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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Campos%2C+M+D">M. D. Campos</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cargioli%2C+N">N. Cargioli</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacintov%2C+A">A. Di Giacintov</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/hep-ex?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/hep-ex?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/hep-ex?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/hep-ex?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/hep-ex?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/2307.07249">arXiv:2307.07249</a> <span> [<a href="https://arxiv.org/pdf/2307.07249">pdf</a>, <a href="https://arxiv.org/format/2307.07249">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div 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.110.102006">10.1103/PhysRevD.110.102006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter annual modulation with DarkSide-50 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Campos%2C+M+D">M. D. Campos</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cargioli%2C+N">N. Cargioli</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?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="2307.07249v2-abstract-short" style="display: inline;"> Dark matter induced event rate in an Earth-based detector is predicted to show an annual modulation as a result of the Earth's orbital motion around the Sun. We searched for this modulation signature using the ionization signal of the DarkSide-50 liquid argon time projection chamber. No significant signature compatible with dark matter is observed in the electron recoil equivalent energy range abo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.07249v2-abstract-full').style.display = 'inline'; document.getElementById('2307.07249v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.07249v2-abstract-full" style="display: none;"> Dark matter induced event rate in an Earth-based detector is predicted to show an annual modulation as a result of the Earth's orbital motion around the Sun. We searched for this modulation signature using the ionization signal of the DarkSide-50 liquid argon time projection chamber. No significant signature compatible with dark matter is observed in the electron recoil equivalent energy range above $40~{\rm eV_{ee}}$, the lowest threshold ever achieved in such a search. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.07249v2-abstract-full').style.display = 'none'; document.getElementById('2307.07249v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">10 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D110, 102006 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.13876">arXiv:2303.13876</a> <span> [<a href="https://arxiv.org/pdf/2303.13876">pdf</a>, <a href="https://arxiv.org/ps/2303.13876">ps</a>, <a href="https://arxiv.org/format/2303.13876">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div 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/s10052-023-11688-4">10.1140/epjc/s10052-023-11688-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Borexino's search for low-energy neutrinos associated with gravitational wave events from GWTC-3 database </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=BOREXINO+Collaboration"> BOREXINO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Angelo%2C+D+D">D. D' Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/hep-ex?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/hep-ex?searchtype=author&query=Ianni%2C+A">Aldo 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="2303.13876v2-abstract-short" style="display: inline;"> The search for neutrino events in correlation with gravitational wave (GW) events for three observing runs (O1, O2 and O3) from 09/2015 to 03/2020 has been performed using the Borexino data-set of the same period. We have searched for signals of neutrino-electron scattering with visible energies above 250 keV within a time window of 1000 s centered at the detection moment of a particular GW event.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13876v2-abstract-full').style.display = 'inline'; document.getElementById('2303.13876v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.13876v2-abstract-full" style="display: none;"> The search for neutrino events in correlation with gravitational wave (GW) events for three observing runs (O1, O2 and O3) from 09/2015 to 03/2020 has been performed using the Borexino data-set of the same period. We have searched for signals of neutrino-electron scattering with visible energies above 250 keV within a time window of 1000 s centered at the detection moment of a particular GW event. The search was done with three visible energy thresholds of 0.25, 0.8 and 3.0 MeV.Two types of incoming neutrino spectra were considered: the mono-energetic line and the spectrum expected from supernovae. The same spectra were considered for electron antineutrinos detected through inverse beta-decay (IBD) reaction. GW candidates originated by merging binaries of black holes (BHBH), neutron stars (NSNS) and neutron star and black hole (NSBH) were analysed separately. Additionally, the subset of most intensive BHBH mergers at closer distances and with larger radiative mass than the rest was considered. In total, follow-ups of 74 out of 93 gravitational waves reported in the GWTC-3 catalog were analyzed and no statistically significant excess over the background was observed. As a result, the strongest upper limits on GW-associated neutrino and antineutrino fluences for all flavors (谓_e, 谓_渭, 谓_蟿) have been obtained in the (0.5 - 5.0) MeV neutrino energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13876v2-abstract-full').style.display = 'none'; document.getElementById('2303.13876v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 8 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 (2023) 83:538 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.01830">arXiv:2302.01830</a> <span> [<a href="https://arxiv.org/pdf/2302.01830">pdf</a>, <a href="https://arxiv.org/format/2302.01830">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div 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/s10052-023-11410-4">10.1140/epjc/s10052-023-11410-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for low mass dark matter in DarkSide-50: the bayesian network approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Campos%2C+M+D">M. D. Campos</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cargioli%2C+N">N. Cargioli</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a> , et al. (119 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="2302.01830v2-abstract-short" style="display: inline;"> We present a novel approach for the search of dark matter in the DarkSide-50 experiment, relying on Bayesian Networks. This method incorporates the detector response model into the likelihood function, explicitly maintaining the connection with the quantity of interest. No assumptions about the linearity of the problem or the shape of the probability distribution functions are required, and there… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01830v2-abstract-full').style.display = 'inline'; document.getElementById('2302.01830v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.01830v2-abstract-full" style="display: none;"> We present a novel approach for the search of dark matter in the DarkSide-50 experiment, relying on Bayesian Networks. This method incorporates the detector response model into the likelihood function, explicitly maintaining the connection with the quantity of interest. No assumptions about the linearity of the problem or the shape of the probability distribution functions are required, and there is no need to morph signal and background spectra as a function of nuisance parameters. By expressing the problem in terms of Bayesian Networks, we have developed an inference algorithm based on a Markov Chain Monte Carlo to calculate the posterior probability. A clever description of the detector response model in terms of parametric matrices allows us to study the impact of systematic variations of any parameter on the final results. Our approach not only provides the desired information on the parameter of interest, but also potential constraints on the response model. Our results are consistent with recent published analyses and further refine the parameters of the detector response model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01830v2-abstract-full').style.display = 'none'; document.getElementById('2302.01830v2-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">24 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> Eur. Phys. J. C 83, 322 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.01177">arXiv:2209.01177</a> <span> [<a href="https://arxiv.org/pdf/2209.01177">pdf</a>, <a href="https://arxiv.org/format/2209.01177">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/10.1103/PhysRevD.107.112006">10.1103/PhysRevD.107.112006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity projections for a dual-phase argon TPC optimized for light dark matter searches through the ionization channel </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+I">I. Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Albergo%2C+S">S. Albergo</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Amaudruz%2C+P">P. Amaudruz</a>, <a href="/search/hep-ex?searchtype=author&query=Corona%2C+M+A">M. Atzori Corona</a>, <a href="/search/hep-ex?searchtype=author&query=Auty%2C+D+J">D. J. Auty</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Avetisov%2C+I+C">I. Ch. Avetisov</a>, <a href="/search/hep-ex?searchtype=author&query=Avetisov%2C+R+I">R. I. Avetisov</a>, <a href="/search/hep-ex?searchtype=author&query=Azzolini%2C+O">O. Azzolini</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Balmforth%2C+Z">Z. Balmforth</a>, <a href="/search/hep-ex?searchtype=author&query=Barbarian%2C+V">V. Barbarian</a>, <a href="/search/hep-ex?searchtype=author&query=Olmedo%2C+A+B">A. Barrado Olmedo</a>, <a href="/search/hep-ex?searchtype=author&query=Barrillon%2C+P">P. Barrillon</a>, <a href="/search/hep-ex?searchtype=author&query=Basco%2C+A">A. Basco</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Berzin%2C+E">E. Berzin</a>, <a href="/search/hep-ex?searchtype=author&query=Bondar%2C+A">A. Bondar</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Borisova%2C+E">E. Borisova</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a> , et al. (274 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="2209.01177v2-abstract-short" style="display: inline;"> Dark matter lighter than 10 GeV/c$^2$ encompasses a promising range of candidates. A conceptual design for a new detector, DarkSide-LowMass, is presented, based on the DarkSide-50 detector and progress toward DarkSide-20k, optimized for a low-threshold electron-counting measurement. Sensitivity to light dark matter is explored for various potential energy thresholds and background rates. These stu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.01177v2-abstract-full').style.display = 'inline'; document.getElementById('2209.01177v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.01177v2-abstract-full" style="display: none;"> Dark matter lighter than 10 GeV/c$^2$ encompasses a promising range of candidates. A conceptual design for a new detector, DarkSide-LowMass, is presented, based on the DarkSide-50 detector and progress toward DarkSide-20k, optimized for a low-threshold electron-counting measurement. Sensitivity to light dark matter is explored for various potential energy thresholds and background rates. These studies show that DarkSide-LowMass can achieve sensitivity to light dark matter down to the solar neutrino floor for GeV-scale masses and significant sensitivity down to 10 MeV/c$^2$ considering the Migdal effect or interactions with electrons. Requirements for optimizing the detector's sensitivity are explored, as are potential sensitivity gains from modeling and mitigating spurious electron backgrounds that may dominate the signal at the lowest energies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.01177v2-abstract-full').style.display = 'none'; document.getElementById('2209.01177v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 107, 112006 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.11968">arXiv:2207.11968</a> <span> [<a href="https://arxiv.org/pdf/2207.11968">pdf</a>, <a href="https://arxiv.org/format/2207.11968">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div 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.130.101002">10.1103/PhysRevLett.130.101002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter particle interactions with electron final states with DarkSide-50 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Campos%2C+M+D">M. D. Campos</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a>, <a href="/search/hep-ex?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a> , et al. (120 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="2207.11968v2-abstract-short" style="display: inline;"> We present a search for dark matter particles with sub-GeV/$c^2$ masses whose interactions have final state electrons using the DarkSide-50 experiment's (12306 $\pm$ 184) kg d low-radioactivity liquid argon exposure. By analyzing the ionization signals, we exclude new parameter space for the dark matter-electron cross section $\bar蟽_e$, the axioelectric coupling constant $g_{Ae}$, and the dark pho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.11968v2-abstract-full').style.display = 'inline'; document.getElementById('2207.11968v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.11968v2-abstract-full" style="display: none;"> We present a search for dark matter particles with sub-GeV/$c^2$ masses whose interactions have final state electrons using the DarkSide-50 experiment's (12306 $\pm$ 184) kg d low-radioactivity liquid argon exposure. By analyzing the ionization signals, we exclude new parameter space for the dark matter-electron cross section $\bar蟽_e$, the axioelectric coupling constant $g_{Ae}$, and the dark photon kinetic mixing parameter $魏$. We also set the first dark matter direct-detection constraints on the mixing angle $\left|U_{e4}\right|^2$ for keV sterile neutrinos. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.11968v2-abstract-full').style.display = 'none'; document.getElementById('2207.11968v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">6 pages, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett. 130 (2023) 10, 101002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.11967">arXiv:2207.11967</a> <span> [<a href="https://arxiv.org/pdf/2207.11967">pdf</a>, <a href="https://arxiv.org/format/2207.11967">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div 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.130.101001">10.1103/PhysRevLett.130.101001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter-nucleon interactions via Migdal effect with DarkSide-50 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Campos%2C+M+D">M. D. Campos</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a>, <a href="/search/hep-ex?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="2207.11967v2-abstract-short" style="display: inline;"> Dark matter elastic scattering off nuclei can result in the excitation and ionization of the recoiling atom through the so-called Migdal effect. The energy deposition from the ionization electron adds to the energy deposited by the recoiling nuclear system and allows for the detection of interactions of sub-GeV/c$^2$ mass dark matter. We present new constraints for sub-GeV/c$^2$ dark matter using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.11967v2-abstract-full').style.display = 'inline'; document.getElementById('2207.11967v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.11967v2-abstract-full" style="display: none;"> Dark matter elastic scattering off nuclei can result in the excitation and ionization of the recoiling atom through the so-called Migdal effect. The energy deposition from the ionization electron adds to the energy deposited by the recoiling nuclear system and allows for the detection of interactions of sub-GeV/c$^2$ mass dark matter. We present new constraints for sub-GeV/c$^2$ dark matter using the dual-phase liquid argon time projection chamber of the DarkSide-50 experiment with an exposure of (12306 $\pm$ 184) kg d. The analysis is based on the ionization signal alone and significantly enhances the sensitivity of DarkSide-50, enabling sensitivity to dark matter with masses down to 40 MeV/c$^2$. Furthermore, it sets the most stringent upper limit on the spin independent dark matter nucleon cross section for masses below $3.6$ GeV/c$^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.11967v2-abstract-full').style.display = 'none'; document.getElementById('2207.11967v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">7 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett. 130 (2023) 10, 101001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.11966">arXiv:2207.11966</a> <span> [<a href="https://arxiv.org/pdf/2207.11966">pdf</a>, <a href="https://arxiv.org/format/2207.11966">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div 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.107.063001">10.1103/PhysRevD.107.063001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for low-mass dark matter WIMPs with 12 ton-day exposure of DarkSide-50 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a>, <a href="/search/hep-ex?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a> , et al. (119 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="2207.11966v3-abstract-short" style="display: inline;"> We report on the search for dark matter WIMPs in the mass range below 10 GeV/c$^2$, from the analysis of the entire dataset acquired with a low-radioactivity argon target by the DarkSide-50 experiment at LNGS. The new analysis benefits from more accurate calibration of the detector response, improved background model, and better determination of systematic uncertainties, allowing us to accurately… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.11966v3-abstract-full').style.display = 'inline'; document.getElementById('2207.11966v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.11966v3-abstract-full" style="display: none;"> We report on the search for dark matter WIMPs in the mass range below 10 GeV/c$^2$, from the analysis of the entire dataset acquired with a low-radioactivity argon target by the DarkSide-50 experiment at LNGS. The new analysis benefits from more accurate calibration of the detector response, improved background model, and better determination of systematic uncertainties, allowing us to accurately model the background rate and spectra down to 0.06 keV$_{er}$. A 90% C.L. exclusion limit for the spin-independent cross section of 3 GeV/c$^2$ mass WIMP on nucleons is set at 6$\times$10$^{-43}$ cm$^2$, about a factor 10 better than the previous DarkSide-50 limit. This analysis extends the exclusion region for spin-independent dark matter interactions below the current experimental constraints in the $[1.2, 3.6]$ GeV/c$^2$ WIMP mass range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.11966v3-abstract-full').style.display = 'none'; document.getElementById('2207.11966v3-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">11 pages, 12 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 107 (2023) 6, 063001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.15975">arXiv:2205.15975</a> <span> [<a href="https://arxiv.org/pdf/2205.15975">pdf</a>, <a href="https://arxiv.org/format/2205.15975">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> </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.129.252701">10.1103/PhysRevLett.129.252701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved measurement of solar neutrinos from the Carbon-Nitrogen-Oxygen cycle by Borexino and its implications for the Standard Solar Model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=G%C3%B6ttel%2C+A+S">A. S. G枚ttel</a> , et al. (57 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="2205.15975v1-abstract-short" style="display: inline;"> We present an improved measurement of the CNO solar neutrino interaction rate at Earth obtained with the complete Borexino Phase-III dataset. The measured rate R$_{\rm CNO}$ = $6.7^{+2.0}_{-0.8}$ counts/(day$ \cdot$ 100 tonnes), allows us to exclude the absence of the CNO signal with about 7$蟽$ C.L. The correspondent CNO neutrino flux is $6.6^{+2.0}_{-0.9} \times 10^8$ cm$^{-2}$ s$^{-1}$, taking i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.15975v1-abstract-full').style.display = 'inline'; document.getElementById('2205.15975v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.15975v1-abstract-full" style="display: none;"> We present an improved measurement of the CNO solar neutrino interaction rate at Earth obtained with the complete Borexino Phase-III dataset. The measured rate R$_{\rm CNO}$ = $6.7^{+2.0}_{-0.8}$ counts/(day$ \cdot$ 100 tonnes), allows us to exclude the absence of the CNO signal with about 7$蟽$ C.L. The correspondent CNO neutrino flux is $6.6^{+2.0}_{-0.9} \times 10^8$ cm$^{-2}$ s$^{-1}$, taking into account the neutrino flavor conversion. We use the new CNO measurement to evaluate the C and N abundances in the Sun with respect to the H abundance for the first time with solar neutrinos. Our result of $N_{\rm CN}$ = $(5.78^{+1.86}_{-1.00})\times10^{-4}$ displays a $\sim$2$蟽$ tension with the "low metallicity" spectroscopic photospheric measurements. On the other hand, our result used together with the $^7$Be and $^8$B solar neutrino fluxes, also measured by Borexino, permits to disfavour at 3.1$蟽$ C.L. the "low metallicity" SSM B16-AGSS09met as an alternative to the "high metallicity" SSM B16-GS98. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.15975v1-abstract-full').style.display = 'none'; document.getElementById('2205.15975v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 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, 6 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/2204.07029">arXiv:2204.07029</a> <span> [<a href="https://arxiv.org/pdf/2204.07029">pdf</a>, <a href="https://arxiv.org/format/2204.07029">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="Earth and Planetary Astrophysics">astro-ph.EP</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="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2022.102778">10.1016/j.astropartphys.2022.102778 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Independent determination of the Earth's orbital parameters with solar neutrinos in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Goettel%2C+A+S">A. S. Goettel</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a> , et al. (54 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="2204.07029v1-abstract-short" style="display: inline;"> Since the beginning of 2012, the Borexino collaboration has been reporting precision measurements of the solar neutrino fluxes, emitted in the proton-proton chain and in the Carbon-Nitrogen-Oxygen cycle. The experimental sensitivity achieved in Phase-II and Phase-III of the Borexino data taking made it possible to detect the annual modulation of the solar neutrino interaction rate due to the eccen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.07029v1-abstract-full').style.display = 'inline'; document.getElementById('2204.07029v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.07029v1-abstract-full" style="display: none;"> Since the beginning of 2012, the Borexino collaboration has been reporting precision measurements of the solar neutrino fluxes, emitted in the proton-proton chain and in the Carbon-Nitrogen-Oxygen cycle. The experimental sensitivity achieved in Phase-II and Phase-III of the Borexino data taking made it possible to detect the annual modulation of the solar neutrino interaction rate due to the eccentricity of Earth's orbit, with a statistical significance greater than 5$蟽$. This is the first precise measurement of the Earth's orbital parameters based solely on solar neutrinos and an additional signature of the solar origin of the Borexino signal. The complete periodogram of the time series of the Borexino solar neutrino detection rate is also reported, exploring frequencies between one cycle/year and one cycle/day. No other significant modulation frequencies are found. The present results were uniquely made possible by Borexino's decade-long high-precision solar neutrino detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.07029v1-abstract-full').style.display = 'none'; document.getElementById('2204.07029v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">12 pages, 10 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/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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?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/2111.14500">arXiv:2111.14500</a> <span> [<a href="https://arxiv.org/pdf/2111.14500">pdf</a>, <a href="https://arxiv.org/ps/2111.14500">ps</a>, <a href="https://arxiv.org/format/2111.14500">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </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/s10052-022-10197-0">10.1140/epjc/s10052-022-10197-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Low-Energy Signals from Fast Radio Bursts with the Borexino Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Gottel%2C+A+S">A. S. Gottel</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a> , et al. (55 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.14500v2-abstract-short" style="display: inline;"> The search for neutrino events in correlation with several of the most intense fast radio bursts (FRBs) has been performed using the Borexino data. We have searched for signals with visible energies above $250$~keV within a time window of $\pm$1000~s corresponding to the detection time of a particular FRB. We also applied an alternative approach based on searching for specific shapes of neutrino-e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14500v2-abstract-full').style.display = 'inline'; document.getElementById('2111.14500v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.14500v2-abstract-full" style="display: none;"> The search for neutrino events in correlation with several of the most intense fast radio bursts (FRBs) has been performed using the Borexino data. We have searched for signals with visible energies above $250$~keV within a time window of $\pm$1000~s corresponding to the detection time of a particular FRB. We also applied an alternative approach based on searching for specific shapes of neutrino-electron scattering spectra in the full exposure spectrum of the Borexino detector. In particular, two incoming neutrino spectra were considered: the monoenergetic line and the spectrum expected from supernovae. The same spectra were considered for electron antineutrinos detected through the inverse beta-decay reaction. No statistically significant excess over the background was observed. As a result, the strongest upper limits on FRB-associated neutrino fluences of all flavors have been obtained in the $0.5 - 50$~MeV neutrino energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14500v2-abstract-full').style.display = 'none'; document.getElementById('2111.14500v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">14 pages, 10 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 (2022) 82:278 </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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=The+DarkSide+collaboration"> The DarkSide collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a>, <a href="/search/hep-ex?searchtype=author&query=Catalanotti%2C+S">S. Catalanotti</a>, <a href="/search/hep-ex?searchtype=author&query=Cataudella%2C+V">V. Cataudella</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Carpinelli%2C+M">M. Carpinelli</a>, <a href="/search/hep-ex?searchtype=author&query=Catalanotti%2C+S">S. Catalanotti</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacintio%2C+A">A. Di Giacintio</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Kumaran%2C+S">S. Kumaran</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?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/2105.09211">arXiv:2105.09211</a> <span> [<a href="https://arxiv.org/pdf/2105.09211">pdf</a>, <a href="https://arxiv.org/format/2105.09211">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> First detection of CNO neutrinos with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Settanta%2C+G">G. Settanta</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?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="2105.09211v1-abstract-short" style="display: inline;"> Neutrinos are elementary particles which are known since many years as fundamental messengers from the interior of the Sun. The Standard Solar Model, which gives a theoretical description of all nuclear processes which happen in our star, predicts that roughly 99% of the energy produced is coming from a series of processes known as the "pp chain". Such processes have been studied in detail over th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09211v1-abstract-full').style.display = 'inline'; document.getElementById('2105.09211v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.09211v1-abstract-full" style="display: none;"> Neutrinos are elementary particles which are known since many years as fundamental messengers from the interior of the Sun. The Standard Solar Model, which gives a theoretical description of all nuclear processes which happen in our star, predicts that roughly 99% of the energy produced is coming from a series of processes known as the "pp chain". Such processes have been studied in detail over the last years by means of neutrinos, thanks also to the important measurements provided by the Borexino experiment. The remaining 1% is instead predicted to come from a separate loop-process, known as the "CNO cycle". This sub-dominant process is theoretically well understood, but has so far escaped any direct observation. Another fundamental aspect is that the CNO cycle is indeed the main nuclear engine in stars more massive than the Sun. In 2020, thanks to the unprecedented radio-purity and temperature control achieved by the Borexino detector over recent years, the first ever detection of neutrinos from the CNO cycle has been finally announced. The milestone result confirms the existence of this nuclear fusion process in our Universe. Here, the details of the detector stabilization and the analysis techniques adopted are reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09211v1-abstract-full').style.display = 'none'; document.getElementById('2105.09211v1-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">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures. 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/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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?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/2004.02024">arXiv:2004.02024</a> <span> [<a href="https://arxiv.org/pdf/2004.02024">pdf</a>, <a href="https://arxiv.org/format/2004.02024">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-020-08801-2">10.1140/epjc/s10052-020-08801-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SiPM-matrix readout of two-phase argon detectors using electroluminescence in the visible and near infrared range </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+DarkSide+collaboration"> The DarkSide collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Aalseth%2C+C+E">C. E. Aalseth</a>, <a href="/search/hep-ex?searchtype=author&query=Abdelhakim%2C+S">S. Abdelhakim</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Ajaj%2C+R">R. Ajaj</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alici%2C+A">A. Alici</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Amaudruz%2C+P">P. Amaudruz</a>, <a href="/search/hep-ex?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/hep-ex?searchtype=author&query=Anstey%2C+J">J. Anstey</a>, <a href="/search/hep-ex?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/hep-ex?searchtype=author&query=Arba%2C+M">M. Arba</a>, <a href="/search/hep-ex?searchtype=author&query=Arcelli%2C+S">S. Arcelli</a>, <a href="/search/hep-ex?searchtype=author&query=Ardito%2C+R">R. Ardito</a>, <a href="/search/hep-ex?searchtype=author&query=Arnquist%2C+I+J">I. J. Arnquist</a>, <a href="/search/hep-ex?searchtype=author&query=Arpaia%2C+P">P. Arpaia</a>, <a href="/search/hep-ex?searchtype=author&query=Asner%2C+D+M">D. M. Asner</a>, <a href="/search/hep-ex?searchtype=author&query=Asunskis%2C+A">A. Asunskis</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Barbaryan%2C+V">V. Barbaryan</a>, <a href="/search/hep-ex?searchtype=author&query=Olmedo%2C+A+B">A. Barrado Olmedo</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a> , et al. (290 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2004.02024v2-abstract-short" style="display: inline;"> Proportional electroluminescence (EL) in noble gases is used in two-phase detectors for dark matter searches to record (in the gas phase) the ionization signal induced by particle scattering in the liquid phase. The "standard" EL mechanism is considered to be due to noble gas excimer emission in the vacuum ultraviolet (VUV). In addition, there are two alternative mechanisms, producing light in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.02024v2-abstract-full').style.display = 'inline'; document.getElementById('2004.02024v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.02024v2-abstract-full" style="display: none;"> Proportional electroluminescence (EL) in noble gases is used in two-phase detectors for dark matter searches to record (in the gas phase) the ionization signal induced by particle scattering in the liquid phase. The "standard" EL mechanism is considered to be due to noble gas excimer emission in the vacuum ultraviolet (VUV). In addition, there are two alternative mechanisms, producing light in the visible and near infrared (NIR) ranges. The first is due to bremsstrahlung of electrons scattered on neutral atoms ("neutral bremsstrahlung", NBrS). The second, responsible for electron avalanche scintillation in the NIR at higher electric fields, is due to transitions between excited atomic states. In this work, we have for the first time demonstrated two alternative techniques of the optical readout of two-phase argon detectors, in the visible and NIR range, using a silicon photomultiplier matrix and electroluminescence due to either neutral bremsstrahlung or avalanche scintillation. The amplitude yield and position resolution were measured for these readout techniques, which allowed to assess the detection threshold for electron and nuclear recoils in two-phase argon detectors for dark matter searches. To the best of our knowledge, this is the first practical application of the NBrS effect in detection science. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.02024v2-abstract-full').style.display = 'none'; document.getElementById('2004.02024v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 22 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C (2021) 81: 153 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/hep-ex?searchtype=author&query=Collaboration%2C+T+D">The DarkSide-50 Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Agnes%2C+P">P. Agnes</a>, <a href="/search/hep-ex?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+A+K">A. K. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Batignani%2C+G">G. Batignani</a>, <a href="/search/hep-ex?searchtype=author&query=Biery%2C+K">K. Biery</a>, <a href="/search/hep-ex?searchtype=author&query=Bocci%2C+V">V. Bocci</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bonivento%2C+W+M">W. M. Bonivento</a>, <a href="/search/hep-ex?searchtype=author&query=Bottino%2C+B">B. Bottino</a>, <a href="/search/hep-ex?searchtype=author&query=Bussino%2C+S">S. Bussino</a>, <a href="/search/hep-ex?searchtype=author&query=Cadeddu%2C+M">M. Cadeddu</a>, <a href="/search/hep-ex?searchtype=author&query=Cadoni%2C+M">M. Cadoni</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/hep-ex?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/hep-ex?searchtype=author&query=Caravati%2C+M">M. Caravati</a>, <a href="/search/hep-ex?searchtype=author&query=Cariello%2C+M">M. Cariello</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=The+Borexino+Collaboration"> The Borexino Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?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/1709.00756">arXiv:1709.00756</a> <span> [<a href="https://arxiv.org/pdf/1709.00756">pdf</a>, <a href="https://arxiv.org/format/1709.00756">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> </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.101.062001">10.1103/PhysRevD.101.062001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved measurement of $^8$B solar neutrinos with 1.5 kt y of Borexino exposure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+Borexino+Collaboration"> The Borexino Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</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="1709.00756v2-abstract-short" style="display: inline;"> We report on an improved measurement of the $^8$B solar neutrino interaction rate with the Borexino experiment at the Laboratori Nazionali del Gran Sasso. Neutrinos are detected via their elastic scattering on electrons in a large volume of liquid scintillator. The measured rate of scattered electrons above 3 MeV of energy is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.00756v2-abstract-full').style.display = 'inline'; document.getElementById('1709.00756v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.00756v2-abstract-full" style="display: none;"> We report on an improved measurement of the $^8$B solar neutrino interaction rate with the Borexino experiment at the Laboratori Nazionali del Gran Sasso. Neutrinos are detected via their elastic scattering on electrons in a large volume of liquid scintillator. The measured rate of scattered electrons above 3 MeV of energy is $0.223\substack{+0.015 \\ -0.016}\,(stat)\,\substack{+0.006 \\ -0.006}\,(syst)$ cpd/100 t, which corresponds to an observed solar neutrino flux assuming no neutrino flavor conversion of $桅\substack{\rm ES \\ ^8\rm B}=2.57\substack{+0.17 \\ -0.18}(stat)\substack{+0.07\\ -0.07}(syst)\times$10$^6$ cm$^{-2}\,$s$^{-1}$. This measurement exploits the active volume of the detector in almost its entirety for the first time, and takes advantage of a reduced radioactive background following the 2011 scintillator purification campaign and of novel analysis tools providing a more precise modeling of the background. Additionally, we set a new limit on the interaction rate of solar $hep$ neutrinos, searched via their elastic scattering on electrons as well as their neutral current-mediated inelastic scattering on carbon, $^{12}$C($谓,谓'$)$^{12}$C* ($E_纬$= 15.1 MeV). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.00756v2-abstract-full').style.display = 'none'; document.getElementById('1709.00756v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">14 pages, 13 figures, 4 tables</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, 062001 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.09355">arXiv:1707.09355</a> <span> [<a href="https://arxiv.org/pdf/1707.09355">pdf</a>, <a href="https://arxiv.org/format/1707.09355">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> </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.96.091103">10.1103/PhysRevD.96.091103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limiting neutrino magnetic moments with Borexino Phase-II solar neutrino data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?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="1707.09355v3-abstract-short" style="display: inline;"> A search for the solar neutrino effective magnetic moment has been performed using data from 1291.5 days exposure during the second phase of the Borexino experiment. No significant deviations from the expected shape of the electron recoil spectrum from solar neutrinos have been found, and a new upper limit on the effective neutrino magnetic moment of $渭_谓^{eff}$ $<$ 2.8$\cdot$10$^{-11}$ $渭_{B}$ at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09355v3-abstract-full').style.display = 'inline'; document.getElementById('1707.09355v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.09355v3-abstract-full" style="display: none;"> A search for the solar neutrino effective magnetic moment has been performed using data from 1291.5 days exposure during the second phase of the Borexino experiment. No significant deviations from the expected shape of the electron recoil spectrum from solar neutrinos have been found, and a new upper limit on the effective neutrino magnetic moment of $渭_谓^{eff}$ $<$ 2.8$\cdot$10$^{-11}$ $渭_{B}$ at 90\% c.l. has been set using constraints on the sum of the solar neutrino fluxes implied by the radiochemical gallium experiments.Using the limit for the effective neutrino moment, new limits for the magnetic moments of the neutrino flavor states, and for the elements of the neutrino magnetic moments matrix for Dirac and Majorana neutrinos, are derived. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09355v3-abstract-full').style.display = 'none'; document.getElementById('1707.09355v3-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 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 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">7 pages, 2 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 96, 091103 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.09279">arXiv:1707.09279</a> <span> [<a href="https://arxiv.org/pdf/1707.09279">pdf</a>, <a href="https://arxiv.org/format/1707.09279">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> </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.100.082004">10.1103/PhysRevD.100.082004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simultaneous Precision Spectroscopy of $pp$, $^7$Be, and $pep$ Solar Neutrinos with Borexino Phase-II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?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="1707.09279v3-abstract-short" style="display: inline;"> We present the first simultaneous measurement of the interaction rates of $pp$, $^7$Be, and $pep$ solar neutrinos performed with a global fit to the Borexino data in an extended energy range (0.19-2.93)$\,$MeV. This result was obtained by analyzing 1291.51$\,$days of Borexino Phase-II data, collected between December 2011 and May 2016 after an extensive scintillator purification campaign. We find:… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09279v3-abstract-full').style.display = 'inline'; document.getElementById('1707.09279v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.09279v3-abstract-full" style="display: none;"> We present the first simultaneous measurement of the interaction rates of $pp$, $^7$Be, and $pep$ solar neutrinos performed with a global fit to the Borexino data in an extended energy range (0.19-2.93)$\,$MeV. This result was obtained by analyzing 1291.51$\,$days of Borexino Phase-II data, collected between December 2011 and May 2016 after an extensive scintillator purification campaign. We find: rate($pp$)$\,$=$\,$$134$$\,$$\pm$$\,$$10$$\,$($stat$)$\,$$^{\rm +6}_{\rm -10}$$\,$($sys$)$\,$cpd/100$\,$t, rate($^7$Be)$\,$=$\,$$48.3$$\,$$\pm$$\,$$1.1$$\,$($stat$)$\,$$^{\rm +0.4}_{\rm -0.7}$$\,$($sys$)$\,$cpd/100$\,$t, and rate($pep$)$\,$=$\,$$2.43$$\pm$$\,$$0.36$$\,$($stat$)$^{+0.15}_{-0.22}$$\,$($sys$)$\,$cpd/100$\,$t. These numbers are in agreement with and improve the precision of our previous measurements. In particular, the interaction rate of $^7$Be $谓$'s is measured with an unprecedented precision of 2.7%, showing that discriminating between the high and low metallicity solar models is now largely dominated by theoretical uncertainties. The absence of $pep$ neutrinos is rejected for the first time at more than 5$\,$$蟽$. An upper limit of $8.1$$\,$cpd/100$\,$t (95%$\,$C.L.) on the CNO neutrino rate is obtained by setting an additional constraint on the ratio between the $pp$ and $pep$ neutrino rates in the fit. This limit has the same significance as that obtained by the Borexino Phase-I (currently providing the tightest bound on this component), but is obtained by applying a less stringent constraint on the $pep$ $谓$ flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09279v3-abstract-full').style.display = 'none'; document.getElementById('1707.09279v3-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 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">8 pages, 7 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 100, 082004 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.10176">arXiv:1706.10176</a> <span> [<a href="https://arxiv.org/pdf/1706.10176">pdf</a>, <a href="https://arxiv.org/ps/1706.10176">ps</a>, <a href="https://arxiv.org/format/1706.10176">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aa9521">10.3847/1538-4357/aa9521 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for low-energy neutrinos correlated with gravitational wave events GW150914, GW151226 and GW170104 with the Borexino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</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="1706.10176v1-abstract-short" style="display: inline;"> We present the results of a low-energy neutrino search using the Borexino detector in coincidence with the gravitational wave (GW) events GW150914, GW151226 and GW170104. We searched for correlated neutrino events with energies greater than 250 keV within a time window of $\pm500$ s centered around the GW detection time. A total of five candidates were found for all three GW150914, GW151226 and GW… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.10176v1-abstract-full').style.display = 'inline'; document.getElementById('1706.10176v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.10176v1-abstract-full" style="display: none;"> We present the results of a low-energy neutrino search using the Borexino detector in coincidence with the gravitational wave (GW) events GW150914, GW151226 and GW170104. We searched for correlated neutrino events with energies greater than 250 keV within a time window of $\pm500$ s centered around the GW detection time. A total of five candidates were found for all three GW150914, GW151226 and GW170104. This is consistent with the number of expected solar neutrino and background events. As a result, we have obtained the best current upper limits on the GW event neutrino fluence of all flavors ($谓_e, 谓_渭, 谓_蟿$) in the energy range $(0.5 - 5.0)$ MeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.10176v1-abstract-full').style.display = 'none'; document.getElementById('1706.10176v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">8 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2017 Astrophys. J. 850 21 </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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Borodikhina%2C+L">L. Borodikhina</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Borodikhina%2C+L">L. Borodikhina</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Muratova%2C+V">V. Muratova</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Formozov%2C+A">A. Formozov</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?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/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/hep-ex?searchtype=author&query=Borexino+Collaboration"> Borexino Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Mosteiro%2C+P">P. Mosteiro</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Smirnov%2C+O+Y">O. Y. Smirnov</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Borexino+collaboration"> Borexino collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=DAngelo%2C+D">D. DAngelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fiorentini%2C+G">G. Fiorentini</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?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/1410.0779">arXiv:1410.0779</a> <span> [<a href="https://arxiv.org/pdf/1410.0779">pdf</a>, <a href="https://arxiv.org/format/1410.0779">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/10.1134/S1063779615020185">10.1134/S1063779615020185 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solar neutrino with Borexino: results and perspectives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Smirnov%2C+O">O. Smirnov</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Fiorentini%2C+G">G. Fiorentini</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a> , et al. (65 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="1410.0779v1-abstract-short" style="display: inline;"> Borexino is a unique detector able to perform measurement of solar neutrinos fluxes in the energy region around 1 MeV or below due to its low level of radioactive background. It was constructed at the LNGS underground laboratory with a goal of solar $^{7}$Be neutrino flux measurement with 5\% precision. The goal has been successfully achieved marking the end of the first stage of the experiment. A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.0779v1-abstract-full').style.display = 'inline'; document.getElementById('1410.0779v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.0779v1-abstract-full" style="display: none;"> Borexino is a unique detector able to perform measurement of solar neutrinos fluxes in the energy region around 1 MeV or below due to its low level of radioactive background. It was constructed at the LNGS underground laboratory with a goal of solar $^{7}$Be neutrino flux measurement with 5\% precision. The goal has been successfully achieved marking the end of the first stage of the experiment. A number of other important measurements of solar neutrino fluxes have been performed during the first stage. Recently the collaboration conducted successful liquid scintillator repurification campaign aiming to reduce main contaminants in the sub-MeV energy range. With the new levels of radiopurity Borexino can improve existing and challenge a number of new measurements including: improvement of the results on the Solar and terrestrial neutrino fluxes measurements; measurement of pp and CNO solar neutrino fluxes; search for non-standard interactions of neutrino; study of the neutrino oscillations on the short baseline with an artificial neutrino source (search for sterile neutrino) in context of SOX project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.0779v1-abstract-full').style.display = 'none'; document.getElementById('1410.0779v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 4 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/1405.7919">arXiv:1405.7919</a> <span> [<a href="https://arxiv.org/pdf/1405.7919">pdf</a>, <a href="https://arxiv.org/format/1405.7919">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"> Recent Borexino results and prospects for the near future </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=von+Feilitzsch%2C+F">F. von Feilitzsch</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1405.7919v1-abstract-short" style="display: inline;"> The Borexino experiment, located in the Gran Sasso National Laboratory, is an organic liquid scintillator detector conceived for the real time spectroscopy of low energy solar neutrinos. The data taking campaign phase I (2007 - 2010) has allowed the first independent measurements of 7Be, 8B and pep fluxes as well as the first measurement of anti-neutrinos from the earth. After a purification of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.7919v1-abstract-full').style.display = 'inline'; document.getElementById('1405.7919v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.7919v1-abstract-full" style="display: none;"> The Borexino experiment, located in the Gran Sasso National Laboratory, is an organic liquid scintillator detector conceived for the real time spectroscopy of low energy solar neutrinos. The data taking campaign phase I (2007 - 2010) has allowed the first independent measurements of 7Be, 8B and pep fluxes as well as the first measurement of anti-neutrinos from the earth. After a purification of the scintillator, Borexino is now in phase II since 2011. We review here the recent results achieved during 2013, concerning the seasonal modulation in the 7Be signal, the study of cosmogenic backgrounds and the updated measurement of geo-neutrinos. We also review the upcoming measurements from phase II data (pp, pep, CNO) and the project SOX devoted to the study of sterile neutrinos via the use of a 51Cr neutrino source and a 144Ce-144Pr antineutrino source placed in close proximity of the active material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.7919v1-abstract-full').style.display = 'none'; document.getElementById('1405.7919v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 11 figures. To be published as proceedings of Rencontres de Moriond EW 2014</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1311.5347">arXiv:1311.5347</a> <span> [<a href="https://arxiv.org/pdf/1311.5347">pdf</a>, <a href="https://arxiv.org/ps/1311.5347">ps</a>, <a href="https://arxiv.org/format/1311.5347">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="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.88.072010">10.1103/PhysRevD.88.072010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New limits on heavy sterile neutrino mixing in ${^{8}\rm{B}}$-decay obtained with the Borexino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Borexino+collaboration"> Borexino collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=DAngelo%2C+D">D. DAngelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a> , et al. (65 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="1311.5347v1-abstract-short" style="display: inline;"> If heavy neutrinos with mass $m_{谓_{H}}\geq$2$ m_e $ are produced in the Sun via the decay ${^8\rm{B}} \rightarrow {^8\rm{Be}} + e^+ + 谓_H$ in a side branch of pp-chain, they would undergo the observable decay into an electron, a positron and a light neutrino $谓_{H}\rightarrow谓_{L}+e^++e^-$. In the present work Borexino data are used to set a bound on the existence of such decays. We constrain the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.5347v1-abstract-full').style.display = 'inline'; document.getElementById('1311.5347v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1311.5347v1-abstract-full" style="display: none;"> If heavy neutrinos with mass $m_{谓_{H}}\geq$2$ m_e $ are produced in the Sun via the decay ${^8\rm{B}} \rightarrow {^8\rm{Be}} + e^+ + 谓_H$ in a side branch of pp-chain, they would undergo the observable decay into an electron, a positron and a light neutrino $谓_{H}\rightarrow谓_{L}+e^++e^-$. In the present work Borexino data are used to set a bound on the existence of such decays. We constrain the mixing of a heavy neutrino with mass 1.5 MeV $\leq m_{谓_{H}} \le$ 14 MeV to be $|U_{eH}|^2\leq (10^{-3}-4\times10^{-6})$ respectively. These are tighter limits on the mixing parameters than obtained in previous experiments at nuclear reactors and accelerators. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.5347v1-abstract-full').style.display = 'none'; document.getElementById('1311.5347v1-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 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 6 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 88, 072010 (2013) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1308.0443">arXiv:1308.0443</a> <span> [<a href="https://arxiv.org/pdf/1308.0443">pdf</a>, <a href="https://arxiv.org/format/1308.0443">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.89.112007">10.1103/PhysRevD.89.112007 <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 Phase-I on low energy solar neutrino spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Borexino+Collaboration"> Borexino Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Avanzini%2C+M+B">M. B. Avanzini</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a> , et al. (65 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="1308.0443v2-abstract-short" style="display: inline;"> Borexino has been running since May 2007 at the LNGS with the primary goal of detecting solar neutrinos. The detector, a large, unsegmented liquid scintillator calorimeter characterized by unprecedented low levels of intrinsic radioactivity, is optimized for the study of the lower energy part of the spectrum. During the Phase-I (2007-2010) Borexino first detected and then precisely measured the fl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.0443v2-abstract-full').style.display = 'inline'; document.getElementById('1308.0443v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1308.0443v2-abstract-full" style="display: none;"> Borexino has been running since May 2007 at the LNGS with the primary goal of detecting solar neutrinos. The detector, a large, unsegmented liquid scintillator calorimeter characterized by unprecedented low levels of intrinsic radioactivity, is optimized for the study of the lower energy part of the spectrum. During the Phase-I (2007-2010) Borexino first detected and then precisely measured the flux of the 7Be solar neutrinos, ruled out any significant day-night asymmetry of their interaction rate, made the first direct observation of the pep neutrinos, and set the tightest upper limit on the flux of CNO neutrinos. In this paper we discuss the signal signature and provide a comprehensive description of the backgrounds, quantify their event rates, describe the methods for their identification, selection or subtraction, and describe data analysis. Key features are an extensive in situ calibration program using radioactive sources, the detailed modeling of the detector response, the ability to define an innermost fiducial volume with extremely low background via software cuts, and the excellent pulse-shape discrimination capability of the scintillator that allows particle identification. We report a measurement of the annual modulation of the 7 Be neutrino interaction rate. The period, the amplitude, and the phase of the observed modulation are consistent with the solar origin of these events, and the absence of their annual modulation is rejected with higher than 99% C.L. The physics implications of phase-I results in the context of the neutrino oscillation physics and solar models are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.0443v2-abstract-full').style.display = 'none'; document.getElementById('1308.0443v2-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 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 89, 112007 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1304.7381">arXiv:1304.7381</a> <span> [<a href="https://arxiv.org/pdf/1304.7381">pdf</a>, <a href="https://arxiv.org/format/1304.7381">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/10.1088/1475-7516/2013/08/049">10.1088/1475-7516/2013/08/049 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmogenic Backgrounds in Borexino at 3800 m water-equivalent depth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=G%C3%B6ger-Neff%2C+M">M. G枚ger-Neff</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1304.7381v2-abstract-short" style="display: inline;"> The solar neutrino experiment Borexino, which is located in the Gran Sasso underground laboratories, is in a unique position to study muon-induced backgrounds in an organic liquid scintillator. In this study, a large sample of cosmic muons is identified and tracked by a muon veto detector external to the liquid scintillator, and by the specific light patterns observed when muons cross the scintill… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.7381v2-abstract-full').style.display = 'inline'; document.getElementById('1304.7381v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1304.7381v2-abstract-full" style="display: none;"> The solar neutrino experiment Borexino, which is located in the Gran Sasso underground laboratories, is in a unique position to study muon-induced backgrounds in an organic liquid scintillator. In this study, a large sample of cosmic muons is identified and tracked by a muon veto detector external to the liquid scintillator, and by the specific light patterns observed when muons cross the scintillator volume. The yield of muon-induced neutrons is found to be Yn =(3.10+-0.11)10-4 n/(渭 (g/cm2)). The distance profile between the parent muon track and the neutron capture point has the average value 位 = (81.5 +- 2.7)cm. Additionally the yields of a number of cosmogenic radioisotopes are measured for 12N, 12B, 8He, 9C, 9Li, 8B, 6He, 8Li, 11Be, 10C and 11C. All results are compared with Monte Carlo simulation predictions using the Fluka and Geant4 packages. General agreement between data and simulation is observed for the cosmogenic production yields with a few exceptions, the most prominent case being 11C yield for which both codes return about 50% lower values. The predicted 渭-n distance profile and the neutron multiplicity distribution are found to be overall consistent with data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.7381v2-abstract-full').style.display = 'none'; document.getElementById('1304.7381v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 13 figures (in 14 files), 4 tables. 3 extra data files. accepted by 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/1303.2571">arXiv:1303.2571</a> <span> [<a href="https://arxiv.org/pdf/1303.2571">pdf</a>, <a href="https://arxiv.org/format/1303.2571">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.physletb.2013.04.030">10.1016/j.physletb.2013.04.030 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of geo-neutrinos from 1353 days of Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fiorentini%2C+G">G. Fiorentini</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a> , et al. (68 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="1303.2571v2-abstract-short" style="display: inline;"> We present a measurement of the geo--neutrino signal obtained from 1353 days of data with the Borexino detector at Laboratori Nazionali del Gran Sasso in Italy. With a fiducial exposure of (3.69 $\pm$ 0.16) $\times$ $10^{31}$ proton $\times$ year after all selection cuts and background subtraction, we detected (14.3 $\pm$ 4.4) geo-neutrino events assuming a fixed chondritic mass Th/U ratio of 3.9.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1303.2571v2-abstract-full').style.display = 'inline'; document.getElementById('1303.2571v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1303.2571v2-abstract-full" style="display: none;"> We present a measurement of the geo--neutrino signal obtained from 1353 days of data with the Borexino detector at Laboratori Nazionali del Gran Sasso in Italy. With a fiducial exposure of (3.69 $\pm$ 0.16) $\times$ $10^{31}$ proton $\times$ year after all selection cuts and background subtraction, we detected (14.3 $\pm$ 4.4) geo-neutrino events assuming a fixed chondritic mass Th/U ratio of 3.9. This corresponds to a geo-neutrino signal $S_{geo}$ = (38.8 $\pm$ 12.0) TNU with just a 6 $\times$ $10^{-6}$ probability for a null geo-neutrino measurement. With U and Th left as free parameters in the fit, the relative signals are $S_{\mathrm{Th}}$ = (10.6 $\pm$ 12.7) TNU and $S_\mathrm{U}$ = (26.5 $\pm$ 19.5) TNU. Borexino data alone are compatible with a mantle geo--neutrino signal of (15.4 $\pm$ 12.3) TNU, while a combined analysis with the KamLAND data allows to extract a mantle signal of (14.1 $\pm$ 8.1) TNU. Our measurement of a reactor anti--neutrino signal $S_{react}$ = 84.5$^{+19.3}_{-18.9}$ TNU is in agreement with expectations in the presence of neutrino oscillations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1303.2571v2-abstract-full').style.display = 'none'; document.getElementById('1303.2571v2-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 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 March, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Lett. B 722 (2013) 295-300 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1205.2989">arXiv:1205.2989</a> <span> [<a href="https://arxiv.org/pdf/1205.2989">pdf</a>, <a href="https://arxiv.org/format/1205.2989">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> </div> </div> <p class="title is-5 mathjax"> Solar neutrino physics with Borexino I </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Ludhova%2C+L">L. Ludhova</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Carraro%2C+C">C. Carraro</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goeger-Nef%2C+M">M. Goeger-Nef</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a> , et al. (65 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="1205.2989v1-abstract-short" style="display: inline;"> Borexino is a large-volume liquid scintillator detector installed in the underground halls of the Laboratori Nazionali del Gran Sasso in Italy. After several years of construction, data taking started in May 2007. The Borexino phase I ended after about three years of data taking. Borexino provided the first real time measurement of the $^{7}$Be solar neutrino interaction rate with accuracy better… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.2989v1-abstract-full').style.display = 'inline'; document.getElementById('1205.2989v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1205.2989v1-abstract-full" style="display: none;"> Borexino is a large-volume liquid scintillator detector installed in the underground halls of the Laboratori Nazionali del Gran Sasso in Italy. After several years of construction, data taking started in May 2007. The Borexino phase I ended after about three years of data taking. Borexino provided the first real time measurement of the $^{7}$Be solar neutrino interaction rate with accuracy better than 5% and confirmed the absence of its day-night asymmetry with 1.4% precision. This latter Borexino results alone rejects the LOW region of solar neutrino oscillation parameters at more than 8.5 $蟽$ C.L. Combined with the other solar neutrino data, Borexino measurements isolate the MSW-LMA solution of neutrino oscillations without assuming CPT invariance in the neutrino sector. Borexino has also directly observed solar neutrinos in the 1.0-1.5 MeV energy range, leading to the first direct evidence of the $pep$ solar neutrino signal and the strongest constraint of the CNO solar neutrino flux up to date. Borexino provided the measurement of the solar $^{8}$B neutrino rate with 3 MeV energy threshold. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.2989v1-abstract-full').style.display = 'none'; document.getElementById('1205.2989v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 May, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 4 figures, proceedings to Moriond 2012 EW session</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1204.6218">arXiv:1204.6218</a> <span> [<a href="https://arxiv.org/pdf/1204.6218">pdf</a>, <a href="https://arxiv.org/format/1204.6218">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy 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.2013.08.004">10.1016/j.astropartphys.2013.08.004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Light Yield in DarkSide-10: a Prototype Two-phase Liquid Argon TPC for Dark Matter Searches </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Alexander%2C+T">T. Alexander</a>, <a href="/search/hep-ex?searchtype=author&query=Alton%2C+D">D. Alton</a>, <a href="/search/hep-ex?searchtype=author&query=Arisaka%2C+K">K. Arisaka</a>, <a href="/search/hep-ex?searchtype=author&query=Back%2C+H+O">H. O. Back</a>, <a href="/search/hep-ex?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/hep-ex?searchtype=author&query=Brodsky%2C+J">J. Brodsky</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Candela%2C+A">A. Candela</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+H">H. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Cline%2C+D">D. Cline</a>, <a href="/search/hep-ex?searchtype=author&query=Cocco%2C+A+G">A. G. Cocco</a>, <a href="/search/hep-ex?searchtype=author&query=Condon%2C+C">C. Condon</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=De+Haas%2C+E">E. De Haas</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Pietro%2C+G">G. Di Pietro</a>, <a href="/search/hep-ex?searchtype=author&query=Dratchnev%2C+I">I. Dratchnev</a> , et al. (97 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="1204.6218v2-abstract-short" style="display: inline;"> As part of the DarkSide program of direct dark matter searches using liquid argon TPCs, a prototype detector with an active volume containing 10 kg of liquid argon, DarkSide-10, was built and operated underground in the Gran Sasso National Laboratory in Italy. A critically important parameter for such devices is the scintillation light yield, as photon statistics limits the rejection of electron-r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1204.6218v2-abstract-full').style.display = 'inline'; document.getElementById('1204.6218v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1204.6218v2-abstract-full" style="display: none;"> As part of the DarkSide program of direct dark matter searches using liquid argon TPCs, a prototype detector with an active volume containing 10 kg of liquid argon, DarkSide-10, was built and operated underground in the Gran Sasso National Laboratory in Italy. A critically important parameter for such devices is the scintillation light yield, as photon statistics limits the rejection of electron-recoil backgrounds by pulse shape discrimination. We have measured the light yield of DarkSide-10 using the readily-identifiable full-absorption peaks from gamma ray sources combined with single-photoelectron calibrations using low-occupancy laser pulses. For gamma lines of energies in the range 122-1275 keV, we get consistent light yields averaging 8.887+-0.003(stat)+-0.444(sys) p.e./keVee. With additional purification, the light yield measured at 511 keV increased to 9.142+-0.006(stat) p.e./keVee. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1204.6218v2-abstract-full').style.display = 'none'; document.getElementById('1204.6218v2-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 August, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 April, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 figures, Accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1202.6403">arXiv:1202.6403</a> <span> [<a href="https://arxiv.org/pdf/1202.6403">pdf</a>, <a href="https://arxiv.org/format/1202.6403">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="Atmospheric and Oceanic Physics">physics.ao-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/10.1088/1475-7516/2012/05/015">10.1088/1475-7516/2012/05/015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic-muon flux and annual modulation in Borexino at 3800 m water-equivalent depth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Carraro%2C+C">C. Carraro</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=von+Feilitzsch%2C+F">F. von Feilitzsch</a>, <a href="/search/hep-ex?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1202.6403v3-abstract-short" style="display: inline;"> We have measured the muon flux at the underground Gran Sasso National Laboratory (3800 m w.e.) to be (3.41 \pm 0.01) \times 10-4m-2s-1 using four years of Borexino data. A modulation of this signal is observed with a period of (366\pm3) days and a relative amplitude of (1.29 \pm 0.07)%. The measured phase is (179 \pm 6) days, corresponding to a maximum on the 28th of June. Using the most complete… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.6403v3-abstract-full').style.display = 'inline'; document.getElementById('1202.6403v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.6403v3-abstract-full" style="display: none;"> We have measured the muon flux at the underground Gran Sasso National Laboratory (3800 m w.e.) to be (3.41 \pm 0.01) \times 10-4m-2s-1 using four years of Borexino data. A modulation of this signal is observed with a period of (366\pm3) days and a relative amplitude of (1.29 \pm 0.07)%. The measured phase is (179 \pm 6) days, corresponding to a maximum on the 28th of June. Using the most complete atmospheric data models available, muon rate fluctuations are shown to be positively correlated with atmospheric temperature, with an effective coefficient 伪T = 0.93 \pm 0.04. This result represents the most precise study of the muon flux modulation for this site and is in good agreement with expectations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.6403v3-abstract-full').style.display = 'none'; document.getElementById('1202.6403v3-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 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures, published on JCAP as JCAP05(2012)015 on May 15th 2012</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP05(2012)015 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 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