton fluxes at low Earth orbits measured by the PAMELA experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Danilchenko%2C+I+A">I. A. Danilchenko</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a> , et al. (37 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="1412.1258v2-abstract-short" style="display: inline;"> We report an accurate measurement of the geomagnetically trapped proton fluxes for kinetic energy above > 70 MeV performed by the PAMELA mission at low Earth orbits (350-610 km). Data were analyzed in the frame of the adiabatic theory of charged particle motion in the geomagnetic field. Flux properties were investigated in detail, providing a full characterization of the particle radiation in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1258v2-abstract-full').style.display = 'inline'; document.getElementById('1412.1258v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.1258v2-abstract-full" style="display: none;"> We report an accurate measurement of the geomagnetically trapped proton fluxes for kinetic energy above > 70 MeV performed by the PAMELA mission at low Earth orbits (350-610 km). Data were analyzed in the frame of the adiabatic theory of charged particle motion in the geomagnetic field. Flux properties were investigated in detail, providing a full characterization of the particle radiation in the South Atlantic Anomaly region, including locations, energy spectra and pitch angle distributions. PAMELA results significantly improve the description of the Earth's radiation environment at low altitudes placing important constraints on the trapping and interaction processes, and can be used to validate current trapped particle radiation models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1258v2-abstract-full').style.display = 'none'; document.getElementById('1412.1258v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">22 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 799 L4, 2015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.1127">arXiv:1409.1127</a> <span> [<a href="https://arxiv.org/pdf/1409.1127">pdf</a>, <a href="https://arxiv.org/ps/1409.1127">ps</a>, <a href="https://arxiv.org/format/1409.1127">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physleta.2014.11.025">10.1016/j.physleta.2014.11.025 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Theoretical and computational study of the energy dependence of the muon transfer rate from hydrogen to higher-Z gases </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bakalov%2C+D">Dimitar Bakalov</a>, <a href="/search/physics?searchtype=author&query=Adamczak%2C+A">Andrzej Adamczak</a>, <a href="/search/physics?searchtype=author&query=Stoilov%2C+M">Mihail Stoilov</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">Andrea Vacchi</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="1409.1127v2-abstract-short" style="display: inline;"> The recent PSI Lamb shift experiment and the controversy about proton size revived the interest in measuring the hyperfine splitting in muonic hydrogen as an alternative possibility for comparing ordinary and muonic hydrogen spectroscopy data on proton electromagnetic structure. This measurement critically depends on the energy dependence of the muon transfer rate to heavier gases in the epitherma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.1127v2-abstract-full').style.display = 'inline'; document.getElementById('1409.1127v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.1127v2-abstract-full" style="display: none;"> The recent PSI Lamb shift experiment and the controversy about proton size revived the interest in measuring the hyperfine splitting in muonic hydrogen as an alternative possibility for comparing ordinary and muonic hydrogen spectroscopy data on proton electromagnetic structure. This measurement critically depends on the energy dependence of the muon transfer rate to heavier gases in the epithermal range. The available data provide only qualitative information, and the theoretical predictions have not been verified. We propose a new method by measurements of the transfer rate in thermalized target at different temperatures, estimate its accuracy and investigate the optimal experimental conditions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.1127v2-abstract-full').style.display = 'none'; document.getElementById('1409.1127v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.6548">arXiv:1408.6548</a> <span> [<a href="https://arxiv.org/pdf/1408.6548">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <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/10.1117/12.2055747">10.1117/12.2055747 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radiation tests of the Silicon Drift Detectors for LOFT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/physics?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/physics?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/physics?searchtype=author&query=Bugiel%2C+S">S. Bugiel</a>, <a href="/search/physics?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/physics?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/physics?searchtype=author&query=Kendziorra%2C+E">E. Kendziorra</a>, <a href="/search/physics?searchtype=author&query=Muleri%2C+F">F. Muleri</a>, <a href="/search/physics?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/physics?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/physics?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</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="1408.6548v1-abstract-short" style="display: inline;"> During the three years long assessment phase of the LOFT mission, candidate to the M3 launch opportunity of the ESA Cosmic Vision programme, we estimated and measured the radiation damage of the silicon drift detectors (SDDs) of the satellite instrumentation. In particular, we irradiated the detectors with protons (of 0.8 and 11 MeV energy) to study the increment of leakage current and the variati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.6548v1-abstract-full').style.display = 'inline'; document.getElementById('1408.6548v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.6548v1-abstract-full" style="display: none;"> During the three years long assessment phase of the LOFT mission, candidate to the M3 launch opportunity of the ESA Cosmic Vision programme, we estimated and measured the radiation damage of the silicon drift detectors (SDDs) of the satellite instrumentation. In particular, we irradiated the detectors with protons (of 0.8 and 11 MeV energy) to study the increment of leakage current and the variation of the charge collection efficiency produced by the displacement damage, and we "bombarded" the detectors with hypervelocity dust grains to measure the effect of the debris impacts. In this paper we describe the measurements and discuss the results in the context of the LOFT mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.6548v1-abstract-full').style.display = 'none'; document.getElementById('1408.6548v1-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> 27 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 914464</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.1710">arXiv:1407.1710</a> <span> [<a href="https://arxiv.org/pdf/1407.1710">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/9/08/P08008">10.1088/1748-0221/9/08/P08008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the VEGA ASIC coupled to large area position-sensitive Silicon Drift Detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Campana%2C+R">R. Campana</a>, <a href="/search/physics?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/physics?searchtype=author&query=Fuschino%2C+F">F. Fuschino</a>, <a href="/search/physics?searchtype=author&query=Ahangarianabhari%2C+M">M. Ahangarianabhari</a>, <a href="/search/physics?searchtype=author&query=Macera%2C+D">D. Macera</a>, <a href="/search/physics?searchtype=author&query=Bertuccio%2C+G">G. Bertuccio</a>, <a href="/search/physics?searchtype=author&query=Grassi%2C+M">M. Grassi</a>, <a href="/search/physics?searchtype=author&query=Labanti%2C+C">C. Labanti</a>, <a href="/search/physics?searchtype=author&query=Marisaldi%2C+M">M. Marisaldi</a>, <a href="/search/physics?searchtype=author&query=Malcovati%2C+P">P. Malcovati</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/physics?searchtype=author&query=Andreani%2C+L">L. Andreani</a>, <a href="/search/physics?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a>, <a href="/search/physics?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/physics?searchtype=author&query=Favre%2C+Y">Y. Favre</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/physics?searchtype=author&query=Muleri%2C+F">F. Muleri</a>, <a href="/search/physics?searchtype=author&query=Rashevskaya%2C+I">I. Rashevskaya</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Ficorella%2C+F">F. Ficorella</a>, <a href="/search/physics?searchtype=author&query=Giacomini%2C+G">G. Giacomini</a>, <a href="/search/physics?searchtype=author&query=Picciotto%2C+A">A. Picciotto</a>, <a href="/search/physics?searchtype=author&query=Zuffa%2C+M">M. Zuffa</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="1407.1710v1-abstract-short" style="display: inline;"> Low-noise, position-sensitive Silicon Drift Detectors (SDDs) are particularly useful for experiments in which a good energy resolution combined with a large sensitive area is required, as in the case of X-ray astronomy space missions and medical applications. This paper presents the experimental characterization of VEGA, a custom Application Specific Integrated Circuit (ASIC) used as the front-end… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.1710v1-abstract-full').style.display = 'inline'; document.getElementById('1407.1710v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.1710v1-abstract-full" style="display: none;"> Low-noise, position-sensitive Silicon Drift Detectors (SDDs) are particularly useful for experiments in which a good energy resolution combined with a large sensitive area is required, as in the case of X-ray astronomy space missions and medical applications. This paper presents the experimental characterization of VEGA, a custom Application Specific Integrated Circuit (ASIC) used as the front-end electronics for XDXL-2, a large-area (30.5 cm^2) SDD prototype. The ASICs were integrated on a specifically developed PCB hosting also the detector. Results on the ASIC noise performances, both stand-alone and bonded to the large area SDD, are presented and discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.1710v1-abstract-full').style.display = 'none'; document.getElementById('1407.1710v1-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">15 pages, 11 figures. Accepted for publication in Journal of Instrumentation (JINST)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation, Volume 9, August 2014 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.5466">arXiv:1405.5466</a> <span> [<a href="https://arxiv.org/pdf/1405.5466">pdf</a>, <a href="https://arxiv.org/ps/1405.5466">ps</a>, <a href="https://arxiv.org/format/1405.5466">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 Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1088/1748-0221/9/07/P07016">10.1088/1748-0221/9/07/P07016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the effect of Non Ionising Energy Losses on the leakage current of Silicon Drift Detector prototypes for the LOFT satellite </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/physics?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/physics?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+R">R. Campana</a>, <a href="/search/physics?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/physics?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/physics?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/physics?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</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="1405.5466v3-abstract-short" style="display: inline;"> The silicon drift detectors are at the basis of the instrumentation aboard the Large Observatory For x-ray Timing (LOFT) satellite mission, which underwent a three year assessment phase within the "Cosmic Vision 2015 - 2025" long-term science plan of the European Space Agency. Silicon detectors are especially sensitive to the displacement damage, produced by the non ionising energy losses of charg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.5466v3-abstract-full').style.display = 'inline'; document.getElementById('1405.5466v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.5466v3-abstract-full" style="display: none;"> The silicon drift detectors are at the basis of the instrumentation aboard the Large Observatory For x-ray Timing (LOFT) satellite mission, which underwent a three year assessment phase within the "Cosmic Vision 2015 - 2025" long-term science plan of the European Space Agency. Silicon detectors are especially sensitive to the displacement damage, produced by the non ionising energy losses of charged and neutral particles, leading to an increase of the device leakage current and thus worsening the spectral resolution. During the LOFT assessment phase, we irradiated two silicon drift detectors with a proton beam at the Proton Irradiation Facility in the accelerator of the Paul Scherrer Institute and we measured the increase in leakage current. In this paper we report the results of the irradiation and we discuss the impact of the radiation damage on the LOFT scientific performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.5466v3-abstract-full').style.display = 'none'; document.getElementById('1405.5466v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">21 pages, 7 figures, 2 tables. Accepted for publication by Journal of Instrumentation (JINST)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation, Volume 9, July 2014 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.7967">arXiv:1307.7967</a> <span> [<a href="https://arxiv.org/pdf/1307.7967">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> </div> </div> <p class="title is-5 mathjax"> IRIDE White Book, An Interdisciplinary Research Infrastructure based on Dual Electron linacs&lasers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Alesini%2C+D">D. Alesini</a>, <a href="/search/physics?searchtype=author&query=Alessandroni%2C+M">M. Alessandroni</a>, <a href="/search/physics?searchtype=author&query=Anania%2C+M+P">M. P. Anania</a>, <a href="/search/physics?searchtype=author&query=Andreas%2C+S">S. Andreas</a>, <a href="/search/physics?searchtype=author&query=Angelone%2C+M">M. Angelone</a>, <a href="/search/physics?searchtype=author&query=Arcovito%2C+A">A. Arcovito</a>, <a href="/search/physics?searchtype=author&query=Arnesano%2C+F">F. Arnesano</a>, <a href="/search/physics?searchtype=author&query=Artioli%2C+M">M. Artioli</a>, <a href="/search/physics?searchtype=author&query=Avaldi%2C+L">L. Avaldi</a>, <a href="/search/physics?searchtype=author&query=Babusci%2C+D">D. Babusci</a>, <a href="/search/physics?searchtype=author&query=Bacci%2C+A">A. Bacci</a>, <a href="/search/physics?searchtype=author&query=Balerna%2C+A">A. Balerna</a>, <a href="/search/physics?searchtype=author&query=Bartalucci%2C+S">S. Bartalucci</a>, <a href="/search/physics?searchtype=author&query=Bedogni%2C+R">R. Bedogni</a>, <a href="/search/physics?searchtype=author&query=Bellaveglia%2C+M">M. Bellaveglia</a>, <a href="/search/physics?searchtype=author&query=Bencivenga%2C+F">F. Bencivenga</a>, <a href="/search/physics?searchtype=author&query=Benfatto%2C+M">M. Benfatto</a>, <a href="/search/physics?searchtype=author&query=Biedron%2C+S">S. Biedron</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/physics?searchtype=author&query=Bolognesi%2C+M">M. Bolognesi</a>, <a href="/search/physics?searchtype=author&query=Bolognesi%2C+P">P. Bolognesi</a>, <a href="/search/physics?searchtype=author&query=Boni%2C+R">R. Boni</a>, <a href="/search/physics?searchtype=author&query=Bonifacio%2C+R">R. Bonifacio</a>, <a href="/search/physics?searchtype=author&query=Boscolo%2C+M">M. Boscolo</a>, <a href="/search/physics?searchtype=author&query=Boscherini%2C+F">F. Boscherini</a> , et al. (189 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="1307.7967v1-abstract-short" style="display: inline;"> This report describes the scientific aims and potentials as well as the preliminary technical design of IRIDE, an innovative tool for multi-disciplinary investigations in a wide field of scientific, technological and industrial applications. IRIDE will be a high intensity 'particle factory', based on a combination of a high duty cycle radio-frequency superconducting electron linac and of high ener… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.7967v1-abstract-full').style.display = 'inline'; document.getElementById('1307.7967v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.7967v1-abstract-full" style="display: none;"> This report describes the scientific aims and potentials as well as the preliminary technical design of IRIDE, an innovative tool for multi-disciplinary investigations in a wide field of scientific, technological and industrial applications. IRIDE will be a high intensity 'particle factory', based on a combination of a high duty cycle radio-frequency superconducting electron linac and of high energy lasers. Conceived to provide unique research possibilities for particle physics, for condensed matter physics, chemistry and material science, for structural biology and industrial applications, IRIDE will open completely new research possibilities and advance our knowledge in many branches of science and technology. IRIDE will contribute to open new avenues of discoveries and to address most important riddles: What does matter consist of? What is the structure of proteins that have a fundamental role in life processes? What can we learn from protein structure to improve the treatment of diseases and to design more efficient drugs? But also how does an electronic chip behave under the effect of radiations? How can the heat flow in a large heat exchanger be optimized? The scientific potential of IRIDE is far reaching and justifies the construction of such a large facility in Italy in synergy with the national research institutes and companies and in the framework of the European and international research. It will impact also on R&D work for ILC, FEL, and will be complementarity to other large scale accelerator projects. IRIDE is also intended to be realized in subsequent stages of development depending on the assigned priorities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.7967v1-abstract-full').style.display = 'none'; document.getElementById('1307.7967v1-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 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">270 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/1307.4204">arXiv:1307.4204</a> <span> [<a href="https://arxiv.org/pdf/1307.4204">pdf</a>, <a href="https://arxiv.org/format/1307.4204">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 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/10.1016/j.nima.2013.04.049">10.1016/j.nima.2013.04.049 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A setup for soft proton irradiation of X-ray detectors for future astronomical space missions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Diebold%2C+S">Sebastian Diebold</a>, <a href="/search/physics?searchtype=author&query=Azzarello%2C+P">Philipp Azzarello</a>, <a href="/search/physics?searchtype=author&query=Del+Monte%2C+E">Ettore Del Monte</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">Marco Feroci</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">Josef Jochum</a>, <a href="/search/physics?searchtype=author&query=Kendziorra%2C+E">Eckhard Kendziorra</a>, <a href="/search/physics?searchtype=author&query=Perinati%2C+E">Emanuele Perinati</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">Alexandre Rachevski</a>, <a href="/search/physics?searchtype=author&query=Santangelo%2C+A">Andrea Santangelo</a>, <a href="/search/physics?searchtype=author&query=Tenzer%2C+C">Christoph Tenzer</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">Andrea Vacchi</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">Gianluigi Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">Nicola Zampa</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="1307.4204v1-abstract-short" style="display: inline;"> Protons that are trapped in the Earth's magnetic field are one of the main threats to astronomical X-ray observatories. Soft protons, in the range from tens of keV up to a few MeV, impinging on silicon X-ray detectors can lead to a significant degradation of the detector performance. Especially in low earth orbits an enhancement of the soft proton flux has been found. A setup to irradiate detector… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.4204v1-abstract-full').style.display = 'inline'; document.getElementById('1307.4204v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.4204v1-abstract-full" style="display: none;"> Protons that are trapped in the Earth's magnetic field are one of the main threats to astronomical X-ray observatories. Soft protons, in the range from tens of keV up to a few MeV, impinging on silicon X-ray detectors can lead to a significant degradation of the detector performance. Especially in low earth orbits an enhancement of the soft proton flux has been found. A setup to irradiate detectors with soft protons has been constructed at the Van-de-Graaff accelerator of the Physikalisches Institut of the University of T眉bingen. Key advantages are a high flux uniformity over a large area, to enable irradiations of large detectors, and a monitoring system for the applied fluence, the beam uniformity, and the spectrum, that allows testing of detector prototypes in early development phases, when readout electronics are not yet available. Two irradiation campaigns have been performed so far with this setup. The irradiated detectors are silicon drift detectors, designated for the use on-board the LOFT space mission. This paper gives a description of the experimental setup and the associated monitoring system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.4204v1-abstract-full').style.display = 'none'; document.getElementById('1307.4204v1-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 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">20 pages, 10 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Instruments and Methods in Physics Research Section A, Volume 721 (2013), Pages 65-72 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1209.3094">arXiv:1209.3094</a> <span> [<a href="https://arxiv.org/pdf/1209.3094">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <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/10.1117/12.926118">10.1117/12.926118 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Accelerator experiments with soft protons and hyper-velocity dust particles: application to ongoing projects of future X-ray missions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/physics?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/physics?searchtype=author&query=Kendziorra%2C+E">E. Kendziorra</a>, <a href="/search/physics?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/physics?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/physics?searchtype=author&query=Bugiel%2C+S">S. Bugiel</a>, <a href="/search/physics?searchtype=author&query=Srama%2C+R">R. Srama</a>, <a href="/search/physics?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/physics?searchtype=author&query=Rubini%2C+A">A. Rubini</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/physics?searchtype=author&query=Rashevskaya%2C+I">I. Rashevskaya</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/physics?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/physics?searchtype=author&query=Herder%2C+J+-+d">J. -W. den Herder</a>, <a href="/search/physics?searchtype=author&query=Zane%2C+S">S. Zane</a>, <a href="/search/physics?searchtype=author&query=Brandt%2C+S">S. Brandt</a>, <a href="/search/physics?searchtype=author&query=Hernanz%2C+M">M. Hernanz</a>, <a href="/search/physics?searchtype=author&query=Leutenegger%2C+M+A">M. A. Leutenegger</a>, <a href="/search/physics?searchtype=author&query=Kelley%2C+R+L">R. L. Kelley</a>, <a href="/search/physics?searchtype=author&query=Kilbourne%2C+C+A">C. A. Kilbourne</a> , et al. (9 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="1209.3094v1-abstract-short" style="display: inline;"> We report on our activities, currently in progress, aimed at performing accelerator experiments with soft protons and hyper-velocity dust particles. They include tests of different types of X-ray detectors and related components (such as filters) and measurements of scattering of soft protons and hyper-velocity dust particles off X-ray mirror shells. These activities have been identified as a goal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.3094v1-abstract-full').style.display = 'inline'; document.getElementById('1209.3094v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1209.3094v1-abstract-full" style="display: none;"> We report on our activities, currently in progress, aimed at performing accelerator experiments with soft protons and hyper-velocity dust particles. They include tests of different types of X-ray detectors and related components (such as filters) and measurements of scattering of soft protons and hyper-velocity dust particles off X-ray mirror shells. These activities have been identified as a goal in the context of a number of ongoing space projects in order to assess the risk posed by environmental radiation and dust and qualify the adopted instrumentation with respect to possible damage or performance degradation. In this paper we focus on tests for the Silicon Drift Detectors (SDDs) used aboard the LOFT space mission. We use the Van de Graaff accelerators at the University of T眉bingen and at the Max Planck Institute for Nuclear Physics (MPIK) in Heidelberg, for soft proton and hyper-velocity dust tests respectively. We present the experimental set-up adopted to perform the tests, status of the activities and some very preliminary results achieved at present time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.3094v1-abstract-full').style.display = 'none'; document.getElementById('1209.3094v1-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 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">Proceedings of SPIE, Vol. 8443, Paper No. 8443-24, 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/1209.1501">arXiv:1209.1501</a> <span> [<a href="https://arxiv.org/pdf/1209.1501">pdf</a>, <a href="https://arxiv.org/format/1209.1501">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 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/10.1117/12.926000">10.1117/12.926000 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simulations of the X-ray imaging capabilities of the Silicon Drift Detectors (SDD) for the LOFT Wide Field Monitor </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+R">R. Campana</a>, <a href="/search/physics?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/physics?searchtype=author&query=Donnarumma%2C+I">I. Donnarumma</a>, <a href="/search/physics?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/physics?searchtype=author&query=Muleri%2C+F">F. Muleri</a>, <a href="/search/physics?searchtype=author&query=Pacciani%2C+L">L. Pacciani</a>, <a href="/search/physics?searchtype=author&query=Soffitta%2C+P">P. Soffitta</a>, <a href="/search/physics?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/physics?searchtype=author&query=Suchy%2C+S">S. Suchy</a>, <a href="/search/physics?searchtype=author&query=Brandt%2C+S">S. Brandt</a>, <a href="/search/physics?searchtype=author&query=Budtz-J%C3%B8rgensen%2C+C">C. Budtz-J酶rgensen</a>, <a href="/search/physics?searchtype=author&query=Hernanz%2C+M">M. Hernanz</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="1209.1501v1-abstract-short" style="display: inline;"> The Large Observatory For X-ray Timing (LOFT), selected by ESA as one of the four Cosmic Vision M3 candidate missions to undergo an assessment phase, will revolutionize the study of compact objects in our galaxy and of the brightest supermassive black holes in active galactic nuclei. The Large Area Detector (LAD), carrying an unprecedented effective area of 10 m^2, is complemented by a coded-mask… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.1501v1-abstract-full').style.display = 'inline'; document.getElementById('1209.1501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1209.1501v1-abstract-full" style="display: none;"> The Large Observatory For X-ray Timing (LOFT), selected by ESA as one of the four Cosmic Vision M3 candidate missions to undergo an assessment phase, will revolutionize the study of compact objects in our galaxy and of the brightest supermassive black holes in active galactic nuclei. The Large Area Detector (LAD), carrying an unprecedented effective area of 10 m^2, is complemented by a coded-mask Wide Field Monitor, in charge of monitoring a large fraction of the sky potentially accessible to the LAD, to provide the history and context for the sources observed by LAD and to trigger its observations on their most interesting and extreme states. In this paper we present detailed simulations of the imaging capabilities of the Silicon Drift Detectors developed for the LOFT Wide Field Monitor detection plane. The simulations explore a large parameter space for both the detector design and the environmental conditions, allowing us to optimize the detector characteristics and demonstrating the X-ray imaging performance of the large-area SDDs in the 2-50 keV energy band. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.1501v1-abstract-full').style.display = 'none'; document.getElementById('1209.1501v1-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 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">Proceedings of SPIE, Vol. 8443, Paper No. 8443-210, 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/physics/0512057">arXiv:physics/0512057</a> <span> [<a href="https://arxiv.org/pdf/physics/0512057">pdf</a>, <a href="https://arxiv.org/ps/physics/0512057">ps</a>, <a href="https://arxiv.org/format/physics/0512057">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2006.05.057">10.1016/j.nima.2006.05.057 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Beam test results of the irradiated Silicon Drift Detector for ALICE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Kushpil%2C+S">S. Kushpil</a>, <a href="/search/physics?searchtype=author&query=Crescio%2C+E">E. Crescio</a>, <a href="/search/physics?searchtype=author&query=Giubellino%2C+P">P. Giubellino</a>, <a href="/search/physics?searchtype=author&query=Idzik%2C+M">M. Idzik</a>, <a href="/search/physics?searchtype=author&query=Kolozhvari%2C+A">A. Kolozhvari</a>, <a href="/search/physics?searchtype=author&query=Kushpil%2C+V">V. Kushpil</a>, <a href="/search/physics?searchtype=author&query=Martinez%2C+M+I">M. I. Martinez</a>, <a href="/search/physics?searchtype=author&query=Mazza%2C+G">G. Mazza</a>, <a href="/search/physics?searchtype=author&query=Mazzoni%2C+A">A. Mazzoni</a>, <a href="/search/physics?searchtype=author&query=Meddi%2C+F">F. Meddi</a>, <a href="/search/physics?searchtype=author&query=Nouais%2C+D">D. Nouais</a>, <a href="/search/physics?searchtype=author&query=Petracek%2C+V">V. Petracek</a>, <a href="/search/physics?searchtype=author&query=Piemonte%2C+C">C. Piemonte</a>, <a href="/search/physics?searchtype=author&query=Rashevsky%2C+A">A. Rashevsky</a>, <a href="/search/physics?searchtype=author&query=Riccati%2C+L">L. Riccati</a>, <a href="/search/physics?searchtype=author&query=Rivetti%2C+A">A. Rivetti</a>, <a href="/search/physics?searchtype=author&query=Tosello%2C+F">F. Tosello</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Wheadon%2C+R">R. Wheadon</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="physics/0512057v1-abstract-short" style="display: inline;"> The Silicon Drift Detectors will equip two of the six cylindrical layers of high precision position sensitive detectors in the ITS of the ALICE experiment at LHC. In this paper we report the beam test results of a SDD irradiated with 1 GeV electrons. The aim of this test was to verify the radiation tolerance of the device under an electron fluence equivalent to twice particle fluence expected du… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/0512057v1-abstract-full').style.display = 'inline'; document.getElementById('physics/0512057v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="physics/0512057v1-abstract-full" style="display: none;"> The Silicon Drift Detectors will equip two of the six cylindrical layers of high precision position sensitive detectors in the ITS of the ALICE experiment at LHC. In this paper we report the beam test results of a SDD irradiated with 1 GeV electrons. The aim of this test was to verify the radiation tolerance of the device under an electron fluence equivalent to twice particle fluence expected during 10 years of ALICE operation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/0512057v1-abstract-full').style.display = 'none'; document.getElementById('physics/0512057v1-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 December, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2005. </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,6 figures, to appear in the proceedings of International Workshop In high Multiplicity Environments (TIME'05), 3-7 October 2005, Zurich,Switzerland</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Instrum.Meth.A566:94-99,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/physics/0109010">arXiv:physics/0109010</a> <span> [<a href="https://arxiv.org/pdf/physics/0109010">pdf</a>, <a href="https://arxiv.org/ps/physics/0109010">ps</a>, <a href="https://arxiv.org/format/physics/0109010">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="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/S0168-9002(01)02186-6">10.1016/S0168-9002(01)02186-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A High Granularity Imaging Calorimeter for Cosmic-Ray Physics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Mocchiutti%2C+E">E. Mocchiutti</a>, <a href="/search/physics?searchtype=author&query=Schiavon%2C+P">P. Schiavon</a>, <a href="/search/physics?searchtype=author&query=Scian%2C+G">G. Scian</a>, <a href="/search/physics?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/physics?searchtype=author&query=Zampa%2C+N">N. Zampa</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="physics/0109010v1-abstract-short" style="display: inline;"> An imaging calorimeter has been designed and is being built for the PAMELA satellite-borne experiment. The physics goals of the experiment are the measurement of the flux of antiprotons, positrons and light isotopes in the cosmic radiation. The calorimeter is designed to perform a precise measurement of the total energy deposited, to reconstruct the spatial development of the showers (both in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/0109010v1-abstract-full').style.display = 'inline'; document.getElementById('physics/0109010v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="physics/0109010v1-abstract-full" style="display: none;"> An imaging calorimeter has been designed and is being built for the PAMELA satellite-borne experiment. The physics goals of the experiment are the measurement of the flux of antiprotons, positrons and light isotopes in the cosmic radiation. The calorimeter is designed to perform a precise measurement of the total energy deposited, to reconstruct the spatial development of the showers (both in the longitudinal and in the transverse directions), and to measure the energy distribution along the shower itself. From this information, the calorimeter will identify antiprotons from a electron background and positrons in a background of protons with an efficiency of about 95% and a rejection power better than 10^-4. Furthermore, a self-trigger system has been implemented with the calorimeter that will be employed to measure high-energy (from about 300 GeV to more than 1 TeV) electrons. The instrument is composed of 22 layers of tungsten, each sandwiched between two "views" of silicon strip detectors (X and Y). The signals are read out by a custom VLSI front-end chip, the CR1.4P, specifically designed for the PAMELA calorimeter, with a dynamic range of 7.14 pC or 1400 mip (minimum ionizing particle). We report on the simulated performance and prototype design. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/0109010v1-abstract-full').style.display = 'none'; document.getElementById('physics/0109010v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">26 pages, 19 figures, elsart LATEX style, submitted to Nucl. Instrum. and Meth</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Instrum.Meth. A487 (2002) 407-422 </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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