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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Calaprice%2C+F&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Calaprice%2C+F&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Calaprice%2C+F&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <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/2311.18647">arXiv:2311.18647</a> <span> [<a href="https://arxiv.org/pdf/2311.18647">pdf</a>, <a href="https://arxiv.org/format/2311.18647">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1088/1748-0221/19/05/P05057">10.1088/1748-0221/19/05/P05057 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Long-term temporal stability of the DarkSide-50 dark matter detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</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=Alton%2C+A+K">A. K. Alton</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=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Campos%2C+M+D">M. D. Campos</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cargioli%2C+N">N. Cargioli</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a> , et al. (121 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="2311.18647v3-abstract-short" style="display: inline;"> The stability of a dark matter detector on the timescale of a few years is a key requirement due to the large exposure needed to achieve a competitive sensitivity. It is especially crucial to enable the detector to potentially detect any annual event rate modulation, an expected dark matter signature. In this work, we present the performance history of the DarkSide-50 dual-phase argon time project… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.18647v3-abstract-full').style.display = 'inline'; document.getElementById('2311.18647v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.18647v3-abstract-full" style="display: none;"> The stability of a dark matter detector on the timescale of a few years is a key requirement due to the large exposure needed to achieve a competitive sensitivity. It is especially crucial to enable the detector to potentially detect any annual event rate modulation, an expected dark matter signature. In this work, we present the performance history of the DarkSide-50 dual-phase argon time projection chamber over its almost three-year low-radioactivity argon run. In particular, we focus on the electroluminescence signal that enables sensitivity to sub-keV energy depositions. The stability of the electroluminescence yield is found to be better than 0.5%. Finally, we show the temporal evolution of the observed event rate around the sub-keV region being consistent to the background prediction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.18647v3-abstract-full').style.display = 'none'; document.getElementById('2311.18647v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">13 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 19 P05057 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.11826">arXiv:2310.11826</a> <span> [<a href="https://arxiv.org/pdf/2310.11826">pdf</a>, <a href="https://arxiv.org/format/2310.11826">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.112014">10.1103/PhysRevD.109.112014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Novel techniques for alpha/beta pulse shape discrimination in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacintov%2C+A">A. Di Giacintov</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/physics?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/physics?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Andrea Ianni</a> , et al. (49 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="2310.11826v1-abstract-short" style="display: inline;"> Borexino could efficiently distinguish between alpha and beta radiation in its liquid scintillator by the characteristic time profile of their scintillation pulse. This alpha/beta discrimination, first demonstrated at the tonne scale in the Counting Test Facility prototype, was used throughout the lifetime of the experiment between 2007 and 2021. With this method, alpha events are identified and s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11826v1-abstract-full').style.display = 'inline'; document.getElementById('2310.11826v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.11826v1-abstract-full" style="display: none;"> Borexino could efficiently distinguish between alpha and beta radiation in its liquid scintillator by the characteristic time profile of their scintillation pulse. This alpha/beta discrimination, first demonstrated at the tonne scale in the Counting Test Facility prototype, was used throughout the lifetime of the experiment between 2007 and 2021. With this method, alpha events are identified and subtracted from the beta-like solar neutrino events. This is particularly important in liquid scintillator as alpha scintillation is quenched many-fold. In Borexino, the prominent Po-210 decay peak was a background in the energy range of electrons scattered from Be-7 solar neutrinos. Optimal alpha-beta discrimination was achieved with a "multi-layer perceptron neural network", which its higher ability to leverage the timing information of the scintillation photons detected by the photomultiplier tubes. An event-by-event, high efficiency, stable, and uniform pulse shape discrimination was essential in characterising the spatial distribution of background in the detector. This benefited most Borexino measurements, including solar neutrinos in the \pp chain and the first direct observation of the CNO cycle in the Sun. This paper presents the key milestones in alpha/beta discrimination in Borexino as a term of comparison for current and future large liquid scintillator detectors <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11826v1-abstract-full').style.display = 'none'; document.getElementById('2310.11826v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">13 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109, 112014, 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.14636">arXiv:2307.14636</a> <span> [<a href="https://arxiv.org/pdf/2307.14636">pdf</a>, <a href="https://arxiv.org/format/2307.14636">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.108.102005">10.1103/PhysRevD.108.102005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Final results of Borexino on CNO solar neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/physics?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/physics?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Andrea Ianni</a> , et al. (50 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.14636v1-abstract-short" style="display: inline;"> We report the first measurement of CNO solar neutrinos by Borexino that uses the Correlated Integrated Directionality (CID) method, exploiting the sub-dominant Cherenkov light in the liquid scintillator detector. The directional information of the solar origin of the neutrinos is preserved by the fast Cherenkov photons from the neutrino scattered electrons, and is used to discriminate between sign… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14636v1-abstract-full').style.display = 'inline'; document.getElementById('2307.14636v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.14636v1-abstract-full" style="display: none;"> We report the first measurement of CNO solar neutrinos by Borexino that uses the Correlated Integrated Directionality (CID) method, exploiting the sub-dominant Cherenkov light in the liquid scintillator detector. The directional information of the solar origin of the neutrinos is preserved by the fast Cherenkov photons from the neutrino scattered electrons, and is used to discriminate between signal and background. The directional information is independent from the spectral information on which the previous CNO solar neutrino measurements by Borexino were based. While the CNO spectral analysis could only be applied on the Phase-III dataset, the directional analysis can use the complete Borexino data taking period from 2007 to 2021. The absence of CNO neutrinos has been rejected with >5蟽 credible level using the Bayesian statistics. The directional CNO measurement is obtained without an external constraint on the $^{210}$Bi contamination of the liquid scintillator, which was applied in the spectral analysis approach. The final and the most precise CNO measurement of Borexino is then obtained by combining the new CID-based CNO result with an improved spectral fit of the Phase-III dataset. Including the statistical and the systematic errors, the extracted CNO interaction rate is $R(\mathrm{CNO})=6.7^{+1.2}_{-0.8} \, \mathrm{cpd/100 \, tonnes}$. Taking into account the neutrino flavor conversion, the resulting CNO neutrino flux at Earth is $桅_\mathrm{CNO}=6.7 ^{+1.2}_{-0.8} \times 10^8 \, \mathrm{cm^{-2} s^{-1}}$, in agreement with the high metallicity Standard Solar Models. The results described in this work reinforce the role of the event directional information in large-scale liquid scintillator detectors and open up new avenues for the next-generation liquid scintillator or hybrid neutrino experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14636v1-abstract-full').style.display = 'none'; document.getElementById('2307.14636v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.00321">arXiv:2210.00321</a> <span> [<a href="https://arxiv.org/pdf/2210.00321">pdf</a>, <a href="https://arxiv.org/format/2210.00321">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"> Status and prospects of SABRE North </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Mariani%2C+A">A. Mariani</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J+B">J. B. Benziger</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Copello%2C+S">S. Copello</a>, <a href="/search/physics?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=D%27Imperio%2C+G">G. D'Imperio</a>, <a href="/search/physics?searchtype=author&query=Di+Carlo%2C+G">G. Di Carlo</a>, <a href="/search/physics?searchtype=author&query=Diemoz%2C+M">M. Diemoz</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Ianna%2C+M">M. Ianna</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">A. Ianni</a>, <a href="/search/physics?searchtype=author&query=Milana%2C+S">S. Milana</a>, <a href="/search/physics?searchtype=author&query=Orlandi%2C+D">D. Orlandi</a>, <a href="/search/physics?searchtype=author&query=Pettinacci%2C+V">V. Pettinacci</a>, <a href="/search/physics?searchtype=author&query=Pietrofaccia%2C+L">L. Pietrofaccia</a>, <a href="/search/physics?searchtype=author&query=Rahatlou%2C+S">S. Rahatlou</a>, <a href="/search/physics?searchtype=author&query=Suerfu%2C+B">B. Suerfu</a>, <a href="/search/physics?searchtype=author&query=Tomei%2C+C">C. Tomei</a>, <a href="/search/physics?searchtype=author&query=Vignoli%2C+C">C. Vignoli</a>, <a href="/search/physics?searchtype=author&query=Zani%2C+A">A. Zani</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="2210.00321v2-abstract-short" style="display: inline;"> We present the characterization of a low background NaI(Tl) crystal for the SABRE North experiment. The crystal NaI-33, was studied in two different setups at Laboratori Nazionali del Gran Sasso, Italy. The Proof-of-Principle (PoP) detector was equipped with a liquid scintillator veto and collected data for about one month (90 kg$\times$days). The PoP-dry setup consisted of NaI-33 in a purely pass… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.00321v2-abstract-full').style.display = 'inline'; document.getElementById('2210.00321v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.00321v2-abstract-full" style="display: none;"> We present the characterization of a low background NaI(Tl) crystal for the SABRE North experiment. The crystal NaI-33, was studied in two different setups at Laboratori Nazionali del Gran Sasso, Italy. The Proof-of-Principle (PoP) detector was equipped with a liquid scintillator veto and collected data for about one month (90 kg$\times$days). The PoP-dry setup consisted of NaI-33 in a purely passive shielding and collected data for almost one year (891 kg$\times$days). The average background in the energy region of interest (1-6 keV) for dark matter search was 1.20 $\pm$ 0.05 and 1.39 $\pm$ 0.02 counts/day/kg/keV within the PoP and the PoP-dry setup, respectively. This result opens to a new shielding design for the physics phase of the SABRE North detector, that does not foresee the use of an organic liquid scintillator external veto. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.00321v2-abstract-full').style.display = 'none'; document.getElementById('2210.00321v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">5 pages, 2 figures. arXiv admin note: substantial text overlap with arXiv:2205.13876</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.13876">arXiv:2205.13876</a> <span> [<a href="https://arxiv.org/pdf/2205.13876">pdf</a>, <a href="https://arxiv.org/format/2205.13876">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/10.1140/epjc/s10052-022-11108-z">10.1140/epjc/s10052-022-11108-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance of the SABRE detector module in a purely passive shielding </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J+B">J. B. Benziger</a>, <a href="/search/physics?searchtype=author&query=Copello%2C+S">S. Copello</a>, <a href="/search/physics?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=D%27Imperio%2C+G">G. D'Imperio</a>, <a href="/search/physics?searchtype=author&query=Di+Carlo%2C+G">G. Di Carlo</a>, <a href="/search/physics?searchtype=author&query=Diemoz%2C+M">M. Diemoz</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Ianna%2C+M">M. Ianna</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">A. Ianni</a>, <a href="/search/physics?searchtype=author&query=Mariani%2C+A">A. Mariani</a>, <a href="/search/physics?searchtype=author&query=Milana%2C+S">S. Milana</a>, <a href="/search/physics?searchtype=author&query=Orlandi%2C+D">D. Orlandi</a>, <a href="/search/physics?searchtype=author&query=Pettinacci%2C+V">V. Pettinacci</a>, <a href="/search/physics?searchtype=author&query=Pietrofaccia%2C+L">L. Pietrofaccia</a>, <a href="/search/physics?searchtype=author&query=Rahatlou%2C+S">S. Rahatlou</a>, <a href="/search/physics?searchtype=author&query=Suerfu%2C+B">B. Suerfu</a>, <a href="/search/physics?searchtype=author&query=Tomei%2C+C">C. Tomei</a>, <a href="/search/physics?searchtype=author&query=Vignoli%2C+C">C. Vignoli</a>, <a href="/search/physics?searchtype=author&query=Zani%2C+A">A. Zani</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="2205.13876v4-abstract-short" style="display: inline;"> We present here a characterization of the low background NaI(Tl) crystal NaI-33 based on a period of almost one year of data taking (891 kgxdays exposure) in a detector configuration with no use of organic scintillator veto. This remarkably radio-pure crystal already showed a low background in the SABRE Proof-of-Principle (PoP) detector, in the low energy region of interest (1-6 keV) for the searc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.13876v4-abstract-full').style.display = 'inline'; document.getElementById('2205.13876v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.13876v4-abstract-full" style="display: none;"> We present here a characterization of the low background NaI(Tl) crystal NaI-33 based on a period of almost one year of data taking (891 kgxdays exposure) in a detector configuration with no use of organic scintillator veto. This remarkably radio-pure crystal already showed a low background in the SABRE Proof-of-Principle (PoP) detector, in the low energy region of interest (1-6 keV) for the search of dark matter interaction via the annual modulation signature. As the vetoable background components, such as $^{40}$K, are here sub-dominant, we reassembled the PoP setup with a fully passive shielding. We upgraded the selection of events based on a Boosted Decision Tree algorithm that rejects most of the PMT-induced noise while retaining scintillation signals with > 90% efficiency in 1-6 keV. We find an average background of 1.39 $\pm$ 0.02 counts/day/kg/keV in the region of interest and a spectrum consistent with data previously acquired in the PoP setup, where the external veto background suppression was in place. Our background model indicates that the dominant background component is due to decays of $^{210}$Pb, only partly residing in the crystal itself. The other location of $^{210}$Pb is the reflector foil that wraps the crystal. We now proceed to design the experimental setup for the physics phase of the SABRE North detector, based on an array of similar crystals, using a low radioactivity PTFE reflector and further improving the passive shielding strategy, in compliance with the new safety and environmental requirements of Laboratori Nazionali del Gran Sasso. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.13876v4-abstract-full').style.display = 'none'; document.getElementById('2205.13876v4-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">8 pages, 9 figures</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 82, 1158 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.11816">arXiv:2112.11816</a> <span> [<a href="https://arxiv.org/pdf/2112.11816">pdf</a>, <a href="https://arxiv.org/format/2112.11816">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.128.091803">10.1103/PhysRevLett.128.091803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Directional Measurement of sub-MeV Solar Neutrinos with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (72 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="2112.11816v1-abstract-short" style="display: inline;"> We report the measurement of sub-MeV solar neutrinos through the use of their associated Cherenkov radiation, performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso. The measurement is achieved using a novel technique that correlates individual photon hits of events to the known position of the Sun. In an energy window between 0.54 MeV to 0.74 MeV, selected using the domin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11816v1-abstract-full').style.display = 'inline'; document.getElementById('2112.11816v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.11816v1-abstract-full" style="display: none;"> We report the measurement of sub-MeV solar neutrinos through the use of their associated Cherenkov radiation, performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso. The measurement is achieved using a novel technique that correlates individual photon hits of events to the known position of the Sun. In an energy window between 0.54 MeV to 0.74 MeV, selected using the dominant scintillation light, we have measured 10887$^{+2386}_{-2103} (\mathrm{stat.})\pm 947 (\mathrm{syst.})$ ($68\%$ confidence interval) solar neutrinos out of 19904 total events. This corresponds to a $^{7}$Be neutrino interaction rate of 51.6$^{+13.9}_{-12.5}$ counts/(day$\cdot$ 100 ton), which is in agreement with the Standard Solar Model predictions and the previous spectroscopic results of Borexino. The no-neutrino hypothesis can be excluded with $>$5$蟽$ confidence level. For the first time, we have demonstrated the possibility of utilizing the directional Cherenkov information for sub-MeV solar neutrinos, in a large-scale, high light yield liquid scintillator detector. This measurement provides an experimental proof of principle for future hybrid event reconstruction using both Cherenkov and scintillation signatures simultaneously. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11816v1-abstract-full').style.display = 'none'; document.getElementById('2112.11816v1-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 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">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 4 figures, short letter of arXiv:2109.04770</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.11688">arXiv:2112.11688</a> <span> [<a href="https://arxiv.org/pdf/2112.11688">pdf</a>, <a href="https://arxiv.org/format/2112.11688">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/17/05/P05018">10.1088/1748-0221/17/05/P05018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigation of the cryogenic scintillation of pure and doped sodium-iodine </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Clark%2C+M">M. Clark</a>, <a href="/search/physics?searchtype=author&query=Froborg%2C+F">F. Froborg</a>, <a href="/search/physics?searchtype=author&query=Di+Stefano%2C+P+C+F">P. C. F. Di Stefano</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</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="2112.11688v1-abstract-short" style="display: inline;"> We have studied the scintillation of pure and doped sodium iodide crystals handled in low humidity conditions under external $伪$ and $纬$ excitation from room temperature down to 4K. The light yield of pure sodium iodide was seen to increase at low temperatures by a factor 30 compared to room temperature, up to a maximum of 40 photons/keV under $纬$ excitation at 60K, stabilizing to 30 photons/keV a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11688v1-abstract-full').style.display = 'inline'; document.getElementById('2112.11688v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.11688v1-abstract-full" style="display: none;"> We have studied the scintillation of pure and doped sodium iodide crystals handled in low humidity conditions under external $伪$ and $纬$ excitation from room temperature down to 4K. The light yield of pure sodium iodide was seen to increase at low temperatures by a factor 30 compared to room temperature, up to a maximum of 40 photons/keV under $纬$ excitation at 60K, stabilizing to 30 photons/keV at lower temperatures. Thallium doped sodium iodide fluctuates by 20% around the room temperature value, stabilizing at 40 photons/keV at low temperature. $伪/ 纬$ quenching factor stabilizes at roughly 0.7 for both materials beneath 50K. Time constants of both materials slow greatly at low temperature, reaching tens of microseconds. Cryogenic applications of these materials are complexified by their mechanical fragility and hygroscopicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11688v1-abstract-full').style.display = 'none'; document.getElementById('2112.11688v1-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 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">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.04770">arXiv:2109.04770</a> <span> [<a href="https://arxiv.org/pdf/2109.04770">pdf</a>, <a href="https://arxiv.org/format/2109.04770">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.105.052002">10.1103/PhysRevD.105.052002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Correlated and Integrated Directionality for sub-MeV solar neutrinos in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (72 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="2109.04770v2-abstract-short" style="display: inline;"> Liquid scintillator detectors play a central role in the detection of neutrinos from various sources. In particular, it is the only technique used so far for the precision spectroscopy of sub-MeV solar neutrinos, as demonstrated by the Borexino experiment at the Gran Sasso National Laboratory in Italy. The benefit of a high light yield, and thus a low energy threshold and a good energy resolution,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.04770v2-abstract-full').style.display = 'inline'; document.getElementById('2109.04770v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.04770v2-abstract-full" style="display: none;"> Liquid scintillator detectors play a central role in the detection of neutrinos from various sources. In particular, it is the only technique used so far for the precision spectroscopy of sub-MeV solar neutrinos, as demonstrated by the Borexino experiment at the Gran Sasso National Laboratory in Italy. The benefit of a high light yield, and thus a low energy threshold and a good energy resolution, comes at the cost of the directional information featured by water Cherenkov detectors, measuring $^8$B solar neutrinos above a few MeV. In this paper we provide the first directionality measurement of sub-MeV solar neutrinos which exploits the correlation between the first few detected photons in each event and the known position of the Sun for each event. This is also the first signature of directionality in neutrinos elastically scattering off electrons in a liquid scintillator target. This measurement exploits the sub-dominant, fast Cherenkov light emission that precedes the dominant yet slower scintillation light signal. Through this measurement, we have also been able to extract the rate of $^{7}$Be solar neutrinos in Borexino. The demonstration of directional sensitivity in a traditional liquid scintillator target paves the way for the possible exploitation of the Cherenkov light signal in future kton-scale experiments using liquid scintillator targets. Directionality is important for background suppression as well as the disentanglement of signals from various sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.04770v2-abstract-full').style.display = 'none'; document.getElementById('2109.04770v2-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 15 Figures, revised version after comments from PRD Referees, shorter letter submitted with the title: "First Directional Measurement of sub-MeV Solar Neutrinos with Borexino"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.08087">arXiv:2107.08087</a> <span> [<a href="https://arxiv.org/pdf/2107.08087">pdf</a>, <a href="https://arxiv.org/format/2107.08087">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/10.1103/PhysRevD.104.082005">10.1103/PhysRevD.104.082005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration of the liquid argon ionization response to low energy electronic and nuclear recoils with DarkSide-50 </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=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=Alton%2C+A+K">A. K. Alton</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=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a>, <a href="/search/physics?searchtype=author&query=Catalanotti%2C+S">S. Catalanotti</a>, <a href="/search/physics?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a> , et al. (114 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="2107.08087v2-abstract-short" style="display: inline;"> DarkSide-50 has demonstrated the high potential of dual-phase liquid argon time projection chambers in exploring interactions of WIMPs in the GeV/c$^2$ mass range. The technique, based on the detection of the ionization signal amplified via electroluminescence in the gas phase, allows to explore recoil energies down to the sub-keV range. We report here on the DarkSide-50 measurement of the ionizat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08087v2-abstract-full').style.display = 'inline'; document.getElementById('2107.08087v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08087v2-abstract-full" style="display: none;"> DarkSide-50 has demonstrated the high potential of dual-phase liquid argon time projection chambers in exploring interactions of WIMPs in the GeV/c$^2$ mass range. The technique, based on the detection of the ionization signal amplified via electroluminescence in the gas phase, allows to explore recoil energies down to the sub-keV range. We report here on the DarkSide-50 measurement of the ionization yield of electronic recoils down to $\sim$180~eV$_{er}$, exploiting $^{37}$Ar and $^{39}$Ar decays, and extrapolated to a few ionization electrons with the Thomas-Imel box model. Moreover, we present a model-dependent determination of the ionization response to nuclear recoils down to $\sim$500~eV$_{nr}$, the lowest ever achieved in liquid argon, using \textit{in situ} neutron calibration sources and external datasets from neutron beam experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08087v2-abstract-full').style.display = 'none'; document.getElementById('2107.08087v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">11 pages, 12 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 104, 082005 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.08015">arXiv:2107.08015</a> <span> [<a href="https://arxiv.org/pdf/2107.08015">pdf</a>, <a href="https://arxiv.org/format/2107.08015">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"> A study of events with photoelectric emission in the DarkSide-50 liquid argon Time Projection Chamber </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</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=Alton%2C+A+K">A. K. Alton</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=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a>, <a href="/search/physics?searchtype=author&query=Catalanotti%2C+S">S. Catalanotti</a>, <a href="/search/physics?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a> , et al. (114 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="2107.08015v2-abstract-short" style="display: inline;"> Finding unequivocal evidence of dark matter interactions in a particle detector is a major objective of physics research. Liquid argon time projection chambers offer a path to probe Weakly Interacting Massive Particles scattering cross sections on nucleus down to the so-called neutrino floor, in a mass range from few GeV's to hundredths of TeV's. Based on the successful operation of the DarkSide-5… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08015v2-abstract-full').style.display = 'inline'; document.getElementById('2107.08015v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08015v2-abstract-full" style="display: none;"> Finding unequivocal evidence of dark matter interactions in a particle detector is a major objective of physics research. Liquid argon time projection chambers offer a path to probe Weakly Interacting Massive Particles scattering cross sections on nucleus down to the so-called neutrino floor, in a mass range from few GeV's to hundredths of TeV's. Based on the successful operation of the DarkSide-50 detector at LNGS, a new and more sensitive experiment, DarkSide-20k, has been designed and is now under construction. A thorough understanding of the DarkSide-50 detector response and, therefore, of all kind of observed events, is essential for an optimal design of the new experiment. In this paper, we report on a particular set of events, which were not used for dark matter searches. Namely, standard two-pulse scintillation-ionization signals accompanied by a small amplitude third pulse, originating from single or few electrons, in a time window of less than a maximum drift time. We compare our findings to those of a recent paper of the LUX Collaboration (D.S.Akerib et al. Phys.Rev.D 102, 092004). Indeed, both experiments observe events related to photoionization of the cathode. From the measured rate of these events, we estimate for the first time the quantum efficiency of the tetraphenyl butadiene deposited on the DarkSide-50 cathode at wavelengths around 128 nm, in liquid argon. Also, both experiments observe events likely related to photoionization of impurities in the liquid. The probability of photoelectron emission per unit length turns out to be one order of magnitude smaller in DarkSide-50 than in LUX. This result, together with the much larger measured electron lifetime, coherently hints toward a lower concentration of contaminants in DarkSide-50 than in LUX. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08015v2-abstract-full').style.display = 'none'; document.getElementById('2107.08015v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">10 pages, 8 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.10973">arXiv:2106.10973</a> <span> [<a href="https://arxiv.org/pdf/2106.10973">pdf</a>, <a href="https://arxiv.org/format/2106.10973">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/10.1140/epjc/s10052-021-09799-x">10.1140/epjc/s10052-021-09799-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Identification of the cosmogenic $^{11}$C background in large volumes of liquid scintillators with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacintio%2C+A">A. Di Giacintio</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (71 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="2106.10973v2-abstract-short" style="display: inline;"> Cosmogenic radio-nuclei are an important source of background for low-energy neutrino experiments. In Borexino, cosmogenic $^{11}$C decays outnumber solar $pep$ and CNO neutrino events by about ten to one. Highly efficient identification of this background is mandatory for these neutrino analyses. We present here the details of the most consolidated strategy, used throughout Borexino solar neutrin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10973v2-abstract-full').style.display = 'inline'; document.getElementById('2106.10973v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.10973v2-abstract-full" style="display: none;"> Cosmogenic radio-nuclei are an important source of background for low-energy neutrino experiments. In Borexino, cosmogenic $^{11}$C decays outnumber solar $pep$ and CNO neutrino events by about ten to one. Highly efficient identification of this background is mandatory for these neutrino analyses. We present here the details of the most consolidated strategy, used throughout Borexino solar neutrino measurements. It hinges upon finding the space-time correlations between $^{11}$C decays, the preceding parent muons and the accompanying neutrons. This article describes the working principles and evaluates the performance of this Three-Fold Coincidence (TFC) technique in its two current implementations: a hard-cut and a likelihood-based approach. Both show stable performances throughout Borexino Phases II (2012-2016) and III (2016-2020) data sets, with a $^{11}$C tagging efficiency of $\sim$90 % and $\sim$63-66 % of the exposure surviving the tagging. We present also a novel technique that targets specifically $^{11}$C produced in high-multiplicity during major spallation events. Such $^{11}$C appear as a burst of events, whose space-time correlation can be exploited. Burst identification can be combined with the TFC to obtain about the same tagging efficiency of $\sim$90 % but with a higher fraction of the exposure surviving, in the range of $\sim$66-68 %. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10973v2-abstract-full').style.display = 'none'; document.getElementById('2106.10973v2-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> 1 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">21 pages, 14 figures (but 15 files, one figure being made of 2 images), 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.13209">arXiv:2105.13209</a> <span> [<a href="https://arxiv.org/pdf/2105.13209">pdf</a>, <a href="https://arxiv.org/format/2105.13209">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> The Low Polonium Field of Borexino and its significance for the CNO neutrino detection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Kumaran%2C+S">S. Kumaran</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a> , et al. (71 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="2105.13209v1-abstract-short" style="display: inline;"> Borexino is a liquid scintillator detector located at the Laboratori Nazionale del Gran Sasso, Italy with the main goal to measure solar neutrinos. The experiment recently provided the first direct experimental evidence of CNO-cycle neutrinos in the Sun, rejecting the no-CNO signal hypothesis with a significance greater than 5$蟽$ at 99\%C.L. The intrinsic $^{210}$Bi is an important background for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13209v1-abstract-full').style.display = 'inline'; document.getElementById('2105.13209v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.13209v1-abstract-full" style="display: none;"> Borexino is a liquid scintillator detector located at the Laboratori Nazionale del Gran Sasso, Italy with the main goal to measure solar neutrinos. The experiment recently provided the first direct experimental evidence of CNO-cycle neutrinos in the Sun, rejecting the no-CNO signal hypothesis with a significance greater than 5$蟽$ at 99\%C.L. The intrinsic $^{210}$Bi is an important background for this analysis due to its similar spectral shape to that of CNO neutrinos. $^{210}$Bi can be measured through its daughter $^{210}$Po which can be distinguished through an event-by-event basis via pulse shape discrimination. However, this required reducing the convective motions in the scintillator that brought additional $^{210}$Po from peripheral sources. This was made possible through the thermal insulation and stabilization campaign performed between 2015 and 2016. This article will explain the strategy and the different methods performed to extract the $^{210}$Bi upper limit in Phase-III (Jul 2016- Feb 2020) of the experiment through the analysis of $^{210}$Po in the cleanest region of the detector called the Low Polonium Field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13209v1-abstract-full').style.display = 'none'; document.getElementById('2105.13209v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">Contribution to the 2021 Neutrinos session of the 55th Rencontres de Moriond</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.09225">arXiv:2105.09225</a> <span> [<a href="https://arxiv.org/pdf/2105.09225">pdf</a>, <a href="https://arxiv.org/format/2105.09225">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.L021302">10.1103/PhysRevD.104.L021302 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High sensitivity characterization of an ultra-high purity NaI(Tl) crystal scintillator with the SABRE proof-of-principle detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Copello%2C+S">S. Copello</a>, <a href="/search/physics?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=D%27Imperio%2C+G">G. D'Imperio</a>, <a href="/search/physics?searchtype=author&query=Di+Carlo%2C+G">G. Di Carlo</a>, <a href="/search/physics?searchtype=author&query=Diemoz%2C+M">M. Diemoz</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">A. Ianni</a>, <a href="/search/physics?searchtype=author&query=Iannone%2C+M">M. Iannone</a>, <a href="/search/physics?searchtype=author&query=Marchegiani%2C+F">F. Marchegiani</a>, <a href="/search/physics?searchtype=author&query=Mariani%2C+A">A. Mariani</a>, <a href="/search/physics?searchtype=author&query=Milana%2C+S">S. Milana</a>, <a href="/search/physics?searchtype=author&query=Nisi%2C+S">S. Nisi</a>, <a href="/search/physics?searchtype=author&query=Nuti%2C+F">F. Nuti</a>, <a href="/search/physics?searchtype=author&query=Orlandi%2C+D">D. Orlandi</a>, <a href="/search/physics?searchtype=author&query=Pettinacci%2C+V">V. Pettinacci</a>, <a href="/search/physics?searchtype=author&query=Pietrofaccia%2C+L">L. Pietrofaccia</a>, <a href="/search/physics?searchtype=author&query=Rahatlou%2C+S">S. Rahatlou</a>, <a href="/search/physics?searchtype=author&query=Souza%2C+M">M. Souza</a>, <a href="/search/physics?searchtype=author&query=Suerfu%2C+B">B. Suerfu</a>, <a href="/search/physics?searchtype=author&query=Tomei%2C+C">C. Tomei</a>, <a href="/search/physics?searchtype=author&query=Vignoli%2C+C">C. Vignoli</a>, <a href="/search/physics?searchtype=author&query=Wada%2C+M">M. Wada</a> , et al. (1 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="2105.09225v1-abstract-short" style="display: inline;"> We present new results on the radiopurity of a 3.4-kg NaI(Tl) crystal scintillator operated in the SABRE proof-of-principle detector setup. The amount of potassium contamination, determined by the direct counting of radioactive $^{40}$K, is found to be $2.2\pm1.5$ ppb, lowest ever achieved for NaI(Tl) crystals. With the active veto, the average background rate in the crystal in the 1-6 keV energy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09225v1-abstract-full').style.display = 'inline'; document.getElementById('2105.09225v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.09225v1-abstract-full" style="display: none;"> We present new results on the radiopurity of a 3.4-kg NaI(Tl) crystal scintillator operated in the SABRE proof-of-principle detector setup. The amount of potassium contamination, determined by the direct counting of radioactive $^{40}$K, is found to be $2.2\pm1.5$ ppb, lowest ever achieved for NaI(Tl) crystals. With the active veto, the average background rate in the crystal in the 1-6 keV energy region-of-interest (ROI) is $1.20\pm0.05$ counts/day/kg/keV, which is a breakthrough since the DAMA/LIBRA experiment. Our background model indicates that the rate is dominated by $^{210}$Pb and that about half of this contamination is located in the PTFE reflector. We discuss ongoing developments of the crystal manufacture aimed at the further reduction of the background, including data from purification by zone refining. A projected background rate lower than $\sim$0.2 counts/day/kg/keV in the ROI is within reach. These results represent a benchmark for the development of next-generation NaI(Tl) detector arrays for the direct detection of dark matter particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09225v1-abstract-full').style.display = 'none'; document.getElementById('2105.09225v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 104, 021302 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.06431">arXiv:2105.06431</a> <span> [<a href="https://arxiv.org/pdf/2105.06431">pdf</a>, <a href="https://arxiv.org/format/2105.06431">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="Materials Science">cond-mat.mtrl-sci</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/PhysRevApplied.16.014060">10.1103/PhysRevApplied.16.014060 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Zone refining of ultra-high purity sodium iodide for low-background detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Suerfu%2C+B">Burkhant Suerfu</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">Frank Calaprice</a>, <a href="/search/physics?searchtype=author&query=Souza%2C+M">Michael Souza</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="2105.06431v1-abstract-short" style="display: inline;"> There has been a growing interest in ultra-high purity, low-background NaI(Tl) crystals for dark matter direct searches. Past research indicates that zone refining is an efficient and scalable way to purify NaI. In particular, K and Rb -- two elements with radioisotopes that can cause scintillation backgrounds -- can be efficiently removed by zone refining. However, zone refining has never been de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06431v1-abstract-full').style.display = 'inline'; document.getElementById('2105.06431v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.06431v1-abstract-full" style="display: none;"> There has been a growing interest in ultra-high purity, low-background NaI(Tl) crystals for dark matter direct searches. Past research indicates that zone refining is an efficient and scalable way to purify NaI. In particular, K and Rb -- two elements with radioisotopes that can cause scintillation backgrounds -- can be efficiently removed by zone refining. However, zone refining has never been demonstrated for ultra-high purity NaI which became commercially available recently. In this article, we show that many common metallic impurities can be efficiently removed via zone refining. A numerical model for predicting the final impurity distribution was developed and used to fit the ICP-MS measurement data to determine the segregation coefficient and the initial concentration. Under this scheme, the segregation coefficient for K is estimated to be 0.57, indicating that zone refining is still effective in removing K from ultra-high purity NaI. As zone refining tends to move the impurities to one end, elements with concentrations too low to be measured directly in the unprocessed powder can potentially be detected in the end due to the enrichment. We also present an analysis technique to estimate the initial concentrations of impurities with partial data, which effectively enhances the sensitivity of the spectrometer. Using this technique, the initial concentration of $^{85}$Rb is estimated to be between 5 ppt and 14 ppt at 90% CL, at least 14 times lower than the detection limit of ICP-MS and 7 times lower than the current most stringent limit set by the DAMA collaboration by direct counting of radioactive $^{87}$Rb. These results imply that zone refining is a key technique in developing next-generation, NaI-based crystal scintillators for dark matter direct detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06431v1-abstract-full').style.display = 'none'; document.getElementById('2105.06431v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Applied 16, 014060 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02610">arXiv:2012.02610</a> <span> [<a href="https://arxiv.org/pdf/2012.02610">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/10.1140/epjc/s10052-021-09098-5">10.1140/epjc/s10052-021-09098-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of SABRE crystal NaI-33 with direct underground counting </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Antonello%2C+M">M. Antonello</a>, <a href="/search/physics?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/physics?searchtype=author&query=Barberio%2C+E">E. Barberio</a>, <a href="/search/physics?searchtype=author&query=Baroncelli%2C+T">T. Baroncelli</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bignell%2C+L+J">L. J. Bignell</a>, <a href="/search/physics?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Copello%2C+S">S. Copello</a>, <a href="/search/physics?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=D%27Imperio%2C+G">G. D'Imperio</a>, <a href="/search/physics?searchtype=author&query=D%27Incecco%2C+M">M. D'Incecco</a>, <a href="/search/physics?searchtype=author&query=Di+Carlo%2C+G">G. Di Carlo</a>, <a href="/search/physics?searchtype=author&query=Diemoz%2C+M">M. Diemoz</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Dix%2C+W">W. Dix</a>, <a href="/search/physics?searchtype=author&query=Duffy%2C+A+R">A. R. Duffy</a>, <a href="/search/physics?searchtype=author&query=Hoppe%2C+E">E. Hoppe</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">A. Ianni</a>, <a href="/search/physics?searchtype=author&query=Iannone%2C+M">M. Iannone</a>, <a href="/search/physics?searchtype=author&query=Ioannucci%2C+L">L. Ioannucci</a>, <a href="/search/physics?searchtype=author&query=Krishnan%2C+S">S. Krishnan</a>, <a href="/search/physics?searchtype=author&query=Lane%2C+G+J">G. J. Lane</a> , et al. (21 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="2012.02610v2-abstract-short" style="display: inline;"> Ultra-pure NaI(Tl) crystals are the key element for a model-independent verification of the long standing DAMA result and a powerful means to search for the annual modulation signature of dark matter interactions. The SABRE collaboration has been developing cutting-edge techniques for the reduction of intrinsic backgrounds over several years. In this paper we report the first characterization of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02610v2-abstract-full').style.display = 'inline'; document.getElementById('2012.02610v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02610v2-abstract-full" style="display: none;"> Ultra-pure NaI(Tl) crystals are the key element for a model-independent verification of the long standing DAMA result and a powerful means to search for the annual modulation signature of dark matter interactions. The SABRE collaboration has been developing cutting-edge techniques for the reduction of intrinsic backgrounds over several years. In this paper we report the first characterization of a 3.4 kg crystal, named NaI-33, performed in an underground passive shielding setup at LNGS. NaI-33 has a record low $^{39}$K contamination of 4.3$\pm$0.2 ppb as determined by mass spectrometry. We measured a light yield of 11.1$\pm$0.2 photoelectrons/keV and an energy resolution of 13.2% (FWHM/E) at 59.5 keV. We evaluated the activities of $^{226}$Ra and $^{228}$Th inside the crystal to be $5.9\pm0.6 渭$Bq/kg and $1.6\pm0.3 渭$Bq/kg, respectively, which would indicate a contamination from $^{238}$U and $^{232}$Th at part-per-trillion level. We measured an activity of 0.51$\pm$0.02 mBq/kg due to $^{210}$Pb out of equilibrium and a $伪$ quenching factor of 0.63$\pm$0.01 at 5304 keV. We illustrate the analyses techniques developed to reject electronic noise in the lower part of the energy spectrum. A cut-based strategy and a multivariate approach indicated a rate, attributed to the intrinsic radioactivity of the crystal, of $\sim$1 count/day/kg/keV in the [5-20] keV region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02610v2-abstract-full').style.display = 'none'; document.getElementById('2012.02610v2-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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, 299 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.15115">arXiv:2006.15115</a> <span> [<a href="https://arxiv.org/pdf/2006.15115">pdf</a>, <a href="https://arxiv.org/format/2006.15115">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-020-2934-0">10.1038/s41586-020-2934-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (71 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="2006.15115v2-abstract-short" style="display: inline;"> For most of their existence stars are fueled by the fusion of hydrogen into helium proceeding via two theoretically well understood processes, namely the $pp$ chain and the CNO cycle. Neutrinos emitted along such fusion processes in the solar core are the only direct probe of the deep interior of the star. A complete spectroscopy of neutrinos from the {\it pp} chain, producing about 99\% of the so… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.15115v2-abstract-full').style.display = 'inline'; document.getElementById('2006.15115v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.15115v2-abstract-full" style="display: none;"> For most of their existence stars are fueled by the fusion of hydrogen into helium proceeding via two theoretically well understood processes, namely the $pp$ chain and the CNO cycle. Neutrinos emitted along such fusion processes in the solar core are the only direct probe of the deep interior of the star. A complete spectroscopy of neutrinos from the {\it pp} chain, producing about 99\% of the solar energy, has already been performed \cite{bib:Nature-2018}. Here, we report the direct observation, with a high statistical significance, of neutrinos produced in the CNO cycle in the Sun. This is the first experimental evidence of this process obtained with the unprecedentedly radio-pure large-volume liquid-scintillator Borexino detector located at the underground Laboratori Nazionali del Gran Sasso in Italy. The main difficulty of this experimental effort is to identify the excess of the few counts per day per 100 tonnes of target due to CNO neutrino interactions above the backgrounds. A novel method to constrain the rate of \bi contaminating the scintillator relies on the thermal stabilisation of the detector achieved over the past 5 years. In the CNO cycle, the hydrogen fusion is catalyzed by the carbon (C) - nitrogen (N) - oxygen (O) and thus its rate, as well as the flux of emitted CNO neutrinos, directly depends on the abundance of these elements in solar core. Therefore, this result paves the way to a direct measurement of the solar metallicity by CNO neutrinos. While this result quantifies the relative contribution of the CNO fusion in the Sun to be of the order of 1\%, this process is dominant in the energy production of massive stars. The occurrence of the primary mechanism for the stellar conversion of hydrogen into helium in the Universe has been proven. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.15115v2-abstract-full').style.display = 'none'; document.getElementById('2006.15115v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">43 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-05 <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> G.3.1 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.12829">arXiv:2005.12829</a> <span> [<a href="https://arxiv.org/pdf/2005.12829">pdf</a>, <a href="https://arxiv.org/format/2005.12829">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div 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/s10052-020-08534-2">10.1140/epjc/s10052-020-08534-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity to neutrinos from the solar CNO cycle in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (69 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.12829v3-abstract-short" style="display: inline;"> Neutrinos emitted in the carbon, nitrogen, oxygen (CNO) fusion cycle in the Sun are a sub-dominant, yet crucial component of solar neutrinos whose flux has not been measured yet. The Borexino experiment at the Laboratori Nazionali del Gran Sasso (Italy) has a unique opportunity to detect them directly thanks to the detector's radiopurity and the precise understanding of the detector backgrounds. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12829v3-abstract-full').style.display = 'inline'; document.getElementById('2005.12829v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.12829v3-abstract-full" style="display: none;"> Neutrinos emitted in the carbon, nitrogen, oxygen (CNO) fusion cycle in the Sun are a sub-dominant, yet crucial component of solar neutrinos whose flux has not been measured yet. The Borexino experiment at the Laboratori Nazionali del Gran Sasso (Italy) has a unique opportunity to detect them directly thanks to the detector's radiopurity and the precise understanding of the detector backgrounds. We discuss the sensitivity of Borexino to CNO neutrinos, which is based on the strategies we adopted to constrain the rates of the two most relevant background sources, pep neutrinos from the solar pp-chain and Bi-210 beta decays originating in the intrinsic contamination of the liquid scintillator with Pb-210. Assuming the CNO flux predicted by the high-metallicity Standard Solar Model and an exposure of 1000 daysx71.3 t, Borexino has a median sensitivity to CNO neutrino higher than 3 sigma. With the same hypothesis the expected experimental uncertainty on the CNO neutrino flux is 23%, provided the uncertainty on the independent estimate of the Bi-210 interaction rate is 1.5 cpd/100t. Finally, we evaluated the expected uncertainty of the C and N abundances and the expected discrimination significance between the high and low metallicity Standard Solar Models (HZ and LZ) with future more precise measurement of the CNO solar neutrino flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12829v3-abstract-full').style.display = 'none'; document.getElementById('2005.12829v3-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> BX-DocDB-674 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 80, 1091 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.07794">arXiv:2002.07794</a> <span> [<a href="https://arxiv.org/pdf/2002.07794">pdf</a>, <a href="https://arxiv.org/format/2002.07794">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Effective field theory interactions for liquid argon target in DarkSide-50 experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</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=Alton%2C+A+K">A. K. Alton</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=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a> , et al. (143 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="2002.07794v1-abstract-short" style="display: inline;"> We reanalize data collected with the DarkSide-50 experiment and recently used to set limits on the spin-independent interaction rate of weakly interacting massive particles (WIMPs) on argon nuclei with an effective field theory framework. The dataset corresponds to a total (16660 $\pm$ 270) kg d exposure using a target of low-radioactivity argon extracted from underground sources. We obtain upper… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.07794v1-abstract-full').style.display = 'inline'; document.getElementById('2002.07794v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.07794v1-abstract-full" style="display: none;"> We reanalize data collected with the DarkSide-50 experiment and recently used to set limits on the spin-independent interaction rate of weakly interacting massive particles (WIMPs) on argon nuclei with an effective field theory framework. The dataset corresponds to a total (16660 $\pm$ 270) kg d exposure using a target of low-radioactivity argon extracted from underground sources. We obtain upper limits on the effective couplings of the 12 leading operators in the nonrelativistic systematic expansion. For each effective coupling we set constraints on WIMP-nucleon cross sections, setting upper limits between $2.4 \times 10^{-45} \, \mathrm{cm}^2$ and $2.3 \times 10^{-42} \, \mathrm{cm}^2$ (8.9 $\times 10^{-45} \, \mathrm{cm}^2$ and 6.0 $\times 10^{-42} \, \mathrm{cm}^2$) for WIMPs of mass of 100 $\mathrm{GeV/c^2}$ (1000 $\mathrm{GeV/c^2}$) at 90\% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.07794v1-abstract-full').style.display = 'none'; document.getElementById('2002.07794v1-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 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">Accepted by PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.03782">arXiv:1910.03782</a> <span> [<a href="https://arxiv.org/pdf/1910.03782">pdf</a>, <a href="https://arxiv.org/format/1910.03782">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevResearch.2.013223">10.1103/PhysRevResearch.2.013223 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Growth of Ultra-high Purity NaI(Tl) Crystal for Dark Matter Searches </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Suerfu%2C+B">Burkhant Suerfu</a>, <a href="/search/physics?searchtype=author&query=Wada%2C+M">Masayuki Wada</a>, <a href="/search/physics?searchtype=author&query=Peloso%2C+W">Winston Peloso</a>, <a href="/search/physics?searchtype=author&query=Souza%2C+M">Michael Souza</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">Frank Calaprice</a>, <a href="/search/physics?searchtype=author&query=Tower%2C+J">Joshua Tower</a>, <a href="/search/physics?searchtype=author&query=Ciampi%2C+G">Guido Ciampi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.03782v2-abstract-short" style="display: inline;"> The annual modulation of scintillation event rate observed by the DAMA/LIBRA experiment has been a long-standing controversy in the quest of the direct detection of dark matter. The effort to definitively confirm or refute the annual modulation has turned out to be challenging due to the lack of NaI(Tl) crystals with high enough radio-purity. Most recently, we successfully grew a 6-kg ingot free f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.03782v2-abstract-full').style.display = 'inline'; document.getElementById('1910.03782v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.03782v2-abstract-full" style="display: none;"> The annual modulation of scintillation event rate observed by the DAMA/LIBRA experiment has been a long-standing controversy in the quest of the direct detection of dark matter. The effort to definitively confirm or refute the annual modulation has turned out to be challenging due to the lack of NaI(Tl) crystals with high enough radio-purity. Most recently, we successfully grew a 6-kg ingot free from contamination during growth, from which a 3.4-kg crystal scintillator was made. The $^{39}$K concentration in the final crystal is estimated to be 4.3$\pm$0.2~ppb, unprecedented for NaI(Tl) crystals. The $^{210}$Pb activity is estimated to be 0.34$\pm$0.04~mBq/kg via $伪$ counting of $^{210}$Po, among the lowest of currently-running NaI-based dark matter experiments except DAMA/LIBRA. More importantly, the techniques and protocols we have developed will further contribute to the growth of higher purity NaI(Tl) crystals for dark matter searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.03782v2-abstract-full').style.display = 'none'; document.getElementById('1910.03782v2-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Research 2, 013223 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.02422">arXiv:1909.02422</a> <span> [<a href="https://arxiv.org/pdf/1909.02422">pdf</a>, <a href="https://arxiv.org/format/1909.02422">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Search for low-energy neutrinos from astrophysical sources with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a> , et al. (79 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="1909.02422v1-abstract-short" style="display: inline;"> We report on searches for neutrinos and antineutrinos from astrophysical sources performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. Electron antineutrinos ($\bar谓_e$) are detected in an organic liquid scintillator through the inverse $尾$-decay reaction. In the present work we set model-independent upper limits in the energy range 1.8-16.8 MeV on neutrino flux… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02422v1-abstract-full').style.display = 'inline'; document.getElementById('1909.02422v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.02422v1-abstract-full" style="display: none;"> We report on searches for neutrinos and antineutrinos from astrophysical sources performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. Electron antineutrinos ($\bar谓_e$) are detected in an organic liquid scintillator through the inverse $尾$-decay reaction. In the present work we set model-independent upper limits in the energy range 1.8-16.8 MeV on neutrino fluxes from unknown sources that improve our previous results, on average, by a factor 2.5. Using the same data set, we first obtain experimental constraints on the diffuse supernova $\bar谓_e$ fluxes in the previously unexplored region below 8 MeV. A search for $\bar谓_e$ in the solar neutrino flux is also presented: the presence of $\bar谓_e$ would be a manifestation of a non-zero anomalous magnetic moment of the neutrino, making possible its conversion to antineutrinos in the strong magnetic field of the Sun. We obtain a limit for a solar $\bar谓_e$ flux of 384 cm$^{-2}$s$^{-1}$ (90% C.L.), assuming an undistorted solar $^{8}$B neutrinos energy spectrum, that corresponds to a transition probability $p_{ 谓_e \rightarrow \bar谓_{e}}<$ 7.2$\times$10$^{-5}$ (90% C.L.) for E$_{\bar 谓_e}$ $>$ 1.8 MeV. At lower energies, by investigating the spectral shape of elastic scattering events, we obtain a new limit on solar $^{7}$Be-$谓_e$ conversion into $\bar谓_e$ of $p_{ 谓_e \rightarrow \bar 谓_{e}}<$ 0.14 (90% C.L.) at 0.862 keV. Last, we investigate solar flares as possible neutrino sources and obtain the strongest up-to-date limits on the fluence of neutrinos of all flavor neutrino below 3-7 ,MeV. Assuming the neutrino flux to be proportional to the flare's intensity, we exclude an intense solar flare as the cause of the observed excess of events in run 117 of the Cl-Ar Homestake experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02422v1-abstract-full').style.display = 'none'; document.getElementById('1909.02422v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">18 pages, 8 figures, 4 tables, 73 references</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.02257">arXiv:1909.02257</a> <span> [<a href="https://arxiv.org/pdf/1909.02257">pdf</a>, <a href="https://arxiv.org/format/1909.02257">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-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/PhysRevD.101.012009">10.1103/PhysRevD.101.012009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comprehensive geoneutrino analysis with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a> , et al. (87 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="1909.02257v2-abstract-short" style="display: inline;"> This paper presents a geoneutrino measurement using 3262.74 days of data taken with the Borexino detector at LNGS in Italy. By observing $52.6 ^{+9.4}_{-8.6} ({\rm stat}) ^{+2.7}_{-2.1}({\rm sys})$ geoneutrinos (68% interval) from $^{238}$U and $^{232}$Th, a signal of $47.0^{+8.4}_{-7.7}\,({\rm stat)}^{+2.4}_{-1.9}\,({\rm sys})$ TNU with $^{+18.3}_{-17.2}$% total precision was obtained. This resul… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02257v2-abstract-full').style.display = 'inline'; document.getElementById('1909.02257v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.02257v2-abstract-full" style="display: none;"> This paper presents a geoneutrino measurement using 3262.74 days of data taken with the Borexino detector at LNGS in Italy. By observing $52.6 ^{+9.4}_{-8.6} ({\rm stat}) ^{+2.7}_{-2.1}({\rm sys})$ geoneutrinos (68% interval) from $^{238}$U and $^{232}$Th, a signal of $47.0^{+8.4}_{-7.7}\,({\rm stat)}^{+2.4}_{-1.9}\,({\rm sys})$ TNU with $^{+18.3}_{-17.2}$% total precision was obtained. This result assumes the same Th/U mass ratio found in chondritic CI meteorites but compatible results were found when contributions from $^{238}$U and $^{232}$Th were fit as free parameters. Antineutrino background from reactors is fit unconstrained and found compatible with the expectations. The null-hypothesis of observing a signal from the mantle is excluded at a 99.0% C.L. when exploiting the knowledge of the local crust. Measured mantle signal of $21.2 ^{+9.6}_{-9.0} ({\rm stat})^{+1.1}_{-0.9} ({\rm sys})$ TNU corresponds to the production of a radiogenic heat of $24.6 ^{+11.1}_{-10.4}$ TW (68% interval) from $^{238}$U and $^{232}$Th in the mantle. Assuming 18% contribution of $^{40}$K in the mantle and $8.1^{+1.9}_{-1.4}$ TW of radiogenic heat of the lithosphere, the Borexino estimate of the total Earth radiogenic heat is $38.2 ^{+13.6}_{-12.7}$ TW, corresponding to a convective Urey ratio of 0.78$^{+0.41}_{-0.28}$. These values are compatible with different geological models, however there is a 2.4$蟽$ tension with those which predict the lowest concentration of heat-producing elements. By fitting the data with a constraint on the reactor antineutrino background, the existence of a hypothetical georeactor at the center of the Earth having power greater than 2.4 TW at 95% C.L. is excluded. Particular attention is given to all analysis details, which should be of interest for the next generation geoneutrino measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02257v2-abstract-full').style.display = 'none'; document.getElementById('1909.02257v2-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 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">69 pages, 56 Figures (some composed of multiple files), 17 Tables, 135 References</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 012009 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.09332">arXiv:1907.09332</a> <span> [<a href="https://arxiv.org/pdf/1907.09332">pdf</a>, <a href="https://arxiv.org/format/1907.09332">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/10.1088/1748-0221/14/11/P11018">10.1088/1748-0221/14/11/P11018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the ion fraction and mobility of $^{218}$Po produced in $^{222}$Rn decays in liquid argon </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=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=Alton%2C+A+K">A. K. Alton</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=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/physics?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a>, <a href="/search/physics?searchtype=author&query=Catalanotti%2C+S">S. Catalanotti</a>, <a href="/search/physics?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a> , et al. (141 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="1907.09332v2-abstract-short" style="display: inline;"> We report measurements of the charged daughter fraction of $^{218}$Po as a result of the $^{222}$Rn alpha decay, and the mobility of $^{218}$Po$^+$ ions, using radon-polonium coincidences from the $^{238}$U chain identified in 532 live-days of DarkSide-50 WIMP-search data. The fraction of $^{218}$Po that is charged is found to be 0.37$\pm$0.03 and the mobility of $^{218}$Po$^+$ is (8.6$\pm$0.1)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.09332v2-abstract-full').style.display = 'inline'; document.getElementById('1907.09332v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.09332v2-abstract-full" style="display: none;"> We report measurements of the charged daughter fraction of $^{218}$Po as a result of the $^{222}$Rn alpha decay, and the mobility of $^{218}$Po$^+$ ions, using radon-polonium coincidences from the $^{238}$U chain identified in 532 live-days of DarkSide-50 WIMP-search data. The fraction of $^{218}$Po that is charged is found to be 0.37$\pm$0.03 and the mobility of $^{218}$Po$^+$ is (8.6$\pm$0.1)$\times$10$^{-4}$$\frac{\text{cm}^2}{\text{Vs}}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.09332v2-abstract-full').style.display = 'none'; document.getElementById('1907.09332v2-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 14 P11018 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.03512">arXiv:1905.03512</a> <span> [<a href="https://arxiv.org/pdf/1905.03512">pdf</a>, <a href="https://arxiv.org/format/1905.03512">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1007/JHEP02(2020)038">10.1007/JHEP02(2020)038 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on Flavor-Diagonal Non-Standard Neutrino Interactions from Borexino Phase-II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a> , et al. (81 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="1905.03512v2-abstract-short" style="display: inline;"> The Borexino detector measures solar neutrino fluxes via neutrino-electron elastic scattering. Observed spectra are determined by the solar-$谓_{e}$ survival probability $P_{ee}(E)$, and the chiral couplings of the neutrino and electron. Some theories of physics beyond the Standard Model postulate the existence of Non-Standard Interactions (NSI's) which modify the chiral couplings and $P_{ee}(E)$.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03512v2-abstract-full').style.display = 'inline'; document.getElementById('1905.03512v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.03512v2-abstract-full" style="display: none;"> The Borexino detector measures solar neutrino fluxes via neutrino-electron elastic scattering. Observed spectra are determined by the solar-$谓_{e}$ survival probability $P_{ee}(E)$, and the chiral couplings of the neutrino and electron. Some theories of physics beyond the Standard Model postulate the existence of Non-Standard Interactions (NSI's) which modify the chiral couplings and $P_{ee}(E)$. In this paper, we search for such NSI's, in particular, flavor-diagonal neutral current interactions that modify the $谓_e e$ and $谓_蟿e$ couplings using Borexino Phase II data. Standard Solar Model predictions of the solar neutrino fluxes for both high- and low-metallicity assumptions are considered. No indication of new physics is found at the level of sensitivity of the detector and constraints on the parameters of the NSI's are placed. In addition, with the same dataset the value of $\sin^2胃_W$ is obtained with a precision comparable to that achieved in reactor antineutrino experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03512v2-abstract-full').style.display = 'none'; document.getElementById('1905.03512v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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">28 pages, 7 figures. Slight modifications in the title, abstract, and conclusion. Few references added. Text expanded for clarity. Accepted in JHEP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> IP/BBSR/2019-2 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 2002 (2020) 038 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.04207">arXiv:1808.04207</a> <span> [<a href="https://arxiv.org/pdf/1808.04207">pdf</a>, <a href="https://arxiv.org/format/1808.04207">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2019/02/046">10.1088/1475-7516/2019/02/046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modulations of the Cosmic Muon Signal in Ten Years of Borexino Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+Borexino+Collaboration"> The Borexino Collaboration</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a> , et al. (91 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="1808.04207v3-abstract-short" style="display: inline;"> We have measured the flux of cosmic muons in the Laboratori Nazionali del Gran Sasso at 3800\,m\,w.e. to be $(3.432 \pm 0.003)\cdot 10^{-4}\,\mathrm{{m^{-2}s^{-1}}}$ based on ten years of Borexino data acquired between May 2007 and May 2017. A seasonal modulation with a period of $(366.3 \pm 0.6)\,\mathrm{d}$ and a relative amplitude of $(1.36 \pm0.04)\%$ is observed. The phase is measured to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.04207v3-abstract-full').style.display = 'inline'; document.getElementById('1808.04207v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.04207v3-abstract-full" style="display: none;"> We have measured the flux of cosmic muons in the Laboratori Nazionali del Gran Sasso at 3800\,m\,w.e. to be $(3.432 \pm 0.003)\cdot 10^{-4}\,\mathrm{{m^{-2}s^{-1}}}$ based on ten years of Borexino data acquired between May 2007 and May 2017. A seasonal modulation with a period of $(366.3 \pm 0.6)\,\mathrm{d}$ and a relative amplitude of $(1.36 \pm0.04)\%$ is observed. The phase is measured to be $(181.7 \pm 0.4)\,\mathrm{d}$, corresponding to a maximum at the 1$^\mathrm{st}$ of July. Using data inferred from global atmospheric models, we show the muon flux to be positively correlated with the atmospheric temperature and measure the effective temperature coefficient $伪_\mathrm{T} = 0.90 \pm 0.02$. The origin of cosmic muons from pion and kaon decays in the atmosphere allows to interpret the effective temperature coefficient as an indirect measurement of the atmospheric kaon-to-pion production ratio $r_{\mathrm{K}/蟺} = 0.11^{+0.11}_{-0.07}$ for primary energies above $18\,\mathrm{TeV}$. We find evidence for a long-term modulation of the muon flux with a period of $\sim 3000\,\mathrm{d}$ and a maximum in June 2012 that is not present in the atmospheric temperature data. A possible correlation between this modulation and the solar activity is investigated. The cosmogenic neutron production rate is found to show a seasonal modulation in phase with the cosmic muon flux but with an increased amplitude of $(2.6 \pm 0.4)\%$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.04207v3-abstract-full').style.display = 'none'; document.getElementById('1808.04207v3-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">30 pages, 16 figures, proofreading for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.09344">arXiv:1806.09344</a> <span> [<a href="https://arxiv.org/pdf/1806.09344">pdf</a>, <a href="https://arxiv.org/format/1806.09344">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/10.1016/j.astropartphys.2018.10.005">10.1016/j.astropartphys.2018.10.005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monte Carlo simulation of the SABRE PoP background </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Antonello%2C+M">M. Antonello</a>, <a href="/search/physics?searchtype=author&query=Barberio%2C+E">E. Barberio</a>, <a href="/search/physics?searchtype=author&query=Baroncelli%2C+T">T. Baroncelli</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bignell%2C+L+J">L. J. Bignell</a>, <a href="/search/physics?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Copello%2C+S">S. Copello</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=D%27Imperio%2C+G">G. D'Imperio</a>, <a href="/search/physics?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/physics?searchtype=author&query=Di+Carlo%2C+G">G. Di Carlo</a>, <a href="/search/physics?searchtype=author&query=Diemoz%2C+M">M. Diemoz</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Duffy%2C+A+R">A. R. Duffy</a>, <a href="/search/physics?searchtype=author&query=Froborg%2C+F">F. Froborg</a>, <a href="/search/physics?searchtype=author&query=Giovanetti%2C+G+K">G. K. Giovanetti</a>, <a href="/search/physics?searchtype=author&query=Hoppe%2C+E">E. Hoppe</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">A. Ianni</a>, <a href="/search/physics?searchtype=author&query=Ioannucci%2C+L">L. Ioannucci</a>, <a href="/search/physics?searchtype=author&query=Krishnan%2C+S">S. Krishnan</a>, <a href="/search/physics?searchtype=author&query=Lane%2C+G+J">G. J. Lane</a>, <a href="/search/physics?searchtype=author&query=Mahmood%2C+I">I. Mahmood</a>, <a href="/search/physics?searchtype=author&query=Mariani%2C+A">A. Mariani</a>, <a href="/search/physics?searchtype=author&query=McGee%2C+P">P. McGee</a> , et al. (23 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="1806.09344v3-abstract-short" style="display: inline;"> SABRE (Sodium-iodide with Active Background REjection) is a direct dark matter search experiment based on an array of radio-pure NaI(Tl) crystals surrounded by a liquid scintillator veto. Twin SABRE experiments in the Northern and Southern Hemispheres will differentiate a dark matter signal from seasonal and local effects. The experiment is currently in a Proof-of-Principle (PoP) phase, whose goal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09344v3-abstract-full').style.display = 'inline'; document.getElementById('1806.09344v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.09344v3-abstract-full" style="display: none;"> SABRE (Sodium-iodide with Active Background REjection) is a direct dark matter search experiment based on an array of radio-pure NaI(Tl) crystals surrounded by a liquid scintillator veto. Twin SABRE experiments in the Northern and Southern Hemispheres will differentiate a dark matter signal from seasonal and local effects. The experiment is currently in a Proof-of-Principle (PoP) phase, whose goal is to demonstrate that the background rate is low enough to carry out an independent search for a dark matter signal, with sufficient sensitivity to confirm or refute the DAMA result during the following full-scale experimental phase. The impact of background radiation from the detector materials and the experimental site needs to be carefully investigated, including both intrinsic and cosmogenically activated radioactivity. Based on the best knowledge of the most relevant sources of background, we have performed a detailed Monte Carlo study evaluating the expected background in the dark matter search spectral region. The simulation model described in this paper guides the design of the full-scale experiment and will be fundamental for the interpretation of the measured background and hence for the extraction of a possible dark matter signal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09344v3-abstract-full').style.display = 'none'; document.getElementById('1806.09344v3-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 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 106, 1 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.09340">arXiv:1806.09340</a> <span> [<a href="https://arxiv.org/pdf/1806.09340">pdf</a>, <a href="https://arxiv.org/format/1806.09340">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/10.1140/epjc/s10052-019-6860-y">10.1140/epjc/s10052-019-6860-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SABRE project and the SABRE PoP </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Antonello%2C+M">M. Antonello</a>, <a href="/search/physics?searchtype=author&query=Barberio%2C+E">E. Barberio</a>, <a href="/search/physics?searchtype=author&query=Baroncelli%2C+T">T. Baroncelli</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bignell%2C+L+J">L. J. Bignell</a>, <a href="/search/physics?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Copello%2C+S">S. Copello</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=D%27Imperio%2C+G">G. D'Imperio</a>, <a href="/search/physics?searchtype=author&query=Dafinei%2C+I">I. Dafinei</a>, <a href="/search/physics?searchtype=author&query=Di+Carlo%2C+G">G. Di Carlo</a>, <a href="/search/physics?searchtype=author&query=Diemoz%2C+M">M. Diemoz</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Dix%2C+W">W. Dix</a>, <a href="/search/physics?searchtype=author&query=Duffy%2C+A+R">A. R. Duffy</a>, <a href="/search/physics?searchtype=author&query=Froborg%2C+F">F. Froborg</a>, <a href="/search/physics?searchtype=author&query=Giovanetti%2C+G+K">G. K. Giovanetti</a>, <a href="/search/physics?searchtype=author&query=Hoppe%2C+E">E. Hoppe</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">A. Ianni</a>, <a href="/search/physics?searchtype=author&query=Ioannucci%2C+L">L. Ioannucci</a>, <a href="/search/physics?searchtype=author&query=Krishnan%2C+S">S. Krishnan</a>, <a href="/search/physics?searchtype=author&query=Lane%2C+G+J">G. J. Lane</a>, <a href="/search/physics?searchtype=author&query=Mahmood%2C+I">I. Mahmood</a>, <a href="/search/physics?searchtype=author&query=Mariani%2C+A">A. Mariani</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="1806.09340v2-abstract-short" style="display: inline;"> SABRE aims to directly measure the annual modulation of the dark matter interaction rate with NaI(Tl) crystals. A modulation compatible with the standard hypothesis in which our Galaxy is embedded in a dark matter halo has been measured by the DAMA experiment in the same target material. Other direct detection experiments, using different target materials, seem to exclude the interpretation of suc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09340v2-abstract-full').style.display = 'inline'; document.getElementById('1806.09340v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.09340v2-abstract-full" style="display: none;"> SABRE aims to directly measure the annual modulation of the dark matter interaction rate with NaI(Tl) crystals. A modulation compatible with the standard hypothesis in which our Galaxy is embedded in a dark matter halo has been measured by the DAMA experiment in the same target material. Other direct detection experiments, using different target materials, seem to exclude the interpretation of such modulation in the simplest scenario of WIMP-nucleon elastic scattering. The SABRE experiment aims to carry out an independent search with sufficient sensitivity to confirm or refute the DAMA claim. The SABRE concept and goal is to obtain a background rate of the order of 0.1 cpd/kg/keVee in the energy region of interest. This challenging goal is achievable by operating high-purity crystals inside a liquid scintillator veto for active background rejection. In addition, twin detectors will be located in the northern and southern hemispheres to identify possible contributions to the modulation from seasonal or site-related effects. The SABRE project includes an initial Proof-of-Principle phase at LNGS (Italy), to assess the radio-purity of the crystals and the efficiency of the liquid scintillator veto. This paper describes the general concept of SABRE and the expected sensitivity to WIMP annual modulation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09340v2-abstract-full').style.display = 'none'; document.getElementById('1806.09340v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">7 pages, 4 figures</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 (2019) 79: 363 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.11125">arXiv:1805.11125</a> <span> [<a href="https://arxiv.org/pdf/1805.11125">pdf</a>, <a href="https://arxiv.org/format/1805.11125">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-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/10.1088/1742-6596/1342/1/012115">10.1088/1742-6596/1342/1/012115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Speeding up complex multivariate data analysis in Borexino with parallel computing based on Graphics Processing Unit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a> , et al. (82 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="1805.11125v1-abstract-short" style="display: inline;"> A spectral fitter based on the graphics processor unit (GPU) has been developed for Borexino solar neutrino analysis. It is able to shorten the fitting time to a superior level compared to the CPU fitting procedure. In Borexino solar neutrino spectral analysis, fitting usually requires around one hour to converge since it includes time-consuming convolutions in order to account for the detector re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11125v1-abstract-full').style.display = 'inline'; document.getElementById('1805.11125v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.11125v1-abstract-full" style="display: none;"> A spectral fitter based on the graphics processor unit (GPU) has been developed for Borexino solar neutrino analysis. It is able to shorten the fitting time to a superior level compared to the CPU fitting procedure. In Borexino solar neutrino spectral analysis, fitting usually requires around one hour to converge since it includes time-consuming convolutions in order to account for the detector response and pile-up effects. Moreover, the convergence time increases to more than two days when including extra computations for the discrimination of $^{11}$C and external $纬$s. In sharp contrast, with the GPU-based fitter it takes less than 10 seconds and less than four minutes, respectively. This fitter is developed utilizing the GooFit project with customized likelihoods, pdfs and infrastructures supporting certain analysis methods. In this proceeding the design of the package, developed features and the comparison with the original CPU fitter are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11125v1-abstract-full').style.display = 'none'; document.getElementById('1805.11125v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">5 pages, 2 figures, proceeding for TAUP 2017 XV International Conference on Topics in Astroparticle and Underground Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> 1342 no. 012115 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Physics: Conference Series (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.06895">arXiv:1804.06895</a> <span> [<a href="https://arxiv.org/pdf/1804.06895">pdf</a>, <a href="https://arxiv.org/format/1804.06895">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/10.1103/PhysRevD.98.062002">10.1103/PhysRevD.98.062002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Surface background suppression in liquid argon dark matter detectors using a newly discovered time component of tetraphenyl-butadiene scintillation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Stanford%2C+C">Chris Stanford</a>, <a href="/search/physics?searchtype=author&query=Westerdale%2C+S">Shawn Westerdale</a>, <a href="/search/physics?searchtype=author&query=Xu%2C+J">Jingke Xu</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">Frank Calaprice</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="1804.06895v4-abstract-short" style="display: inline;"> Decays of radioisotopes on inner detector surfaces can pose a major background concern for the direct detection of dark matter. While these backgrounds are conventionally mitigated with position cuts, these cuts reduce the exposure of the detector by decreasing the sensitive mass, and uncertainty in position determination may make it impossible to adequately remove such events in certain detectors… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.06895v4-abstract-full').style.display = 'inline'; document.getElementById('1804.06895v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.06895v4-abstract-full" style="display: none;"> Decays of radioisotopes on inner detector surfaces can pose a major background concern for the direct detection of dark matter. While these backgrounds are conventionally mitigated with position cuts, these cuts reduce the exposure of the detector by decreasing the sensitive mass, and uncertainty in position determination may make it impossible to adequately remove such events in certain detectors. In this paper, we provide a new technique for substantially reducing these surface backgrounds in liquid argon (LAr) detectors, independent of position cuts. These detectors typically use a coating of tetraphenyl-butadiene (TPB) on the inner surfaces as a wavelength shifter to convert vacuum ultraviolet (VUV) LAr scintillation light to the visible spectrum. We find that TPB scintillation contains a component with a previously unreported exceptionally long lifetime ($\sim$ms). We discovered that this component differs significantly in magnitude between alpha, beta, and VUV excitation, which enables the use of pulse shape discrimination to suppress surface backgrounds by more than a factor of $10^3$ with negligible loss of dark matter sensitivity. We also discuss how this technique can be extended beyond just LAr experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.06895v4-abstract-full').style.display = 'none'; document.getElementById('1804.06895v4-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 98, 062002 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.01427">arXiv:1802.01427</a> <span> [<a href="https://arxiv.org/pdf/1802.01427">pdf</a>, <a href="https://arxiv.org/format/1802.01427">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.2018.06.077">10.1016/j.nima.2018.06.077 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Electroluminescence pulse shape and electron diffusion in liquid argon measured in a dual-phase TPC </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=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=Alton%2C+A+K">A. K. Alton</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+P">M. P. Ave</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Baldin%2C+B">B. Baldin</a>, <a href="/search/physics?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</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=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a> , et al. (141 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="1802.01427v2-abstract-short" style="display: inline;"> We report the measurement of the longitudinal diffusion constant in liquid argon with the DarkSide-50 dual-phase time projection chamber. The measurement is performed at drift electric fields of 100 V/cm, 150 V/cm, and 200 V/cm using high statistics $^{39}$Ar decays from atmospheric argon. We derive an expression to describe the pulse shape of the electroluminescence signal (S2) in dual-phase TPCs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.01427v2-abstract-full').style.display = 'inline'; document.getElementById('1802.01427v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.01427v2-abstract-full" style="display: none;"> We report the measurement of the longitudinal diffusion constant in liquid argon with the DarkSide-50 dual-phase time projection chamber. The measurement is performed at drift electric fields of 100 V/cm, 150 V/cm, and 200 V/cm using high statistics $^{39}$Ar decays from atmospheric argon. We derive an expression to describe the pulse shape of the electroluminescence signal (S2) in dual-phase TPCs. The derived S2 pulse shape is fit to events from the uppermost portion of the TPC in order to characterize the radial dependence of the signal. The results are provided as inputs to the measurement of the longitudinal diffusion constant DL, which we find to be (4.12 $\pm$ 0.04) cm$^2$/s for a selection of 140keV electron recoil events in 200V/cm drift field and 2.8kV/cm extraction field. To study the systematics of our measurement we examine datasets of varying event energy, field strength, and detector volume yielding a weighted average value for the diffusion constant of (4.09 $\pm$ 0.09) cm$^2$ /s. The measured longitudinal diffusion constant is observed to have an energy dependence, and within the studied energy range the result is systematically lower than other results in the literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.01427v2-abstract-full').style.display = 'none'; document.getElementById('1802.01427v2-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1712.05709">arXiv:1712.05709</a> <span> [<a href="https://arxiv.org/pdf/1712.05709">pdf</a>, <a href="https://arxiv.org/format/1712.05709">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/10.1016/j.nima.2017.12.047">10.1016/j.nima.2017.12.047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Borexino Thermal Monitoring & Management System and simulations of the fluid-dynamics of the Borexino detector under asymmetrical, changing boundary conditions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bravo-Bergu%C3%B1o%2C+D">D. Bravo-Bergu帽o</a>, <a href="/search/physics?searchtype=author&query=Mereu%2C+R">R. Mereu</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">A. Ianni</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/physics?searchtype=author&query=Wright%2C+T">T. Wright</a>, <a href="/search/physics?searchtype=author&query=Yokley%2C+Z">Z. Yokley</a>, <a href="/search/physics?searchtype=author&query=Vogelaar%2C+R+B">R. B. Vogelaar</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Inzoli%2C+F">F. Inzoli</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="1712.05709v1-abstract-short" style="display: inline;"> A comprehensive monitoring system for the thermal environment inside the Borexino neutrino detector was developed and installed in order to reduce uncertainties in determining temperatures throughout the detector. A complementary thermal management system limits undesirable thermal couplings between the environment and Borexino's active sections. This strategy is bringing improved radioactive back… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.05709v1-abstract-full').style.display = 'inline'; document.getElementById('1712.05709v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.05709v1-abstract-full" style="display: none;"> A comprehensive monitoring system for the thermal environment inside the Borexino neutrino detector was developed and installed in order to reduce uncertainties in determining temperatures throughout the detector. A complementary thermal management system limits undesirable thermal couplings between the environment and Borexino's active sections. This strategy is bringing improved radioactive background conditions to the region of interest for the physics signal thanks to reduced fluid mixing induced in the liquid scintillator. Although fluid-dynamical equilibrium has not yet been fully reached, and thermal fine-tuning is possible, the system has proven extremely effective at stabilizing the detector's thermal conditions while offering precise insights into its mechanisms of internal thermal transport. Furthermore, a Computational Fluid-Dynamics analysis has been performed, based on the empirical measurements provided by the thermal monitoring system, and providing information into present and future thermal trends. A two-dimensional modeling approach was implemented in order to achieve a proper understanding of the thermal and fluid-dynamics in Borexino. It was optimized for different regions and periods of interest, focusing on the most critical effects that were identified as influencing background concentrations. Literature experimental case studies were reproduced to benchmark the method and settings, and a Borexino-specific benchmark was implemented in order to validate the modeling approach for thermal transport. Finally, fully-convective models were applied to understand general and specific fluid motions impacting the detector's Active Volume. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.05709v1-abstract-full').style.display = 'none'; document.getElementById('1712.05709v1-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">originally announced</span> December 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">arXiv admin note: substantial text overlap with arXiv:1705.09078, arXiv:1705.09658</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.09889">arXiv:1707.09889</a> <span> [<a href="https://arxiv.org/pdf/1707.09889">pdf</a>, <a href="https://arxiv.org/format/1707.09889">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/10.1088/1748-0221/12/12/P12011">10.1088/1748-0221/12/12/P12011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Electronics, Trigger and Data Acquisition System for the Liquid Argon Time Projection Chamber of the DarkSide-50 Search for Dark Matter </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=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=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Arisaka%2C+K">K. Arisaka</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=Baldin%2C+B">B. Baldin</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</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=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Brodsky%2C+J">J. Brodsky</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a> , et al. (155 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="1707.09889v2-abstract-short" style="display: inline;"> The DarkSide-50 experiment at the Laboratori Nazionali del Gran Sasso is a search for dark matter using a dual phase time projection chamber with 50 kg of low radioactivity argon as target. Light signals from interactions in the argon are detected by a system of 38 photo-multiplier tubes (PMTs), 19 above and 19 below the TPC volume inside the argon cryostat. We describe the electronics which proce… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09889v2-abstract-full').style.display = 'inline'; document.getElementById('1707.09889v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.09889v2-abstract-full" style="display: none;"> The DarkSide-50 experiment at the Laboratori Nazionali del Gran Sasso is a search for dark matter using a dual phase time projection chamber with 50 kg of low radioactivity argon as target. Light signals from interactions in the argon are detected by a system of 38 photo-multiplier tubes (PMTs), 19 above and 19 below the TPC volume inside the argon cryostat. We describe the electronics which processes the signals from the photo-multipliers, the trigger system which identifies events of interest, and the data-acquisition system which records the data for further analysis. The electronics include resistive voltage dividers on the PMTs, custom pre-amplifiers mounted directly on the PMT voltage dividers in the liquid argon, and custom amplifier/discriminators (at room temperature). After amplification, the PMT signals are digitized in CAEN waveform digitizers, and CAEN logic modules are used to construct the trigger, the data acquisition system for the TPC is based on the Fermilab "artdaq" software. The system has been in operation since early 2014. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09889v2-abstract-full').style.display = 'none'; document.getElementById('1707.09889v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 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">Comments:</span> <span class="has-text-grey-dark mathjax">24 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/1707.05630">arXiv:1707.05630</a> <span> [<a href="https://arxiv.org/pdf/1707.05630">pdf</a>, <a href="https://arxiv.org/format/1707.05630">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/10.1088/1748-0221/12/10/P10015">10.1088/1748-0221/12/10/P10015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simulation of argon response and light detection in the DarkSide-50 dual phase TPC </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=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=Alton%2C+A+K">A. K. Alton</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=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</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=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Catalanotti%2C+S">S. Catalanotti</a>, <a href="/search/physics?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a> , et al. (125 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="1707.05630v3-abstract-short" style="display: inline;"> A Geant4-based Monte Carlo package named G4DS has been developed to simulate the response of DarkSide-50, an experiment operating since 2013 at LNGS, designed to detect WIMP interactions in liquid argon. In the process of WIMP searches, DarkSide-50 has achieved two fundamental milestones: the rejection of electron recoil background with a power of ~10^7, using the pulse shape discrimination techni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.05630v3-abstract-full').style.display = 'inline'; document.getElementById('1707.05630v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.05630v3-abstract-full" style="display: none;"> A Geant4-based Monte Carlo package named G4DS has been developed to simulate the response of DarkSide-50, an experiment operating since 2013 at LNGS, designed to detect WIMP interactions in liquid argon. In the process of WIMP searches, DarkSide-50 has achieved two fundamental milestones: the rejection of electron recoil background with a power of ~10^7, using the pulse shape discrimination technique, and the measurement of the residual 39Ar contamination in underground argon, ~3 orders of magnitude lower with respect to atmospheric argon. These results rely on the accurate simulation of the detector response to the liquid argon scintillation, its ionization, and electron-ion recombination processes. This work provides a complete overview of the DarkSide Monte Carlo and of its performance, with a particular focus on PARIS, the custom-made liquid argon response model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.05630v3-abstract-full').style.display = 'none'; document.getElementById('1707.05630v3-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 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 23 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.09078">arXiv:1705.09078</a> <span> [<a href="https://arxiv.org/pdf/1705.09078">pdf</a>, <a href="https://arxiv.org/format/1705.09078">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> The Borexino Thermal Monitoring and Management System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bravo-Bergu%C3%B1o%2C+D">David Bravo-Bergu帽o</a>, <a href="/search/physics?searchtype=author&query=Mereu%2C+R">Riccardo Mereu</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">Paolo Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">Marco Carlini</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Andrea Ianni</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">Augusto Goretti</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">Federico Gabriele</a>, <a href="/search/physics?searchtype=author&query=Wright%2C+T">Tristan Wright</a>, <a href="/search/physics?searchtype=author&query=Yokley%2C+Z">Zachary Yokley</a>, <a href="/search/physics?searchtype=author&query=Vogelaar%2C+R+B">Robert Bruce Vogelaar</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">Frank Calaprice</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="1705.09078v3-abstract-short" style="display: inline;"> A monitoring and management system for the thermal environment inside the Borexino neutrino detector was developed and installed in order to reduce uncertainties in temperature determination and limit undesirable thermal couplings between the environment and Borexino's active sections. This strategy is bringing improved radioactive background conditions to the physics signal thanks to the reduced… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.09078v3-abstract-full').style.display = 'inline'; document.getElementById('1705.09078v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.09078v3-abstract-full" style="display: none;"> A monitoring and management system for the thermal environment inside the Borexino neutrino detector was developed and installed in order to reduce uncertainties in temperature determination and limit undesirable thermal couplings between the environment and Borexino's active sections. This strategy is bringing improved radioactive background conditions to the physics signal thanks to the reduced mixing taking place in the liquid scintillator. While equilibrium has not yet been reached, and fine-tuning is possible, the system has proven extremely effective at greatly stabilizing the detector while offering precise insight into its internal thermal conditions and transport. Numerical simulations have also been used to feed this empirical data into a global model, providing information into present and future thermal trends. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.09078v3-abstract-full').style.display = 'none'; document.getElementById('1705.09078v3-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 8 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/1704.02291">arXiv:1704.02291</a> <span> [<a href="https://arxiv.org/pdf/1704.02291">pdf</a>, <a href="https://arxiv.org/format/1704.02291">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/10.1016/j.astropartphys.2017.10.003">10.1016/j.astropartphys.2017.10.003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Monte Carlo simulation of the Borexino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Borodikhina%2C+L">L. Borodikhina</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a> , et al. (75 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="1704.02291v1-abstract-short" style="display: inline;"> We describe the Monte Carlo (MC) simulation package of the Borexino detector and discuss the agreement of its output with data. The Borexino MC 'ab initio' simulates the energy loss of particles in all detector components and generates the resulting scintillation photons and their propagation within the liquid scintillator volume. The simulation accounts for absorption, reemission, and scattering… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.02291v1-abstract-full').style.display = 'inline'; document.getElementById('1704.02291v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.02291v1-abstract-full" style="display: none;"> We describe the Monte Carlo (MC) simulation package of the Borexino detector and discuss the agreement of its output with data. The Borexino MC 'ab initio' simulates the energy loss of particles in all detector components and generates the resulting scintillation photons and their propagation within the liquid scintillator volume. The simulation accounts for absorption, reemission, and scattering of the optical photons and tracks them until they either are absorbed or reach the photocathode of one of the photomultiplier tubes. Photon detection is followed by a comprehensive simulation of the readout electronics response. The algorithm proceeds with a detailed simulation of the electronics chain. The MC is tuned using data collected with radioactive calibration sources deployed inside and around the scintillator volume. The simulation reproduces the energy response of the detector, its uniformity within the fiducial scintillator volume relevant to neutrino physics, and the time distribution of detected photons to better than 1% between 100 keV and several MeV. The techniques developed to simulate the Borexino detector and their level of refinement are of possible interest to the neutrino community, especially for current and future large-volume liquid scintillator experiments such as Kamland-Zen, SNO+, and Juno. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.02291v1-abstract-full').style.display = 'none'; document.getElementById('1704.02291v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.07214">arXiv:1703.07214</a> <span> [<a href="https://arxiv.org/pdf/1703.07214">pdf</a>, <a href="https://arxiv.org/format/1703.07214">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-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/10.1088/1748-0221/12/08/P08002">10.1088/1748-0221/12/08/P08002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Quenching Measurements and Modeling of a Boron-Loaded Organic Liquid Scintillator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Westerdale%2C+S">Shawn Westerdale</a>, <a href="/search/physics?searchtype=author&query=Xu%2C+J">Jingke Xu</a>, <a href="/search/physics?searchtype=author&query=Shields%2C+E">Emily Shields</a>, <a href="/search/physics?searchtype=author&query=Froborg%2C+F">Francis Froborg</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">Frank Calaprice</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">Thomas Alexander</a>, <a href="/search/physics?searchtype=author&query=Aprahamian%2C+A">Ani Aprahamian</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">Henning O. Back</a>, <a href="/search/physics?searchtype=author&query=Casarella%2C+C">Clark Casarella</a>, <a href="/search/physics?searchtype=author&query=Fang%2C+X">Xiao Fang</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+Y+K">Yogesh K. Gupta</a>, <a href="/search/physics?searchtype=author&query=Lamere%2C+E">Edward Lamere</a>, <a href="/search/physics?searchtype=author&query=Liu%2C+Q">Qian Liu</a>, <a href="/search/physics?searchtype=author&query=Lyons%2C+S">Stephanie Lyons</a>, <a href="/search/physics?searchtype=author&query=Smith%2C+M">Mallory Smith</a>, <a href="/search/physics?searchtype=author&query=Tan%2C+W">Wanpeng Tan</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="1703.07214v5-abstract-short" style="display: inline;"> Organic liquid scintillators are used in a wide variety of applications in experimental nuclear and particle physics. Boron-loaded scintillators are particularly useful for detecting neutron captures, due to the high thermal neutron capture cross section of $^{10}$B. These scintillators are commonly used in neutron detectors, including the DarkSide-50 neutron veto, where the neutron may produce a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.07214v5-abstract-full').style.display = 'inline'; document.getElementById('1703.07214v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.07214v5-abstract-full" style="display: none;"> Organic liquid scintillators are used in a wide variety of applications in experimental nuclear and particle physics. Boron-loaded scintillators are particularly useful for detecting neutron captures, due to the high thermal neutron capture cross section of $^{10}$B. These scintillators are commonly used in neutron detectors, including the DarkSide-50 neutron veto, where the neutron may produce a signal when it scatters off protons in the scintillator or when it captures on $^{10}$B. Reconstructing the energy of these recoils is complicated by scintillation quenching. Understanding how nuclear recoils are quenched in these scintillators is an important and difficult problem. In this article, we present a set of measurements of neutron-induced proton recoils in a boron-loaded organic liquid scintillator at recoil energies ranging from 57--467 keV, and we compare these measurements to predictions from different quenching models. We find that a modified Birks' model whose denominator is quadratic in $dE/dx$ best describes the measurements, with $蠂^2$/NDF$=1.6$. This result will help model nuclear recoil scintillation in similar detectors and can be used to improve their neutron tagging efficiency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.07214v5-abstract-full').style.display = 'none'; document.getElementById('1703.07214v5-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.07970">arXiv:1701.07970</a> <span> [<a href="https://arxiv.org/pdf/1701.07970">pdf</a>, <a href="https://arxiv.org/format/1701.07970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2017.04.004">10.1016/j.astropartphys.2017.04.004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Seasonal Modulation of the $^7$Be Solar Neutrino Rate in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Borodikhina%2C+L">L. Borodikhina</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a> , et al. (77 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="1701.07970v2-abstract-short" style="display: inline;"> We detected the seasonal modulation of the $^7$Be neutrino interaction rate with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. The period, amplitude, and phase of the observed time evolution of the signal are consistent with its solar origin, and the absence of an annual modulation is rejected at 99.99\% C.L. The data are analyzed using three methods: the sinusoidal fi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.07970v2-abstract-full').style.display = 'inline'; document.getElementById('1701.07970v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.07970v2-abstract-full" style="display: none;"> We detected the seasonal modulation of the $^7$Be neutrino interaction rate with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. The period, amplitude, and phase of the observed time evolution of the signal are consistent with its solar origin, and the absence of an annual modulation is rejected at 99.99\% C.L. The data are analyzed using three methods: the sinusoidal fit, the Lomb-Scargle and the Empirical Mode Decomposition techniques, which all yield results in excellent agreement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.07970v2-abstract-full').style.display = 'none'; document.getElementById('1701.07970v2-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 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">11 palese, 13 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/1611.02750">arXiv:1611.02750</a> <span> [<a href="https://arxiv.org/pdf/1611.02750">pdf</a>, <a href="https://arxiv.org/format/1611.02750">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/10.1088/1748-0221/12/12/T12004">10.1088/1748-0221/12/12/T12004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CALIS - a CALibration Insertion System for the DarkSide-50 dark matter search experiment </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=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=Alton%2C+A+K">A. K. Alton</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=Baldin%2C+B">B. Baldin</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</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=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Brodsky%2C+J">J. Brodsky</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a> , et al. (140 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="1611.02750v4-abstract-short" style="display: inline;"> This paper describes the design, fabrication, commissioning and use of a CALibration source Insertion System (CALIS) in the DarkSide-50 direct dark matter search experiment. CALIS deploys radioactive sources into the liquid scintillator veto to characterize the detector response and detection efficiency of the DarkSide-50 Liquid Argon Time Projection Chamber, and the surrounding 30 t organic liqui… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.02750v4-abstract-full').style.display = 'inline'; document.getElementById('1611.02750v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.02750v4-abstract-full" style="display: none;"> This paper describes the design, fabrication, commissioning and use of a CALibration source Insertion System (CALIS) in the DarkSide-50 direct dark matter search experiment. CALIS deploys radioactive sources into the liquid scintillator veto to characterize the detector response and detection efficiency of the DarkSide-50 Liquid Argon Time Projection Chamber, and the surrounding 30 t organic liquid scintillator neutron veto. It was commissioned in September 2014 and has been used successfully in several gamma and neutron source campaigns since then. A description of the hardware and an excerpt of calibration analysis results are given below. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.02750v4-abstract-full').style.display = 'none'; document.getElementById('1611.02750v4-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 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">21 pages, 11 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/1611.00241">arXiv:1611.00241</a> <span> [<a href="https://arxiv.org/pdf/1611.00241">pdf</a>, <a href="https://arxiv.org/format/1611.00241">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="Nuclear Experiment">nucl-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/10.1088/1748-0221/12/01/P01021">10.1088/1748-0221/12/01/P01021 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Effect of Low Electric Fields on Alpha Scintillation Light Yield in Liquid Argon </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=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=Alton%2C+A+K">A. K. Alton</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=Baldin%2C+B">B. Baldin</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bocci%2C+V">V. Bocci</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=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Brodsky%2C+J">J. Brodsky</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a> , et al. (136 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="1611.00241v2-abstract-short" style="display: inline;"> Measurements were made of scintillation light yield of alpha particles from the $^{222}$Rn decay chain within the DarkSide-50 liquid argon time projection chamber. The light yield was found to increase as the applied electric field increased, with alphas in a 200 V/cm electric field exhibiting a 2% increase in light yield compared to alphas in no field. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.00241v2-abstract-full" style="display: none;"> Measurements were made of scintillation light yield of alpha particles from the $^{222}$Rn decay chain within the DarkSide-50 liquid argon time projection chamber. The light yield was found to increase as the applied electric field increased, with alphas in a 200 V/cm electric field exhibiting a 2% increase in light yield compared to alphas in no field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00241v2-abstract-full').style.display = 'none'; document.getElementById('1611.00241v2-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 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">5 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> P. Agnes et al 2017 JINST 12 P01021 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.07089">arXiv:1609.07089</a> <span> [<a href="https://arxiv.org/pdf/1609.07089">pdf</a>, <a href="https://arxiv.org/format/1609.07089">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/10.1103/PhysRevD.96.061101">10.1103/PhysRevD.96.061101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First measurement of surface nuclear recoil background for argon dark matter searches </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Xu%2C+J">Jingke Xu</a>, <a href="/search/physics?searchtype=author&query=Stanford%2C+C">Chris Stanford</a>, <a href="/search/physics?searchtype=author&query=Westerdale%2C+S">Shawn Westerdale</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">Frank Calaprice</a>, <a href="/search/physics?searchtype=author&query=Wright%2C+A">Alexander Wright</a>, <a href="/search/physics?searchtype=author&query=Shi%2C+Z">Zhiming Shi</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="1609.07089v1-abstract-short" style="display: inline;"> One major background in direct searches for weakly interacting massive particles (WIMPs) comes from the deposition of radon progeny on detector surfaces. The most dangerous surface background is the $^{206}$Pb recoils produced by $^{210}$Po decays. In this letter, we report the first characterization of this background in liquid argon. The scintillation signal of low energy Pb recoils is measured… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.07089v1-abstract-full').style.display = 'inline'; document.getElementById('1609.07089v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.07089v1-abstract-full" style="display: none;"> One major background in direct searches for weakly interacting massive particles (WIMPs) comes from the deposition of radon progeny on detector surfaces. The most dangerous surface background is the $^{206}$Pb recoils produced by $^{210}$Po decays. In this letter, we report the first characterization of this background in liquid argon. The scintillation signal of low energy Pb recoils is measured to be highly quenched in argon, and we estimate that the 103keV $^{206}$Pb recoil background will produce a signal equal to that of a ~5keV (30keV) electron recoil ($^{40}$Ar recoil). In addition, we demonstrate that this dangerous $^{210}$Po surface background can be suppressed by a factor of ~100 or higher using pulse shape discrimination methods, which can make argon dark matter detectors near background-free and enhance their potential for discovery of medium- and high-mass WIMPs. We also discuss the impact on other low background experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.07089v1-abstract-full').style.display = 'none'; document.getElementById('1609.07089v1-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 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">4 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LLNL-JRNL-703423-DRAFT </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 96, 061101 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.03316">arXiv:1606.03316</a> <span> [<a href="https://arxiv.org/pdf/1606.03316">pdf</a>, <a href="https://arxiv.org/format/1606.03316">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/10.1088/1748-0221/11/12/P12007">10.1088/1748-0221/11/12/P12007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Electronics and Data Acquisition System for the DarkSide-50 Veto Detectors </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=Agostino%2C+L">L. Agostino</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=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Arisaka%2C+K">K. Arisaka</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Baldin%2C+B">B. Baldin</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</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=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Brodsky%2C+J">J. Brodsky</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Cao%2C+H">H. Cao</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Catalanotti%2C+S">S. Catalanotti</a> , et al. (133 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="1606.03316v1-abstract-short" style="display: inline;"> DarkSide-50 is a detector for dark matter candidates in the form of weakly interacting massive particles (WIMPs). It utilizes a liquid argon time projection chamber (LAr TPC) for the inner main detector. The TPC is surrounded by a liquid scintillator veto (LSV) and a water Cherenkov veto detector (WCV). The LSV and WCV, both instrumented with PMTs, act as the neutron and cosmogenic muon veto detec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.03316v1-abstract-full').style.display = 'inline'; document.getElementById('1606.03316v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.03316v1-abstract-full" style="display: none;"> DarkSide-50 is a detector for dark matter candidates in the form of weakly interacting massive particles (WIMPs). It utilizes a liquid argon time projection chamber (LAr TPC) for the inner main detector. The TPC is surrounded by a liquid scintillator veto (LSV) and a water Cherenkov veto detector (WCV). The LSV and WCV, both instrumented with PMTs, act as the neutron and cosmogenic muon veto detectors for DarkSide-50. This paper describes the electronics and data acquisition system used for these two detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.03316v1-abstract-full').style.display = 'none'; document.getElementById('1606.03316v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation, 11 (2016): P12007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.06795">arXiv:1605.06795</a> <span> [<a href="https://arxiv.org/pdf/1605.06795">pdf</a>, <a href="https://arxiv.org/format/1605.06795">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> The Main Results of the Borexino Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Muratova%2C+V">V. Muratova</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a> , et al. (74 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="1605.06795v1-abstract-short" style="display: inline;"> The main physical results on the registration of solar neutrinos and the search for rare processes obtained by the Borexino collaboration to date are presented. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.06795v1-abstract-full" style="display: none;"> The main physical results on the registration of solar neutrinos and the search for rare processes obtained by the Borexino collaboration to date are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.06795v1-abstract-full').style.display = 'none'; document.getElementById('1605.06795v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">8 pages, 8 figgures, To be published as Proceedings of the Third Annual Large Hadron Collider Physics Conference, St. Petersburg, Russia, 2015</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.07896">arXiv:1512.07896</a> <span> [<a href="https://arxiv.org/pdf/1512.07896">pdf</a>, <a href="https://arxiv.org/format/1512.07896">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/10.1088/1748-0221/11/03/P03016">10.1088/1748-0221/11/03/P03016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The veto system of the DarkSide-50 experiment </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=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Agostino%2C+L">L. Agostino</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=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Arisaka%2C+K">K. Arisaka</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Baldin%2C+B">B. Baldin</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</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=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Brodsky%2C+J">J. Brodsky</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Cao%2C+H">H. Cao</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a> , et al. (136 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="1512.07896v1-abstract-short" style="display: inline;"> Nuclear recoil events produced by neutron scatters form one of the most important classes of background in WIMP direct detection experiments, as they may produce nuclear recoils that look exactly like WIMP interactions. In DarkSide-50, we both actively suppress and measure the rate of neutron-induced background events using our neutron veto, composed of a boron-loaded liquid scintillator detector… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.07896v1-abstract-full').style.display = 'inline'; document.getElementById('1512.07896v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.07896v1-abstract-full" style="display: none;"> Nuclear recoil events produced by neutron scatters form one of the most important classes of background in WIMP direct detection experiments, as they may produce nuclear recoils that look exactly like WIMP interactions. In DarkSide-50, we both actively suppress and measure the rate of neutron-induced background events using our neutron veto, composed of a boron-loaded liquid scintillator detector within a water Cherenkov detector. This paper is devoted to the description of the neutron veto system of DarkSide-50, including the detector structure, the fundamentals of event reconstruction and data analysis, and basic performance parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.07896v1-abstract-full').style.display = 'none'; document.getElementById('1512.07896v1-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 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation, 11 (2016): P03016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.00702">arXiv:1510.00702</a> <span> [<a href="https://arxiv.org/pdf/1510.00702">pdf</a>, <a href="https://arxiv.org/format/1510.00702">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1103/PhysRevD.93.081101">10.1103/PhysRevD.93.081101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Results from the first use of low radioactivity argon in a dark matter search </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=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Agostino%2C+L">L. Agostino</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=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/physics?searchtype=author&query=Arisaka%2C+K">K. Arisaka</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Baldin%2C+B">B. Baldin</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</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=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Brodsky%2C+J">J. Brodsky</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/physics?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Cao%2C+H">H. Cao</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a> , et al. (136 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="1510.00702v3-abstract-short" style="display: inline;"> Liquid argon is a bright scintillator with potent particle identification properties, making it an attractive target for direct-detection dark matter searches. The DarkSide-50 dark matter search here reports the first WIMP search results obtained using a target of low-radioactivity argon. DarkSide-50 is a dark matter detector, using two-phase liquid argon time projection chamber, located at the La… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.00702v3-abstract-full').style.display = 'inline'; document.getElementById('1510.00702v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.00702v3-abstract-full" style="display: none;"> Liquid argon is a bright scintillator with potent particle identification properties, making it an attractive target for direct-detection dark matter searches. The DarkSide-50 dark matter search here reports the first WIMP search results obtained using a target of low-radioactivity argon. DarkSide-50 is a dark matter detector, using two-phase liquid argon time projection chamber, located at the Laboratori Nazionali del Gran Sasso. The underground argon is shown to contain Ar-39 at a level reduced by a factor (1.4 +- 0.2) x 10^3 relative to atmospheric argon. We report a background-free null result from (2616 +- 43) kg d of data, accumulated over 70.9 live-days. When combined with our previous search using an atmospheric argon, the 90 % C.L. upper limit on the WIMP-nucleon spin-independent cross section based on zero events found in the WIMP search regions, is 2.0 x 10^-44 cm^2 (8.6 x 10^-44 cm^2, 8.0 x 10^-43 cm^2) for a WIMP mass of 100 GeV/c^2 (1 TeV/c^2 , 10 TeV/c^2). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.00702v3-abstract-full').style.display = 'none'; document.getElementById('1510.00702v3-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 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Accepted by Phys. Rev. D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 93, 081101 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.02782">arXiv:1509.02782</a> <span> [<a href="https://arxiv.org/pdf/1509.02782">pdf</a>, <a href="https://arxiv.org/format/1509.02782">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/10.1016/j.astropartphys.2016.01.005">10.1016/j.astropartphys.2016.01.005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Prototype Neutron Veto for Dark Matter Detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Westerdale%2C+S">Shawn Westerdale</a>, <a href="/search/physics?searchtype=author&query=Shields%2C+E">Emily Shields</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">Frank Calaprice</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="1509.02782v3-abstract-short" style="display: inline;"> Neutrons are a particularly dangerous background for direct WIMP dark matter searches; their nuclear recoils with the target nucleus are often indistinguishable from nuclear recoils produced by WIMP-nuclear collisions. In this study, we explore the concept of a liquid scintillator neutron veto detector that would allow direct dark matter detectors to potentially reject neutrons with greater than 9… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02782v3-abstract-full').style.display = 'inline'; document.getElementById('1509.02782v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.02782v3-abstract-full" style="display: none;"> Neutrons are a particularly dangerous background for direct WIMP dark matter searches; their nuclear recoils with the target nucleus are often indistinguishable from nuclear recoils produced by WIMP-nuclear collisions. In this study, we explore the concept of a liquid scintillator neutron veto detector that would allow direct dark matter detectors to potentially reject neutrons with greater than 99% efficiency. Here we outline the construction and testing of a small prototype detector and the potential implications of this technology for future dark matter detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02782v3-abstract-full').style.display = 'none'; document.getElementById('1509.02782v3-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 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.01223">arXiv:1509.01223</a> <span> [<a href="https://arxiv.org/pdf/1509.01223">pdf</a>, <a href="https://arxiv.org/ps/1509.01223">ps</a>, <a href="https://arxiv.org/format/1509.01223">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.115.231802">10.1103/PhysRevLett.115.231802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A test of electric charge conservation with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Borexino+Collaboration"> Borexino Collaboration</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a> , et al. (73 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="1509.01223v2-abstract-short" style="display: inline;"> Borexino is a liquid scintillation detector located deep underground at the Laboratori Nazionali del Gran Sasso (LNGS, Italy). Thanks to the unmatched radio-purity of the scintillator, and to the well understood detector response at low energy, a new limit on the stability of the electron for decay into a neutrino and a single mono-energetic photon was obtained. This new bound, tau > 6.6 10**28 yr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.01223v2-abstract-full').style.display = 'inline'; document.getElementById('1509.01223v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.01223v2-abstract-full" style="display: none;"> Borexino is a liquid scintillation detector located deep underground at the Laboratori Nazionali del Gran Sasso (LNGS, Italy). Thanks to the unmatched radio-purity of the scintillator, and to the well understood detector response at low energy, a new limit on the stability of the electron for decay into a neutrino and a single mono-energetic photon was obtained. This new bound, tau > 6.6 10**28 yr at 90 % C.L., is two orders of magnitude better than the previous limit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.01223v2-abstract-full').style.display = 'none'; document.getElementById('1509.01223v2-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">5 pages, 1 figure</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 115, 231802 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.05379">arXiv:1508.05379</a> <span> [<a href="https://arxiv.org/pdf/1508.05379">pdf</a>, <a href="https://arxiv.org/format/1508.05379">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div 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.nuclphysbps.2015.06.023">10.1016/j.nuclphysbps.2015.06.023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-energy (anti)neutrino physics with Borexino: Neutrinos from the primary proton-proton fusion process in the Sun </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Mosteiro%2C+P">P. Mosteiro</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a> , et al. (66 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1508.05379v1-abstract-short" style="display: inline;"> The Sun is fueled by a series of nuclear reactions that produce the energy that makes it shine. The primary reaction is the fusion of two protons into a deuteron, a positron and a neutrino. These neutrinos constitute the vast majority of neutrinos reaching Earth, providing us with key information about what goes on at the core of our star. Several experiments have now confirmed the observation of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.05379v1-abstract-full').style.display = 'inline'; document.getElementById('1508.05379v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.05379v1-abstract-full" style="display: none;"> The Sun is fueled by a series of nuclear reactions that produce the energy that makes it shine. The primary reaction is the fusion of two protons into a deuteron, a positron and a neutrino. These neutrinos constitute the vast majority of neutrinos reaching Earth, providing us with key information about what goes on at the core of our star. Several experiments have now confirmed the observation of neutrino oscillations by detecting neutrinos from secondary nuclear processes in the Sun; this is the first direct spectral measurement of the neutrinos from the keystone proton-proton fusion. This observation is a crucial step towards the completion of the spectroscopy of pp-chain neutrinos, as well as further validation of the LMA-MSW model of neutrino oscillations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.05379v1-abstract-full').style.display = 'none'; document.getElementById('1508.05379v1-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 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Proceedings from NOW (Neutrino Oscillation Workshop) 2014</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear and Particle Physics Proceedings 265-266 (2015) 87-92 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.02432">arXiv:1507.02432</a> <span> [<a href="https://arxiv.org/pdf/1507.02432">pdf</a>, <a href="https://arxiv.org/ps/1507.02432">ps</a>, <a href="https://arxiv.org/format/1507.02432">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div 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/10.1134/S106377961606023X">10.1134/S106377961606023X <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of neutrino flux from the primary proton--proton fusion process in the Sun with Borexino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Smirnov%2C+O+Y">O. Y. Smirnov</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a> , et al. (72 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="1507.02432v1-abstract-short" style="display: inline;"> Neutrino produced in a chain of nuclear reactions in the Sun starting from the fusion of two protons, for the first time has been detected in a real-time detector in spectrometric mode. The unique properties of the Borexino detector provided an oppurtunity to disentangle pp-neutrino spectrum from the background components. A comparison of the total neutrino flux from the Sun with Solar luminosity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.02432v1-abstract-full').style.display = 'inline'; document.getElementById('1507.02432v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.02432v1-abstract-full" style="display: none;"> Neutrino produced in a chain of nuclear reactions in the Sun starting from the fusion of two protons, for the first time has been detected in a real-time detector in spectrometric mode. The unique properties of the Borexino detector provided an oppurtunity to disentangle pp-neutrino spectrum from the background components. A comparison of the total neutrino flux from the Sun with Solar luminosity in photons provides a test of the stability of the Sun on the 10$^{5}$ years time scale, and sets a strong limit on the power production in the unknown energy sources in the Sun of no more than 4\% of the total energy production at 90\% C.L. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.02432v1-abstract-full').style.display = 'none'; document.getElementById('1507.02432v1-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 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">15 pages, 2 tables, 3 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/1506.04610">arXiv:1506.04610</a> <span> [<a href="https://arxiv.org/pdf/1506.04610">pdf</a>, <a href="https://arxiv.org/format/1506.04610">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.92.031101">10.1103/PhysRevD.92.031101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopy of geo-neutrinos from 2056 days of Borexino data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Borexino+collaboration"> Borexino collaboration</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=DAngelo%2C+D">D. DAngelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fiorentini%2C+G">G. Fiorentini</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a> , et al. (77 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="1506.04610v2-abstract-short" style="display: inline;"> We report an improved geo-neutrino measurement with Borexino from 2056 days of data taking. The present exposure is $(5.5\pm0.3)\times10^{31}$ proton$\times$yr. Assuming a chondritic Th/U mass ratio of 3.9, we obtain $23.7 ^{+6.5}_{-5.7} (stat) ^{+0.9}_{-0.6} (sys)$ geo-neutrino events. The null observation of geo-neutrinos with Borexino alone has a probability of $3.6 \times 10^{-9}$ (5.9$蟽$). A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.04610v2-abstract-full').style.display = 'inline'; document.getElementById('1506.04610v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.04610v2-abstract-full" style="display: none;"> We report an improved geo-neutrino measurement with Borexino from 2056 days of data taking. The present exposure is $(5.5\pm0.3)\times10^{31}$ proton$\times$yr. Assuming a chondritic Th/U mass ratio of 3.9, we obtain $23.7 ^{+6.5}_{-5.7} (stat) ^{+0.9}_{-0.6} (sys)$ geo-neutrino events. The null observation of geo-neutrinos with Borexino alone has a probability of $3.6 \times 10^{-9}$ (5.9$蟽$). A geo-neutrino signal from the mantle is obtained at 98\% C.L. The radiogenic heat production for U and Th from the present best-fit result is restricted to the range 23-36 TW, taking into account the uncertainty on the distribution of heat producing elements inside the Earth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.04610v2-abstract-full').style.display = 'none'; document.getElementById('1506.04610v2-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 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">4 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 92, 031101 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.07212">arXiv:1503.07212</a> <span> [<a href="https://arxiv.org/pdf/1503.07212">pdf</a>, <a href="https://arxiv.org/format/1503.07212">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/10.1103/PhysRevC.92.015807">10.1103/PhysRevC.92.015807 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Scintillation efficiency measurement of Na recoils in NaI(Tl) below the DAMA/LIBRA energy threshold </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Xu%2C+J">Jingke Xu</a>, <a href="/search/physics?searchtype=author&query=Shields%2C+E">Emily Shields</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">Frank Calaprice</a>, <a href="/search/physics?searchtype=author&query=Westerdale%2C+S">Shawn Westerdale</a>, <a href="/search/physics?searchtype=author&query=Froborg%2C+F">Francis Froborg</a>, <a href="/search/physics?searchtype=author&query=Suerfu%2C+B">Burkhant Suerfu</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">Thomas Alexander</a>, <a href="/search/physics?searchtype=author&query=Aprahamian%2C+A">Ani Aprahamian</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">Henning O. Back</a>, <a href="/search/physics?searchtype=author&query=Casarella%2C+C">Clark Casarella</a>, <a href="/search/physics?searchtype=author&query=Fang%2C+X">Xiao Fang</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+Y+K">Yogesh K. Gupta</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/physics?searchtype=author&query=Lamere%2C+E">Edward Lamere</a>, <a href="/search/physics?searchtype=author&query=Lippincott%2C+W+H">W. Hugh Lippincott</a>, <a href="/search/physics?searchtype=author&query=Liu%2C+Q">Qian Liu</a>, <a href="/search/physics?searchtype=author&query=Lyons%2C+S">Stephanie Lyons</a>, <a href="/search/physics?searchtype=author&query=Siegl%2C+K">Kevin Siegl</a>, <a href="/search/physics?searchtype=author&query=Smith%2C+M">Mallory Smith</a>, <a href="/search/physics?searchtype=author&query=Tan%2C+W">Wanpeng Tan</a>, <a href="/search/physics?searchtype=author&query=Kolk%2C+B+V">Bryant Vande Kolk</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="1503.07212v1-abstract-short" style="display: inline;"> The dark matter interpretation of the DAMA modulation signal depends on the NaI(Tl) scintillation efficiency of nuclear recoils. Previous measurements for Na recoils have large discrepancies, especially in the DAMA/LIBRA modulation energy region. We report a quenching effect measurement of Na recoils in NaI(Tl) from 3keV$_{\text{nr}}$ to 52keV$_{\text{nr}}$, covering the whole DAMA/LIBRA energy re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.07212v1-abstract-full').style.display = 'inline'; document.getElementById('1503.07212v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.07212v1-abstract-full" style="display: none;"> The dark matter interpretation of the DAMA modulation signal depends on the NaI(Tl) scintillation efficiency of nuclear recoils. Previous measurements for Na recoils have large discrepancies, especially in the DAMA/LIBRA modulation energy region. We report a quenching effect measurement of Na recoils in NaI(Tl) from 3keV$_{\text{nr}}$ to 52keV$_{\text{nr}}$, covering the whole DAMA/LIBRA energy region for light WIMP interpretations. By using a low-energy, pulsed neutron beam, a double time-of-flight technique, and pulse-shape discrimination methods, we obtained the most accurate measurement of this kind for NaI(Tl) to date. The results differ significantly from the DAMA reported values at low energies, but fall between the other previous measurements. We present the implications of the new quenching results for the dark matter interpretation of the DAMA modulation signal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.07212v1-abstract-full').style.display = 'none'; document.getElementById('1503.07212v1-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 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">Journal ref:</span> Phys. Rev. C 92, 015807 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.2969">arXiv:1412.2969</a> <span> [<a href="https://arxiv.org/pdf/1412.2969">pdf</a>, <a href="https://arxiv.org/ps/1412.2969">ps</a>, <a href="https://arxiv.org/format/1412.2969">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> <p class="title is-5 mathjax"> The Electronics and Data Acquisition System of the DarkSide Dark Matter Search </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=Agnes%2C+P">P. Agnes</a>, <a href="/search/physics?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/physics?searchtype=author&query=Alton%2C+A">A. Alton</a>, <a href="/search/physics?searchtype=author&query=Arisaka%2C+K">K. Arisaka</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/physics?searchtype=author&query=Baldin%2C+B">B. Baldin</a>, <a href="/search/physics?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bossa%2C+M">M. Bossa</a>, <a href="/search/physics?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Brodsky%2C+J">J. Brodsky</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+F">F. Budano</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/physics?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/physics?searchtype=author&query=Cao%2C+H">H. Cao</a>, <a href="/search/physics?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Cocco%2C+A+G">A. G. Cocco</a>, <a href="/search/physics?searchtype=author&query=Crippa%2C+L">L. Crippa</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a> , et al. (121 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="1412.2969v2-abstract-short" style="display: inline;"> It is generally inferred from astronomical measurements that Dark Matter (DM) comprises approximately 27\% of the energy-density of the universe. If DM is a subatomic particle, a possible candidate is a Weakly Interacting Massive Particle (WIMP), and the DarkSide-50 (DS) experiment is a direct search for evidence of WIMP-nuclear collisions. DS is located underground at the Laboratori Nazionali del… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.2969v2-abstract-full').style.display = 'inline'; document.getElementById('1412.2969v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.2969v2-abstract-full" style="display: none;"> It is generally inferred from astronomical measurements that Dark Matter (DM) comprises approximately 27\% of the energy-density of the universe. If DM is a subatomic particle, a possible candidate is a Weakly Interacting Massive Particle (WIMP), and the DarkSide-50 (DS) experiment is a direct search for evidence of WIMP-nuclear collisions. DS is located underground at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy, and consists of three active, embedded components; an outer water veto (CTF), a liquid scintillator veto (LSV), and a liquid argon (LAr) time projection chamber (TPC). This paper describes the data acquisition and electronic systems of the DS detectors, designed to detect the residual ionization from such collisions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.2969v2-abstract-full').style.display = 'none'; document.getElementById('1412.2969v2-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Calaprice%2C+F&start=50" class="pagination-next" >Next </a> <ul 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