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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.09988">arXiv:2501.09988</a> <span> [<a href="https://arxiv.org/pdf/2501.09988">pdf</a>, <a href="https://arxiv.org/format/2501.09988">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"> Fluorescence emission of the JUNO liquid scintillator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/physics?searchtype=author&query=Houria%2C+F">F. Houria</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Caslini%2C+A">A. Caslini</a>, <a href="/search/physics?searchtype=author&query=Landini%2C+C">C. Landini</a>, <a href="/search/physics?searchtype=author&query=Lombardi%2C+P">P. Lombardi</a>, <a href="/search/physics?searchtype=author&query=Pelicci%2C+L">L. Pelicci</a>, <a href="/search/physics?searchtype=author&query=Percalli%2C+E">E. Percalli</a>, <a href="/search/physics?searchtype=author&query=Ranucci%2C+G">G. Ranucci</a>, <a href="/search/physics?searchtype=author&query=Re%2C+A+C">A. C. Re</a>, <a href="/search/physics?searchtype=author&query=Clementi%2C+C">C. Clementi</a>, <a href="/search/physics?searchtype=author&query=Ortica%2C+F">F. Ortica</a>, <a href="/search/physics?searchtype=author&query=Romani%2C+A">A. Romani</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M+G">M. G. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Miramonti%2C+L">L. Miramonti</a>, <a href="/search/physics?searchtype=author&query=Saggese%2C+P">P. Saggese</a>, <a href="/search/physics?searchtype=author&query=Torri%2C+M+D+C">M. D. C. Torri</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">A. Bergnoli</a> , et al. (43 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="2501.09988v2-abstract-short" style="display: inline;"> JUNO is a huge neutrino detector that will use 20 kton of organic liquid scintillator as its detection medium. The scintillator is a mixture of linear alkyl benzene (LAB), 2.5 g/L of 2,5-diphenyloxazole (PPO) and 3 mg/L of 1,4-Bis(2-methylstyryl)benzene (Bis-MSB). The main goal of JUNO is to determine the Neutrino Mass Ordering [1, 2, 3]. In order to achieve this purpose, good energy and position… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.09988v2-abstract-full').style.display = 'inline'; document.getElementById('2501.09988v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.09988v2-abstract-full" style="display: none;"> JUNO is a huge neutrino detector that will use 20 kton of organic liquid scintillator as its detection medium. The scintillator is a mixture of linear alkyl benzene (LAB), 2.5 g/L of 2,5-diphenyloxazole (PPO) and 3 mg/L of 1,4-Bis(2-methylstyryl)benzene (Bis-MSB). The main goal of JUNO is to determine the Neutrino Mass Ordering [1, 2, 3]. In order to achieve this purpose, good energy and position reconstruction is required, hence a complete understanding of the optical characteristics of the liquid scintillator is mandatory. In this paper we present the measurements on the JUNO scintillator emission spectrum, absorption length and fluorescence time distribution performed respectively with a spectrofluorimeter, a spectrophotometer and a custom made setup <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.09988v2-abstract-full').style.display = 'none'; document.getElementById('2501.09988v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.12901">arXiv:2406.12901</a> <span> [<a href="https://arxiv.org/pdf/2406.12901">pdf</a>, <a href="https://arxiv.org/format/2406.12901">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="Machine Learning">cs.LG</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="Data Analysis, Statistics and Probability">physics.data-an</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2024.139141">10.1016/j.physletb.2024.139141 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Interpretable machine learning approach for electron antineutrino selection in a large liquid scintillator detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Gavrikov%2C+A">A. Gavrikov</a>, <a href="/search/physics?searchtype=author&query=Cerrone%2C+V">V. Cerrone</a>, <a href="/search/physics?searchtype=author&query=Serafini%2C+A">A. Serafini</a>, <a href="/search/physics?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/physics?searchtype=author&query=Garfagnini%2C+A">A. Garfagnini</a>, <a href="/search/physics?searchtype=author&query=Grassi%2C+M">M. Grassi</a>, <a href="/search/physics?searchtype=author&query=Jelmini%2C+B">B. Jelmini</a>, <a href="/search/physics?searchtype=author&query=Lastrucci%2C+L">L. Lastrucci</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">A. Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Borghesi%2C+M">M. Borghesi</a>, <a href="/search/physics?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+R">R. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+A">A. Budano</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cammi%2C+A">A. Cammi</a>, <a href="/search/physics?searchtype=author&query=Caruso%2C+R">R. Caruso</a>, <a href="/search/physics?searchtype=author&query=Chiesa%2C+D">D. Chiesa</a>, <a href="/search/physics?searchtype=author&query=Clementi%2C+C">C. Clementi</a>, <a href="/search/physics?searchtype=author&query=Dusini%2C+S">S. Dusini</a> , et al. (43 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="2406.12901v2-abstract-short" style="display: inline;"> Several neutrino detectors, KamLAND, Daya Bay, Double Chooz, RENO, and the forthcoming large-scale JUNO, rely on liquid scintillator to detect reactor antineutrino interactions. In this context, inverse beta decay represents the golden channel for antineutrino detection, providing a pair of correlated events, thus a strong experimental signature to distinguish the signal from a variety of backgrou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12901v2-abstract-full').style.display = 'inline'; document.getElementById('2406.12901v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.12901v2-abstract-full" style="display: none;"> Several neutrino detectors, KamLAND, Daya Bay, Double Chooz, RENO, and the forthcoming large-scale JUNO, rely on liquid scintillator to detect reactor antineutrino interactions. In this context, inverse beta decay represents the golden channel for antineutrino detection, providing a pair of correlated events, thus a strong experimental signature to distinguish the signal from a variety of backgrounds. However, given the low cross-section of antineutrino interactions, the development of a powerful event selection algorithm becomes imperative to achieve effective discrimination between signal and backgrounds. In this study, we introduce a machine learning (ML) model to achieve this goal: a fully connected neural network as a powerful signal-background discriminator for a large liquid scintillator detector. We demonstrate, using the JUNO detector as an example, that, despite the already high efficiency of a cut-based approach, the presented ML model can further improve the overall event selection efficiency. Moreover, it allows for the retention of signal events at the detector edges that would otherwise be rejected because of the overwhelming amount of background events in that region. We also present the first interpretable analysis of the ML approach for event selection in reactor neutrino experiments. This method provides insights into the decision-making process of the model and offers valuable information for improving and updating traditional event selection approaches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12901v2-abstract-full').style.display = 'none'; document.getElementById('2406.12901v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </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">This is a post-peer-review, pre-copyedit version of an article published in Phys. Lett. B. The final published version is available online: https://www.sciencedirect.com/science/article/pii/S0370269324006993</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physics Letters B 860, 139141 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.01381">arXiv:2406.01381</a> <span> [<a href="https://arxiv.org/pdf/2406.01381">pdf</a>, <a href="https://arxiv.org/format/2406.01381">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"> Distillation and Stripping purification plants for JUNO liquid scintillator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Landini%2C+C">C. Landini</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/physics?searchtype=author&query=Lombardi%2C+P">P. Lombardi</a>, <a href="/search/physics?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Montuschi%2C+M">M. Montuschi</a>, <a href="/search/physics?searchtype=author&query=Parmeggiano%2C+S">S. Parmeggiano</a>, <a href="/search/physics?searchtype=author&query=Ranucci%2C+G">G. Ranucci</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M+G">M. G. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Miramonti%2C+L">L. Miramonti</a>, <a href="/search/physics?searchtype=author&query=Percalli%2C+E">E. Percalli</a>, <a href="/search/physics?searchtype=author&query=Re%2C+A+C">A. C. Re</a>, <a href="/search/physics?searchtype=author&query=Saggese%2C+P">P. Saggese</a>, <a href="/search/physics?searchtype=author&query=Torri%2C+M+D+C">M. D. C. Torri</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">A. Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Borghesi%2C+M">M. Borghesi</a>, <a href="/search/physics?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+R">R. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+A">A. Budano</a>, <a href="/search/physics?searchtype=author&query=Cammi%2C+A">A. Cammi</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.01381v1-abstract-short" style="display: inline;"> The optical and radiochemical purification of the scintillating liquid, which will fill the central detector of the JUNO experiment, plays a crucial role in achieving its scientific goals. Given its gigantic mass and dimensions and an unprecedented target value of about 3% @ 1 MeV in energy resolution, JUNO has set severe requirements on the parameters of its scintillator, such as attenuation leng… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01381v1-abstract-full').style.display = 'inline'; document.getElementById('2406.01381v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.01381v1-abstract-full" style="display: none;"> The optical and radiochemical purification of the scintillating liquid, which will fill the central detector of the JUNO experiment, plays a crucial role in achieving its scientific goals. Given its gigantic mass and dimensions and an unprecedented target value of about 3% @ 1 MeV in energy resolution, JUNO has set severe requirements on the parameters of its scintillator, such as attenuation length (Lat>20 m at 430 nm), transparency, light yield, and content of radioactive contaminants (238U,232Th<10-15 g/g). To accomplish these needs, the scintillator will be processed using several purification methods, including distillation in partial vacuum and gas stripping, which are performed in two large scale plants installed at the JUNO site. In this paper, layout, operating principles, and technical aspects which have driven the design and construction of the distil- lation and gas stripping plants are reviewed. The distillation is effective in enhancing the optical properties and removing heavy radio-impurities (238U,232Th, 40K), while the stripping process exploits pure water steam and high-purity nitrogen to extract gaseous contaminants (222Rn, 39Ar, 85Kr, O2) from the scintillator. The plant operating parameters have been tuned during the recent com- missioning phase at the JUNO site and several QA/QC measurements and tests have been performed to evaluate the performances of the plants. Some preliminary results on the efficiency of these purification processes will be shown. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01381v1-abstract-full').style.display = 'none'; document.getElementById('2406.01381v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.19879">arXiv:2405.19879</a> <span> [<a href="https://arxiv.org/pdf/2405.19879">pdf</a>, <a href="https://arxiv.org/format/2405.19879">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2024.169730">10.1016/j.nima.2024.169730 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Refractive index in the JUNO liquid scintillator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Zhang%2C+H+S">H. S. Zhang</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/physics?searchtype=author&query=Cialdi%2C+S">S. Cialdi</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+C+X">C. X. Yang</a>, <a href="/search/physics?searchtype=author&query=Huang%2C+J+H">J. H. Huang</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/physics?searchtype=author&query=Reina%2C+G">G. Reina</a>, <a href="/search/physics?searchtype=author&query=Deng%2C+Z+Y">Z. Y. Deng</a>, <a href="/search/physics?searchtype=author&query=Suerra%2C+E">E. Suerra</a>, <a href="/search/physics?searchtype=author&query=Altilia%2C+S">S. Altilia</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M+G">M. G. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Landini%2C+C">C. Landini</a>, <a href="/search/physics?searchtype=author&query=Lombardi%2C+P">P. Lombardi</a>, <a href="/search/physics?searchtype=author&query=Miramonti%2C+L">L. Miramonti</a>, <a href="/search/physics?searchtype=author&query=Percalli%2C+E">E. Percalli</a>, <a href="/search/physics?searchtype=author&query=Ranucci%2C+G">G. Ranucci</a>, <a href="/search/physics?searchtype=author&query=Re%2C+A+C">A. C. Re</a>, <a href="/search/physics?searchtype=author&query=Saggese%2C+P">P. Saggese</a>, <a href="/search/physics?searchtype=author&query=Torri%2C+M+D+C">M. D. C. Torri</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">S. Aiello</a> , et al. (51 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="2405.19879v1-abstract-short" style="display: inline;"> In the field of rare event physics, it is common to have huge masses of organic liquid scintillator as detection medium. In particular, they are widely used to study neutrino properties or astrophysical neutrinos. Thanks to its safety properties (such as low toxicity and high flash point) and easy scalability, linear alkyl benzene is the most common solvent used to produce liquid scintillators for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19879v1-abstract-full').style.display = 'inline'; document.getElementById('2405.19879v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.19879v1-abstract-full" style="display: none;"> In the field of rare event physics, it is common to have huge masses of organic liquid scintillator as detection medium. In particular, they are widely used to study neutrino properties or astrophysical neutrinos. Thanks to its safety properties (such as low toxicity and high flash point) and easy scalability, linear alkyl benzene is the most common solvent used to produce liquid scintillators for large mass experiments. The knowledge of the refractive index is a pivotal point to understand the detector response, as this quantity (and its wavelength dependence) affects the Cherenkov radiation and photon propagation in the medium. In this paper, we report the measurement of the refractive index of the JUNO liquid scintillator between 260-1064 nm performed with two different methods (an ellipsometer and a refractometer), with a sub percent level precision. In addition, we used an interferometer to measure the group velocity in the JUNO liquid scintillator and verify the expected value derived from the refractive index measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19879v1-abstract-full').style.display = 'none'; document.getElementById('2405.19879v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </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, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.17860">arXiv:2405.17860</a> <span> [<a href="https://arxiv.org/pdf/2405.17860">pdf</a>, <a href="https://arxiv.org/format/2405.17860">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/10.1088/1674-1137/ad83aa">10.1088/1674-1137/ad83aa <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prediction of Energy Resolution in the JUNO Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Adamowicz%2C+K">Kai Adamowicz</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">Marco Beretta</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">Daniel Bick</a> , et al. (629 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="2405.17860v2-abstract-short" style="display: inline;"> This paper presents an energy resolution study of the JUNO experiment, incorporating the latest knowledge acquired during the detector construction phase. The determination of neutrino mass ordering in JUNO requires an exceptional energy resolution better than 3\% at 1~MeV. To achieve this ambitious goal, significant efforts have been undertaken in the design and production of the key components o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17860v2-abstract-full').style.display = 'inline'; document.getElementById('2405.17860v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17860v2-abstract-full" style="display: none;"> This paper presents an energy resolution study of the JUNO experiment, incorporating the latest knowledge acquired during the detector construction phase. The determination of neutrino mass ordering in JUNO requires an exceptional energy resolution better than 3\% at 1~MeV. To achieve this ambitious goal, significant efforts have been undertaken in the design and production of the key components of the JUNO detector. Various factors affecting the detection of inverse beta decay signals have an impact on the energy resolution, extending beyond the statistical fluctuations of the detected number of photons, such as the properties of the liquid scintillator, performance of photomultiplier tubes, and the energy reconstruction algorithm. To account for these effects, a full JUNO simulation and reconstruction approach is employed. This enables the modeling of all relevant effects and the evaluation of associated inputs to accurately estimate the energy resolution. The results of study reveal an energy resolution of 2.95\% at 1~MeV. Furthermore, this study assesses the contribution of major effects to the overall energy resolution budget. This analysis serves as a reference for interpreting future measurements of energy resolution during JUNO data collection. Moreover, it provides a guideline for comprehending the energy resolution characteristics of liquid scintillator-based detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17860v2-abstract-full').style.display = 'none'; document.getElementById('2405.17860v2-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Chinese Phys. C 49 013003 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.12540">arXiv:2311.12540</a> <span> [<a href="https://arxiv.org/pdf/2311.12540">pdf</a>, <a href="https://arxiv.org/format/2311.12540">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjp/s13360-024-05704-z">10.1140/epjp/s13360-024-05704-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Analysis of reactor burnup simulation uncertainties for antineutrino spectrum prediction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/physics?searchtype=author&query=Borghesi%2C+M">M. Borghesi</a>, <a href="/search/physics?searchtype=author&query=Cammi%2C+A">A. Cammi</a>, <a href="/search/physics?searchtype=author&query=Chiesa%2C+D">D. Chiesa</a>, <a href="/search/physics?searchtype=author&query=Loi%2C+L">L. Loi</a>, <a href="/search/physics?searchtype=author&query=Nastasi%2C+M">M. Nastasi</a>, <a href="/search/physics?searchtype=author&query=Previtali%2C+E">E. Previtali</a>, <a href="/search/physics?searchtype=author&query=Sisti%2C+M">M. Sisti</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">A. Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/physics?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+R">R. Bruno</a>, <a href="/search/physics?searchtype=author&query=Budano%2C+A">A. Budano</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cerrone%2C+V">V. Cerrone</a>, <a href="/search/physics?searchtype=author&query=Caruso%2C+R">R. Caruso</a>, <a href="/search/physics?searchtype=author&query=Clementi%2C+C">C. Clementi</a>, <a href="/search/physics?searchtype=author&query=Dusini%2C+S">S. Dusini</a>, <a href="/search/physics?searchtype=author&query=Fabbri%2C+A">A. Fabbri</a>, <a href="/search/physics?searchtype=author&query=Felici%2C+G">G. Felici</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.12540v3-abstract-short" style="display: inline;"> Nuclear reactors are a source of electron antineutrinos due to the presence of unstable fission products that undergo $尾^-$ decay. They will be exploited by the JUNO experiment to determine the neutrino mass ordering and to get very precise measurements of the neutrino oscillation parameters. This requires the reactor antineutrino spectrum to be characterized as precisely as possible both through… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12540v3-abstract-full').style.display = 'inline'; document.getElementById('2311.12540v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.12540v3-abstract-full" style="display: none;"> Nuclear reactors are a source of electron antineutrinos due to the presence of unstable fission products that undergo $尾^-$ decay. They will be exploited by the JUNO experiment to determine the neutrino mass ordering and to get very precise measurements of the neutrino oscillation parameters. This requires the reactor antineutrino spectrum to be characterized as precisely as possible both through high resolution measurements, as foreseen by the TAO experiment, and detailed simulation models. In this paper we present a benchmark analysis utilizing Serpent Monte Carlo simulations in comparison with real pressurized water reactor spent fuel data. Our objective is to study the accuracy of fission fraction predictions as a function of different reactor simulation approximations. Then, utilizing the BetaShape software, we construct fissile antineutrino spectra using the summation method, thereby assessing the influence of simulation uncertainties on reactor antineutrino spectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12540v3-abstract-full').style.display = 'none'; document.getElementById('2311.12540v3-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. Plus 139, 952 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.11826">arXiv:2310.11826</a> <span> [<a href="https://arxiv.org/pdf/2310.11826">pdf</a>, <a href="https://arxiv.org/format/2310.11826">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.112014">10.1103/PhysRevD.109.112014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Novel techniques for alpha/beta pulse shape discrimination in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacintov%2C+A">A. Di Giacintov</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/physics?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/physics?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Andrea Ianni</a> , et al. (49 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.11826v1-abstract-short" style="display: inline;"> Borexino could efficiently distinguish between alpha and beta radiation in its liquid scintillator by the characteristic time profile of their scintillation pulse. This alpha/beta discrimination, first demonstrated at the tonne scale in the Counting Test Facility prototype, was used throughout the lifetime of the experiment between 2007 and 2021. With this method, alpha events are identified and s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11826v1-abstract-full').style.display = 'inline'; document.getElementById('2310.11826v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.11826v1-abstract-full" style="display: none;"> Borexino could efficiently distinguish between alpha and beta radiation in its liquid scintillator by the characteristic time profile of their scintillation pulse. This alpha/beta discrimination, first demonstrated at the tonne scale in the Counting Test Facility prototype, was used throughout the lifetime of the experiment between 2007 and 2021. With this method, alpha events are identified and subtracted from the beta-like solar neutrino events. This is particularly important in liquid scintillator as alpha scintillation is quenched many-fold. In Borexino, the prominent Po-210 decay peak was a background in the energy range of electrons scattered from Be-7 solar neutrinos. Optimal alpha-beta discrimination was achieved with a "multi-layer perceptron neural network", which its higher ability to leverage the timing information of the scintillation photons detected by the photomultiplier tubes. An event-by-event, high efficiency, stable, and uniform pulse shape discrimination was essential in characterising the spatial distribution of background in the detector. This benefited most Borexino measurements, including solar neutrinos in the \pp chain and the first direct observation of the CNO cycle in the Sun. This paper presents the key milestones in alpha/beta discrimination in Borexino as a term of comparison for current and future large liquid scintillator detectors <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11826v1-abstract-full').style.display = 'none'; document.getElementById('2310.11826v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109, 112014, 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.14636">arXiv:2307.14636</a> <span> [<a href="https://arxiv.org/pdf/2307.14636">pdf</a>, <a href="https://arxiv.org/format/2307.14636">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.108.102005">10.1103/PhysRevD.108.102005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Final results of Borexino on CNO solar neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/physics?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/physics?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/physics?searchtype=author&query=Ianni%2C+A">Andrea Ianni</a> , et al. (50 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.14636v1-abstract-short" style="display: inline;"> We report the first measurement of CNO solar neutrinos by Borexino that uses the Correlated Integrated Directionality (CID) method, exploiting the sub-dominant Cherenkov light in the liquid scintillator detector. The directional information of the solar origin of the neutrinos is preserved by the fast Cherenkov photons from the neutrino scattered electrons, and is used to discriminate between sign… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14636v1-abstract-full').style.display = 'inline'; document.getElementById('2307.14636v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.14636v1-abstract-full" style="display: none;"> We report the first measurement of CNO solar neutrinos by Borexino that uses the Correlated Integrated Directionality (CID) method, exploiting the sub-dominant Cherenkov light in the liquid scintillator detector. The directional information of the solar origin of the neutrinos is preserved by the fast Cherenkov photons from the neutrino scattered electrons, and is used to discriminate between signal and background. The directional information is independent from the spectral information on which the previous CNO solar neutrino measurements by Borexino were based. While the CNO spectral analysis could only be applied on the Phase-III dataset, the directional analysis can use the complete Borexino data taking period from 2007 to 2021. The absence of CNO neutrinos has been rejected with >5蟽 credible level using the Bayesian statistics. The directional CNO measurement is obtained without an external constraint on the $^{210}$Bi contamination of the liquid scintillator, which was applied in the spectral analysis approach. The final and the most precise CNO measurement of Borexino is then obtained by combining the new CID-based CNO result with an improved spectral fit of the Phase-III dataset. Including the statistical and the systematic errors, the extracted CNO interaction rate is $R(\mathrm{CNO})=6.7^{+1.2}_{-0.8} \, \mathrm{cpd/100 \, tonnes}$. Taking into account the neutrino flavor conversion, the resulting CNO neutrino flux at Earth is $桅_\mathrm{CNO}=6.7 ^{+1.2}_{-0.8} \times 10^8 \, \mathrm{cm^{-2} s^{-1}}$, in agreement with the high metallicity Standard Solar Models. The results described in this work reinforce the role of the event directional information in large-scale liquid scintillator detectors and open up new avenues for the next-generation liquid scintillator or hybrid neutrino experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14636v1-abstract-full').style.display = 'none'; document.getElementById('2307.14636v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.05172">arXiv:2303.05172</a> <span> [<a href="https://arxiv.org/pdf/2303.05172">pdf</a>, <a href="https://arxiv.org/format/2303.05172">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.nima.2023.168680">10.1016/j.nima.2023.168680 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The JUNO experiment Top Tracker </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/physics?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a> , et al. (592 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.05172v1-abstract-short" style="display: inline;"> The main task of the Top Tracker detector of the neutrino reactor experiment Jiangmen Underground Neutrino Observatory (JUNO) is to reconstruct and extrapolate atmospheric muon tracks down to the central detector. This muon tracker will help to evaluate the contribution of the cosmogenic background to the signal. The Top Tracker is located above JUNO's water Cherenkov Detector and Central Detector… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.05172v1-abstract-full').style.display = 'inline'; document.getElementById('2303.05172v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.05172v1-abstract-full" style="display: none;"> The main task of the Top Tracker detector of the neutrino reactor experiment Jiangmen Underground Neutrino Observatory (JUNO) is to reconstruct and extrapolate atmospheric muon tracks down to the central detector. This muon tracker will help to evaluate the contribution of the cosmogenic background to the signal. The Top Tracker is located above JUNO's water Cherenkov Detector and Central Detector, covering about 60% of the surface above them. The JUNO Top Tracker is constituted by the decommissioned OPERA experiment Target Tracker modules. The technology used consists in walls of two planes of plastic scintillator strips, one per transverse direction. Wavelength shifting fibres collect the light signal emitted by the scintillator strips and guide it to both ends where it is read by multianode photomultiplier tubes. Compared to the OPERA Target Tracker, the JUNO Top Tracker uses new electronics able to cope with the high rate produced by the high rock radioactivity compared to the one in Gran Sasso underground laboratory. This paper will present the new electronics and mechanical structure developed for the Top Tracker of JUNO along with its expected performance based on the current detector simulation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.05172v1-abstract-full').style.display = 'none'; document.getElementById('2303.05172v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Instrum.Meth.A 1057 (2023) 168680 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.03910">arXiv:2303.03910</a> <span> [<a href="https://arxiv.org/pdf/2303.03910">pdf</a>, <a href="https://arxiv.org/format/2303.03910">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"> JUNO sensitivity to $^7$Be, $pep$, and CNO solar neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/physics?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">Marco Beretta</a> , et al. (592 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.03910v1-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO), the first multi-kton liquid scintillator detector, which is under construction in China, will have a unique potential to perform a real-time measurement of solar neutrinos well below the few MeV threshold typical for Water Cherenkov detectors. JUNO's large target mass and excellent energy resolution are prerequisites for reaching unprecedented… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03910v1-abstract-full').style.display = 'inline'; document.getElementById('2303.03910v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.03910v1-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO), the first multi-kton liquid scintillator detector, which is under construction in China, will have a unique potential to perform a real-time measurement of solar neutrinos well below the few MeV threshold typical for Water Cherenkov detectors. JUNO's large target mass and excellent energy resolution are prerequisites for reaching unprecedented levels of precision. In this paper, we provide estimation of the JUNO sensitivity to 7Be, pep, and CNO solar neutrinos that can be obtained via a spectral analysis above the 0.45 MeV threshold. This study is performed assuming different scenarios of the liquid scintillator radiopurity, ranging from the most opti mistic one corresponding to the radiopurity levels obtained by the Borexino experiment, up to the minimum requirements needed to perform the neutrino mass ordering determination with reactor antineutrinos - the main goal of JUNO. Our study shows that in most scenarios, JUNO will be able to improve the current best measurements on 7Be, pep, and CNO solar neutrino fluxes. We also perform a study on the JUNO capability to detect periodical time variations in the solar neutrino flux, such as the day-night modulation induced by neutrino flavor regeneration in Earth, and the modulations induced by temperature changes driven by helioseismic waves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03910v1-abstract-full').style.display = 'none'; document.getElementById('2303.03910v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.10133">arXiv:2302.10133</a> <span> [<a href="https://arxiv.org/pdf/2302.10133">pdf</a>, <a href="https://arxiv.org/format/2302.10133">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2023.168339">10.1016/j.nima.2023.168339 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Implementation and performances of the IPbus protocol for the JUNO Large-PMT readout electronics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Triozzi%2C+R">Riccardo Triozzi</a>, <a href="/search/physics?searchtype=author&query=Serafini%2C+A">Andrea Serafini</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Bolognesi%2C+M">Matteo Bolognesi</a>, <a href="/search/physics?searchtype=author&query=Brugnera%2C+R">Riccardo Brugnera</a>, <a href="/search/physics?searchtype=author&query=Cerrone%2C+V">Vanessa Cerrone</a>, <a href="/search/physics?searchtype=author&query=Chen%2C+C">Chao Chen</a>, <a href="/search/physics?searchtype=author&query=Clerbaux%2C+B">Barbara Clerbaux</a>, <a href="/search/physics?searchtype=author&query=Coppi%2C+A">Alberto Coppi</a>, <a href="/search/physics?searchtype=author&query=Corti%2C+D">Daniele Corti</a>, <a href="/search/physics?searchtype=author&query=Corso%2C+F+d">Flavio dal Corso</a>, <a href="/search/physics?searchtype=author&query=Dong%2C+J">Jianmeng Dong</a>, <a href="/search/physics?searchtype=author&query=Dou%2C+W">Wei Dou</a>, <a href="/search/physics?searchtype=author&query=Fan%2C+L">Lei Fan</a>, <a href="/search/physics?searchtype=author&query=Garfagnini%2C+A">Alberto Garfagnini</a>, <a href="/search/physics?searchtype=author&query=Gavrikov%2C+A">Arsenii Gavrikov</a>, <a href="/search/physics?searchtype=author&query=Gong%2C+G">Guanghua Gong</a>, <a href="/search/physics?searchtype=author&query=Grassi%2C+M">Marco Grassi</a>, <a href="/search/physics?searchtype=author&query=Guizzetti%2C+R+M">Rosa Maria Guizzetti</a>, <a href="/search/physics?searchtype=author&query=Hang%2C+S">Shuang Hang</a>, <a href="/search/physics?searchtype=author&query=He%2C+C">Cong He</a>, <a href="/search/physics?searchtype=author&query=Hu%2C+J">Jun Hu</a>, <a href="/search/physics?searchtype=author&query=Isocrate%2C+R">Roberto Isocrate</a>, <a href="/search/physics?searchtype=author&query=Jelmini%2C+B">Beatrice Jelmini</a> , et al. (107 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.10133v1-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a large neutrino detector currently under construction in China. Thanks to the tight requirements on its optical and radio-purity properties, it will be able to perform leading measurements detecting terrestrial and astrophysical neutrinos in a wide energy range from tens of keV to hundreds of MeV. A key requirement for the success of the exp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10133v1-abstract-full').style.display = 'inline'; document.getElementById('2302.10133v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.10133v1-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a large neutrino detector currently under construction in China. Thanks to the tight requirements on its optical and radio-purity properties, it will be able to perform leading measurements detecting terrestrial and astrophysical neutrinos in a wide energy range from tens of keV to hundreds of MeV. A key requirement for the success of the experiment is an unprecedented 3% energy resolution, guaranteed by its large active mass (20 kton) and the use of more than 20,000 20-inch photo-multiplier tubes (PMTs) acquired by high-speed, high-resolution sampling electronics located very close to the PMTs. As the Front-End and Read-Out electronics is expected to continuously run underwater for 30 years, a reliable readout acquisition system capable of handling the timestamped data stream coming from the Large-PMTs and permitting to simultaneously monitor and operate remotely the inaccessible electronics had to be developed. In this contribution, the firmware and hardware implementation of the IPbus based readout protocol will be presented, together with the performances measured on final modules during the mass production of the electronics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10133v1-abstract-full').style.display = 'none'; document.getElementById('2302.10133v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.04379">arXiv:2301.04379</a> <span> [<a href="https://arxiv.org/pdf/2301.04379">pdf</a>, <a href="https://arxiv.org/format/2301.04379">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2023.168255">10.1016/j.nima.2023.168255 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mass testing of the JUNO experiment 20-inch PMTs readout electronics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Coppi%2C+A">Alberto Coppi</a>, <a href="/search/physics?searchtype=author&query=Jelmini%2C+B">Beatrice Jelmini</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Bolognesi%2C+M">Matteo Bolognesi</a>, <a href="/search/physics?searchtype=author&query=Brugnera%2C+R">Riccardo Brugnera</a>, <a href="/search/physics?searchtype=author&query=Cerrone%2C+V">Vanessa Cerrone</a>, <a href="/search/physics?searchtype=author&query=Chen%2C+C">Chao Chen</a>, <a href="/search/physics?searchtype=author&query=Clerbaux%2C+B">Barbara Clerbaux</a>, <a href="/search/physics?searchtype=author&query=Corti%2C+D">Daniele Corti</a>, <a href="/search/physics?searchtype=author&query=Corso%2C+F+d">Flavio dal Corso</a>, <a href="/search/physics?searchtype=author&query=Dong%2C+J">Jianmeng Dong</a>, <a href="/search/physics?searchtype=author&query=Dou%2C+W">Wei Dou</a>, <a href="/search/physics?searchtype=author&query=Fan%2C+L">Lei Fan</a>, <a href="/search/physics?searchtype=author&query=Garfagnini%2C+A">Alberto Garfagnini</a>, <a href="/search/physics?searchtype=author&query=Gavrikov%2C+A">Arsenii Gavrikov</a>, <a href="/search/physics?searchtype=author&query=Gong%2C+G">Guanghua Gong</a>, <a href="/search/physics?searchtype=author&query=Grassi%2C+M">Marco Grassi</a>, <a href="/search/physics?searchtype=author&query=Guizzetti%2C+R+M">Rosa Maria Guizzetti</a>, <a href="/search/physics?searchtype=author&query=Hang%2C+S">Shuang Hang</a>, <a href="/search/physics?searchtype=author&query=He%2C+C">Cong He</a>, <a href="/search/physics?searchtype=author&query=Hu%2C+J">Jun Hu</a>, <a href="/search/physics?searchtype=author&query=Isocrate%2C+R">Roberto Isocrate</a>, <a href="/search/physics?searchtype=author&query=Ji%2C+X">Xiaolu Ji</a>, <a href="/search/physics?searchtype=author&query=Jiang%2C+X">Xiaoshan Jiang</a> , et al. (107 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="2301.04379v1-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a multi-purpose, large size, liquid scintillator experiment under construction in China. JUNO will perform leading measurements detecting neutrinos from different sources (reactor, terrestrial and astrophysical neutrinos) covering a wide energy range (from 200 keV to several GeV). This paper focuses on the design and development of a test pro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04379v1-abstract-full').style.display = 'inline'; document.getElementById('2301.04379v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.04379v1-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a multi-purpose, large size, liquid scintillator experiment under construction in China. JUNO will perform leading measurements detecting neutrinos from different sources (reactor, terrestrial and astrophysical neutrinos) covering a wide energy range (from 200 keV to several GeV). This paper focuses on the design and development of a test protocol for the 20-inch PMT underwater readout electronics, performed in parallel to the mass production line. In a time period of about ten months, a total number of 6950 electronic boards were tested with an acceptance yield of 99.1%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04379v1-abstract-full').style.display = 'none'; document.getElementById('2301.04379v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.08454">arXiv:2212.08454</a> <span> [<a href="https://arxiv.org/pdf/2212.08454">pdf</a>, <a href="https://arxiv.org/format/2212.08454">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2023.168322">10.1016/j.nima.2023.168322 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Validation and integration tests of the JUNO 20-inch PMTs readout electronics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Cerrone%2C+V">Vanessa Cerrone</a>, <a href="/search/physics?searchtype=author&query=von+Sturm%2C+K">Katharina von Sturm</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Bolognesi%2C+M">Matteo Bolognesi</a>, <a href="/search/physics?searchtype=author&query=Brugnera%2C+R">Riccardo Brugnera</a>, <a href="/search/physics?searchtype=author&query=Chen%2C+C">Chao Chen</a>, <a href="/search/physics?searchtype=author&query=Clerbaux%2C+B">Barbara Clerbaux</a>, <a href="/search/physics?searchtype=author&query=Coppi%2C+A">Alberto Coppi</a>, <a href="/search/physics?searchtype=author&query=Corso%2C+F+d">Flavio dal Corso</a>, <a href="/search/physics?searchtype=author&query=Corti%2C+D">Daniele Corti</a>, <a href="/search/physics?searchtype=author&query=Dong%2C+J">Jianmeng Dong</a>, <a href="/search/physics?searchtype=author&query=Dou%2C+W">Wei Dou</a>, <a href="/search/physics?searchtype=author&query=Fan%2C+L">Lei Fan</a>, <a href="/search/physics?searchtype=author&query=Garfagnini%2C+A">Alberto Garfagnini</a>, <a href="/search/physics?searchtype=author&query=Gong%2C+G">Guanghua Gong</a>, <a href="/search/physics?searchtype=author&query=Grassi%2C+M">Marco Grassi</a>, <a href="/search/physics?searchtype=author&query=Hang%2C+S">Shuang Hang</a>, <a href="/search/physics?searchtype=author&query=Guizzetti%2C+R+M">Rosa Maria Guizzetti</a>, <a href="/search/physics?searchtype=author&query=He%2C+C">Cong He</a>, <a href="/search/physics?searchtype=author&query=Hu%2C+J">Jun Hu</a>, <a href="/search/physics?searchtype=author&query=Isocrate%2C+R">Roberto Isocrate</a>, <a href="/search/physics?searchtype=author&query=Jelmini%2C+B">Beatrice Jelmini</a>, <a href="/search/physics?searchtype=author&query=Ji%2C+X">Xiaolu Ji</a>, <a href="/search/physics?searchtype=author&query=Jiang%2C+X">Xiaoshan Jiang</a> , et al. (105 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="2212.08454v1-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a large neutrino detector currently under construction in China. JUNO will be able to study the neutrino mass ordering and to perform leading measurements detecting terrestrial and astrophysical neutrinos in a wide energy range, spanning from 200 keV to several GeV. Given the ambitious physics goals of JUNO, the electronic system has to meet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.08454v1-abstract-full').style.display = 'inline'; document.getElementById('2212.08454v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.08454v1-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a large neutrino detector currently under construction in China. JUNO will be able to study the neutrino mass ordering and to perform leading measurements detecting terrestrial and astrophysical neutrinos in a wide energy range, spanning from 200 keV to several GeV. Given the ambitious physics goals of JUNO, the electronic system has to meet specific tight requirements, and a thorough characterization is required. The present paper describes the tests performed on the readout modules to measure their performances. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.08454v1-abstract-full').style.display = 'none'; document.getElementById('2212.08454v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">20 pages, 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/2205.08830">arXiv:2205.08830</a> <span> [<a href="https://arxiv.org/pdf/2205.08830">pdf</a>, <a href="https://arxiv.org/format/2205.08830">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 Astrophysical Phenomena">astro-ph.HE</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 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/10.1088/1475-7516/2022/10/033">10.1088/1475-7516/2022/10/033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for Detecting the Diffuse Supernova Neutrino Background with JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a>, <a href="/search/physics?searchtype=author&query=Blin%2C+S">Sylvie Blin</a> , et al. (577 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="2205.08830v2-abstract-short" style="display: inline;"> We present the detection potential for the diffuse supernova neutrino background (DSNB) at the Jiangmen Underground Neutrino Observatory (JUNO), using the inverse-beta-decay (IBD) detection channel on free protons. We employ the latest information on the DSNB flux predictions, and investigate in detail the background and its reduction for the DSNB search at JUNO. The atmospheric neutrino induced n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08830v2-abstract-full').style.display = 'inline'; document.getElementById('2205.08830v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.08830v2-abstract-full" style="display: none;"> We present the detection potential for the diffuse supernova neutrino background (DSNB) at the Jiangmen Underground Neutrino Observatory (JUNO), using the inverse-beta-decay (IBD) detection channel on free protons. We employ the latest information on the DSNB flux predictions, and investigate in detail the background and its reduction for the DSNB search at JUNO. The atmospheric neutrino induced neutral current (NC) background turns out to be the most critical background, whose uncertainty is carefully evaluated from both the spread of model predictions and an envisaged \textit{in situ} measurement. We also make a careful study on the background suppression with the pulse shape discrimination (PSD) and triple coincidence (TC) cuts. With latest DSNB signal predictions, more realistic background evaluation and PSD efficiency optimization, and additional TC cut, JUNO can reach the significance of 3$蟽$ for 3 years of data taking, and achieve better than 5$蟽$ after 10 years for a reference DSNB model. In the pessimistic scenario of non-observation, JUNO would strongly improve the limits and exclude a significant region of the model parameter space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08830v2-abstract-full').style.display = 'none'; document.getElementById('2205.08830v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">29 pages, 11 figures, final published version in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 10 (2022) 033 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.08629">arXiv:2205.08629</a> <span> [<a href="https://arxiv.org/pdf/2205.08629">pdf</a>, <a href="https://arxiv.org/format/2205.08629">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-022-11002-8">10.1140/epjc/s10052-022-11002-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mass Testing and Characterization of 20-inch PMTs for JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/physics?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andre%2C+J+P+A+M">Joao Pedro Athayde Marcondes de Andre</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a> , et al. (541 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="2205.08629v2-abstract-short" style="display: inline;"> Main goal of the JUNO experiment is to determine the neutrino mass ordering using a 20kt liquid-scintillator detector. Its key feature is an excellent energy resolution of at least 3 % at 1 MeV, for which its instruments need to meet a certain quality and thus have to be fully characterized. More than 20,000 20-inch PMTs have been received and assessed by JUNO after a detailed testing program whic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08629v2-abstract-full').style.display = 'inline'; document.getElementById('2205.08629v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.08629v2-abstract-full" style="display: none;"> Main goal of the JUNO experiment is to determine the neutrino mass ordering using a 20kt liquid-scintillator detector. Its key feature is an excellent energy resolution of at least 3 % at 1 MeV, for which its instruments need to meet a certain quality and thus have to be fully characterized. More than 20,000 20-inch PMTs have been received and assessed by JUNO after a detailed testing program which began in 2017 and elapsed for about four years. Based on this mass characterization and a set of specific requirements, a good quality of all accepted PMTs could be ascertained. This paper presents the performed testing procedure with the designed testing systems as well as the statistical characteristics of all 20-inch PMTs intended to be used in the JUNO experiment, covering more than fifteen performance parameters including the photocathode uniformity. This constitutes the largest sample of 20-inch PMTs ever produced and studied in detail to date, i.e. 15,000 of the newly developed 20-inch MCP-PMTs from Northern Night Vision Technology Co. (NNVT) and 5,000 of dynode PMTs from Hamamatsu Photonics K. K.(HPK). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08629v2-abstract-full').style.display = 'none'; document.getElementById('2205.08629v2-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.11816">arXiv:2112.11816</a> <span> [<a href="https://arxiv.org/pdf/2112.11816">pdf</a>, <a href="https://arxiv.org/format/2112.11816">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.128.091803">10.1103/PhysRevLett.128.091803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Directional Measurement of sub-MeV Solar Neutrinos with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (72 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.11816v1-abstract-short" style="display: inline;"> We report the measurement of sub-MeV solar neutrinos through the use of their associated Cherenkov radiation, performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso. The measurement is achieved using a novel technique that correlates individual photon hits of events to the known position of the Sun. In an energy window between 0.54 MeV to 0.74 MeV, selected using the domin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11816v1-abstract-full').style.display = 'inline'; document.getElementById('2112.11816v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.11816v1-abstract-full" style="display: none;"> We report the measurement of sub-MeV solar neutrinos through the use of their associated Cherenkov radiation, performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso. The measurement is achieved using a novel technique that correlates individual photon hits of events to the known position of the Sun. In an energy window between 0.54 MeV to 0.74 MeV, selected using the dominant scintillation light, we have measured 10887$^{+2386}_{-2103} (\mathrm{stat.})\pm 947 (\mathrm{syst.})$ ($68\%$ confidence interval) solar neutrinos out of 19904 total events. This corresponds to a $^{7}$Be neutrino interaction rate of 51.6$^{+13.9}_{-12.5}$ counts/(day$\cdot$ 100 ton), which is in agreement with the Standard Solar Model predictions and the previous spectroscopic results of Borexino. The no-neutrino hypothesis can be excluded with $>$5$蟽$ confidence level. For the first time, we have demonstrated the possibility of utilizing the directional Cherenkov information for sub-MeV solar neutrinos, in a large-scale, high light yield liquid scintillator detector. This measurement provides an experimental proof of principle for future hybrid event reconstruction using both Cherenkov and scintillation signatures simultaneously. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11816v1-abstract-full').style.display = 'none'; document.getElementById('2112.11816v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 4 figures, short letter of arXiv:2109.04770</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.04770">arXiv:2109.04770</a> <span> [<a href="https://arxiv.org/pdf/2109.04770">pdf</a>, <a href="https://arxiv.org/format/2109.04770">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.105.052002">10.1103/PhysRevD.105.052002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Correlated and Integrated Directionality for sub-MeV solar neutrinos in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (72 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.04770v2-abstract-short" style="display: inline;"> Liquid scintillator detectors play a central role in the detection of neutrinos from various sources. In particular, it is the only technique used so far for the precision spectroscopy of sub-MeV solar neutrinos, as demonstrated by the Borexino experiment at the Gran Sasso National Laboratory in Italy. The benefit of a high light yield, and thus a low energy threshold and a good energy resolution,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.04770v2-abstract-full').style.display = 'inline'; document.getElementById('2109.04770v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.04770v2-abstract-full" style="display: none;"> Liquid scintillator detectors play a central role in the detection of neutrinos from various sources. In particular, it is the only technique used so far for the precision spectroscopy of sub-MeV solar neutrinos, as demonstrated by the Borexino experiment at the Gran Sasso National Laboratory in Italy. The benefit of a high light yield, and thus a low energy threshold and a good energy resolution, comes at the cost of the directional information featured by water Cherenkov detectors, measuring $^8$B solar neutrinos above a few MeV. In this paper we provide the first directionality measurement of sub-MeV solar neutrinos which exploits the correlation between the first few detected photons in each event and the known position of the Sun for each event. This is also the first signature of directionality in neutrinos elastically scattering off electrons in a liquid scintillator target. This measurement exploits the sub-dominant, fast Cherenkov light emission that precedes the dominant yet slower scintillation light signal. Through this measurement, we have also been able to extract the rate of $^{7}$Be solar neutrinos in Borexino. The demonstration of directional sensitivity in a traditional liquid scintillator target paves the way for the possible exploitation of the Cherenkov light signal in future kton-scale experiments using liquid scintillator targets. Directionality is important for background suppression as well as the disentanglement of signals from various sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.04770v2-abstract-full').style.display = 'none'; document.getElementById('2109.04770v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 15 Figures, revised version after comments from PRD Referees, shorter letter submitted with the title: "First Directional Measurement of sub-MeV Solar Neutrinos with Borexino"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.10973">arXiv:2106.10973</a> <span> [<a href="https://arxiv.org/pdf/2106.10973">pdf</a>, <a href="https://arxiv.org/format/2106.10973">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-021-09799-x">10.1140/epjc/s10052-021-09799-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Identification of the cosmogenic $^{11}$C background in large volumes of liquid scintillators with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacintio%2C+A">A. Di Giacintio</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.10973v2-abstract-short" style="display: inline;"> Cosmogenic radio-nuclei are an important source of background for low-energy neutrino experiments. In Borexino, cosmogenic $^{11}$C decays outnumber solar $pep$ and CNO neutrino events by about ten to one. Highly efficient identification of this background is mandatory for these neutrino analyses. We present here the details of the most consolidated strategy, used throughout Borexino solar neutrin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10973v2-abstract-full').style.display = 'inline'; document.getElementById('2106.10973v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.10973v2-abstract-full" style="display: none;"> Cosmogenic radio-nuclei are an important source of background for low-energy neutrino experiments. In Borexino, cosmogenic $^{11}$C decays outnumber solar $pep$ and CNO neutrino events by about ten to one. Highly efficient identification of this background is mandatory for these neutrino analyses. We present here the details of the most consolidated strategy, used throughout Borexino solar neutrino measurements. It hinges upon finding the space-time correlations between $^{11}$C decays, the preceding parent muons and the accompanying neutrons. This article describes the working principles and evaluates the performance of this Three-Fold Coincidence (TFC) technique in its two current implementations: a hard-cut and a likelihood-based approach. Both show stable performances throughout Borexino Phases II (2012-2016) and III (2016-2020) data sets, with a $^{11}$C tagging efficiency of $\sim$90 % and $\sim$63-66 % of the exposure surviving the tagging. We present also a novel technique that targets specifically $^{11}$C produced in high-multiplicity during major spallation events. Such $^{11}$C appear as a burst of events, whose space-time correlation can be exploited. Burst identification can be combined with the TFC to obtain about the same tagging efficiency of $\sim$90 % but with a higher fraction of the exposure surviving, in the range of $\sim$66-68 %. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10973v2-abstract-full').style.display = 'none'; document.getElementById('2106.10973v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 14 figures (but 15 files, one figure being made of 2 images), 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.13209">arXiv:2105.13209</a> <span> [<a href="https://arxiv.org/pdf/2105.13209">pdf</a>, <a href="https://arxiv.org/format/2105.13209">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> The Low Polonium Field of Borexino and its significance for the CNO neutrino detection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Kumaran%2C+S">S. Kumaran</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.13209v1-abstract-short" style="display: inline;"> Borexino is a liquid scintillator detector located at the Laboratori Nazionale del Gran Sasso, Italy with the main goal to measure solar neutrinos. The experiment recently provided the first direct experimental evidence of CNO-cycle neutrinos in the Sun, rejecting the no-CNO signal hypothesis with a significance greater than 5$蟽$ at 99\%C.L. The intrinsic $^{210}$Bi is an important background for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13209v1-abstract-full').style.display = 'inline'; document.getElementById('2105.13209v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.13209v1-abstract-full" style="display: none;"> Borexino is a liquid scintillator detector located at the Laboratori Nazionale del Gran Sasso, Italy with the main goal to measure solar neutrinos. The experiment recently provided the first direct experimental evidence of CNO-cycle neutrinos in the Sun, rejecting the no-CNO signal hypothesis with a significance greater than 5$蟽$ at 99\%C.L. The intrinsic $^{210}$Bi is an important background for this analysis due to its similar spectral shape to that of CNO neutrinos. $^{210}$Bi can be measured through its daughter $^{210}$Po which can be distinguished through an event-by-event basis via pulse shape discrimination. However, this required reducing the convective motions in the scintillator that brought additional $^{210}$Po from peripheral sources. This was made possible through the thermal insulation and stabilization campaign performed between 2015 and 2016. This article will explain the strategy and the different methods performed to extract the $^{210}$Bi upper limit in Phase-III (Jul 2016- Feb 2020) of the experiment through the analysis of $^{210}$Po in the cleanest region of the detector called the Low Polonium Field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13209v1-abstract-full').style.display = 'none'; document.getElementById('2105.13209v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to the 2021 Neutrinos session of the 55th Rencontres de Moriond</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.15115">arXiv:2006.15115</a> <span> [<a href="https://arxiv.org/pdf/2006.15115">pdf</a>, <a href="https://arxiv.org/format/2006.15115">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-020-2934-0">10.1038/s41586-020-2934-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.15115v2-abstract-short" style="display: inline;"> For most of their existence stars are fueled by the fusion of hydrogen into helium proceeding via two theoretically well understood processes, namely the $pp$ chain and the CNO cycle. Neutrinos emitted along such fusion processes in the solar core are the only direct probe of the deep interior of the star. A complete spectroscopy of neutrinos from the {\it pp} chain, producing about 99\% of the so… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.15115v2-abstract-full').style.display = 'inline'; document.getElementById('2006.15115v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.15115v2-abstract-full" style="display: none;"> For most of their existence stars are fueled by the fusion of hydrogen into helium proceeding via two theoretically well understood processes, namely the $pp$ chain and the CNO cycle. Neutrinos emitted along such fusion processes in the solar core are the only direct probe of the deep interior of the star. A complete spectroscopy of neutrinos from the {\it pp} chain, producing about 99\% of the solar energy, has already been performed \cite{bib:Nature-2018}. Here, we report the direct observation, with a high statistical significance, of neutrinos produced in the CNO cycle in the Sun. This is the first experimental evidence of this process obtained with the unprecedentedly radio-pure large-volume liquid-scintillator Borexino detector located at the underground Laboratori Nazionali del Gran Sasso in Italy. The main difficulty of this experimental effort is to identify the excess of the few counts per day per 100 tonnes of target due to CNO neutrino interactions above the backgrounds. A novel method to constrain the rate of \bi contaminating the scintillator relies on the thermal stabilisation of the detector achieved over the past 5 years. In the CNO cycle, the hydrogen fusion is catalyzed by the carbon (C) - nitrogen (N) - oxygen (O) and thus its rate, as well as the flux of emitted CNO neutrinos, directly depends on the abundance of these elements in solar core. Therefore, this result paves the way to a direct measurement of the solar metallicity by CNO neutrinos. While this result quantifies the relative contribution of the CNO fusion in the Sun to be of the order of 1\%, this process is dominant in the energy production of massive stars. The occurrence of the primary mechanism for the stellar conversion of hydrogen into helium in the Universe has been proven. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.15115v2-abstract-full').style.display = 'none'; document.getElementById('2006.15115v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">43 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-05 <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> G.3.1 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.12829">arXiv:2005.12829</a> <span> [<a href="https://arxiv.org/pdf/2005.12829">pdf</a>, <a href="https://arxiv.org/format/2005.12829">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-020-08534-2">10.1140/epjc/s10052-020-08534-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity to neutrinos from the solar CNO cycle in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (69 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.12829v3-abstract-short" style="display: inline;"> Neutrinos emitted in the carbon, nitrogen, oxygen (CNO) fusion cycle in the Sun are a sub-dominant, yet crucial component of solar neutrinos whose flux has not been measured yet. The Borexino experiment at the Laboratori Nazionali del Gran Sasso (Italy) has a unique opportunity to detect them directly thanks to the detector's radiopurity and the precise understanding of the detector backgrounds. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12829v3-abstract-full').style.display = 'inline'; document.getElementById('2005.12829v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.12829v3-abstract-full" style="display: none;"> Neutrinos emitted in the carbon, nitrogen, oxygen (CNO) fusion cycle in the Sun are a sub-dominant, yet crucial component of solar neutrinos whose flux has not been measured yet. The Borexino experiment at the Laboratori Nazionali del Gran Sasso (Italy) has a unique opportunity to detect them directly thanks to the detector's radiopurity and the precise understanding of the detector backgrounds. We discuss the sensitivity of Borexino to CNO neutrinos, which is based on the strategies we adopted to constrain the rates of the two most relevant background sources, pep neutrinos from the solar pp-chain and Bi-210 beta decays originating in the intrinsic contamination of the liquid scintillator with Pb-210. Assuming the CNO flux predicted by the high-metallicity Standard Solar Model and an exposure of 1000 daysx71.3 t, Borexino has a median sensitivity to CNO neutrino higher than 3 sigma. With the same hypothesis the expected experimental uncertainty on the CNO neutrino flux is 23%, provided the uncertainty on the independent estimate of the Bi-210 interaction rate is 1.5 cpd/100t. Finally, we evaluated the expected uncertainty of the C and N abundances and the expected discrimination significance between the high and low metallicity Standard Solar Models (HZ and LZ) with future more precise measurement of the CNO solar neutrino flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12829v3-abstract-full').style.display = 'none'; document.getElementById('2005.12829v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> BX-DocDB-674 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 80, 1091 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.02422">arXiv:1909.02422</a> <span> [<a href="https://arxiv.org/pdf/1909.02422">pdf</a>, <a href="https://arxiv.org/format/1909.02422">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Search for low-energy neutrinos from astrophysical sources with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a> , et al. (79 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.02422v1-abstract-short" style="display: inline;"> We report on searches for neutrinos and antineutrinos from astrophysical sources performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. Electron antineutrinos ($\bar谓_e$) are detected in an organic liquid scintillator through the inverse $尾$-decay reaction. In the present work we set model-independent upper limits in the energy range 1.8-16.8 MeV on neutrino flux… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02422v1-abstract-full').style.display = 'inline'; document.getElementById('1909.02422v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.02422v1-abstract-full" style="display: none;"> We report on searches for neutrinos and antineutrinos from astrophysical sources performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. Electron antineutrinos ($\bar谓_e$) are detected in an organic liquid scintillator through the inverse $尾$-decay reaction. In the present work we set model-independent upper limits in the energy range 1.8-16.8 MeV on neutrino fluxes from unknown sources that improve our previous results, on average, by a factor 2.5. Using the same data set, we first obtain experimental constraints on the diffuse supernova $\bar谓_e$ fluxes in the previously unexplored region below 8 MeV. A search for $\bar谓_e$ in the solar neutrino flux is also presented: the presence of $\bar谓_e$ would be a manifestation of a non-zero anomalous magnetic moment of the neutrino, making possible its conversion to antineutrinos in the strong magnetic field of the Sun. We obtain a limit for a solar $\bar谓_e$ flux of 384 cm$^{-2}$s$^{-1}$ (90% C.L.), assuming an undistorted solar $^{8}$B neutrinos energy spectrum, that corresponds to a transition probability $p_{ 谓_e \rightarrow \bar谓_{e}}<$ 7.2$\times$10$^{-5}$ (90% C.L.) for E$_{\bar 谓_e}$ $>$ 1.8 MeV. At lower energies, by investigating the spectral shape of elastic scattering events, we obtain a new limit on solar $^{7}$Be-$谓_e$ conversion into $\bar谓_e$ of $p_{ 谓_e \rightarrow \bar 谓_{e}}<$ 0.14 (90% C.L.) at 0.862 keV. Last, we investigate solar flares as possible neutrino sources and obtain the strongest up-to-date limits on the fluence of neutrinos of all flavor neutrino below 3-7 ,MeV. Assuming the neutrino flux to be proportional to the flare's intensity, we exclude an intense solar flare as the cause of the observed excess of events in run 117 of the Cl-Ar Homestake experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02422v1-abstract-full').style.display = 'none'; document.getElementById('1909.02422v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 8 figures, 4 tables, 73 references</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.02257">arXiv:1909.02257</a> <span> [<a href="https://arxiv.org/pdf/1909.02257">pdf</a>, <a href="https://arxiv.org/format/1909.02257">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.101.012009">10.1103/PhysRevD.101.012009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comprehensive geoneutrino analysis with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a> , et al. (87 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.02257v2-abstract-short" style="display: inline;"> This paper presents a geoneutrino measurement using 3262.74 days of data taken with the Borexino detector at LNGS in Italy. By observing $52.6 ^{+9.4}_{-8.6} ({\rm stat}) ^{+2.7}_{-2.1}({\rm sys})$ geoneutrinos (68% interval) from $^{238}$U and $^{232}$Th, a signal of $47.0^{+8.4}_{-7.7}\,({\rm stat)}^{+2.4}_{-1.9}\,({\rm sys})$ TNU with $^{+18.3}_{-17.2}$% total precision was obtained. This resul… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02257v2-abstract-full').style.display = 'inline'; document.getElementById('1909.02257v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.02257v2-abstract-full" style="display: none;"> This paper presents a geoneutrino measurement using 3262.74 days of data taken with the Borexino detector at LNGS in Italy. By observing $52.6 ^{+9.4}_{-8.6} ({\rm stat}) ^{+2.7}_{-2.1}({\rm sys})$ geoneutrinos (68% interval) from $^{238}$U and $^{232}$Th, a signal of $47.0^{+8.4}_{-7.7}\,({\rm stat)}^{+2.4}_{-1.9}\,({\rm sys})$ TNU with $^{+18.3}_{-17.2}$% total precision was obtained. This result assumes the same Th/U mass ratio found in chondritic CI meteorites but compatible results were found when contributions from $^{238}$U and $^{232}$Th were fit as free parameters. Antineutrino background from reactors is fit unconstrained and found compatible with the expectations. The null-hypothesis of observing a signal from the mantle is excluded at a 99.0% C.L. when exploiting the knowledge of the local crust. Measured mantle signal of $21.2 ^{+9.6}_{-9.0} ({\rm stat})^{+1.1}_{-0.9} ({\rm sys})$ TNU corresponds to the production of a radiogenic heat of $24.6 ^{+11.1}_{-10.4}$ TW (68% interval) from $^{238}$U and $^{232}$Th in the mantle. Assuming 18% contribution of $^{40}$K in the mantle and $8.1^{+1.9}_{-1.4}$ TW of radiogenic heat of the lithosphere, the Borexino estimate of the total Earth radiogenic heat is $38.2 ^{+13.6}_{-12.7}$ TW, corresponding to a convective Urey ratio of 0.78$^{+0.41}_{-0.28}$. These values are compatible with different geological models, however there is a 2.4$蟽$ tension with those which predict the lowest concentration of heat-producing elements. By fitting the data with a constraint on the reactor antineutrino background, the existence of a hypothetical georeactor at the center of the Earth having power greater than 2.4 TW at 95% C.L. is excluded. Particular attention is given to all analysis details, which should be of interest for the next generation geoneutrino measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02257v2-abstract-full').style.display = 'none'; document.getElementById('1909.02257v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">69 pages, 56 Figures (some composed of multiple files), 17 Tables, 135 References</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 012009 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.03512">arXiv:1905.03512</a> <span> [<a href="https://arxiv.org/pdf/1905.03512">pdf</a>, <a href="https://arxiv.org/format/1905.03512">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/JHEP02(2020)038">10.1007/JHEP02(2020)038 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on Flavor-Diagonal Non-Standard Neutrino Interactions from Borexino Phase-II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/physics?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a> , et al. (81 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1905.03512v2-abstract-short" style="display: inline;"> The Borexino detector measures solar neutrino fluxes via neutrino-electron elastic scattering. Observed spectra are determined by the solar-$谓_{e}$ survival probability $P_{ee}(E)$, and the chiral couplings of the neutrino and electron. Some theories of physics beyond the Standard Model postulate the existence of Non-Standard Interactions (NSI's) which modify the chiral couplings and $P_{ee}(E)$.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03512v2-abstract-full').style.display = 'inline'; document.getElementById('1905.03512v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.03512v2-abstract-full" style="display: none;"> The Borexino detector measures solar neutrino fluxes via neutrino-electron elastic scattering. Observed spectra are determined by the solar-$谓_{e}$ survival probability $P_{ee}(E)$, and the chiral couplings of the neutrino and electron. Some theories of physics beyond the Standard Model postulate the existence of Non-Standard Interactions (NSI's) which modify the chiral couplings and $P_{ee}(E)$. In this paper, we search for such NSI's, in particular, flavor-diagonal neutral current interactions that modify the $谓_e e$ and $谓_蟿e$ couplings using Borexino Phase II data. Standard Solar Model predictions of the solar neutrino fluxes for both high- and low-metallicity assumptions are considered. No indication of new physics is found at the level of sensitivity of the detector and constraints on the parameters of the NSI's are placed. In addition, with the same dataset the value of $\sin^2胃_W$ is obtained with a precision comparable to that achieved in reactor antineutrino experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03512v2-abstract-full').style.display = 'none'; document.getElementById('1905.03512v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 7 figures. Slight modifications in the title, abstract, and conclusion. Few references added. Text expanded for clarity. Accepted in JHEP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> IP/BBSR/2019-2 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 2002 (2020) 038 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.04207">arXiv:1808.04207</a> <span> [<a href="https://arxiv.org/pdf/1808.04207">pdf</a>, <a href="https://arxiv.org/format/1808.04207">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2019/02/046">10.1088/1475-7516/2019/02/046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modulations of the Cosmic Muon Signal in Ten Years of Borexino Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+Borexino+Collaboration"> The Borexino Collaboration</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a> , et al. (91 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1808.04207v3-abstract-short" style="display: inline;"> We have measured the flux of cosmic muons in the Laboratori Nazionali del Gran Sasso at 3800\,m\,w.e. to be $(3.432 \pm 0.003)\cdot 10^{-4}\,\mathrm{{m^{-2}s^{-1}}}$ based on ten years of Borexino data acquired between May 2007 and May 2017. A seasonal modulation with a period of $(366.3 \pm 0.6)\,\mathrm{d}$ and a relative amplitude of $(1.36 \pm0.04)\%$ is observed. The phase is measured to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.04207v3-abstract-full').style.display = 'inline'; document.getElementById('1808.04207v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.04207v3-abstract-full" style="display: none;"> We have measured the flux of cosmic muons in the Laboratori Nazionali del Gran Sasso at 3800\,m\,w.e. to be $(3.432 \pm 0.003)\cdot 10^{-4}\,\mathrm{{m^{-2}s^{-1}}}$ based on ten years of Borexino data acquired between May 2007 and May 2017. A seasonal modulation with a period of $(366.3 \pm 0.6)\,\mathrm{d}$ and a relative amplitude of $(1.36 \pm0.04)\%$ is observed. The phase is measured to be $(181.7 \pm 0.4)\,\mathrm{d}$, corresponding to a maximum at the 1$^\mathrm{st}$ of July. Using data inferred from global atmospheric models, we show the muon flux to be positively correlated with the atmospheric temperature and measure the effective temperature coefficient $伪_\mathrm{T} = 0.90 \pm 0.02$. The origin of cosmic muons from pion and kaon decays in the atmosphere allows to interpret the effective temperature coefficient as an indirect measurement of the atmospheric kaon-to-pion production ratio $r_{\mathrm{K}/蟺} = 0.11^{+0.11}_{-0.07}$ for primary energies above $18\,\mathrm{TeV}$. We find evidence for a long-term modulation of the muon flux with a period of $\sim 3000\,\mathrm{d}$ and a maximum in June 2012 that is not present in the atmospheric temperature data. A possible correlation between this modulation and the solar activity is investigated. The cosmogenic neutron production rate is found to show a seasonal modulation in phase with the cosmic muon flux but with an increased amplitude of $(2.6 \pm 0.4)\%$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.04207v3-abstract-full').style.display = 'none'; document.getElementById('1808.04207v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 16 figures, proofreading for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.11125">arXiv:1805.11125</a> <span> [<a href="https://arxiv.org/pdf/1805.11125">pdf</a>, <a href="https://arxiv.org/format/1805.11125">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/1342/1/012115">10.1088/1742-6596/1342/1/012115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Speeding up complex multivariate data analysis in Borexino with parallel computing based on Graphics Processing Unit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a> , et al. (82 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1805.11125v1-abstract-short" style="display: inline;"> A spectral fitter based on the graphics processor unit (GPU) has been developed for Borexino solar neutrino analysis. It is able to shorten the fitting time to a superior level compared to the CPU fitting procedure. In Borexino solar neutrino spectral analysis, fitting usually requires around one hour to converge since it includes time-consuming convolutions in order to account for the detector re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11125v1-abstract-full').style.display = 'inline'; document.getElementById('1805.11125v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.11125v1-abstract-full" style="display: none;"> A spectral fitter based on the graphics processor unit (GPU) has been developed for Borexino solar neutrino analysis. It is able to shorten the fitting time to a superior level compared to the CPU fitting procedure. In Borexino solar neutrino spectral analysis, fitting usually requires around one hour to converge since it includes time-consuming convolutions in order to account for the detector response and pile-up effects. Moreover, the convergence time increases to more than two days when including extra computations for the discrimination of $^{11}$C and external $纬$s. In sharp contrast, with the GPU-based fitter it takes less than 10 seconds and less than four minutes, respectively. This fitter is developed utilizing the GooFit project with customized likelihoods, pdfs and infrastructures supporting certain analysis methods. In this proceeding the design of the package, developed features and the comparison with the original CPU fitter are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11125v1-abstract-full').style.display = 'none'; document.getElementById('1805.11125v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures, proceeding for TAUP 2017 XV International Conference on Topics in Astroparticle and Underground Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> 1342 no. 012115 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Physics: Conference Series (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1704.02291">arXiv:1704.02291</a> <span> [<a href="https://arxiv.org/pdf/1704.02291">pdf</a>, <a href="https://arxiv.org/format/1704.02291">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2017.10.003">10.1016/j.astropartphys.2017.10.003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Monte Carlo simulation of the Borexino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Borodikhina%2C+L">L. Borodikhina</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a> , et al. (75 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1704.02291v1-abstract-short" style="display: inline;"> We describe the Monte Carlo (MC) simulation package of the Borexino detector and discuss the agreement of its output with data. The Borexino MC 'ab initio' simulates the energy loss of particles in all detector components and generates the resulting scintillation photons and their propagation within the liquid scintillator volume. The simulation accounts for absorption, reemission, and scattering… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.02291v1-abstract-full').style.display = 'inline'; document.getElementById('1704.02291v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.02291v1-abstract-full" style="display: none;"> We describe the Monte Carlo (MC) simulation package of the Borexino detector and discuss the agreement of its output with data. The Borexino MC 'ab initio' simulates the energy loss of particles in all detector components and generates the resulting scintillation photons and their propagation within the liquid scintillator volume. The simulation accounts for absorption, reemission, and scattering of the optical photons and tracks them until they either are absorbed or reach the photocathode of one of the photomultiplier tubes. Photon detection is followed by a comprehensive simulation of the readout electronics response. The algorithm proceeds with a detailed simulation of the electronics chain. The MC is tuned using data collected with radioactive calibration sources deployed inside and around the scintillator volume. The simulation reproduces the energy response of the detector, its uniformity within the fiducial scintillator volume relevant to neutrino physics, and the time distribution of detected photons to better than 1% between 100 keV and several MeV. The techniques developed to simulate the Borexino detector and their level of refinement are of possible interest to the neutrino community, especially for current and future large-volume liquid scintillator experiments such as Kamland-Zen, SNO+, and Juno. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.02291v1-abstract-full').style.display = 'none'; document.getElementById('1704.02291v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.06193">arXiv:1703.06193</a> <span> [<a href="https://arxiv.org/pdf/1703.06193">pdf</a>, <a href="https://arxiv.org/format/1703.06193">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/12/03/P03002">10.1088/1748-0221/12/03/P03002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Muon Counting using Silicon Photomultipliers in the AMIGA detector of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/physics?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/physics?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/physics?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/physics?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/physics?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/physics?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/physics?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/physics?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/physics?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/physics?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/physics?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/physics?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/physics?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/physics?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/physics?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/physics?searchtype=author&query=Arsene%2C+N">N. Arsene</a>, <a href="/search/physics?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/physics?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/physics?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/physics?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/physics?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a> , et al. (400 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="1703.06193v2-abstract-short" style="display: inline;"> AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory designed to extend its energy range of detection and to directly measure the muon content of the cosmic ray primary particle showers. The array will be formed by an infill of surface water-Cherenkov detectors associated with buried scintillation counters employed for muon counting. Each counter is com… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.06193v2-abstract-full').style.display = 'inline'; document.getElementById('1703.06193v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.06193v2-abstract-full" style="display: none;"> AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory designed to extend its energy range of detection and to directly measure the muon content of the cosmic ray primary particle showers. The array will be formed by an infill of surface water-Cherenkov detectors associated with buried scintillation counters employed for muon counting. Each counter is composed of three scintillation modules, with a 10 m$^2$ detection area per module. In this paper, a new generation of detectors, replacing the current multi-pixel photomultiplier tube (PMT) with silicon photo sensors (aka. SiPMs), is proposed. The selection of the new device and its front-end electronics is explained. A method to calibrate the counting system that ensures the performance of the detector is detailed. This method has the advantage of being able to be carried out in a remote place such as the one where the detectors are deployed. High efficiency results, i.e. 98 % efficiency for the highest tested overvoltage, combined with a low probability of accidental counting ($\sim$2 %), show a promising performance for this new system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.06193v2-abstract-full').style.display = 'none'; document.getElementById('1703.06193v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-656-AD-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 12 (2017) P03002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.07970">arXiv:1701.07970</a> <span> [<a href="https://arxiv.org/pdf/1701.07970">pdf</a>, <a href="https://arxiv.org/format/1701.07970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2017.04.004">10.1016/j.astropartphys.2017.04.004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Seasonal Modulation of the $^7$Be Solar Neutrino Rate in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Borodikhina%2C+L">L. Borodikhina</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a> , et al. (77 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1701.07970v2-abstract-short" style="display: inline;"> We detected the seasonal modulation of the $^7$Be neutrino interaction rate with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. The period, amplitude, and phase of the observed time evolution of the signal are consistent with its solar origin, and the absence of an annual modulation is rejected at 99.99\% C.L. The data are analyzed using three methods: the sinusoidal fi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.07970v2-abstract-full').style.display = 'inline'; document.getElementById('1701.07970v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.07970v2-abstract-full" style="display: none;"> We detected the seasonal modulation of the $^7$Be neutrino interaction rate with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. The period, amplitude, and phase of the observed time evolution of the signal are consistent with its solar origin, and the absence of an annual modulation is rejected at 99.99\% C.L. The data are analyzed using three methods: the sinusoidal fit, the Lomb-Scargle and the Empirical Mode Decomposition techniques, which all yield results in excellent agreement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.07970v2-abstract-full').style.display = 'none'; document.getElementById('1701.07970v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 palese, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.06795">arXiv:1605.06795</a> <span> [<a href="https://arxiv.org/pdf/1605.06795">pdf</a>, <a href="https://arxiv.org/format/1605.06795">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> The Main Results of the Borexino Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Muratova%2C+V">V. Muratova</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Formozov%2C+A">A. Formozov</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a> , et al. (74 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1605.06795v1-abstract-short" style="display: inline;"> The main physical results on the registration of solar neutrinos and the search for rare processes obtained by the Borexino collaboration to date are presented. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.06795v1-abstract-full" style="display: none;"> The main physical results on the registration of solar neutrinos and the search for rare processes obtained by the Borexino collaboration to date are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.06795v1-abstract-full').style.display = 'none'; document.getElementById('1605.06795v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 8 figgures, To be published as Proceedings of the Third Annual Large Hadron Collider Physics Conference, St. Petersburg, Russia, 2015</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.01625">arXiv:1605.01625</a> <span> [<a href="https://arxiv.org/pdf/1605.01625">pdf</a>, <a href="https://arxiv.org/format/1605.01625">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/10.1088/1748-0221/11/02/P02012">10.1088/1748-0221/11/02/P02012 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prototype muon detectors for the AMIGA component of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/physics?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/physics?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/physics?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/physics?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/physics?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/physics?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/physics?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/physics?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/physics?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/physics?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/physics?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/physics?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/physics?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/physics?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/physics?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/physics?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/physics?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/physics?searchtype=author&query=Arsene%2C+N">N. Arsene</a>, <a href="/search/physics?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/physics?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/physics?searchtype=author&query=Aublin%2C+J">J. Aublin</a> , et al. (429 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="1605.01625v2-abstract-short" style="display: inline;"> Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory to extend its range of detection and to directly measure the muon content of the particle showers. It consists of an infill of surface water-Cherenkov detectors accompanied by buried scintillator detectors used for muon counting. The main objectives of the AMIGA engineering array, referred to as the Unitary… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.01625v2-abstract-full').style.display = 'inline'; document.getElementById('1605.01625v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.01625v2-abstract-full" style="display: none;"> Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory to extend its range of detection and to directly measure the muon content of the particle showers. It consists of an infill of surface water-Cherenkov detectors accompanied by buried scintillator detectors used for muon counting. The main objectives of the AMIGA engineering array, referred to as the Unitary Cell, are to identify and resolve all engineering issues as well as to understand the muon-number counting uncertainties related to the design of the detector. The mechanical design, fabrication and deployment processes of the muon counters of the Unitary Cell are described in this document. These muon counters modules comprise sealed PVC casings containing plastic scintillation bars, wavelength-shifter optical fibers, 64 pixel photomultiplier tubes, and acquisition electronics. The modules are buried approximately 2.25 m below ground level in order to minimize contamination from electromagnetic shower particles. The mechanical setup, which allows access to the electronics for maintenance, is also described in addition to tests of the modules' response and integrity. The completed Unitary Cell has measured a number of air showers of which a first analysis of a sample event is included here. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.01625v2-abstract-full').style.display = 'none'; document.getElementById('1605.01625v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-164-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 11 (2016) P02012 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.02216">arXiv:1512.02216</a> <span> [<a href="https://arxiv.org/pdf/1512.02216">pdf</a>, <a href="https://arxiv.org/format/1512.02216">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/10.1088/1748-0221/11/01/P01018">10.1088/1748-0221/11/01/P01018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nanosecond-level time synchronization of autonomous radio detector stations for extensive air showers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/physics?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/physics?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/physics?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/physics?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/physics?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/physics?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/physics?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/physics?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/physics?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/physics?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/physics?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/physics?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/physics?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/physics?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/physics?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/physics?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/physics?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/physics?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/physics?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/physics?searchtype=author&query=Arsene%2C+N">N. Arsene</a>, <a href="/search/physics?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/physics?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/physics?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/physics?searchtype=author&query=Avila%2C+G">G. Avila</a> , et al. (426 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="1512.02216v2-abstract-short" style="display: inline;"> To exploit the full potential of radio measurements of cosmic-ray air showers at MHz frequencies, a detector timing synchronization within 1 ns is needed. Large distributed radio detector arrays such as the Auger Engineering Radio Array (AERA) rely on timing via the Global Positioning System (GPS) for the synchronization of individual detector station clocks. Unfortunately, GPS timing is expected… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.02216v2-abstract-full').style.display = 'inline'; document.getElementById('1512.02216v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.02216v2-abstract-full" style="display: none;"> To exploit the full potential of radio measurements of cosmic-ray air showers at MHz frequencies, a detector timing synchronization within 1 ns is needed. Large distributed radio detector arrays such as the Auger Engineering Radio Array (AERA) rely on timing via the Global Positioning System (GPS) for the synchronization of individual detector station clocks. Unfortunately, GPS timing is expected to have an accuracy no better than about 5 ns. In practice, in particular in AERA, the GPS clocks exhibit drifts on the order of tens of ns. We developed a technique to correct for the GPS drifts, and an independent method is used for cross-checks that indeed we reach nanosecond-scale timing accuracy by this correction. First, we operate a "beacon transmitter" which emits defined sine waves detected by AERA antennas recorded within the physics data. The relative phasing of these sine waves can be used to correct for GPS clock drifts. In addition to this, we observe radio pulses emitted by commercial airplanes, the position of which we determine in real time from Automatic Dependent Surveillance Broadcasts intercepted with a software-defined radio. From the known source location and the measured arrival times of the pulses we determine relative timing offsets between radio detector stations. We demonstrate with a combined analysis that the two methods give a consistent timing calibration with an accuracy of 2 ns or better. Consequently, the beacon method alone can be used in the future to continuously determine and correct for GPS clock drifts in each individual event measured by AERA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.02216v2-abstract-full').style.display = 'none'; document.getElementById('1512.02216v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">26 pages. Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-15-560-AD-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 11 (2016) P01018 11 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.01223">arXiv:1509.01223</a> <span> [<a href="https://arxiv.org/pdf/1509.01223">pdf</a>, <a href="https://arxiv.org/ps/1509.01223">ps</a>, <a href="https://arxiv.org/format/1509.01223">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.115.231802">10.1103/PhysRevLett.115.231802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A test of electric charge conservation with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Borexino+Collaboration"> Borexino Collaboration</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a> , et al. (73 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.01223v2-abstract-short" style="display: inline;"> Borexino is a liquid scintillation detector located deep underground at the Laboratori Nazionali del Gran Sasso (LNGS, Italy). Thanks to the unmatched radio-purity of the scintillator, and to the well understood detector response at low energy, a new limit on the stability of the electron for decay into a neutrino and a single mono-energetic photon was obtained. This new bound, tau > 6.6 10**28 yr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.01223v2-abstract-full').style.display = 'inline'; document.getElementById('1509.01223v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.01223v2-abstract-full" style="display: none;"> Borexino is a liquid scintillation detector located deep underground at the Laboratori Nazionali del Gran Sasso (LNGS, Italy). Thanks to the unmatched radio-purity of the scintillator, and to the well understood detector response at low energy, a new limit on the stability of the electron for decay into a neutrino and a single mono-energetic photon was obtained. This new bound, tau > 6.6 10**28 yr at 90 % C.L., is two orders of magnitude better than the previous limit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.01223v2-abstract-full').style.display = 'none'; document.getElementById('1509.01223v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 1 figure</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 115, 231802 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.05379">arXiv:1508.05379</a> <span> [<a href="https://arxiv.org/pdf/1508.05379">pdf</a>, <a href="https://arxiv.org/format/1508.05379">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nuclphysbps.2015.06.023">10.1016/j.nuclphysbps.2015.06.023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-energy (anti)neutrino physics with Borexino: Neutrinos from the primary proton-proton fusion process in the Sun </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Mosteiro%2C+P">P. Mosteiro</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a> , et al. (66 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1508.05379v1-abstract-short" style="display: inline;"> The Sun is fueled by a series of nuclear reactions that produce the energy that makes it shine. The primary reaction is the fusion of two protons into a deuteron, a positron and a neutrino. These neutrinos constitute the vast majority of neutrinos reaching Earth, providing us with key information about what goes on at the core of our star. Several experiments have now confirmed the observation of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.05379v1-abstract-full').style.display = 'inline'; document.getElementById('1508.05379v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.05379v1-abstract-full" style="display: none;"> The Sun is fueled by a series of nuclear reactions that produce the energy that makes it shine. The primary reaction is the fusion of two protons into a deuteron, a positron and a neutrino. These neutrinos constitute the vast majority of neutrinos reaching Earth, providing us with key information about what goes on at the core of our star. Several experiments have now confirmed the observation of neutrino oscillations by detecting neutrinos from secondary nuclear processes in the Sun; this is the first direct spectral measurement of the neutrinos from the keystone proton-proton fusion. This observation is a crucial step towards the completion of the spectroscopy of pp-chain neutrinos, as well as further validation of the LMA-MSW model of neutrino oscillations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.05379v1-abstract-full').style.display = 'none'; document.getElementById('1508.05379v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings from NOW (Neutrino Oscillation Workshop) 2014</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear and Particle Physics Proceedings 265-266 (2015) 87-92 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.02432">arXiv:1507.02432</a> <span> [<a href="https://arxiv.org/pdf/1507.02432">pdf</a>, <a href="https://arxiv.org/ps/1507.02432">ps</a>, <a href="https://arxiv.org/format/1507.02432">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1134/S106377961606023X">10.1134/S106377961606023X <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of neutrino flux from the primary proton--proton fusion process in the Sun with Borexino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Smirnov%2C+O+Y">O. Y. Smirnov</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a> , et al. (72 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1507.02432v1-abstract-short" style="display: inline;"> Neutrino produced in a chain of nuclear reactions in the Sun starting from the fusion of two protons, for the first time has been detected in a real-time detector in spectrometric mode. The unique properties of the Borexino detector provided an oppurtunity to disentangle pp-neutrino spectrum from the background components. A comparison of the total neutrino flux from the Sun with Solar luminosity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.02432v1-abstract-full').style.display = 'inline'; document.getElementById('1507.02432v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.02432v1-abstract-full" style="display: none;"> Neutrino produced in a chain of nuclear reactions in the Sun starting from the fusion of two protons, for the first time has been detected in a real-time detector in spectrometric mode. The unique properties of the Borexino detector provided an oppurtunity to disentangle pp-neutrino spectrum from the background components. A comparison of the total neutrino flux from the Sun with Solar luminosity in photons provides a test of the stability of the Sun on the 10$^{5}$ years time scale, and sets a strong limit on the power production in the unknown energy sources in the Sun of no more than 4\% of the total energy production at 90\% C.L. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.02432v1-abstract-full').style.display = 'none'; document.getElementById('1507.02432v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 2 tables, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1506.04610">arXiv:1506.04610</a> <span> [<a href="https://arxiv.org/pdf/1506.04610">pdf</a>, <a href="https://arxiv.org/format/1506.04610">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.92.031101">10.1103/PhysRevD.92.031101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopy of geo-neutrinos from 2056 days of Borexino data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Borexino+collaboration"> Borexino collaboration</a>, <a href="/search/physics?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/physics?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/physics?searchtype=author&query=DAngelo%2C+D">D. DAngelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/physics?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fiorentini%2C+G">G. Fiorentini</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gabriele%2C+F">F. Gabriele</a> , et al. (77 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1506.04610v2-abstract-short" style="display: inline;"> We report an improved geo-neutrino measurement with Borexino from 2056 days of data taking. The present exposure is $(5.5\pm0.3)\times10^{31}$ proton$\times$yr. Assuming a chondritic Th/U mass ratio of 3.9, we obtain $23.7 ^{+6.5}_{-5.7} (stat) ^{+0.9}_{-0.6} (sys)$ geo-neutrino events. The null observation of geo-neutrinos with Borexino alone has a probability of $3.6 \times 10^{-9}$ (5.9$蟽$). A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.04610v2-abstract-full').style.display = 'inline'; document.getElementById('1506.04610v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.04610v2-abstract-full" style="display: none;"> We report an improved geo-neutrino measurement with Borexino from 2056 days of data taking. The present exposure is $(5.5\pm0.3)\times10^{31}$ proton$\times$yr. Assuming a chondritic Th/U mass ratio of 3.9, we obtain $23.7 ^{+6.5}_{-5.7} (stat) ^{+0.9}_{-0.6} (sys)$ geo-neutrino events. The null observation of geo-neutrinos with Borexino alone has a probability of $3.6 \times 10^{-9}$ (5.9$蟽$). A geo-neutrino signal from the mantle is obtained at 98\% C.L. The radiogenic heat production for U and Th from the present best-fit result is restricted to the range 23-36 TW, taking into account the uncertainty on the distribution of heat producing elements inside the Earth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.04610v2-abstract-full').style.display = 'none'; document.getElementById('1506.04610v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 92, 031101 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1410.0779">arXiv:1410.0779</a> <span> [<a href="https://arxiv.org/pdf/1410.0779">pdf</a>, <a href="https://arxiv.org/format/1410.0779">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1134/S1063779615020185">10.1134/S1063779615020185 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solar neutrino with Borexino: results and perspectives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Smirnov%2C+O">O. Smirnov</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Fiorentini%2C+G">G. Fiorentini</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1410.0779v1-abstract-short" style="display: inline;"> Borexino is a unique detector able to perform measurement of solar neutrinos fluxes in the energy region around 1 MeV or below due to its low level of radioactive background. It was constructed at the LNGS underground laboratory with a goal of solar $^{7}$Be neutrino flux measurement with 5\% precision. The goal has been successfully achieved marking the end of the first stage of the experiment. A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.0779v1-abstract-full').style.display = 'inline'; document.getElementById('1410.0779v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.0779v1-abstract-full" style="display: none;"> Borexino is a unique detector able to perform measurement of solar neutrinos fluxes in the energy region around 1 MeV or below due to its low level of radioactive background. It was constructed at the LNGS underground laboratory with a goal of solar $^{7}$Be neutrino flux measurement with 5\% precision. The goal has been successfully achieved marking the end of the first stage of the experiment. A number of other important measurements of solar neutrino fluxes have been performed during the first stage. Recently the collaboration conducted successful liquid scintillator repurification campaign aiming to reduce main contaminants in the sub-MeV energy range. With the new levels of radiopurity Borexino can improve existing and challenge a number of new measurements including: improvement of the results on the Solar and terrestrial neutrino fluxes measurements; measurement of pp and CNO solar neutrino fluxes; search for non-standard interactions of neutrino; study of the neutrino oscillations on the short baseline with an artificial neutrino source (search for sterile neutrino) in context of SOX project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.0779v1-abstract-full').style.display = 'none'; document.getElementById('1410.0779v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.7919">arXiv:1405.7919</a> <span> [<a href="https://arxiv.org/pdf/1405.7919">pdf</a>, <a href="https://arxiv.org/format/1405.7919">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Recent Borexino results and prospects for the near future </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=von+Feilitzsch%2C+F">F. von Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">A. Goretti</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1405.7919v1-abstract-short" style="display: inline;"> The Borexino experiment, located in the Gran Sasso National Laboratory, is an organic liquid scintillator detector conceived for the real time spectroscopy of low energy solar neutrinos. The data taking campaign phase I (2007 - 2010) has allowed the first independent measurements of 7Be, 8B and pep fluxes as well as the first measurement of anti-neutrinos from the earth. After a purification of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.7919v1-abstract-full').style.display = 'inline'; document.getElementById('1405.7919v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.7919v1-abstract-full" style="display: none;"> The Borexino experiment, located in the Gran Sasso National Laboratory, is an organic liquid scintillator detector conceived for the real time spectroscopy of low energy solar neutrinos. The data taking campaign phase I (2007 - 2010) has allowed the first independent measurements of 7Be, 8B and pep fluxes as well as the first measurement of anti-neutrinos from the earth. After a purification of the scintillator, Borexino is now in phase II since 2011. We review here the recent results achieved during 2013, concerning the seasonal modulation in the 7Be signal, the study of cosmogenic backgrounds and the updated measurement of geo-neutrinos. We also review the upcoming measurements from phase II data (pp, pep, CNO) and the project SOX devoted to the study of sterile neutrinos via the use of a 51Cr neutrino source and a 144Ce-144Pr antineutrino source placed in close proximity of the active material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.7919v1-abstract-full').style.display = 'none'; document.getElementById('1405.7919v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 11 figures. To be published as proceedings of Rencontres de Moriond EW 2014</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1308.0443">arXiv:1308.0443</a> <span> [<a href="https://arxiv.org/pdf/1308.0443">pdf</a>, <a href="https://arxiv.org/format/1308.0443">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.89.112007">10.1103/PhysRevD.89.112007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Final results of Borexino Phase-I on low energy solar neutrino spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Borexino+Collaboration"> Borexino Collaboration</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Avanzini%2C+M+B">M. B. Avanzini</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1308.0443v2-abstract-short" style="display: inline;"> Borexino has been running since May 2007 at the LNGS with the primary goal of detecting solar neutrinos. The detector, a large, unsegmented liquid scintillator calorimeter characterized by unprecedented low levels of intrinsic radioactivity, is optimized for the study of the lower energy part of the spectrum. During the Phase-I (2007-2010) Borexino first detected and then precisely measured the fl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.0443v2-abstract-full').style.display = 'inline'; document.getElementById('1308.0443v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1308.0443v2-abstract-full" style="display: none;"> Borexino has been running since May 2007 at the LNGS with the primary goal of detecting solar neutrinos. The detector, a large, unsegmented liquid scintillator calorimeter characterized by unprecedented low levels of intrinsic radioactivity, is optimized for the study of the lower energy part of the spectrum. During the Phase-I (2007-2010) Borexino first detected and then precisely measured the flux of the 7Be solar neutrinos, ruled out any significant day-night asymmetry of their interaction rate, made the first direct observation of the pep neutrinos, and set the tightest upper limit on the flux of CNO neutrinos. In this paper we discuss the signal signature and provide a comprehensive description of the backgrounds, quantify their event rates, describe the methods for their identification, selection or subtraction, and describe data analysis. Key features are an extensive in situ calibration program using radioactive sources, the detailed modeling of the detector response, the ability to define an innermost fiducial volume with extremely low background via software cuts, and the excellent pulse-shape discrimination capability of the scintillator that allows particle identification. We report a measurement of the annual modulation of the 7 Be neutrino interaction rate. The period, the amplitude, and the phase of the observed modulation are consistent with the solar origin of these events, and the absence of their annual modulation is rejected with higher than 99% C.L. The physics implications of phase-I results in the context of the neutrino oscillation physics and solar models are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.0443v2-abstract-full').style.display = 'none'; document.getElementById('1308.0443v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 89, 112007 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1304.7381">arXiv:1304.7381</a> <span> [<a href="https://arxiv.org/pdf/1304.7381">pdf</a>, <a href="https://arxiv.org/format/1304.7381">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2013/08/049">10.1088/1475-7516/2013/08/049 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmogenic Backgrounds in Borexino at 3800 m water-equivalent depth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=G%C3%B6ger-Neff%2C+M">M. G枚ger-Neff</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">A. Goretti</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1304.7381v2-abstract-short" style="display: inline;"> The solar neutrino experiment Borexino, which is located in the Gran Sasso underground laboratories, is in a unique position to study muon-induced backgrounds in an organic liquid scintillator. In this study, a large sample of cosmic muons is identified and tracked by a muon veto detector external to the liquid scintillator, and by the specific light patterns observed when muons cross the scintill… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.7381v2-abstract-full').style.display = 'inline'; document.getElementById('1304.7381v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1304.7381v2-abstract-full" style="display: none;"> The solar neutrino experiment Borexino, which is located in the Gran Sasso underground laboratories, is in a unique position to study muon-induced backgrounds in an organic liquid scintillator. In this study, a large sample of cosmic muons is identified and tracked by a muon veto detector external to the liquid scintillator, and by the specific light patterns observed when muons cross the scintillator volume. The yield of muon-induced neutrons is found to be Yn =(3.10+-0.11)10-4 n/(渭 (g/cm2)). The distance profile between the parent muon track and the neutron capture point has the average value 位 = (81.5 +- 2.7)cm. Additionally the yields of a number of cosmogenic radioisotopes are measured for 12N, 12B, 8He, 9C, 9Li, 8B, 6He, 8Li, 11Be, 10C and 11C. All results are compared with Monte Carlo simulation predictions using the Fluka and Geant4 packages. General agreement between data and simulation is observed for the cosmogenic production yields with a few exceptions, the most prominent case being 11C yield for which both codes return about 50% lower values. The predicted 渭-n distance profile and the neutron multiplicity distribution are found to be overall consistent with data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.7381v2-abstract-full').style.display = 'none'; document.getElementById('1304.7381v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 13 figures (in 14 files), 4 tables. 3 extra data files. accepted by JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1303.2571">arXiv:1303.2571</a> <span> [<a href="https://arxiv.org/pdf/1303.2571">pdf</a>, <a href="https://arxiv.org/format/1303.2571">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2013.04.030">10.1016/j.physletb.2013.04.030 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of geo-neutrinos from 1353 days of Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Empl%2C+A">A. Empl</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fiorentini%2C+G">G. Fiorentini</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1303.2571v2-abstract-short" style="display: inline;"> We present a measurement of the geo--neutrino signal obtained from 1353 days of data with the Borexino detector at Laboratori Nazionali del Gran Sasso in Italy. With a fiducial exposure of (3.69 $\pm$ 0.16) $\times$ $10^{31}$ proton $\times$ year after all selection cuts and background subtraction, we detected (14.3 $\pm$ 4.4) geo-neutrino events assuming a fixed chondritic mass Th/U ratio of 3.9.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1303.2571v2-abstract-full').style.display = 'inline'; document.getElementById('1303.2571v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1303.2571v2-abstract-full" style="display: none;"> We present a measurement of the geo--neutrino signal obtained from 1353 days of data with the Borexino detector at Laboratori Nazionali del Gran Sasso in Italy. With a fiducial exposure of (3.69 $\pm$ 0.16) $\times$ $10^{31}$ proton $\times$ year after all selection cuts and background subtraction, we detected (14.3 $\pm$ 4.4) geo-neutrino events assuming a fixed chondritic mass Th/U ratio of 3.9. This corresponds to a geo-neutrino signal $S_{geo}$ = (38.8 $\pm$ 12.0) TNU with just a 6 $\times$ $10^{-6}$ probability for a null geo-neutrino measurement. With U and Th left as free parameters in the fit, the relative signals are $S_{\mathrm{Th}}$ = (10.6 $\pm$ 12.7) TNU and $S_\mathrm{U}$ = (26.5 $\pm$ 19.5) TNU. Borexino data alone are compatible with a mantle geo--neutrino signal of (15.4 $\pm$ 12.3) TNU, while a combined analysis with the KamLAND data allows to extract a mantle signal of (14.1 $\pm$ 8.1) TNU. Our measurement of a reactor anti--neutrino signal $S_{react}$ = 84.5$^{+19.3}_{-18.9}$ TNU is in agreement with expectations in the presence of neutrino oscillations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1303.2571v2-abstract-full').style.display = 'none'; document.getElementById('1303.2571v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 March, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Lett. B 722 (2013) 295-300 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1212.1332">arXiv:1212.1332</a> <span> [<a href="https://arxiv.org/pdf/1212.1332">pdf</a>, <a href="https://arxiv.org/ps/1212.1332">ps</a>, <a href="https://arxiv.org/format/1212.1332">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 - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</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"> Lifetime measurements of 214Po and 212Po with the CTF liquid scintillator detector at LNGS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Borexino+Collaboration"> Borexino Collaboration</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Carraro%2C+C">C. Carraro</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=Chubakov%2C+V">V. Chubakov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a> , et al. (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="1212.1332v2-abstract-short" style="display: inline;"> We have studied the alpha decays of 214Po into 210Pb and of 212Po into 208Pb tagged by the coincidence with the preceding beta decays from 214Bi and 212Bi, respectively. The employed 222Rn, 232Th, and 220Rn sources were sealed inside quartz vials and inserted in the Counting Test Facility at the underground Gran Sasso National Laboratory in Italy. We find that the mean lifetime of 214Po is (236.00… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.1332v2-abstract-full').style.display = 'inline'; document.getElementById('1212.1332v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1212.1332v2-abstract-full" style="display: none;"> We have studied the alpha decays of 214Po into 210Pb and of 212Po into 208Pb tagged by the coincidence with the preceding beta decays from 214Bi and 212Bi, respectively. The employed 222Rn, 232Th, and 220Rn sources were sealed inside quartz vials and inserted in the Counting Test Facility at the underground Gran Sasso National Laboratory in Italy. We find that the mean lifetime of 214Po is (236.00 +- 0.42(stat) +- 0.15(syst)) 渭s and that of 212Po is (425.1 +- 0.9(stat) +- 1.2(syst)) ns. Our results, obtained from data with signal-to-background ratio larger than 1000, reduce the overall uncertainties and are compatible with previous measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.1332v2-abstract-full').style.display = 'none'; document.getElementById('1212.1332v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 December, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">RevTex, 11 pages, 5 figures, 3 tables. This second version matches the one accepted for publication in EPJA: minor stylistic changes plus a discussion of calibration of TDC time scale</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.4816">arXiv:1207.4816</a> <span> [<a href="https://arxiv.org/pdf/1207.4816">pdf</a>, <a href="https://arxiv.org/format/1207.4816">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/7/10/P10018">10.1088/1748-0221/7/10/P10018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Borexino calibrations: Hardware, Methods, and Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Borexino+collaboration"> Borexino collaboration</a>, <a href="/search/physics?searchtype=author&query=Back%2C+H">H. Back</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Carraro%2C+C">C. Carraro</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=von+Feilitzsch%2C+F">F. von Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fernandes%2C+G">G. Fernandes</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a> , 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="1207.4816v2-abstract-short" style="display: inline;"> Borexino was the first experiment to detect solar neutrinos in real-time in the sub-MeV region. In order to achieve high precision in the determination of neutrino rates, the detector design includes an internal and an external calibration system. This paper describes both calibration systems and the calibration campaigns that were carried out in the period between 2008 and 2011. We discuss some o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.4816v2-abstract-full').style.display = 'inline'; document.getElementById('1207.4816v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.4816v2-abstract-full" style="display: none;"> Borexino was the first experiment to detect solar neutrinos in real-time in the sub-MeV region. In order to achieve high precision in the determination of neutrino rates, the detector design includes an internal and an external calibration system. This paper describes both calibration systems and the calibration campaigns that were carried out in the period between 2008 and 2011. We discuss some of the results and show that the calibration procedures preserved the radiopurity of the scintillator. The calibrations provided a detailed understanding of the detector response and led to a significant reduction of the systematic uncertainties in the Borexino measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.4816v2-abstract-full').style.display = 'none'; document.getElementById('1207.4816v2-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 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 7 (2012) P10018 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.0591">arXiv:1207.0591</a> <span> [<a href="https://arxiv.org/pdf/1207.0591">pdf</a>, <a href="https://arxiv.org/format/1207.0591">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"> GPS-based CERN-LNGS time link for Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Cerretto%2C+G">G. Cerretto</a>, <a href="/search/physics?searchtype=author&query=Esteban%2C+H">H. Esteban</a>, <a href="/search/physics?searchtype=author&query=Korga%2C+G">G. Korga</a>, <a href="/search/physics?searchtype=author&query=Misiaszek%2C+M">M. Misiaszek</a>, <a href="/search/physics?searchtype=author&query=Orsini%2C+M">M. Orsini</a>, <a href="/search/physics?searchtype=author&query=Pallavicini%2C+M">M. Pallavicini</a>, <a href="/search/physics?searchtype=author&query=Pettiti%2C+V">V. Pettiti</a>, <a href="/search/physics?searchtype=author&query=Plantard%2C+C">C. Plantard</a>, <a href="/search/physics?searchtype=author&query=Razeto%2C+A">A. Razeto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1207.0591v2-abstract-short" style="display: inline;"> We describe the design, the equipment, and the calibration of a new GPS based time link between CERN and the Borexino experiment at the Gran Sasso Laboratory in Italy. This system has been installed and operated in Borexino since March 2012, and used for a precise measurement of CNGS muon neutrinos speed in May 2012. The result of the measurement will be reported in a different letter. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.0591v2-abstract-full" style="display: none;"> We describe the design, the equipment, and the calibration of a new GPS based time link between CERN and the Borexino experiment at the Gran Sasso Laboratory in Italy. This system has been installed and operated in Borexino since March 2012, and used for a precise measurement of CNGS muon neutrinos speed in May 2012. The result of the measurement will be reported in a different letter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.0591v2-abstract-full').style.display = 'none'; document.getElementById('1207.0591v2-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 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1202.6403">arXiv:1202.6403</a> <span> [<a href="https://arxiv.org/pdf/1202.6403">pdf</a>, <a href="https://arxiv.org/format/1202.6403">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Atmospheric and Oceanic Physics">physics.ao-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2012/05/015">10.1088/1475-7516/2012/05/015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic-muon flux and annual modulation in Borexino at 3800 m water-equivalent depth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/physics?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/physics?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Carraro%2C+C">C. Carraro</a>, <a href="/search/physics?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=von+Feilitzsch%2C+F">F. von Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1202.6403v3-abstract-short" style="display: inline;"> We have measured the muon flux at the underground Gran Sasso National Laboratory (3800 m w.e.) to be (3.41 \pm 0.01) \times 10-4m-2s-1 using four years of Borexino data. A modulation of this signal is observed with a period of (366\pm3) days and a relative amplitude of (1.29 \pm 0.07)%. The measured phase is (179 \pm 6) days, corresponding to a maximum on the 28th of June. Using the most complete… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.6403v3-abstract-full').style.display = 'inline'; document.getElementById('1202.6403v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.6403v3-abstract-full" style="display: none;"> We have measured the muon flux at the underground Gran Sasso National Laboratory (3800 m w.e.) to be (3.41 \pm 0.01) \times 10-4m-2s-1 using four years of Borexino data. A modulation of this signal is observed with a period of (366\pm3) days and a relative amplitude of (1.29 \pm 0.07)%. The measured phase is (179 \pm 6) days, corresponding to a maximum on the 28th of June. Using the most complete atmospheric data models available, muon rate fluctuations are shown to be positively correlated with atmospheric temperature, with an effective coefficient 伪T = 0.93 \pm 0.04. This result represents the most precise study of the muon flux modulation for this site and is in good agreement with expectations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.6403v3-abstract-full').style.display = 'none'; document.getElementById('1202.6403v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures, published on JCAP as JCAP05(2012)015 on May 15th 2012</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP05(2012)015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1101.3101">arXiv:1101.3101</a> <span> [<a href="https://arxiv.org/pdf/1101.3101">pdf</a>, <a href="https://arxiv.org/format/1101.3101">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/6/05/P05005">10.1088/1748-0221/6/05/P05005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Muon and Cosmogenic Neutron Detection in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Borexino+Collaboration"> Borexino Collaboration</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/physics?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/physics?searchtype=author&query=Bonetti%2C+S">S. Bonetti</a>, <a href="/search/physics?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/physics?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/physics?searchtype=author&query=Cadonati%2C+L">L. Cadonati</a>, <a href="/search/physics?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/physics?searchtype=author&query=Carraro%2C+C">C. Carraro</a>, <a href="/search/physics?searchtype=author&query=Chavarria%2C+A">A. Chavarria</a>, <a href="/search/physics?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/physics?searchtype=author&query=von+Feilitzsch%2C+F">F. von Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fomenko%2C+K">K. Fomenko</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/physics?searchtype=author&query=Gazzana%2C+S">S. Gazzana</a>, <a href="/search/physics?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/physics?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/physics?searchtype=author&query=Goeger-Neff%2C+M">M. Goeger-Neff</a>, <a href="/search/physics?searchtype=author&query=Goretti%2C+A">A. Goretti</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1101.3101v2-abstract-short" style="display: inline;"> Borexino, a liquid scintillator detector at LNGS, is designed for the detection of neutrinos and antineutrinos from the Sun, supernovae, nuclear reactors, and the Earth. The feeble nature of these signals requires a strong suppression of backgrounds below a few MeV. Very low intrinsic radiogenic contamination of all detector components needs to be accompanied by the efficient identification of muo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.3101v2-abstract-full').style.display = 'inline'; document.getElementById('1101.3101v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1101.3101v2-abstract-full" style="display: none;"> Borexino, a liquid scintillator detector at LNGS, is designed for the detection of neutrinos and antineutrinos from the Sun, supernovae, nuclear reactors, and the Earth. The feeble nature of these signals requires a strong suppression of backgrounds below a few MeV. Very low intrinsic radiogenic contamination of all detector components needs to be accompanied by the efficient identification of muons and of muon-induced backgrounds. Muons produce unstable nuclei by spallation processes along their trajectory through the detector whose decays can mimic the expected signals; for isotopes with half-lives longer than a few seconds, the dead time induced by a muon-related veto becomes unacceptably long, unless its application can be restricted to a sub-volume along the muon track. Consequently, not only the identification of muons with very high efficiency but also a precise reconstruction of their tracks is of primary importance for the physics program of the experiment. The Borexino inner detector is surrounded by an outer water-Cherenkov detector that plays a fundamental role in accomplishing this task. The detector design principles and their implementation are described. The strategies adopted to identify muons are reviewed and their efficiency is evaluated. The overall muon veto efficiency is found to be 99.992% or better. Ad-hoc track reconstruction algorithms developed are presented. Their performance is tested against muon events of known direction such as those from the CNGS neutrino beam, test tracks available from a dedicated External Muon Tracker and cosmic muons whose angular distribution reflects the local overburden profile. The achieved angular resolution is 3-5 deg and the lateral resolution is 35-50 cm, depending on the impact parameter of the crossing muon. The methods implemented to efficiently tag cosmogenic neutrons are also presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.3101v2-abstract-full').style.display = 'none'; document.getElementById('1101.3101v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 February, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 January, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2011. </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">42 pages. 32 figures on 37 files. Uses JINST.cls. 1 auxiliary file (defines.tex) with TEX macros. submitted to Journal of Instrumentation</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 6:P05005,2011 </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 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