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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/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/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/2009.05515">arXiv:2009.05515</a> <span> [<a href="https://arxiv.org/pdf/2009.05515">pdf</a>, <a href="https://arxiv.org/format/2009.05515">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/10.1140/epjc/s10052-021-09459-0">10.1140/epjc/s10052-021-09459-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Signatures of Sterile Neutrinos with Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+Double+Chooz+Collaboration"> The Double Chooz Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/hep-ex?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/hep-ex?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/hep-ex?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/hep-ex?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/hep-ex?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/hep-ex?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/hep-ex?searchtype=author&query=Corpace%2C+O">O. Corpace</a>, <a href="/search/hep-ex?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/hep-ex?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Furuta%2C+H">H. Furuta</a>, <a href="/search/hep-ex?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</a>, <a href="/search/hep-ex?searchtype=author&query=Givaudan%2C+A">A. Givaudan</a>, <a href="/search/hep-ex?searchtype=author&query=Gomez%2C+H">H. Gomez</a> , et al. (70 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="2009.05515v3-abstract-short" style="display: inline;"> We present a search for signatures of neutrino mixing of electron anti-neutrinos with additional hypothetical sterile neutrino flavors using the Double Chooz experiment. The search is based on data from 5 years of operation of Double Chooz, including 2 years in the two-detector configuration. The analysis is based on a profile likelihood, i.e.\ comparing the data to the model prediction of disappe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05515v3-abstract-full').style.display = 'inline'; document.getElementById('2009.05515v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.05515v3-abstract-full" style="display: none;"> We present a search for signatures of neutrino mixing of electron anti-neutrinos with additional hypothetical sterile neutrino flavors using the Double Chooz experiment. The search is based on data from 5 years of operation of Double Chooz, including 2 years in the two-detector configuration. The analysis is based on a profile likelihood, i.e.\ comparing the data to the model prediction of disappearance in a data-to-data comparison of the two respective detectors. The analysis is optimized for a model of three active and one sterile neutrino. It is sensitive in the typical mass range $5 \cdot 10^{-3} $ eV$^2 \lesssim 螖m^2_{41} \lesssim 3\cdot 10^{-1} $ eV$^2$ for mixing angles down to $\sin^2 2胃_{14} \gtrsim 0.02$. No significant disappearance additionally to the conventional disappearance related to $胃_{13} $ is observed and correspondingly exclusion bounds on the sterile mixing parameter $胃_{14} $ as function of $ 螖m^2_{41} $ are obtained. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05515v3-abstract-full').style.display = 'none'; document.getElementById('2009.05515v3-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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 for publication by EPJC</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 62F03 (Primary); 62P35; 65C60 (Secondary) </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 81, 775 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.13431">arXiv:2007.13431</a> <span> [<a href="https://arxiv.org/pdf/2007.13431">pdf</a>, <a href="https://arxiv.org/format/2007.13431">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/10.1007/JHEP01(2021)190">10.1007/JHEP01(2021)190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reactor Rate Modulation oscillation analysis with two detectors in Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Double+Chooz+Collaboration"> Double Chooz Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/hep-ex?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/hep-ex?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/hep-ex?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/hep-ex?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/hep-ex?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/hep-ex?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/hep-ex?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Furuta%2C+H">H. Furuta</a>, <a href="/search/hep-ex?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</a>, <a href="/search/hep-ex?searchtype=author&query=Gonzalez%2C+L+F+G">L. F. G. Gonzalez</a>, <a href="/search/hep-ex?searchtype=author&query=Goodman%2C+M+C">M. C. Goodman</a>, <a href="/search/hep-ex?searchtype=author&query=Hara%2C+T">T. Hara</a>, <a href="/search/hep-ex?searchtype=author&query=Hellwig%2C+D">D. Hellwig</a> , et al. (62 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.13431v2-abstract-short" style="display: inline;"> A $胃_{13}$ oscillation analysis based on the observed antineutrino rates at the Double Chooz far and near detectors for different reactor power conditions is presented. This approach provides a so far unique simultaneous determination of $胃_{13}$ and the total background rates without relying on any assumptions on the specific background contributions. The analysis comprises 865 days of data colle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.13431v2-abstract-full').style.display = 'inline'; document.getElementById('2007.13431v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.13431v2-abstract-full" style="display: none;"> A $胃_{13}$ oscillation analysis based on the observed antineutrino rates at the Double Chooz far and near detectors for different reactor power conditions is presented. This approach provides a so far unique simultaneous determination of $胃_{13}$ and the total background rates without relying on any assumptions on the specific background contributions. The analysis comprises 865 days of data collected in both detectors with at least one reactor in operation. The oscillation results are enhanced by the use of 24.06 days (12.74 days) of reactor-off data in the far (near) detector. The analysis considers the \nue interactions up to a visible energy of 8.5 MeV, using the events at higher energies to build a cosmogenic background model considering fast-neutrons interactions and $^{9}$Li decays. The background-model-independent determination of the mixing angle yields sin$^2(2胃_{13})=0.094\pm0.017$, being the best-fit total background rates fully consistent with the cosmogenic background model. A second oscillation analysis is also performed constraining the total background rates to the cosmogenic background estimates. While the central value is not significantly modified due to the consistency between the reactor-off data and the background estimates, the addition of the background model reduces the uncertainty on $胃_{13}$ to 0.015. Along with the oscillation results, the normalization of the anti-neutrino rate is measured with a precision of 0.86\%, reducing the 1.43\% uncertainty associated to the expectation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.13431v2-abstract-full').style.display = 'none'; document.getElementById('2007.13431v2-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 01 (2021) 190 </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/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/1802.08048">arXiv:1802.08048</a> <span> [<a href="https://arxiv.org/pdf/1802.08048">pdf</a>, <a href="https://arxiv.org/format/1802.08048">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/10.1007/JHEP11(2018)053">10.1007/JHEP11(2018)053 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Yields and production rates of cosmogenic $^9$Li and $^8$He measured with the Double Chooz near and far detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=de+Kerret%2C+H">H. de Kerret</a>, <a href="/search/hep-ex?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/hep-ex?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/hep-ex?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/hep-ex?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/hep-ex?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/hep-ex?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/hep-ex?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/hep-ex?searchtype=author&query=Corpace%2C+O">O. Corpace</a>, <a href="/search/hep-ex?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/hep-ex?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Furuta%2C+H">H. Furuta</a>, <a href="/search/hep-ex?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</a>, <a href="/search/hep-ex?searchtype=author&query=Givaudan%2C+A">A. Givaudan</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="1802.08048v3-abstract-short" style="display: inline;"> The yields and production rates of the radioisotopes $^9$Li and $^8$He created by cosmic muon spallation on $^{12}$C, have been measured by the two detectors of the Double Chooz experiment. The identical detectors are located at separate sites and depths, which means they are subject to different muon spectra. The near (far) detector has an overburden of $\sim$120 m.w.e. ($\sim$300 m.w.e.) corresp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.08048v3-abstract-full').style.display = 'inline'; document.getElementById('1802.08048v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.08048v3-abstract-full" style="display: none;"> The yields and production rates of the radioisotopes $^9$Li and $^8$He created by cosmic muon spallation on $^{12}$C, have been measured by the two detectors of the Double Chooz experiment. The identical detectors are located at separate sites and depths, which means they are subject to different muon spectra. The near (far) detector has an overburden of $\sim$120 m.w.e. ($\sim$300 m.w.e.) corresponding to a mean muon energy of $32.1\pm2.0\,\mathrm{GeV}$ ($63.7\pm5.5\,\mathrm{GeV}$). Comparing the data to a detailed simulation of the $^9$Li and $^8$He decays, the contribution of the $^8$He radioisotope at both detectors is found to be compatible with zero. The observed $^9$Li yields in the near and far detectors are $5.51\pm0.51$ and $7.90\pm0.51$, respectively, in units of $10^{-8}渭^{-1} \mathrm{g^{-1} cm^{2} }$. The shallow overburdens of the near and far detectors give a unique insight when combined with measurements by KamLAND and Borexino to give the first multi--experiment, data driven relationship between the $^9$Li yield and the mean muon energy according to the power law $Y = Y_0( <E_渭 >/ 1\,\mathrm{GeV})^{\overline伪}$, giving $\overline伪=0.72\pm0.06$ and $Y_0=(0.43\pm0.11)\times 10^{-8}渭^{-1} \mathrm{g^{-1} cm^{2}}$. This relationship gives future liquid scintillator based experiments the ability to predict their cosmogenic $^9$Li background rates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.08048v3-abstract-full').style.display = 'none'; document.getElementById('1802.08048v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">15 pages, 5 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/1710.04315">arXiv:1710.04315</a> <span> [<a href="https://arxiv.org/pdf/1710.04315">pdf</a>, <a href="https://arxiv.org/format/1710.04315">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/13/01/P01031">10.1088/1748-0221/13/01/P01031 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Novel event classification based on spectral analysis of scintillation waveforms in Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/hep-ex?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/hep-ex?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/hep-ex?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/hep-ex?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/hep-ex?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/hep-ex?searchtype=author&query=Corpace%2C+O">O. Corpace</a>, <a href="/search/hep-ex?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</a>, <a href="/search/hep-ex?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/hep-ex?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/hep-ex?searchtype=author&query=Fallot%2C+M">M. Fallot</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Furuta%2C+H">H. Furuta</a>, <a href="/search/hep-ex?searchtype=author&query=Gil-Botella%2C+I">I. Gil-Botella</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="1710.04315v3-abstract-short" style="display: inline;"> Liquid scintillators are a common choice for neutrino physics experiments, but their capabilities to perform background rejection by scintillation pulse shape discrimination is generally limited in large detectors. This paper describes a novel approach for a pulse shape based event classification developed in the context of the Double Chooz reactor antineutrino experiment. Unlike previous implemen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.04315v3-abstract-full').style.display = 'inline'; document.getElementById('1710.04315v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.04315v3-abstract-full" style="display: none;"> Liquid scintillators are a common choice for neutrino physics experiments, but their capabilities to perform background rejection by scintillation pulse shape discrimination is generally limited in large detectors. This paper describes a novel approach for a pulse shape based event classification developed in the context of the Double Chooz reactor antineutrino experiment. Unlike previous implementations, this method uses the Fourier power spectra of the scintillation pulse shapes to obtain event-wise information. A classification variable built from spectral information was able to achieve an unprecedented performance, despite the lack of optimization at the detector design level. Several examples of event classification are provided, ranging from differentiation between the detector volumes and an efficient rejection of instrumental light noise, to some sensitivity to the particle type, such as stopping muons, ortho-positronium formation, alpha particles as well as electrons and positrons. In combination with other techniques the method is expected to allow for a versatile and more efficient background rejection in the future, especially if detector optimization is taken into account at the design level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.04315v3-abstract-full').style.display = 'none'; document.getElementById('1710.04315v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">27 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation, Volume 13, Number 01 (2018) P01031 </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/1611.07845">arXiv:1611.07845</a> <span> [<a href="https://arxiv.org/pdf/1611.07845">pdf</a>, <a href="https://arxiv.org/format/1611.07845">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/10.1088/1475-7516/2017/02/017">10.1088/1475-7516/2017/02/017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic-muon characterization and annual modulation measurement with Double Chooz detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/hep-ex?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/hep-ex?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/hep-ex?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/hep-ex?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/hep-ex?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/hep-ex?searchtype=author&query=Corpace%2C+O">O. Corpace</a>, <a href="/search/hep-ex?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</a>, <a href="/search/hep-ex?searchtype=author&query=Dawson%2C+J+V">J. V. Dawson</a>, <a href="/search/hep-ex?searchtype=author&query=Dhooghe%2C+J">J. Dhooghe</a>, <a href="/search/hep-ex?searchtype=author&query=Djurcic%2C+Z">Z. Djurcic</a>, <a href="/search/hep-ex?searchtype=author&query=Dracos%2C+M">M. Dracos</a>, <a href="/search/hep-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a> , et al. (85 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1611.07845v4-abstract-short" style="display: inline;"> A study on cosmic muons has been performed for the two identical near and far neutrino detectors of the Double Chooz experiment, placed at $\sim$120 and $\sim$300 m.w.e. underground respectively, including the corresponding simulations using the MUSIC simulation package. This characterization has allowed to measure the muon flux reaching both detectors to be (3.64 $\pm$ 0.04) $\times$ 10$^{-4}$ cm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.07845v4-abstract-full').style.display = 'inline'; document.getElementById('1611.07845v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.07845v4-abstract-full" style="display: none;"> A study on cosmic muons has been performed for the two identical near and far neutrino detectors of the Double Chooz experiment, placed at $\sim$120 and $\sim$300 m.w.e. underground respectively, including the corresponding simulations using the MUSIC simulation package. This characterization has allowed to measure the muon flux reaching both detectors to be (3.64 $\pm$ 0.04) $\times$ 10$^{-4}$ cm$^{-2}$s$^{-1}$ for the near detector and (7.00 $\pm$ 0.05) $\times$ 10$^{-5}$ cm$^{-2}$s$^{-1}$ for the far one. The seasonal modulation of the signal has also been studied observing a positive correlation with the atmospheric temperature, leading to an effective temperature coefficient of $伪_{T}$ = 0.212 $\pm$ 0.024 and 0.355 $\pm$ 0.019 for the near and far detectors respectively. These measurements, in good agreement with expectations based on theoretical models, represent one of the first measurements of this coefficient in shallow depth installations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.07845v4-abstract-full').style.display = 'none'; document.getElementById('1611.07845v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Cosmology and Astroparticle Physics 02 (2017) 017 </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/1604.06895">arXiv:1604.06895</a> <span> [<a href="https://arxiv.org/pdf/1604.06895">pdf</a>, <a href="https://arxiv.org/format/1604.06895">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/11/08/P08001">10.1088/1748-0221/11/08/P08001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the Spontaneous Light Emission of the PMTs used in the Double Chooz Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Double+Chooz+collaboration"> Double Chooz collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/hep-ex?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/hep-ex?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/hep-ex?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Calvo%2C+E">E. Calvo</a>, <a href="/search/hep-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/hep-ex?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/hep-ex?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/hep-ex?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/hep-ex?searchtype=author&query=Conover%2C+E">E. Conover</a>, <a href="/search/hep-ex?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a> , et al. (124 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1604.06895v2-abstract-short" style="display: inline;"> During the commissioning of the first of the two detectors of the Double Chooz experiment, an unexpected and dominant background caused by the emission of light inside the optical volume has been observed. A specific study of the ensemble of phenomena called "Light Noise" has been carried out in-situ, and in an external laboratory, in order to characterize the signals and to identify the possible… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06895v2-abstract-full').style.display = 'inline'; document.getElementById('1604.06895v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.06895v2-abstract-full" style="display: none;"> During the commissioning of the first of the two detectors of the Double Chooz experiment, an unexpected and dominant background caused by the emission of light inside the optical volume has been observed. A specific study of the ensemble of phenomena called "Light Noise" has been carried out in-situ, and in an external laboratory, in order to characterize the signals and to identify the possible processes underlying the effect. Some mechanisms of instrumental noise originating from the PMTs were identified and it has been found that the leading one arises from the light emission localized on the photomultiplier base and produced by the combined effect of heat and high voltage across the transparent epoxy resin covering the electric components. The correlation of the rate and the amplitude of the signal with the temperature has been observed. For the first detector in operation the induced background has been mitigated using online and offline analysis selections based on timing and light pattern of the signals, while a modification of the photomultiplier assembly has been implemented for the second detector in order to blacken the PMT bases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06895v2-abstract-full').style.display = 'none'; document.getElementById('1604.06895v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 24 figures. Minor revision to be published in the Journal of Instrumentation (JINST), Corresponding author: R. Santorelli</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 11 (2016) no.08, P08001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.07562">arXiv:1512.07562</a> <span> [<a href="https://arxiv.org/pdf/1512.07562">pdf</a>, <a href="https://arxiv.org/ps/1512.07562">ps</a>, <a href="https://arxiv.org/format/1512.07562">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/PhysRevC.93.054608">10.1103/PhysRevC.93.054608 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Muon capture on light isotopes in Double Chooz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Double+Chooz+collaboration"> Double Chooz collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/hep-ex?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/hep-ex?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/hep-ex?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/hep-ex?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/hep-ex?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/hep-ex?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/hep-ex?searchtype=author&query=Conover%2C+E">E. Conover</a>, <a href="/search/hep-ex?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a> , et al. (122 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1512.07562v2-abstract-short" style="display: inline;"> Using the Double Chooz detector, designed to measure the neutrino mixing angle $胃_{13}$, the products of $渭^-$ capture on $^{12}$C, $^{13}$C, $^{14}$N and $^{16}$O have been measured. Over a period of 489.5 days, $2.3\times10^6$ stopping cosmic $渭^-$ have been collected, of which $1.8\times10^5$ captured on carbon, nitrogen, or oxygen nuclei in the inner detector scintillator or acrylic vessels. T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.07562v2-abstract-full').style.display = 'inline'; document.getElementById('1512.07562v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.07562v2-abstract-full" style="display: none;"> Using the Double Chooz detector, designed to measure the neutrino mixing angle $胃_{13}$, the products of $渭^-$ capture on $^{12}$C, $^{13}$C, $^{14}$N and $^{16}$O have been measured. Over a period of 489.5 days, $2.3\times10^6$ stopping cosmic $渭^-$ have been collected, of which $1.8\times10^5$ captured on carbon, nitrogen, or oxygen nuclei in the inner detector scintillator or acrylic vessels. The resulting isotopes were tagged using prompt neutron emission (when applicable), the subsequent beta decays, and, in some cases, $尾$-delayed neutrons. The most precise measurement of the rate of $^{12}\mathrm C(渭^-,谓)^{12}\mathrm B$ to date is reported: $6.57^{+0.11}_{-0.21}\times10^{3}\,\mathrm s^{-1}$, or $(17.35^{+0.35}_{-0.59})\%$ of nuclear captures. By tagging excited states emitting gammas, the ground state transition rate to $^{12}$B has been determined to be $5.68^{+0.14}_{-0.23}\times10^3\,\mathrm s^{-1}$. The heretofore unobserved reactions $^{12}\mathrm C(渭^-,谓伪)^{8}\mathrm{Li}$, $^{13}\mathrm C(渭^-,谓\mathrm n伪)^{8}\mathrm{Li}$, and $^{13}\mathrm C(渭^-,谓\mathrm n)^{12}\mathrm B$ are measured. Further, a population of $尾$n decays following stopping muons is identified with $5.5蟽$ significance. Statistics limit our ability to identify these decays definitively. Assuming negligible production of $^{8}$He, the reaction $^{13}\mathrm C(渭^-,谓伪)^{9}\mathrm{Li}$ is found to be present at the $2.7蟽$ level. Limits are set on a variety of other processes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.07562v2-abstract-full').style.display = 'none'; document.getElementById('1512.07562v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 14 figures. Minor revisions. Corresponding author: M. Strait</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 93, 054608 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.08937">arXiv:1510.08937</a> <span> [<a href="https://arxiv.org/pdf/1510.08937">pdf</a>, <a href="https://arxiv.org/ps/1510.08937">ps</a>, <a href="https://arxiv.org/format/1510.08937">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/10.1007/JHEP01(2016)163">10.1007/JHEP01(2016)163 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of $胃_{13}$ in Double Chooz using neutron captures on hydrogen with novel background rejection techniques </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abe%2C+Y">Y. Abe</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Abrah%C3%A3o%2C+T">T. Abrah茫o</a>, <a href="/search/hep-ex?searchtype=author&query=Almazan%2C+H">H. Almazan</a>, <a href="/search/hep-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/hep-ex?searchtype=author&query=Anjos%2C+J+C+d">J. C. dos Anjos</a>, <a href="/search/hep-ex?searchtype=author&query=Barriere%2C+J+C">J. C. Barriere</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bekman%2C+I">I. Bekman</a>, <a href="/search/hep-ex?searchtype=author&query=Bergevin%2C+M">M. Bergevin</a>, <a href="/search/hep-ex?searchtype=author&query=Bezerra%2C+T+J+C">T. J. C. Bezerra</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Blucher%2C+E">E. Blucher</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Buck%2C+C">C. Buck</a>, <a href="/search/hep-ex?searchtype=author&query=Busenitz%2C+J">J. Busenitz</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/hep-ex?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrada%2C+M">M. Cerrada</a>, <a href="/search/hep-ex?searchtype=author&query=Chauveau%2C+E">E. Chauveau</a>, <a href="/search/hep-ex?searchtype=author&query=Chimenti%2C+P">P. Chimenti</a>, <a href="/search/hep-ex?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a>, <a href="/search/hep-ex?searchtype=author&query=Conrad%2C+J+M">J. M. Conrad</a>, <a href="/search/hep-ex?searchtype=author&query=Crespo-Anad%C3%B3n%2C+J+I">J. I. Crespo-Anad贸n</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="1510.08937v2-abstract-short" style="display: inline;"> The Double Chooz collaboration presents a measurement of the neutrino mixing angle $胃_{13}$ using reactor $\overline谓_{e}$ observed via the inverse beta decay reaction in which the neutron is captured on hydrogen. This measurement is based on 462.72 live days data, approximately twice as much data as in the previous such analysis, collected with a detector positioned at an average distance of 1050… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.08937v2-abstract-full').style.display = 'inline'; document.getElementById('1510.08937v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.08937v2-abstract-full" style="display: none;"> The Double Chooz collaboration presents a measurement of the neutrino mixing angle $胃_{13}$ using reactor $\overline谓_{e}$ observed via the inverse beta decay reaction in which the neutron is captured on hydrogen. This measurement is based on 462.72 live days data, approximately twice as much data as in the previous such analysis, collected with a detector positioned at an average distance of 1050m from two reactor cores. Several novel techniques have been developed to achieve significant reductions of the backgrounds and systematic uncertainties. Accidental coincidences, the dominant background in this analysis, are suppressed by more than an order of magnitude with respect to our previous publication by a multi-variate analysis. These improvements demonstrate the capability of precise measurement of reactor $\overline谓_{e}$ without gadolinium loading. Spectral distortions from the $\overline谓_{e}$ reactor flux predictions previously reported with the neutron capture on gadolinium events are confirmed in the independent data sample presented here. A value of $\sin^{2}2胃_{13} = 0.095^{+0.038}_{-0.039}$(stat+syst) is obtained from a fit to the observed event rate as a function of the reactor power, a method insensitive to the energy spectrum shape. A simultaneous fit of the hydrogen capture events and of the gadolinium capture events yields a measurement of $\sin^{2}2胃_{13} = 0.088\pm0.033$(stat+syst). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.08937v2-abstract-full').style.display = 'none'; document.getElementById('1510.08937v2-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 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 01 (2016) 163 </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/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> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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