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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/2305.17762">arXiv:2305.17762</a> <span> [<a href="https://arxiv.org/pdf/2305.17762">pdf</a>, <a href="https://arxiv.org/format/2305.17762">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Measurements of the Cherenkov effect in direct detection of charged particles with SiPMs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Carnesecchi%2C+F">F. Carnesecchi</a>, <a href="/search/physics?searchtype=author&query=Sabiu%2C+B">B. Sabiu</a>, <a href="/search/physics?searchtype=author&query=Strazzi%2C+S">S. Strazzi</a>, <a href="/search/physics?searchtype=author&query=Vignola%2C+G">G. Vignola</a>, <a href="/search/physics?searchtype=author&query=Agrawal%2C+N">N. Agrawal</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/physics?searchtype=author&query=Cavazza%2C+D">D. Cavazza</a>, <a href="/search/physics?searchtype=author&query=Cifarelli%2C+L">L. Cifarelli</a>, <a href="/search/physics?searchtype=author&query=Colocci%2C+M">M. Colocci</a>, <a href="/search/physics?searchtype=author&query=Durando%2C+S">S. Durando</a>, <a href="/search/physics?searchtype=author&query=Ercolessi%2C+F">F. Ercolessi</a>, <a href="/search/physics?searchtype=author&query=Falchieri%2C+D">D. Falchieri</a>, <a href="/search/physics?searchtype=author&query=Ficorella%2C+A">A. Ficorella</a>, <a href="/search/physics?searchtype=author&query=Fraticelli%2C+C">C. Fraticelli</a>, <a href="/search/physics?searchtype=author&query=Garbini%2C+M">M. Garbini</a>, <a href="/search/physics?searchtype=author&query=Giacalone%2C+M">M. Giacalone</a>, <a href="/search/physics?searchtype=author&query=Gola%2C+A">A. Gola</a>, <a href="/search/physics?searchtype=author&query=Hatzifotiadou%2C+D">D. Hatzifotiadou</a>, <a href="/search/physics?searchtype=author&query=Jacazio%2C+N">N. Jacazio</a>, <a href="/search/physics?searchtype=author&query=Margotti%2C+A">A. Margotti</a>, <a href="/search/physics?searchtype=author&query=Malfattore%2C+G">G. Malfattore</a>, <a href="/search/physics?searchtype=author&query=Nania%2C+R">R. Nania</a> , et al. (12 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="2305.17762v1-abstract-short" style="display: inline;"> In this paper, different Silicon PhotoMultiplier (SiPM) sensors have been tested with charged particles to characterize the Cherenkov light produced in the sensor protection layer. A careful position scan of the SiPM response has been performed with different prototypes, confirming the large number of firing cells and proving almost full efficiency, with the SiPM filling factor essentially negligi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.17762v1-abstract-full').style.display = 'inline'; document.getElementById('2305.17762v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.17762v1-abstract-full" style="display: none;"> In this paper, different Silicon PhotoMultiplier (SiPM) sensors have been tested with charged particles to characterize the Cherenkov light produced in the sensor protection layer. A careful position scan of the SiPM response has been performed with different prototypes, confirming the large number of firing cells and proving almost full efficiency, with the SiPM filling factor essentially negligible. This study also allowed us to study the time resolution of such devices as a function of the number of firing cells, reaching values below 20 ps. These measurements provide significant insight into the capabilities of SiPM sensors in direct detection of charged particles and their potential for several applications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.17762v1-abstract-full').style.display = 'none'; document.getElementById('2305.17762v1-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.13244">arXiv:2210.13244</a> <span> [<a href="https://arxiv.org/pdf/2210.13244">pdf</a>, <a href="https://arxiv.org/format/2210.13244">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Understanding the direct detection of charged particles with SiPMs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Carnesecchi%2C+F">F. Carnesecchi</a>, <a href="/search/physics?searchtype=author&query=Vignola%2C+G">G. Vignola</a>, <a href="/search/physics?searchtype=author&query=Agrawal%2C+N">N. Agrawal</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/physics?searchtype=author&query=Cavazza%2C+D">D. Cavazza</a>, <a href="/search/physics?searchtype=author&query=Cifarelli%2C+L">L. Cifarelli</a>, <a href="/search/physics?searchtype=author&query=Colocci%2C+M">M. Colocci</a>, <a href="/search/physics?searchtype=author&query=Durando%2C+S">S. Durando</a>, <a href="/search/physics?searchtype=author&query=Ercolessi%2C+F">F. Ercolessi</a>, <a href="/search/physics?searchtype=author&query=Ficorella%2C+A">A. Ficorella</a>, <a href="/search/physics?searchtype=author&query=Fraticelli%2C+C">C. Fraticelli</a>, <a href="/search/physics?searchtype=author&query=Garbini%2C+M">M. Garbini</a>, <a href="/search/physics?searchtype=author&query=Giacalone%2C+M">M. Giacalone</a>, <a href="/search/physics?searchtype=author&query=Gola%2C+A">A. Gola</a>, <a href="/search/physics?searchtype=author&query=Hatzifotiadou%2C+D">D. Hatzifotiadou</a>, <a href="/search/physics?searchtype=author&query=Jacazio%2C+N">N. Jacazio</a>, <a href="/search/physics?searchtype=author&query=Margotti%2C+A">A. Margotti</a>, <a href="/search/physics?searchtype=author&query=Malfattore%2C+G">G. Malfattore</a>, <a href="/search/physics?searchtype=author&query=Nania%2C+R">R. Nania</a>, <a href="/search/physics?searchtype=author&query=Noferini%2C+F">F. Noferini</a>, <a href="/search/physics?searchtype=author&query=Paternoster%2C+G">G. Paternoster</a>, <a href="/search/physics?searchtype=author&query=Pinazza%2C+O">O. Pinazza</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.13244v1-abstract-short" style="display: inline;"> In this paper evidence that the increased response of SiPM sensors to the passage of charged particles is related mainly to Cherenkov light produced in the protection layer is reported. The response and timing properties of sensors with different protection layers have been studied. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.13244v1-abstract-full" style="display: none;"> In this paper evidence that the increased response of SiPM sensors to the passage of charged particles is related mainly to Cherenkov light produced in the protection layer is reported. The response and timing properties of sensors with different protection layers have been studied. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.13244v1-abstract-full').style.display = 'none'; document.getElementById('2210.13244v1-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.04160">arXiv:2202.04160</a> <span> [<a href="https://arxiv.org/pdf/2202.04160">pdf</a>, <a href="https://arxiv.org/format/2202.04160">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/10.1088/1748-0221/17/06/P06007">10.1088/1748-0221/17/06/P06007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct detection of charged particles with SiPMs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Carnesecchi%2C+F">F. Carnesecchi</a>, <a href="/search/physics?searchtype=author&query=Vignola%2C+G">G. Vignola</a>, <a href="/search/physics?searchtype=author&query=Agrawal%2C+N">N. Agrawal</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+F">F. Bellini</a>, <a href="/search/physics?searchtype=author&query=Cavazza%2C+D">D. Cavazza</a>, <a href="/search/physics?searchtype=author&query=Cifarelli%2C+L">L. Cifarelli</a>, <a href="/search/physics?searchtype=author&query=Colocci%2C+M">M. Colocci</a>, <a href="/search/physics?searchtype=author&query=Durando%2C+S">S. Durando</a>, <a href="/search/physics?searchtype=author&query=Ercolessi%2C+F">F. Ercolessi</a>, <a href="/search/physics?searchtype=author&query=Garbini%2C+M">M. Garbini</a>, <a href="/search/physics?searchtype=author&query=Giacalone%2C+M">M. Giacalone</a>, <a href="/search/physics?searchtype=author&query=Hatzifotiadou%2C+D">D. Hatzifotiadou</a>, <a href="/search/physics?searchtype=author&query=Jacazio%2C+N">N. Jacazio</a>, <a href="/search/physics?searchtype=author&query=Margotti%2C+A">A. Margotti</a>, <a href="/search/physics?searchtype=author&query=Malfattore%2C+G">G. Malfattore</a>, <a href="/search/physics?searchtype=author&query=Nania%2C+R">R. Nania</a>, <a href="/search/physics?searchtype=author&query=Noferini%2C+F">F. Noferini</a>, <a href="/search/physics?searchtype=author&query=Pinazza%2C+O">O. Pinazza</a>, <a href="/search/physics?searchtype=author&query=Preghenella%2C+R">R. Preghenella</a>, <a href="/search/physics?searchtype=author&query=Ricci%2C+R">R. Ricci</a>, <a href="/search/physics?searchtype=author&query=Rignanese%2C+L">L. Rignanese</a>, <a href="/search/physics?searchtype=author&query=Rubini%2C+N">N. Rubini</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.04160v2-abstract-short" style="display: inline;"> The direct response of Silicon PhotoMultipliers being traversed by a MIP charged particle have been studied in a systematic way for the first time. Using beam test data, time resolution and the crosstalk probability have been measured. A characterization of the SiPM by means of a laser beam is also reported. The results obtained for different sensors indicate a measured time resolution around 40-7… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04160v2-abstract-full').style.display = 'inline'; document.getElementById('2202.04160v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.04160v2-abstract-full" style="display: none;"> The direct response of Silicon PhotoMultipliers being traversed by a MIP charged particle have been studied in a systematic way for the first time. Using beam test data, time resolution and the crosstalk probability have been measured. A characterization of the SiPM by means of a laser beam is also reported. The results obtained for different sensors indicate a measured time resolution around 40-70 ps. Although particles are expected to traverse only one SPAD per event, crosstalk measurements on different sensors indicate an unexpected higher value with respect to the one related to the sensor noise. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04160v2-abstract-full').style.display = 'none'; document.getElementById('2202.04160v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 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/2101.08686">arXiv:2101.08686</a> <span> [<a href="https://arxiv.org/pdf/2101.08686">pdf</a>, <a href="https://arxiv.org/format/2101.08686">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/10.1140/epjc/s10052-021-09121-9">10.1140/epjc/s10052-021-09121-9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Separating $^{39}$Ar from $^{40}$Ar by cryogenic distillation with Aria for dark matter searches </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=DarkSide+Collaboration"> DarkSide Collaboration</a>, <a href="/search/physics?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Albergo%2C+S">S. Albergo</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Amaudruz%2C+P">P. Amaudruz</a>, <a href="/search/physics?searchtype=author&query=Arba%2C+M">M. Arba</a>, <a href="/search/physics?searchtype=author&query=Arpaia%2C+P">P. Arpaia</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/physics?searchtype=author&query=Avetissov%2C+I+C">I. Ch. Avetissov</a>, <a href="/search/physics?searchtype=author&query=Avetisov%2C+R+I">R. I. Avetisov</a>, <a href="/search/physics?searchtype=author&query=Azzolini%2C+O">O. Azzolini</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Balmforth%2C+Z">Z. Balmforth</a>, <a href="/search/physics?searchtype=author&query=Barbarian%2C+V">V. Barbarian</a>, <a href="/search/physics?searchtype=author&query=Olmedo%2C+A+B">A. Barrado Olmedo</a>, <a href="/search/physics?searchtype=author&query=Barrillon%2C+P">P. Barrillon</a>, <a href="/search/physics?searchtype=author&query=Basco%2C+A">A. Basco</a>, <a href="/search/physics?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Bondar%2C+A">A. Bondar</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Borisova%2C+E">E. Borisova</a> , et al. (287 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="2101.08686v2-abstract-short" style="display: inline;"> The Aria project consists of a plant, hosting a 350 m cryogenic isotopic distillation column, the tallest ever built, which is currently in the installation phase in a mine shaft at Carbosulcis S.p.A., Nuraxi-Figus (SU), Italy. Aria is one of the pillars of the argon dark-matter search experimental program, lead by the Global Argon Dark Matter Collaboration. Aria was designed to reduce the isotopi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.08686v2-abstract-full').style.display = 'inline'; document.getElementById('2101.08686v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.08686v2-abstract-full" style="display: none;"> The Aria project consists of a plant, hosting a 350 m cryogenic isotopic distillation column, the tallest ever built, which is currently in the installation phase in a mine shaft at Carbosulcis S.p.A., Nuraxi-Figus (SU), Italy. Aria is one of the pillars of the argon dark-matter search experimental program, lead by the Global Argon Dark Matter Collaboration. Aria was designed to reduce the isotopic abundance of $^{39}$Ar, a $尾$-emitter of cosmogenic origin, whose activity poses background and pile-up concerns in the detectors, in the argon used for the dark-matter searches, the so-called Underground Argon (UAr). In this paper, we discuss the requirements, design, construction, tests, and projected performance of the plant for the isotopic cryogenic distillation of argon. We also present the successful results of isotopic cryogenic distillation of nitrogen with a prototype plant, operating the column at total reflux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.08686v2-abstract-full').style.display = 'none'; document.getElementById('2101.08686v2-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">Journal ref:</span> Eur.Phys.J.C 81 (2021) 4, 359 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.07819">arXiv:2011.07819</a> <span> [<a href="https://arxiv.org/pdf/2011.07819">pdf</a>, <a href="https://arxiv.org/format/2011.07819">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/10.1088/1475-7516/2021/03/043">10.1088/1475-7516/2021/03/043 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Albergo%2C+S">S. Albergo</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Amaudruz%2C+P">P. Amaudruz</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/physics?searchtype=author&query=Avetissov%2C+I+C">I. Ch. Avetissov</a>, <a href="/search/physics?searchtype=author&query=Avetisov%2C+R+I">R. I. Avetisov</a>, <a href="/search/physics?searchtype=author&query=Azzolini%2C+O">O. Azzolini</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Balmforth%2C+Z">Z. Balmforth</a>, <a href="/search/physics?searchtype=author&query=Barbarian%2C+V">V. Barbarian</a>, <a href="/search/physics?searchtype=author&query=Olmedo%2C+A+B">A. Barrado Olmedo</a>, <a href="/search/physics?searchtype=author&query=Barrillon%2C+P">P. Barrillon</a>, <a href="/search/physics?searchtype=author&query=Basco%2C+A">A. Basco</a>, <a href="/search/physics?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Bondar%2C+A">A. Bondar</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Borisova%2C+E">E. Borisova</a>, <a href="/search/physics?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/physics?searchtype=author&query=Boulay%2C+M+G">M. G. Boulay</a>, <a href="/search/physics?searchtype=author&query=Buccino%2C+G">G. Buccino</a> , et al. (251 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="2011.07819v2-abstract-short" style="display: inline;"> Future liquid-argon DarkSide-20k and ARGO detectors, designed for direct dark matter search, will be sensitive also to core-collapse supernova neutrinos, via coherent elastic neutrino-nucleus scattering. This interaction channel is flavor-insensitive with a high-cross section, enabling for a high-statistics neutrino detection with target masses of $\sim$50~t and $\sim$360~t for DarkSide-20k and AR… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.07819v2-abstract-full').style.display = 'inline'; document.getElementById('2011.07819v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.07819v2-abstract-full" style="display: none;"> Future liquid-argon DarkSide-20k and ARGO detectors, designed for direct dark matter search, will be sensitive also to core-collapse supernova neutrinos, via coherent elastic neutrino-nucleus scattering. This interaction channel is flavor-insensitive with a high-cross section, enabling for a high-statistics neutrino detection with target masses of $\sim$50~t and $\sim$360~t for DarkSide-20k and ARGO, respectively. Thanks to the low-energy threshold of $\sim$0.5~keV$_{nr}$ achievable by exploiting the ionization channel, DarkSide-20k and ARGO have the potential to discover supernova bursts throughout our galaxy and up to the Small Magellanic Cloud, respectively, assuming a 11-M$_{\odot}$ progenitor star. We report also on the sensitivity to the neutronization burst, whose electron neutrino flux is suppressed by oscillations when detected via charged current and elastic scattering. Finally, the accuracies in the reconstruction of the average and total neutrino energy in the different phases of the supernova burst, as well as its time profile, are also discussed, taking into account the expected background and the detector response. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.07819v2-abstract-full').style.display = 'none'; document.getElementById('2011.07819v2-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> 31 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 03 (2021) 043 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.02024">arXiv:2004.02024</a> <span> [<a href="https://arxiv.org/pdf/2004.02024">pdf</a>, <a href="https://arxiv.org/format/2004.02024">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-020-08801-2">10.1140/epjc/s10052-020-08801-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SiPM-matrix readout of two-phase argon detectors using electroluminescence in the visible and near infrared range </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+DarkSide+collaboration"> The DarkSide collaboration</a>, <a href="/search/physics?searchtype=author&query=Aalseth%2C+C+E">C. E. Aalseth</a>, <a href="/search/physics?searchtype=author&query=Abdelhakim%2C+S">S. Abdelhakim</a>, <a href="/search/physics?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Ajaj%2C+R">R. Ajaj</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Amaudruz%2C+P">P. Amaudruz</a>, <a href="/search/physics?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/physics?searchtype=author&query=Anstey%2C+J">J. Anstey</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Arba%2C+M">M. Arba</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Ardito%2C+R">R. Ardito</a>, <a href="/search/physics?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/physics?searchtype=author&query=Arpaia%2C+P">P. Arpaia</a>, <a href="/search/physics?searchtype=author&query=Asner%2C+D+M">D. M. Asner</a>, <a href="/search/physics?searchtype=author&query=Asunskis%2C+A">A. Asunskis</a>, <a href="/search/physics?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Barbaryan%2C+V">V. Barbaryan</a>, <a href="/search/physics?searchtype=author&query=Olmedo%2C+A+B">A. Barrado Olmedo</a>, <a href="/search/physics?searchtype=author&query=Batignani%2C+G">G. Batignani</a> , et al. (290 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="2004.02024v2-abstract-short" style="display: inline;"> Proportional electroluminescence (EL) in noble gases is used in two-phase detectors for dark matter searches to record (in the gas phase) the ionization signal induced by particle scattering in the liquid phase. The "standard" EL mechanism is considered to be due to noble gas excimer emission in the vacuum ultraviolet (VUV). In addition, there are two alternative mechanisms, producing light in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.02024v2-abstract-full').style.display = 'inline'; document.getElementById('2004.02024v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.02024v2-abstract-full" style="display: none;"> Proportional electroluminescence (EL) in noble gases is used in two-phase detectors for dark matter searches to record (in the gas phase) the ionization signal induced by particle scattering in the liquid phase. The "standard" EL mechanism is considered to be due to noble gas excimer emission in the vacuum ultraviolet (VUV). In addition, there are two alternative mechanisms, producing light in the visible and near infrared (NIR) ranges. The first is due to bremsstrahlung of electrons scattered on neutral atoms ("neutral bremsstrahlung", NBrS). The second, responsible for electron avalanche scintillation in the NIR at higher electric fields, is due to transitions between excited atomic states. In this work, we have for the first time demonstrated two alternative techniques of the optical readout of two-phase argon detectors, in the visible and NIR range, using a silicon photomultiplier matrix and electroluminescence due to either neutral bremsstrahlung or avalanche scintillation. The amplitude yield and position resolution were measured for these readout techniques, which allowed to assess the detection threshold for electron and nuclear recoils in two-phase argon detectors for dark matter searches. To the best of our knowledge, this is the first practical application of the NBrS effect in detection science. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.02024v2-abstract-full').style.display = 'none'; document.getElementById('2004.02024v2-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 22 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C (2021) 81: 153 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.08106">arXiv:2001.08106</a> <span> [<a href="https://arxiv.org/pdf/2001.08106">pdf</a>, <a href="https://arxiv.org/format/2001.08106">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/10.1088/1748-0221/15/02/P02024">10.1088/1748-0221/15/02/P02024 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design and construction of a new detector to measure ultra-low radioactive-isotope contamination of argon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+DarkSide+Collaboration"> The DarkSide Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aalseth%2C+C+E">C. E. Aalseth</a>, <a href="/search/physics?searchtype=author&query=Abdelhakim%2C+S">S. Abdelhakim</a>, <a href="/search/physics?searchtype=author&query=Acerbi%2C+F">F. Acerbi</a>, <a href="/search/physics?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Ajaj%2C+R">R. Ajaj</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Amaudruz%2C+P">P. Amaudruz</a>, <a href="/search/physics?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/physics?searchtype=author&query=Anstey%2C+J">J. Anstey</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Arba%2C+M">M. Arba</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Ardito%2C+R">R. Ardito</a>, <a href="/search/physics?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/physics?searchtype=author&query=Arpaia%2C+P">P. Arpaia</a>, <a href="/search/physics?searchtype=author&query=Asner%2C+D+M">D. M. Asner</a>, <a href="/search/physics?searchtype=author&query=Asunskis%2C+A">A. Asunskis</a>, <a href="/search/physics?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Olmedo%2C+A+B">A. Barrado Olmedo</a>, <a href="/search/physics?searchtype=author&query=Batignani%2C+G">G. Batignani</a> , et al. (306 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="2001.08106v1-abstract-short" style="display: inline;"> Large liquid argon detectors offer one of the best avenues for the detection of galactic weakly interacting massive particles (WIMPs) via their scattering on atomic nuclei. The liquid argon target allows exquisite discrimination between nuclear and electron recoil signals via pulse-shape discrimination of the scintillation signals. Atmospheric argon (AAr), however, has a naturally occurring radioa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08106v1-abstract-full').style.display = 'inline'; document.getElementById('2001.08106v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08106v1-abstract-full" style="display: none;"> Large liquid argon detectors offer one of the best avenues for the detection of galactic weakly interacting massive particles (WIMPs) via their scattering on atomic nuclei. The liquid argon target allows exquisite discrimination between nuclear and electron recoil signals via pulse-shape discrimination of the scintillation signals. Atmospheric argon (AAr), however, has a naturally occurring radioactive isotope, $^{39}$Ar, a $尾$ emitter of cosmogenic origin. For large detectors, the atmospheric $^{39}$Ar activity poses pile-up concerns. The use of argon extracted from underground wells, deprived of $^{39}$Ar, is key to the physics potential of these experiments. The DarkSide-20k dark matter search experiment will operate a dual-phase time projection chamber with 50 tonnes of radio-pure underground argon (UAr), that was shown to be depleted of $^{39}$Ar with respect to AAr by a factor larger than 1400. Assessing the $^{39}$Ar content of the UAr during extraction is crucial for the success of DarkSide-20k, as well as for future experiments of the Global Argon Dark Matter Collaboration (GADMC). This will be carried out by the DArT in ArDM experiment, a small chamber made with extremely radio-pure materials that will be placed at the centre of the ArDM detector, in the Canfranc Underground Laboratory (LSC) in Spain. The ArDM LAr volume acts as an active veto for background radioactivity, mostly $纬$-rays from the ArDM detector materials and the surrounding rock. This article describes the DArT in ArDM project, including the chamber design and construction, and reviews the background required to achieve the expected performance of the detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08106v1-abstract-full').style.display = 'none'; document.getElementById('2001.08106v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 8 figures. Corresponding author: E. S谩nchez Garc铆a</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.08145">arXiv:1707.08145</a> <span> [<a href="https://arxiv.org/pdf/1707.08145">pdf</a>, <a href="https://arxiv.org/format/1707.08145">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjp/i2018-11973-4">10.1140/epjp/i2018-11973-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> DarkSide-20k: A 20 Tonne Two-Phase LAr TPC for Direct Dark Matter Detection at LNGS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aalseth%2C+C+E">C. E. Aalseth</a>, <a href="/search/physics?searchtype=author&query=Acerbi%2C+F">F. Acerbi</a>, <a href="/search/physics?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Ardito%2C+R">R. Ardito</a>, <a href="/search/physics?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/physics?searchtype=author&query=Asner%2C+D+M">D. M. Asner</a>, <a href="/search/physics?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Olmedo%2C+A+I+B">A. I. Barrado Olmedo</a>, <a href="/search/physics?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Bertoldo%2C+E">E. Bertoldo</a>, <a href="/search/physics?searchtype=author&query=Bettarini%2C+S">S. Bettarini</a>, <a href="/search/physics?searchtype=author&query=Bisogni%2C+M+G">M. G. Bisogni</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/physics?searchtype=author&query=Bondar%2C+A">A. Bondar</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W">W. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Bossa%2C+M">M. Bossa</a>, <a href="/search/physics?searchtype=author&query=Bottino%2C+B">B. Bottino</a> , et al. (260 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="1707.08145v1-abstract-short" style="display: inline;"> Building on the successful experience in operating the DarkSide-50 detector, the DarkSide Collaboration is going to construct DarkSide-20k, a direct WIMP search detector using a two-phase Liquid Argon Time Projection Chamber (LArTPC) with an active (fiducial) mass of 23 t (20 t). The DarkSide-20k LArTPC will be deployed within a shield/veto with a spherical Liquid Scintillator Veto (LSV) inside a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.08145v1-abstract-full').style.display = 'inline'; document.getElementById('1707.08145v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.08145v1-abstract-full" style="display: none;"> Building on the successful experience in operating the DarkSide-50 detector, the DarkSide Collaboration is going to construct DarkSide-20k, a direct WIMP search detector using a two-phase Liquid Argon Time Projection Chamber (LArTPC) with an active (fiducial) mass of 23 t (20 t). The DarkSide-20k LArTPC will be deployed within a shield/veto with a spherical Liquid Scintillator Veto (LSV) inside a cylindrical Water Cherenkov Veto (WCV). Operation of DarkSide-50 demonstrated a major reduction in the dominant $^{39}$Ar background when using argon extracted from an underground source, before applying pulse shape analysis. Data from DarkSide-50, in combination with MC simulation and analytical modeling, shows that a rejection factor for discrimination between electron and nuclear recoils of $\gt3\times10^9$ is achievable. This, along with the use of the veto system, is the key to unlocking the path to large LArTPC detector masses, while maintaining an "instrumental background-free" experiment, an experiment in which less than 0.1 events (other than $谓$-induced nuclear recoils) is expected to occur within the WIMP search region during the planned exposure. DarkSide-20k will have ultra-low backgrounds than can be measured in situ. This will give sensitivity to WIMP-nucleon cross sections of $1.2\times10^{-47}$ cm$^2$ ($1.1\times10^{-46}$ cm$^2$) for WIMPs of $1$ TeV$/c^2$ ($10$ TeV$/c^2$) mass, to be achieved during a 5 yr run producing an exposure of 100 t yr free from any instrumental background. DarkSide-20k could then extend its operation to a decade, increasing the exposure to 200 t yr, reaching a sensitivity of $7.4\times10^{-48}$ cm$^2$ ($6.9\times10^{-47}$ cm$^2$) for WIMPs of $1$ TeV$/c^2$ ($10$ TeV$/c^2$) mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.08145v1-abstract-full').style.display = 'none'; document.getElementById('1707.08145v1-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 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-17-298-PPD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Aalseth, C.E., Acerbi, F., Agnes, P. et al. Eur. Phys. J. Plus (2018) 133: 131 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.07028">arXiv:1705.07028</a> <span> [<a href="https://arxiv.org/pdf/1705.07028">pdf</a>, <a href="https://arxiv.org/format/1705.07028">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/10.1088/1748-0221/12/09/P09030">10.1088/1748-0221/12/09/P09030 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cryogenic Characterization of FBK RGB-HD SiPMs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Aalseth%2C+C+E">C. E. Aalseth</a>, <a href="/search/physics?searchtype=author&query=Acerbi%2C+F">F. Acerbi</a>, <a href="/search/physics?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/physics?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/physics?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Ampudia%2C+P">P. Ampudia</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/physics?searchtype=author&query=Ardito%2C+R">R. Ardito</a>, <a href="/search/physics?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/physics?searchtype=author&query=Asner%2C+D+M">D. M. Asner</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Bertoldo%2C+E">E. Bertoldo</a>, <a href="/search/physics?searchtype=author&query=Bettarini%2C+S">S. Bettarini</a>, <a href="/search/physics?searchtype=author&query=Bisogni%2C+M+G">M. G. Bisogni</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/physics?searchtype=author&query=Bondar%2C+A">A. Bondar</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W">W. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Bossa%2C+M">M. Bossa</a>, <a href="/search/physics?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/physics?searchtype=author&query=Bunker%2C+R">R. Bunker</a> , et al. (246 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1705.07028v3-abstract-short" style="display: inline;"> We report on the cryogenic characterization of Red Green Blue - High Density (RGB-HD) SiPMs developed at Fondazione Bruno Kessler (FBK) as part of the DarkSide program of dark matter searches with liquid argon time projection chambers. A dedicated setup was used to measure the primary dark noise, the correlated noise, and the gain of the SiPMs at varying temperatures. A custom-made data acquisitio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.07028v3-abstract-full').style.display = 'inline'; document.getElementById('1705.07028v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.07028v3-abstract-full" style="display: none;"> We report on the cryogenic characterization of Red Green Blue - High Density (RGB-HD) SiPMs developed at Fondazione Bruno Kessler (FBK) as part of the DarkSide program of dark matter searches with liquid argon time projection chambers. A dedicated setup was used to measure the primary dark noise, the correlated noise, and the gain of the SiPMs at varying temperatures. A custom-made data acquisition system and analysis software were used to precisely characterize these parameters. We demonstrate that FBK RGB-HD SiPMs with low quenching resistance (RGB-HD-LR$_q$) can be operated from 40 K to 300 K with gains in the range $10^5$ to $10^6$ and noise rates on the order of a few Hz/mm$^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.07028v3-abstract-full').style.display = 'none'; document.getElementById('1705.07028v3-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 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </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 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