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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/hep-ex?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/hep-ex?searchtype=author&query=Houria%2C+F">F. Houria</a>, <a href="/search/hep-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Caslini%2C+A">A. Caslini</a>, <a href="/search/hep-ex?searchtype=author&query=Landini%2C+C">C. Landini</a>, <a href="/search/hep-ex?searchtype=author&query=Lombardi%2C+P">P. Lombardi</a>, <a href="/search/hep-ex?searchtype=author&query=Pelicci%2C+L">L. Pelicci</a>, <a href="/search/hep-ex?searchtype=author&query=Percalli%2C+E">E. Percalli</a>, <a href="/search/hep-ex?searchtype=author&query=Ranucci%2C+G">G. Ranucci</a>, <a href="/search/hep-ex?searchtype=author&query=Re%2C+A+C">A. C. Re</a>, <a href="/search/hep-ex?searchtype=author&query=Clementi%2C+C">C. Clementi</a>, <a href="/search/hep-ex?searchtype=author&query=Ortica%2C+F">F. Ortica</a>, <a href="/search/hep-ex?searchtype=author&query=Romani%2C+A">A. Romani</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M+G">M. G. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Miramonti%2C+L">L. Miramonti</a>, <a href="/search/hep-ex?searchtype=author&query=Saggese%2C+P">P. Saggese</a>, <a href="/search/hep-ex?searchtype=author&query=Torri%2C+M+D+C">M. D. C. Torri</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Gavrikov%2C+A">A. Gavrikov</a>, <a href="/search/hep-ex?searchtype=author&query=Cerrone%2C+V">V. Cerrone</a>, <a href="/search/hep-ex?searchtype=author&query=Serafini%2C+A">A. Serafini</a>, <a href="/search/hep-ex?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/hep-ex?searchtype=author&query=Garfagnini%2C+A">A. Garfagnini</a>, <a href="/search/hep-ex?searchtype=author&query=Grassi%2C+M">M. Grassi</a>, <a href="/search/hep-ex?searchtype=author&query=Jelmini%2C+B">B. Jelmini</a>, <a href="/search/hep-ex?searchtype=author&query=Lastrucci%2C+L">L. Lastrucci</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/hep-ex?searchtype=author&query=Bergnoli%2C+A">A. Bergnoli</a>, <a href="/search/hep-ex?searchtype=author&query=Borghesi%2C+M">M. Borghesi</a>, <a href="/search/hep-ex?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/hep-ex?searchtype=author&query=Bruno%2C+R">R. Bruno</a>, <a href="/search/hep-ex?searchtype=author&query=Budano%2C+A">A. Budano</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Cammi%2C+A">A. Cammi</a>, <a href="/search/hep-ex?searchtype=author&query=Caruso%2C+R">R. Caruso</a>, <a href="/search/hep-ex?searchtype=author&query=Chiesa%2C+D">D. Chiesa</a>, <a href="/search/hep-ex?searchtype=author&query=Clementi%2C+C">C. Clementi</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Landini%2C+C">C. Landini</a>, <a href="/search/hep-ex?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/hep-ex?searchtype=author&query=Lombardi%2C+P">P. Lombardi</a>, <a href="/search/hep-ex?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/hep-ex?searchtype=author&query=Montuschi%2C+M">M. Montuschi</a>, <a href="/search/hep-ex?searchtype=author&query=Parmeggiano%2C+S">S. Parmeggiano</a>, <a href="/search/hep-ex?searchtype=author&query=Ranucci%2C+G">G. Ranucci</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M+G">M. G. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Miramonti%2C+L">L. Miramonti</a>, <a href="/search/hep-ex?searchtype=author&query=Percalli%2C+E">E. Percalli</a>, <a href="/search/hep-ex?searchtype=author&query=Re%2C+A+C">A. C. Re</a>, <a href="/search/hep-ex?searchtype=author&query=Saggese%2C+P">P. Saggese</a>, <a href="/search/hep-ex?searchtype=author&query=Torri%2C+M+D+C">M. D. C. Torri</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Bergnoli%2C+A">A. Bergnoli</a>, <a href="/search/hep-ex?searchtype=author&query=Borghesi%2C+M">M. Borghesi</a>, <a href="/search/hep-ex?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/hep-ex?searchtype=author&query=Bruno%2C+R">R. Bruno</a>, <a href="/search/hep-ex?searchtype=author&query=Budano%2C+A">A. Budano</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Zhang%2C+H+S">H. S. Zhang</a>, <a href="/search/hep-ex?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/hep-ex?searchtype=author&query=Cialdi%2C+S">S. Cialdi</a>, <a href="/search/hep-ex?searchtype=author&query=Yang%2C+C+X">C. X. Yang</a>, <a href="/search/hep-ex?searchtype=author&query=Huang%2C+J+H">J. H. Huang</a>, <a href="/search/hep-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Reina%2C+G">G. Reina</a>, <a href="/search/hep-ex?searchtype=author&query=Deng%2C+Z+Y">Z. Y. Deng</a>, <a href="/search/hep-ex?searchtype=author&query=Suerra%2C+E">E. Suerra</a>, <a href="/search/hep-ex?searchtype=author&query=Altilia%2C+S">S. Altilia</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M+G">M. G. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Landini%2C+C">C. Landini</a>, <a href="/search/hep-ex?searchtype=author&query=Lombardi%2C+P">P. Lombardi</a>, <a href="/search/hep-ex?searchtype=author&query=Miramonti%2C+L">L. Miramonti</a>, <a href="/search/hep-ex?searchtype=author&query=Percalli%2C+E">E. Percalli</a>, <a href="/search/hep-ex?searchtype=author&query=Ranucci%2C+G">G. Ranucci</a>, <a href="/search/hep-ex?searchtype=author&query=Re%2C+A+C">A. C. Re</a>, <a href="/search/hep-ex?searchtype=author&query=Saggese%2C+P">P. Saggese</a>, <a href="/search/hep-ex?searchtype=author&query=Torri%2C+M+D+C">M. D. C. Torri</a>, <a href="/search/hep-ex?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/2405.18008">arXiv:2405.18008</a> <span> [<a href="https://arxiv.org/pdf/2405.18008">pdf</a>, <a href="https://arxiv.org/format/2405.18008">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div 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/ad7f3e">10.1088/1674-1137/ad7f3e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Potential to identify neutrino mass ordering with reactor antineutrinos at JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Beretta%2C+M">Marco Beretta</a> , et al. (605 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="2405.18008v2-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a multi-purpose neutrino experiment under construction in South China. This paper presents an updated estimate of JUNO's sensitivity to neutrino mass ordering using the reactor antineutrinos emitted from eight nuclear reactor cores in the Taishan and Yangjiang nuclear power plants. This measurement is planned by studying the fine interference… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18008v2-abstract-full').style.display = 'inline'; document.getElementById('2405.18008v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.18008v2-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a multi-purpose neutrino experiment under construction in South China. This paper presents an updated estimate of JUNO's sensitivity to neutrino mass ordering using the reactor antineutrinos emitted from eight nuclear reactor cores in the Taishan and Yangjiang nuclear power plants. This measurement is planned by studying the fine interference pattern caused by quasi-vacuum oscillations in the oscillated antineutrino spectrum at a baseline of 52.5~km and is completely independent of the CP violating phase and neutrino mixing angle $胃_{23}$. The sensitivity is obtained through a joint analysis of JUNO and Taishan Antineutrino Observatory (TAO) detectors utilizing the best available knowledge to date about the location and overburden of the JUNO experimental site, local and global nuclear reactors, JUNO and TAO detector responses, expected event rates and spectra of signals and backgrounds, and systematic uncertainties of analysis inputs. We find that a 3$蟽$ median sensitivity to reject the wrong mass ordering hypothesis can be reached with an exposure to approximately 6.5 years $\times$ 26.6 GW thermal power. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18008v2-abstract-full').style.display = 'none'; document.getElementById('2405.18008v2-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 February, 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">Comments:</span> <span class="has-text-grey-dark mathjax">The version published on Chinese Physics C</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/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Adamowicz%2C+K">Kai Adamowicz</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Beretta%2C+M">Marco Beretta</a>, <a href="/search/hep-ex?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/hep-ex?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/2405.17792">arXiv:2405.17792</a> <span> [<a href="https://arxiv.org/pdf/2405.17792">pdf</a>, <a href="https://arxiv.org/format/2405.17792">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> JUNO Sensitivity to Invisible Decay Modes of Neutrons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Adamowicz%2C+K">Kai Adamowicz</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Beretta%2C+M">Marco Beretta</a>, <a href="/search/hep-ex?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">Daniel Bick</a> , et al. (635 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="2405.17792v2-abstract-short" style="display: inline;"> We explore the decay of bound neutrons into invisible particles (e.g., $n\rightarrow 3 谓$ or $nn \rightarrow 2 谓$) in the JUNO liquid scintillator detector, which do not produce an observable signal. The invisible decay includes two decay modes: $ n \rightarrow { inv} $ and $ nn \rightarrow { inv} $. The invisible decays of $s$-shell neutrons in $^{12}{\rm C}$ will leave a highly excited residual… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17792v2-abstract-full').style.display = 'inline'; document.getElementById('2405.17792v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17792v2-abstract-full" style="display: none;"> We explore the decay of bound neutrons into invisible particles (e.g., $n\rightarrow 3 谓$ or $nn \rightarrow 2 谓$) in the JUNO liquid scintillator detector, which do not produce an observable signal. The invisible decay includes two decay modes: $ n \rightarrow { inv} $ and $ nn \rightarrow { inv} $. The invisible decays of $s$-shell neutrons in $^{12}{\rm C}$ will leave a highly excited residual nucleus. Subsequently, some de-excitation modes of the excited residual nuclei can produce a time- and space-correlated triple coincidence signal in the JUNO detector. Based on a full Monte Carlo simulation informed with the latest available data, we estimate all backgrounds, including inverse beta decay events of the reactor antineutrino $\bar谓_e$, natural radioactivity, cosmogenic isotopes and neutral current interactions of atmospheric neutrinos. Pulse shape discrimination and multivariate analysis techniques are employed to further suppress backgrounds. With two years of exposure, JUNO is expected to give an order of magnitude improvement compared to the current best limits. After 10 years of data taking, the JUNO expected sensitivities at a 90% confidence level are $蟿/B( n \rightarrow { inv} ) > 5.0 \times 10^{31} \, {\rm yr}$ and $蟿/B( nn \rightarrow { inv} ) > 1.4 \times 10^{32} \, {\rm yr}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17792v2-abstract-full').style.display = 'none'; document.getElementById('2405.17792v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 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">31 pages, 10 figures, 4 tables, Published version in EPJC</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.11826">arXiv:2310.11826</a> <span> [<a href="https://arxiv.org/pdf/2310.11826">pdf</a>, <a href="https://arxiv.org/format/2310.11826">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.112014">10.1103/PhysRevD.109.112014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Novel techniques for alpha/beta pulse shape discrimination in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacintov%2C+A">A. Di Giacintov</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/hep-ex?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/hep-ex?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/hep-ex?searchtype=author&query=Ianni%2C+A">Andrea Ianni</a> , et al. (49 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.11826v1-abstract-short" style="display: inline;"> Borexino could efficiently distinguish between alpha and beta radiation in its liquid scintillator by the characteristic time profile of their scintillation pulse. This alpha/beta discrimination, first demonstrated at the tonne scale in the Counting Test Facility prototype, was used throughout the lifetime of the experiment between 2007 and 2021. With this method, alpha events are identified and s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11826v1-abstract-full').style.display = 'inline'; document.getElementById('2310.11826v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.11826v1-abstract-full" style="display: none;"> Borexino could efficiently distinguish between alpha and beta radiation in its liquid scintillator by the characteristic time profile of their scintillation pulse. This alpha/beta discrimination, first demonstrated at the tonne scale in the Counting Test Facility prototype, was used throughout the lifetime of the experiment between 2007 and 2021. With this method, alpha events are identified and subtracted from the beta-like solar neutrino events. This is particularly important in liquid scintillator as alpha scintillation is quenched many-fold. In Borexino, the prominent Po-210 decay peak was a background in the energy range of electrons scattered from Be-7 solar neutrinos. Optimal alpha-beta discrimination was achieved with a "multi-layer perceptron neural network", which its higher ability to leverage the timing information of the scintillation photons detected by the photomultiplier tubes. An event-by-event, high efficiency, stable, and uniform pulse shape discrimination was essential in characterising the spatial distribution of background in the detector. This benefited most Borexino measurements, including solar neutrinos in the \pp chain and the first direct observation of the CNO cycle in the Sun. This paper presents the key milestones in alpha/beta discrimination in Borexino as a term of comparison for current and future large liquid scintillator detectors <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11826v1-abstract-full').style.display = 'none'; document.getElementById('2310.11826v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109, 112014, 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.07109">arXiv:2309.07109</a> <span> [<a href="https://arxiv.org/pdf/2309.07109">pdf</a>, <a href="https://arxiv.org/ps/2309.07109">ps</a>, <a href="https://arxiv.org/format/2309.07109">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> </div> </div> <p class="title is-5 mathjax"> Real-time Monitoring for the Next Core-Collapse Supernova in JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Beretta%2C+M">Marco Beretta</a>, <a href="/search/hep-ex?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a> , et al. (606 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="2309.07109v2-abstract-short" style="display: inline;"> The core-collapse supernova (CCSN) is considered one of the most energetic astrophysical events in the universe. The early and prompt detection of neutrinos before (pre-SN) and during the supernova (SN) burst presents a unique opportunity for multi-messenger observations of CCSN events. In this study, we describe the monitoring concept and present the sensitivity of the system to pre-SN and SN neu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07109v2-abstract-full').style.display = 'inline'; document.getElementById('2309.07109v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.07109v2-abstract-full" style="display: none;"> The core-collapse supernova (CCSN) is considered one of the most energetic astrophysical events in the universe. The early and prompt detection of neutrinos before (pre-SN) and during the supernova (SN) burst presents a unique opportunity for multi-messenger observations of CCSN events. In this study, we describe the monitoring concept and present the sensitivity of the system to pre-SN and SN neutrinos at the Jiangmen Underground Neutrino Observatory (JUNO), a 20 kton liquid scintillator detector currently under construction in South China. The real-time monitoring system is designed to ensure both prompt alert speed and comprehensive coverage of progenitor stars. It incorporates prompt monitors on the electronic board as well as online monitors at the data acquisition stage. Assuming a false alert rate of 1 per year, this monitoring system exhibits sensitivity to pre-SN neutrinos up to a distance of approximately 1.6 (0.9) kiloparsecs and SN neutrinos up to about 370 (360) kiloparsecs for a progenitor mass of 30 solar masses, considering both normal and inverted mass ordering scenarios. The pointing ability of the CCSN is evaluated by analyzing the accumulated event anisotropy of inverse beta decay interactions from pre-SN or SN neutrinos. This, along with the early alert, can play a crucial role in facilitating follow-up multi-messenger observations of the next galactic or nearby extragalactic CCSN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07109v2-abstract-full').style.display = 'none'; document.getElementById('2309.07109v2-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 9 figures, accepted for the publication at 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/2307.14636">arXiv:2307.14636</a> <span> [<a href="https://arxiv.org/pdf/2307.14636">pdf</a>, <a href="https://arxiv.org/format/2307.14636">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.108.102005">10.1103/PhysRevD.108.102005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Final results of Borexino on CNO solar neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/hep-ex?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/hep-ex?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a>, <a href="/search/hep-ex?searchtype=author&query=Ianni%2C+A">Andrea Ianni</a> , et al. (50 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.14636v1-abstract-short" style="display: inline;"> We report the first measurement of CNO solar neutrinos by Borexino that uses the Correlated Integrated Directionality (CID) method, exploiting the sub-dominant Cherenkov light in the liquid scintillator detector. The directional information of the solar origin of the neutrinos is preserved by the fast Cherenkov photons from the neutrino scattered electrons, and is used to discriminate between sign… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14636v1-abstract-full').style.display = 'inline'; document.getElementById('2307.14636v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.14636v1-abstract-full" style="display: none;"> We report the first measurement of CNO solar neutrinos by Borexino that uses the Correlated Integrated Directionality (CID) method, exploiting the sub-dominant Cherenkov light in the liquid scintillator detector. The directional information of the solar origin of the neutrinos is preserved by the fast Cherenkov photons from the neutrino scattered electrons, and is used to discriminate between signal and background. The directional information is independent from the spectral information on which the previous CNO solar neutrino measurements by Borexino were based. While the CNO spectral analysis could only be applied on the Phase-III dataset, the directional analysis can use the complete Borexino data taking period from 2007 to 2021. The absence of CNO neutrinos has been rejected with >5蟽 credible level using the Bayesian statistics. The directional CNO measurement is obtained without an external constraint on the $^{210}$Bi contamination of the liquid scintillator, which was applied in the spectral analysis approach. The final and the most precise CNO measurement of Borexino is then obtained by combining the new CID-based CNO result with an improved spectral fit of the Phase-III dataset. Including the statistical and the systematic errors, the extracted CNO interaction rate is $R(\mathrm{CNO})=6.7^{+1.2}_{-0.8} \, \mathrm{cpd/100 \, tonnes}$. Taking into account the neutrino flavor conversion, the resulting CNO neutrino flux at Earth is $桅_\mathrm{CNO}=6.7 ^{+1.2}_{-0.8} \times 10^8 \, \mathrm{cm^{-2} s^{-1}}$, in agreement with the high metallicity Standard Solar Models. The results described in this work reinforce the role of the event directional information in large-scale liquid scintillator detectors and open up new avenues for the next-generation liquid scintillator or hybrid neutrino experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14636v1-abstract-full').style.display = 'none'; document.getElementById('2307.14636v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.09567">arXiv:2306.09567</a> <span> [<a href="https://arxiv.org/pdf/2306.09567">pdf</a>, <a href="https://arxiv.org/format/2306.09567">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> </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/10.1088/1475-7516/2023/09/001">10.1088/1475-7516/2023/09/001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ex?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a> , et al. (581 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="2306.09567v3-abstract-short" style="display: inline;"> We discuss JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo via detecting inverse beta decay reactions of electron anti-neutrinos resulting from the annihilation. We study possible backgrounds to the signature, including the reactor neutrinos, diffuse supernova neutrino background, charged- and neutral-current interactions of atmospheric neutrinos, backgrounds from muon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09567v3-abstract-full').style.display = 'inline'; document.getElementById('2306.09567v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.09567v3-abstract-full" style="display: none;"> We discuss JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo via detecting inverse beta decay reactions of electron anti-neutrinos resulting from the annihilation. We study possible backgrounds to the signature, including the reactor neutrinos, diffuse supernova neutrino background, charged- and neutral-current interactions of atmospheric neutrinos, backgrounds from muon-induced fast neutrons and cosmogenic isotopes. A fiducial volume cut, as well as the pulse shape discrimination and the muon veto are applied to suppress the above backgrounds. It is shown that JUNO sensitivity to the thermally averaged dark matter annihilation rate in 10 years of exposure would be significantly better than the present-day best limit set by Super-Kamiokande and would be comparable to that expected by Hyper-Kamiokande. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09567v3-abstract-full').style.display = 'none'; document.getElementById('2306.09567v3-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">25 pages, 9 figures, matches the publised version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 09 (2023) 001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.13876">arXiv:2303.13876</a> <span> [<a href="https://arxiv.org/pdf/2303.13876">pdf</a>, <a href="https://arxiv.org/ps/2303.13876">ps</a>, <a href="https://arxiv.org/format/2303.13876">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-023-11688-4">10.1140/epjc/s10052-023-11688-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Borexino's search for low-energy neutrinos associated with gravitational wave events from GWTC-3 database </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=BOREXINO+Collaboration"> BOREXINO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Angelo%2C+D+D">D. D' Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a>, <a href="/search/hep-ex?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/hep-ex?searchtype=author&query=Ianni%2C+A">Aldo Ianni</a> , et al. (50 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.13876v2-abstract-short" style="display: inline;"> The search for neutrino events in correlation with gravitational wave (GW) events for three observing runs (O1, O2 and O3) from 09/2015 to 03/2020 has been performed using the Borexino data-set of the same period. We have searched for signals of neutrino-electron scattering with visible energies above 250 keV within a time window of 1000 s centered at the detection moment of a particular GW event.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13876v2-abstract-full').style.display = 'inline'; document.getElementById('2303.13876v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.13876v2-abstract-full" style="display: none;"> The search for neutrino events in correlation with gravitational wave (GW) events for three observing runs (O1, O2 and O3) from 09/2015 to 03/2020 has been performed using the Borexino data-set of the same period. We have searched for signals of neutrino-electron scattering with visible energies above 250 keV within a time window of 1000 s centered at the detection moment of a particular GW event. The search was done with three visible energy thresholds of 0.25, 0.8 and 3.0 MeV.Two types of incoming neutrino spectra were considered: the mono-energetic line and the spectrum expected from supernovae. The same spectra were considered for electron antineutrinos detected through inverse beta-decay (IBD) reaction. GW candidates originated by merging binaries of black holes (BHBH), neutron stars (NSNS) and neutron star and black hole (NSBH) were analysed separately. Additionally, the subset of most intensive BHBH mergers at closer distances and with larger radiative mass than the rest was considered. In total, follow-ups of 74 out of 93 gravitational waves reported in the GWTC-3 catalog were analyzed and no statistically significant excess over the background was observed. As a result, the strongest upper limits on GW-associated neutrino and antineutrino fluences for all flavors (谓_e, 谓_渭, 谓_蟿) have been obtained in the (0.5 - 5.0) MeV neutrino energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13876v2-abstract-full').style.display = 'none'; document.getElementById('2303.13876v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C (2023) 83:538 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ex?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ex?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?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/2212.08502">arXiv:2212.08502</a> <span> [<a href="https://arxiv.org/pdf/2212.08502">pdf</a>, <a href="https://arxiv.org/format/2212.08502">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1674-1137/ace9c6">10.1088/1674-1137/ace9c6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JUNO Sensitivity on Proton Decay $p\to \bar谓K^+$ Searches </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/hep-ex?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a>, <a href="/search/hep-ex?searchtype=author&query=Blin%2C+S">Sylvie Blin</a> , et al. (586 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="2212.08502v3-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a large liquid scintillator detector designed to explore many topics in fundamental physics. In this paper, the potential on searching for proton decay in $p\to \bar谓K^+$ mode with JUNO is investigated.The kaon and its decay particles feature a clear three-fold coincidence signature that results in a high efficiency for identification. Moreov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.08502v3-abstract-full').style.display = 'inline'; document.getElementById('2212.08502v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.08502v3-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a large liquid scintillator detector designed to explore many topics in fundamental physics. In this paper, the potential on searching for proton decay in $p\to \bar谓K^+$ mode with JUNO is investigated.The kaon and its decay particles feature a clear three-fold coincidence signature that results in a high efficiency for identification. Moreover, the excellent energy resolution of JUNO permits to suppress the sizable background caused by other delayed signals. Based on these advantages, the detection efficiency for the proton decay via $p\to \bar谓K^+$ is 36.9% with a background level of 0.2 events after 10 years of data taking. The estimated sensitivity based on 200 kton-years exposure is $9.6 \times 10^{33}$ years, competitive with the current best limits on the proton lifetime in this channel. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.08502v3-abstract-full').style.display = 'none'; document.getElementById('2212.08502v3-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">14 pages, 12 figures, an author added</span> </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/hep-ex?searchtype=author&query=Cerrone%2C+V">Vanessa Cerrone</a>, <a href="/search/hep-ex?searchtype=author&query=von+Sturm%2C+K">Katharina von Sturm</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/hep-ex?searchtype=author&query=Bolognesi%2C+M">Matteo Bolognesi</a>, <a href="/search/hep-ex?searchtype=author&query=Brugnera%2C+R">Riccardo Brugnera</a>, <a href="/search/hep-ex?searchtype=author&query=Chen%2C+C">Chao Chen</a>, <a href="/search/hep-ex?searchtype=author&query=Clerbaux%2C+B">Barbara Clerbaux</a>, <a href="/search/hep-ex?searchtype=author&query=Coppi%2C+A">Alberto Coppi</a>, <a href="/search/hep-ex?searchtype=author&query=Corso%2C+F+d">Flavio dal Corso</a>, <a href="/search/hep-ex?searchtype=author&query=Corti%2C+D">Daniele Corti</a>, <a href="/search/hep-ex?searchtype=author&query=Dong%2C+J">Jianmeng Dong</a>, <a href="/search/hep-ex?searchtype=author&query=Dou%2C+W">Wei Dou</a>, <a href="/search/hep-ex?searchtype=author&query=Fan%2C+L">Lei Fan</a>, <a href="/search/hep-ex?searchtype=author&query=Garfagnini%2C+A">Alberto Garfagnini</a>, <a href="/search/hep-ex?searchtype=author&query=Gong%2C+G">Guanghua Gong</a>, <a href="/search/hep-ex?searchtype=author&query=Grassi%2C+M">Marco Grassi</a>, <a href="/search/hep-ex?searchtype=author&query=Hang%2C+S">Shuang Hang</a>, <a href="/search/hep-ex?searchtype=author&query=Guizzetti%2C+R+M">Rosa Maria Guizzetti</a>, <a href="/search/hep-ex?searchtype=author&query=He%2C+C">Cong He</a>, <a href="/search/hep-ex?searchtype=author&query=Hu%2C+J">Jun Hu</a>, <a href="/search/hep-ex?searchtype=author&query=Isocrate%2C+R">Roberto Isocrate</a>, <a href="/search/hep-ex?searchtype=author&query=Jelmini%2C+B">Beatrice Jelmini</a>, <a href="/search/hep-ex?searchtype=author&query=Ji%2C+X">Xiaolu Ji</a>, <a href="/search/hep-ex?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/2210.08437">arXiv:2210.08437</a> <span> [<a href="https://arxiv.org/pdf/2210.08437">pdf</a>, <a href="https://arxiv.org/format/2210.08437">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="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad2bfd">10.3847/1538-4357/ad2bfd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Model Independent Approach of the JUNO $^8$B Solar Neutrino Program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Zhao%2C+J">Jie Zhao</a>, <a href="/search/hep-ex?searchtype=author&query=Yue%2C+B">Baobiao Yue</a>, <a href="/search/hep-ex?searchtype=author&query=Lu%2C+H">Haoqi Lu</a>, <a href="/search/hep-ex?searchtype=author&query=Li%2C+Y">Yufeng Li</a>, <a href="/search/hep-ex?searchtype=author&query=Ling%2C+J">Jiajie Ling</a>, <a href="/search/hep-ex?searchtype=author&query=Yu%2C+Z">Zeyuan Yu</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ex?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a> , et al. (579 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.08437v2-abstract-short" style="display: inline;"> The physics potential of detecting $^8$B solar neutrinos will be exploited at the Jiangmen Underground Neutrino Observatory (JUNO), in a model independent manner by using three distinct channels of the charged-current (CC), neutral-current (NC) and elastic scattering (ES) interactions. Due to the largest-ever mass of $^{13}$C nuclei in the liquid-scintillator detectors and the {expected} low backg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08437v2-abstract-full').style.display = 'inline'; document.getElementById('2210.08437v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.08437v2-abstract-full" style="display: none;"> The physics potential of detecting $^8$B solar neutrinos will be exploited at the Jiangmen Underground Neutrino Observatory (JUNO), in a model independent manner by using three distinct channels of the charged-current (CC), neutral-current (NC) and elastic scattering (ES) interactions. Due to the largest-ever mass of $^{13}$C nuclei in the liquid-scintillator detectors and the {expected} low background level, $^8$B solar neutrinos would be observable in the CC and NC interactions on $^{13}$C for the first time. By virtue of optimized event selections and muon veto strategies, backgrounds from the accidental coincidence, muon-induced isotopes, and external backgrounds can be greatly suppressed. Excellent signal-to-background ratios can be achieved in the CC, NC and ES channels to guarantee the $^8$B solar neutrino observation. From the sensitivity studies performed in this work, we show that JUNO, with ten years of data, can reach the {1$蟽$} precision levels of 5%, 8% and 20% for the $^8$B neutrino flux, $\sin^2胃_{12}$, and $螖m^2_{21}$, respectively. It would be unique and helpful to probe the details of both solar physics and neutrino physics. In addition, when combined with SNO, the world-best precision of 3% is expected for the $^8$B neutrino flux measurement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08437v2-abstract-full').style.display = 'none'; document.getElementById('2210.08437v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 7 figures, accepted version to appear in The Astrophysical Journal. Yufeng Li and Jiajie Ling are corresponding authors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophysical Journal 965 (2024) 122 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.15975">arXiv:2205.15975</a> <span> [<a href="https://arxiv.org/pdf/2205.15975">pdf</a>, <a href="https://arxiv.org/format/2205.15975">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.129.252701">10.1103/PhysRevLett.129.252701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved measurement of solar neutrinos from the Carbon-Nitrogen-Oxygen cycle by Borexino and its implications for the Standard Solar Model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=G%C3%B6ttel%2C+A+S">A. S. G枚ttel</a> , et al. (57 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.15975v1-abstract-short" style="display: inline;"> We present an improved measurement of the CNO solar neutrino interaction rate at Earth obtained with the complete Borexino Phase-III dataset. The measured rate R$_{\rm CNO}$ = $6.7^{+2.0}_{-0.8}$ counts/(day$ \cdot$ 100 tonnes), allows us to exclude the absence of the CNO signal with about 7$蟽$ C.L. The correspondent CNO neutrino flux is $6.6^{+2.0}_{-0.9} \times 10^8$ cm$^{-2}$ s$^{-1}$, taking i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.15975v1-abstract-full').style.display = 'inline'; document.getElementById('2205.15975v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.15975v1-abstract-full" style="display: none;"> We present an improved measurement of the CNO solar neutrino interaction rate at Earth obtained with the complete Borexino Phase-III dataset. The measured rate R$_{\rm CNO}$ = $6.7^{+2.0}_{-0.8}$ counts/(day$ \cdot$ 100 tonnes), allows us to exclude the absence of the CNO signal with about 7$蟽$ C.L. The correspondent CNO neutrino flux is $6.6^{+2.0}_{-0.9} \times 10^8$ cm$^{-2}$ s$^{-1}$, taking into account the neutrino flavor conversion. We use the new CNO measurement to evaluate the C and N abundances in the Sun with respect to the H abundance for the first time with solar neutrinos. Our result of $N_{\rm CN}$ = $(5.78^{+1.86}_{-1.00})\times10^{-4}$ displays a $\sim$2$蟽$ tension with the "low metallicity" spectroscopic photospheric measurements. On the other hand, our result used together with the $^7$Be and $^8$B solar neutrino fluxes, also measured by Borexino, permits to disfavour at 3.1$蟽$ C.L. the "low metallicity" SSM B16-AGSS09met as an alternative to the "high metallicity" SSM B16-GS98. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.15975v1-abstract-full').style.display = 'none'; document.getElementById('2205.15975v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 6 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/hep-ex?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ex?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?searchtype=author&query=de+Andre%2C+J+P+A+M">Joao Pedro Athayde Marcondes de Andre</a>, <a href="/search/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ex?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/2204.13249">arXiv:2204.13249</a> <span> [<a href="https://arxiv.org/pdf/2204.13249">pdf</a>, <a href="https://arxiv.org/format/2204.13249">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div 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/ac8bc9">10.1088/1674-1137/ac8bc9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sub-percent Precision Measurement of Neutrino Oscillation Parameters with JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ex?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">Marco Bellato</a> , et al. (581 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.13249v1-abstract-short" style="display: inline;"> JUNO is a multi-purpose neutrino observatory under construction in the south of China. This publication presents new sensitivity estimates for the measurement of the $螖m^2_{31}$, $螖m^2_{21}$, $\sin^2 胃_{12}$, and $\sin^2 胃_{13}$ oscillation parameters using reactor antineutrinos, which is one of the primary physics goals of the experiment. The sensitivities are obtained using the best knowledge av… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13249v1-abstract-full').style.display = 'inline'; document.getElementById('2204.13249v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.13249v1-abstract-full" style="display: none;"> JUNO is a multi-purpose neutrino observatory under construction in the south of China. This publication presents new sensitivity estimates for the measurement of the $螖m^2_{31}$, $螖m^2_{21}$, $\sin^2 胃_{12}$, and $\sin^2 胃_{13}$ oscillation parameters using reactor antineutrinos, which is one of the primary physics goals of the experiment. The sensitivities are obtained using the best knowledge available to date on the location and overburden of the experimental site, the nuclear reactors in the surrounding area and beyond, the detector response uncertainties, and the reactor antineutrino spectral shape constraints expected from the TAO satellite detector. It is found that the $螖m^2_{31}$, $螖m^2_{21}$, and $\sin^2 胃_{12}$ oscillation parameters will be determined to better than 0.5% precision in six years of data collection, which represents approximately an order of magnitude improvement over existing constraints. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13249v1-abstract-full').style.display = 'none'; document.getElementById('2204.13249v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 10 figures, submitted to Chinese Physics C</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.07029">arXiv:2204.07029</a> <span> [<a href="https://arxiv.org/pdf/2204.07029">pdf</a>, <a href="https://arxiv.org/format/2204.07029">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2022.102778">10.1016/j.astropartphys.2022.102778 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Independent determination of the Earth's orbital parameters with solar neutrinos in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Goettel%2C+A+S">A. S. Goettel</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a> , et al. (54 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.07029v1-abstract-short" style="display: inline;"> Since the beginning of 2012, the Borexino collaboration has been reporting precision measurements of the solar neutrino fluxes, emitted in the proton-proton chain and in the Carbon-Nitrogen-Oxygen cycle. The experimental sensitivity achieved in Phase-II and Phase-III of the Borexino data taking made it possible to detect the annual modulation of the solar neutrino interaction rate due to the eccen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.07029v1-abstract-full').style.display = 'inline'; document.getElementById('2204.07029v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.07029v1-abstract-full" style="display: none;"> Since the beginning of 2012, the Borexino collaboration has been reporting precision measurements of the solar neutrino fluxes, emitted in the proton-proton chain and in the Carbon-Nitrogen-Oxygen cycle. The experimental sensitivity achieved in Phase-II and Phase-III of the Borexino data taking made it possible to detect the annual modulation of the solar neutrino interaction rate due to the eccentricity of Earth's orbit, with a statistical significance greater than 5$蟽$. This is the first precise measurement of the Earth's orbital parameters based solely on solar neutrinos and an additional signature of the solar origin of the Borexino signal. The complete periodogram of the time series of the Borexino solar neutrino detection rate is also reported, exploring frequencies between one cycle/year and one cycle/day. No other significant modulation frequencies are found. The present results were uniquely made possible by Borexino's decade-long high-precision solar neutrino detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.07029v1-abstract-full').style.display = 'none'; document.getElementById('2204.07029v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.14450">arXiv:2112.14450</a> <span> [<a href="https://arxiv.org/pdf/2112.14450">pdf</a>, <a href="https://arxiv.org/format/2112.14450">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/JHEP06(2022)062">10.1007/JHEP06(2022)062 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Damping signatures at JUNO, a medium-baseline reactor neutrino oscillation experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=JUNO+collaboration"> JUNO collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Wang%2C+J">Jun Wang</a>, <a href="/search/hep-ex?searchtype=author&query=Liao%2C+J">Jiajun Liao</a>, <a href="/search/hep-ex?searchtype=author&query=Wang%2C+W">Wei Wang</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ex?searchtype=author&query=Babic%2C+A">Andrej Babic</a>, <a href="/search/hep-ex?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">Eric Baussan</a> , et al. (582 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="2112.14450v2-abstract-short" style="display: inline;"> We study damping signatures at the Jiangmen Underground Neutrino Observatory (JUNO), a medium-baseline reactor neutrino oscillation experiment. These damping signatures are motivated by various new physics models, including quantum decoherence, $谓_3$ decay, neutrino absorption, and wave packet decoherence. The phenomenological effects of these models can be characterized by exponential damping fac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.14450v2-abstract-full').style.display = 'inline'; document.getElementById('2112.14450v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.14450v2-abstract-full" style="display: none;"> We study damping signatures at the Jiangmen Underground Neutrino Observatory (JUNO), a medium-baseline reactor neutrino oscillation experiment. These damping signatures are motivated by various new physics models, including quantum decoherence, $谓_3$ decay, neutrino absorption, and wave packet decoherence. The phenomenological effects of these models can be characterized by exponential damping factors at the probability level. We assess how well JUNO can constrain these damping parameters and how to disentangle these different damping signatures at JUNO. Compared to current experimental limits, JUNO can significantly improve the limits on $蟿_3/m_3$ in the $谓_3$ decay model, the width of the neutrino wave packet $蟽_x$, and the intrinsic relative dispersion of neutrino momentum $蟽_{\rm rel}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.14450v2-abstract-full').style.display = 'none'; document.getElementById('2112.14450v2-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">17 pages, 2 figures, 4 tables. Version published in JHEP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP06(2022)062 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.11816">arXiv:2112.11816</a> <span> [<a href="https://arxiv.org/pdf/2112.11816">pdf</a>, <a href="https://arxiv.org/format/2112.11816">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.128.091803">10.1103/PhysRevLett.128.091803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Directional Measurement of sub-MeV Solar Neutrinos with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (72 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.11816v1-abstract-short" style="display: inline;"> We report the measurement of sub-MeV solar neutrinos through the use of their associated Cherenkov radiation, performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso. The measurement is achieved using a novel technique that correlates individual photon hits of events to the known position of the Sun. In an energy window between 0.54 MeV to 0.74 MeV, selected using the domin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11816v1-abstract-full').style.display = 'inline'; document.getElementById('2112.11816v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.11816v1-abstract-full" style="display: none;"> We report the measurement of sub-MeV solar neutrinos through the use of their associated Cherenkov radiation, performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso. The measurement is achieved using a novel technique that correlates individual photon hits of events to the known position of the Sun. In an energy window between 0.54 MeV to 0.74 MeV, selected using the dominant scintillation light, we have measured 10887$^{+2386}_{-2103} (\mathrm{stat.})\pm 947 (\mathrm{syst.})$ ($68\%$ confidence interval) solar neutrinos out of 19904 total events. This corresponds to a $^{7}$Be neutrino interaction rate of 51.6$^{+13.9}_{-12.5}$ counts/(day$\cdot$ 100 ton), which is in agreement with the Standard Solar Model predictions and the previous spectroscopic results of Borexino. The no-neutrino hypothesis can be excluded with $>$5$蟽$ confidence level. For the first time, we have demonstrated the possibility of utilizing the directional Cherenkov information for sub-MeV solar neutrinos, in a large-scale, high light yield liquid scintillator detector. This measurement provides an experimental proof of principle for future hybrid event reconstruction using both Cherenkov and scintillation signatures simultaneously. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11816v1-abstract-full').style.display = 'none'; document.getElementById('2112.11816v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 4 figures, short letter of arXiv:2109.04770</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.14500">arXiv:2111.14500</a> <span> [<a href="https://arxiv.org/pdf/2111.14500">pdf</a>, <a href="https://arxiv.org/ps/2111.14500">ps</a>, <a href="https://arxiv.org/format/2111.14500">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-022-10197-0">10.1140/epjc/s10052-022-10197-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Low-Energy Signals from Fast Radio Bursts with the Borexino Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/hep-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/hep-ex?searchtype=author&query=Ghiano%2C+C">C. Ghiano</a>, <a href="/search/hep-ex?searchtype=author&query=Giammarchi%2C+M">M. Giammarchi</a>, <a href="/search/hep-ex?searchtype=author&query=Goretti%2C+A">A. Goretti</a>, <a href="/search/hep-ex?searchtype=author&query=Gottel%2C+A+S">A. S. Gottel</a>, <a href="/search/hep-ex?searchtype=author&query=Gromov%2C+M">M. Gromov</a> , et al. (55 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.14500v2-abstract-short" style="display: inline;"> The search for neutrino events in correlation with several of the most intense fast radio bursts (FRBs) has been performed using the Borexino data. We have searched for signals with visible energies above $250$~keV within a time window of $\pm$1000~s corresponding to the detection time of a particular FRB. We also applied an alternative approach based on searching for specific shapes of neutrino-e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14500v2-abstract-full').style.display = 'inline'; document.getElementById('2111.14500v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.14500v2-abstract-full" style="display: none;"> The search for neutrino events in correlation with several of the most intense fast radio bursts (FRBs) has been performed using the Borexino data. We have searched for signals with visible energies above $250$~keV within a time window of $\pm$1000~s corresponding to the detection time of a particular FRB. We also applied an alternative approach based on searching for specific shapes of neutrino-electron scattering spectra in the full exposure spectrum of the Borexino detector. In particular, two incoming neutrino spectra were considered: the monoenergetic line and the spectrum expected from supernovae. The same spectra were considered for electron antineutrinos detected through the inverse beta-decay reaction. No statistically significant excess over the background was observed. As a result, the strongest upper limits on FRB-associated neutrino fluences of all flavors have been obtained in the $0.5 - 50$~MeV neutrino energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14500v2-abstract-full').style.display = 'none'; document.getElementById('2111.14500v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C (2022) 82:278 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.04770">arXiv:2109.04770</a> <span> [<a href="https://arxiv.org/pdf/2109.04770">pdf</a>, <a href="https://arxiv.org/format/2109.04770">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.105.052002">10.1103/PhysRevD.105.052002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Correlated and Integrated Directionality for sub-MeV solar neutrinos in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (72 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.04770v2-abstract-short" style="display: inline;"> Liquid scintillator detectors play a central role in the detection of neutrinos from various sources. In particular, it is the only technique used so far for the precision spectroscopy of sub-MeV solar neutrinos, as demonstrated by the Borexino experiment at the Gran Sasso National Laboratory in Italy. The benefit of a high light yield, and thus a low energy threshold and a good energy resolution,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.04770v2-abstract-full').style.display = 'inline'; document.getElementById('2109.04770v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.04770v2-abstract-full" style="display: none;"> Liquid scintillator detectors play a central role in the detection of neutrinos from various sources. In particular, it is the only technique used so far for the precision spectroscopy of sub-MeV solar neutrinos, as demonstrated by the Borexino experiment at the Gran Sasso National Laboratory in Italy. The benefit of a high light yield, and thus a low energy threshold and a good energy resolution, comes at the cost of the directional information featured by water Cherenkov detectors, measuring $^8$B solar neutrinos above a few MeV. In this paper we provide the first directionality measurement of sub-MeV solar neutrinos which exploits the correlation between the first few detected photons in each event and the known position of the Sun for each event. This is also the first signature of directionality in neutrinos elastically scattering off electrons in a liquid scintillator target. This measurement exploits the sub-dominant, fast Cherenkov light emission that precedes the dominant yet slower scintillation light signal. Through this measurement, we have also been able to extract the rate of $^{7}$Be solar neutrinos in Borexino. The demonstration of directional sensitivity in a traditional liquid scintillator target paves the way for the possible exploitation of the Cherenkov light signal in future kton-scale experiments using liquid scintillator targets. Directionality is important for background suppression as well as the disentanglement of signals from various sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.04770v2-abstract-full').style.display = 'none'; document.getElementById('2109.04770v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 15 Figures, revised version after comments from PRD Referees, shorter letter submitted with the title: "First Directional Measurement of sub-MeV Solar Neutrinos with Borexino"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.10973">arXiv:2106.10973</a> <span> [<a href="https://arxiv.org/pdf/2106.10973">pdf</a>, <a href="https://arxiv.org/format/2106.10973">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-021-09799-x">10.1140/epjc/s10052-021-09799-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Identification of the cosmogenic $^{11}$C background in large volumes of liquid scintillators with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacintio%2C+A">A. Di Giacintio</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.10973v2-abstract-short" style="display: inline;"> Cosmogenic radio-nuclei are an important source of background for low-energy neutrino experiments. In Borexino, cosmogenic $^{11}$C decays outnumber solar $pep$ and CNO neutrino events by about ten to one. Highly efficient identification of this background is mandatory for these neutrino analyses. We present here the details of the most consolidated strategy, used throughout Borexino solar neutrin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10973v2-abstract-full').style.display = 'inline'; document.getElementById('2106.10973v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.10973v2-abstract-full" style="display: none;"> Cosmogenic radio-nuclei are an important source of background for low-energy neutrino experiments. In Borexino, cosmogenic $^{11}$C decays outnumber solar $pep$ and CNO neutrino events by about ten to one. Highly efficient identification of this background is mandatory for these neutrino analyses. We present here the details of the most consolidated strategy, used throughout Borexino solar neutrino measurements. It hinges upon finding the space-time correlations between $^{11}$C decays, the preceding parent muons and the accompanying neutrons. This article describes the working principles and evaluates the performance of this Three-Fold Coincidence (TFC) technique in its two current implementations: a hard-cut and a likelihood-based approach. Both show stable performances throughout Borexino Phases II (2012-2016) and III (2016-2020) data sets, with a $^{11}$C tagging efficiency of $\sim$90 % and $\sim$63-66 % of the exposure surviving the tagging. We present also a novel technique that targets specifically $^{11}$C produced in high-multiplicity during major spallation events. Such $^{11}$C appear as a burst of events, whose space-time correlation can be exploited. Burst identification can be combined with the TFC to obtain about the same tagging efficiency of $\sim$90 % but with a higher fraction of the exposure surviving, in the range of $\sim$66-68 %. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10973v2-abstract-full').style.display = 'none'; document.getElementById('2106.10973v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 14 figures (but 15 files, one figure being made of 2 images), 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.13209">arXiv:2105.13209</a> <span> [<a href="https://arxiv.org/pdf/2105.13209">pdf</a>, <a href="https://arxiv.org/format/2105.13209">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> The Low Polonium Field of Borexino and its significance for the CNO neutrino detection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Kumaran%2C+S">S. Kumaran</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.13209v1-abstract-short" style="display: inline;"> Borexino is a liquid scintillator detector located at the Laboratori Nazionale del Gran Sasso, Italy with the main goal to measure solar neutrinos. The experiment recently provided the first direct experimental evidence of CNO-cycle neutrinos in the Sun, rejecting the no-CNO signal hypothesis with a significance greater than 5$蟽$ at 99\%C.L. The intrinsic $^{210}$Bi is an important background for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13209v1-abstract-full').style.display = 'inline'; document.getElementById('2105.13209v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.13209v1-abstract-full" style="display: none;"> Borexino is a liquid scintillator detector located at the Laboratori Nazionale del Gran Sasso, Italy with the main goal to measure solar neutrinos. The experiment recently provided the first direct experimental evidence of CNO-cycle neutrinos in the Sun, rejecting the no-CNO signal hypothesis with a significance greater than 5$蟽$ at 99\%C.L. The intrinsic $^{210}$Bi is an important background for this analysis due to its similar spectral shape to that of CNO neutrinos. $^{210}$Bi can be measured through its daughter $^{210}$Po which can be distinguished through an event-by-event basis via pulse shape discrimination. However, this required reducing the convective motions in the scintillator that brought additional $^{210}$Po from peripheral sources. This was made possible through the thermal insulation and stabilization campaign performed between 2015 and 2016. This article will explain the strategy and the different methods performed to extract the $^{210}$Bi upper limit in Phase-III (Jul 2016- Feb 2020) of the experiment through the analysis of $^{210}$Po in the cleanest region of the detector called the Low Polonium Field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13209v1-abstract-full').style.display = 'none'; document.getElementById('2105.13209v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to the 2021 Neutrinos session of the 55th Rencontres de Moriond</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.09211">arXiv:2105.09211</a> <span> [<a href="https://arxiv.org/pdf/2105.09211">pdf</a>, <a href="https://arxiv.org/format/2105.09211">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> First detection of CNO neutrinos with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Settanta%2C+G">G. Settanta</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.09211v1-abstract-short" style="display: inline;"> Neutrinos are elementary particles which are known since many years as fundamental messengers from the interior of the Sun. The Standard Solar Model, which gives a theoretical description of all nuclear processes which happen in our star, predicts that roughly 99% of the energy produced is coming from a series of processes known as the "pp chain". Such processes have been studied in detail over th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09211v1-abstract-full').style.display = 'inline'; document.getElementById('2105.09211v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.09211v1-abstract-full" style="display: none;"> Neutrinos are elementary particles which are known since many years as fundamental messengers from the interior of the Sun. The Standard Solar Model, which gives a theoretical description of all nuclear processes which happen in our star, predicts that roughly 99% of the energy produced is coming from a series of processes known as the "pp chain". Such processes have been studied in detail over the last years by means of neutrinos, thanks also to the important measurements provided by the Borexino experiment. The remaining 1% is instead predicted to come from a separate loop-process, known as the "CNO cycle". This sub-dominant process is theoretically well understood, but has so far escaped any direct observation. Another fundamental aspect is that the CNO cycle is indeed the main nuclear engine in stars more massive than the Sun. In 2020, thanks to the unprecedented radio-purity and temperature control achieved by the Borexino detector over recent years, the first ever detection of neutrinos from the CNO cycle has been finally announced. The milestone result confirms the existence of this nuclear fusion process in our Universe. Here, the details of the detector stabilization and the analysis techniques adopted are reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09211v1-abstract-full').style.display = 'none'; document.getElementById('2105.09211v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures. Contribution to the 2021 Neutrinos session of the 55th Rencontres de Moriond</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.15115">arXiv:2006.15115</a> <span> [<a href="https://arxiv.org/pdf/2006.15115">pdf</a>, <a href="https://arxiv.org/format/2006.15115">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-020-2934-0">10.1038/s41586-020-2934-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.15115v2-abstract-short" style="display: inline;"> For most of their existence stars are fueled by the fusion of hydrogen into helium proceeding via two theoretically well understood processes, namely the $pp$ chain and the CNO cycle. Neutrinos emitted along such fusion processes in the solar core are the only direct probe of the deep interior of the star. A complete spectroscopy of neutrinos from the {\it pp} chain, producing about 99\% of the so… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.15115v2-abstract-full').style.display = 'inline'; document.getElementById('2006.15115v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.15115v2-abstract-full" style="display: none;"> For most of their existence stars are fueled by the fusion of hydrogen into helium proceeding via two theoretically well understood processes, namely the $pp$ chain and the CNO cycle. Neutrinos emitted along such fusion processes in the solar core are the only direct probe of the deep interior of the star. A complete spectroscopy of neutrinos from the {\it pp} chain, producing about 99\% of the solar energy, has already been performed \cite{bib:Nature-2018}. Here, we report the direct observation, with a high statistical significance, of neutrinos produced in the CNO cycle in the Sun. This is the first experimental evidence of this process obtained with the unprecedentedly radio-pure large-volume liquid-scintillator Borexino detector located at the underground Laboratori Nazionali del Gran Sasso in Italy. The main difficulty of this experimental effort is to identify the excess of the few counts per day per 100 tonnes of target due to CNO neutrino interactions above the backgrounds. A novel method to constrain the rate of \bi contaminating the scintillator relies on the thermal stabilisation of the detector achieved over the past 5 years. In the CNO cycle, the hydrogen fusion is catalyzed by the carbon (C) - nitrogen (N) - oxygen (O) and thus its rate, as well as the flux of emitted CNO neutrinos, directly depends on the abundance of these elements in solar core. Therefore, this result paves the way to a direct measurement of the solar metallicity by CNO neutrinos. While this result quantifies the relative contribution of the CNO fusion in the Sun to be of the order of 1\%, this process is dominant in the energy production of massive stars. The occurrence of the primary mechanism for the stellar conversion of hydrogen into helium in the Universe has been proven. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.15115v2-abstract-full').style.display = 'none'; document.getElementById('2006.15115v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">43 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-05 <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> G.3.1 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.12829">arXiv:2005.12829</a> <span> [<a href="https://arxiv.org/pdf/2005.12829">pdf</a>, <a href="https://arxiv.org/format/2005.12829">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-020-08534-2">10.1140/epjc/s10052-020-08534-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity to neutrinos from the solar CNO cycle in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Biondi%2C+R">R. Biondi</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a>, <a href="/search/hep-ex?searchtype=author&query=Formozov%2C+A">A. Formozov</a> , et al. (69 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.12829v3-abstract-short" style="display: inline;"> Neutrinos emitted in the carbon, nitrogen, oxygen (CNO) fusion cycle in the Sun are a sub-dominant, yet crucial component of solar neutrinos whose flux has not been measured yet. The Borexino experiment at the Laboratori Nazionali del Gran Sasso (Italy) has a unique opportunity to detect them directly thanks to the detector's radiopurity and the precise understanding of the detector backgrounds. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12829v3-abstract-full').style.display = 'inline'; document.getElementById('2005.12829v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.12829v3-abstract-full" style="display: none;"> Neutrinos emitted in the carbon, nitrogen, oxygen (CNO) fusion cycle in the Sun are a sub-dominant, yet crucial component of solar neutrinos whose flux has not been measured yet. The Borexino experiment at the Laboratori Nazionali del Gran Sasso (Italy) has a unique opportunity to detect them directly thanks to the detector's radiopurity and the precise understanding of the detector backgrounds. We discuss the sensitivity of Borexino to CNO neutrinos, which is based on the strategies we adopted to constrain the rates of the two most relevant background sources, pep neutrinos from the solar pp-chain and Bi-210 beta decays originating in the intrinsic contamination of the liquid scintillator with Pb-210. Assuming the CNO flux predicted by the high-metallicity Standard Solar Model and an exposure of 1000 daysx71.3 t, Borexino has a median sensitivity to CNO neutrino higher than 3 sigma. With the same hypothesis the expected experimental uncertainty on the CNO neutrino flux is 23%, provided the uncertainty on the independent estimate of the Bi-210 interaction rate is 1.5 cpd/100t. Finally, we evaluated the expected uncertainty of the C and N abundances and the expected discrimination significance between the high and low metallicity Standard Solar Models (HZ and LZ) with future more precise measurement of the CNO solar neutrino flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12829v3-abstract-full').style.display = 'none'; document.getElementById('2005.12829v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> BX-DocDB-674 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 80, 1091 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.02422">arXiv:1909.02422</a> <span> [<a href="https://arxiv.org/pdf/1909.02422">pdf</a>, <a href="https://arxiv.org/format/1909.02422">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Search for low-energy neutrinos from astrophysical sources with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a> , et al. (79 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.02422v1-abstract-short" style="display: inline;"> We report on searches for neutrinos and antineutrinos from astrophysical sources performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. Electron antineutrinos ($\bar谓_e$) are detected in an organic liquid scintillator through the inverse $尾$-decay reaction. In the present work we set model-independent upper limits in the energy range 1.8-16.8 MeV on neutrino flux… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02422v1-abstract-full').style.display = 'inline'; document.getElementById('1909.02422v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.02422v1-abstract-full" style="display: none;"> We report on searches for neutrinos and antineutrinos from astrophysical sources performed with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. Electron antineutrinos ($\bar谓_e$) are detected in an organic liquid scintillator through the inverse $尾$-decay reaction. In the present work we set model-independent upper limits in the energy range 1.8-16.8 MeV on neutrino fluxes from unknown sources that improve our previous results, on average, by a factor 2.5. Using the same data set, we first obtain experimental constraints on the diffuse supernova $\bar谓_e$ fluxes in the previously unexplored region below 8 MeV. A search for $\bar谓_e$ in the solar neutrino flux is also presented: the presence of $\bar谓_e$ would be a manifestation of a non-zero anomalous magnetic moment of the neutrino, making possible its conversion to antineutrinos in the strong magnetic field of the Sun. We obtain a limit for a solar $\bar谓_e$ flux of 384 cm$^{-2}$s$^{-1}$ (90% C.L.), assuming an undistorted solar $^{8}$B neutrinos energy spectrum, that corresponds to a transition probability $p_{ 谓_e \rightarrow \bar谓_{e}}<$ 7.2$\times$10$^{-5}$ (90% C.L.) for E$_{\bar 谓_e}$ $>$ 1.8 MeV. At lower energies, by investigating the spectral shape of elastic scattering events, we obtain a new limit on solar $^{7}$Be-$谓_e$ conversion into $\bar谓_e$ of $p_{ 谓_e \rightarrow \bar 谓_{e}}<$ 0.14 (90% C.L.) at 0.862 keV. Last, we investigate solar flares as possible neutrino sources and obtain the strongest up-to-date limits on the fluence of neutrinos of all flavor neutrino below 3-7 ,MeV. Assuming the neutrino flux to be proportional to the flare's intensity, we exclude an intense solar flare as the cause of the observed excess of events in run 117 of the Cl-Ar Homestake experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02422v1-abstract-full').style.display = 'none'; document.getElementById('1909.02422v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 8 figures, 4 tables, 73 references</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.02257">arXiv:1909.02257</a> <span> [<a href="https://arxiv.org/pdf/1909.02257">pdf</a>, <a href="https://arxiv.org/format/1909.02257">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.101.012009">10.1103/PhysRevD.101.012009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comprehensive geoneutrino analysis with Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a> , et al. (87 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.02257v2-abstract-short" style="display: inline;"> This paper presents a geoneutrino measurement using 3262.74 days of data taken with the Borexino detector at LNGS in Italy. By observing $52.6 ^{+9.4}_{-8.6} ({\rm stat}) ^{+2.7}_{-2.1}({\rm sys})$ geoneutrinos (68% interval) from $^{238}$U and $^{232}$Th, a signal of $47.0^{+8.4}_{-7.7}\,({\rm stat)}^{+2.4}_{-1.9}\,({\rm sys})$ TNU with $^{+18.3}_{-17.2}$% total precision was obtained. This resul… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02257v2-abstract-full').style.display = 'inline'; document.getElementById('1909.02257v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.02257v2-abstract-full" style="display: none;"> This paper presents a geoneutrino measurement using 3262.74 days of data taken with the Borexino detector at LNGS in Italy. By observing $52.6 ^{+9.4}_{-8.6} ({\rm stat}) ^{+2.7}_{-2.1}({\rm sys})$ geoneutrinos (68% interval) from $^{238}$U and $^{232}$Th, a signal of $47.0^{+8.4}_{-7.7}\,({\rm stat)}^{+2.4}_{-1.9}\,({\rm sys})$ TNU with $^{+18.3}_{-17.2}$% total precision was obtained. This result assumes the same Th/U mass ratio found in chondritic CI meteorites but compatible results were found when contributions from $^{238}$U and $^{232}$Th were fit as free parameters. Antineutrino background from reactors is fit unconstrained and found compatible with the expectations. The null-hypothesis of observing a signal from the mantle is excluded at a 99.0% C.L. when exploiting the knowledge of the local crust. Measured mantle signal of $21.2 ^{+9.6}_{-9.0} ({\rm stat})^{+1.1}_{-0.9} ({\rm sys})$ TNU corresponds to the production of a radiogenic heat of $24.6 ^{+11.1}_{-10.4}$ TW (68% interval) from $^{238}$U and $^{232}$Th in the mantle. Assuming 18% contribution of $^{40}$K in the mantle and $8.1^{+1.9}_{-1.4}$ TW of radiogenic heat of the lithosphere, the Borexino estimate of the total Earth radiogenic heat is $38.2 ^{+13.6}_{-12.7}$ TW, corresponding to a convective Urey ratio of 0.78$^{+0.41}_{-0.28}$. These values are compatible with different geological models, however there is a 2.4$蟽$ tension with those which predict the lowest concentration of heat-producing elements. By fitting the data with a constraint on the reactor antineutrino background, the existence of a hypothetical georeactor at the center of the Earth having power greater than 2.4 TW at 95% C.L. is excluded. Particular attention is given to all analysis details, which should be of interest for the next generation geoneutrino measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02257v2-abstract-full').style.display = 'none'; document.getElementById('1909.02257v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">69 pages, 56 Figures (some composed of multiple files), 17 Tables, 135 References</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 012009 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.03512">arXiv:1905.03512</a> <span> [<a href="https://arxiv.org/pdf/1905.03512">pdf</a>, <a href="https://arxiv.org/format/1905.03512">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/JHEP02(2020)038">10.1007/JHEP02(2020)038 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on Flavor-Diagonal Non-Standard Neutrino Interactions from Borexino Phase-II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cappelli%2C+L">L. Cappelli</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a> , et al. (81 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1905.03512v2-abstract-short" style="display: inline;"> The Borexino detector measures solar neutrino fluxes via neutrino-electron elastic scattering. Observed spectra are determined by the solar-$谓_{e}$ survival probability $P_{ee}(E)$, and the chiral couplings of the neutrino and electron. Some theories of physics beyond the Standard Model postulate the existence of Non-Standard Interactions (NSI's) which modify the chiral couplings and $P_{ee}(E)$.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03512v2-abstract-full').style.display = 'inline'; document.getElementById('1905.03512v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.03512v2-abstract-full" style="display: none;"> The Borexino detector measures solar neutrino fluxes via neutrino-electron elastic scattering. Observed spectra are determined by the solar-$谓_{e}$ survival probability $P_{ee}(E)$, and the chiral couplings of the neutrino and electron. Some theories of physics beyond the Standard Model postulate the existence of Non-Standard Interactions (NSI's) which modify the chiral couplings and $P_{ee}(E)$. In this paper, we search for such NSI's, in particular, flavor-diagonal neutral current interactions that modify the $谓_e e$ and $谓_蟿e$ couplings using Borexino Phase II data. Standard Solar Model predictions of the solar neutrino fluxes for both high- and low-metallicity assumptions are considered. No indication of new physics is found at the level of sensitivity of the detector and constraints on the parameters of the NSI's are placed. In addition, with the same dataset the value of $\sin^2胃_W$ is obtained with a precision comparable to that achieved in reactor antineutrino experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03512v2-abstract-full').style.display = 'none'; document.getElementById('1905.03512v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 7 figures. Slight modifications in the title, abstract, and conclusion. Few references added. Text expanded for clarity. Accepted in JHEP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> IP/BBSR/2019-2 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JHEP 2002 (2020) 038 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.04207">arXiv:1808.04207</a> <span> [<a href="https://arxiv.org/pdf/1808.04207">pdf</a>, <a href="https://arxiv.org/format/1808.04207">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2019/02/046">10.1088/1475-7516/2019/02/046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modulations of the Cosmic Muon Signal in Ten Years of Borexino Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+Borexino+Collaboration"> The Borexino Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bolognino%2C+I">I. Bolognino</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a> , et al. (91 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1808.04207v3-abstract-short" style="display: inline;"> We have measured the flux of cosmic muons in the Laboratori Nazionali del Gran Sasso at 3800\,m\,w.e. to be $(3.432 \pm 0.003)\cdot 10^{-4}\,\mathrm{{m^{-2}s^{-1}}}$ based on ten years of Borexino data acquired between May 2007 and May 2017. A seasonal modulation with a period of $(366.3 \pm 0.6)\,\mathrm{d}$ and a relative amplitude of $(1.36 \pm0.04)\%$ is observed. The phase is measured to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.04207v3-abstract-full').style.display = 'inline'; document.getElementById('1808.04207v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.04207v3-abstract-full" style="display: none;"> We have measured the flux of cosmic muons in the Laboratori Nazionali del Gran Sasso at 3800\,m\,w.e. to be $(3.432 \pm 0.003)\cdot 10^{-4}\,\mathrm{{m^{-2}s^{-1}}}$ based on ten years of Borexino data acquired between May 2007 and May 2017. A seasonal modulation with a period of $(366.3 \pm 0.6)\,\mathrm{d}$ and a relative amplitude of $(1.36 \pm0.04)\%$ is observed. The phase is measured to be $(181.7 \pm 0.4)\,\mathrm{d}$, corresponding to a maximum at the 1$^\mathrm{st}$ of July. Using data inferred from global atmospheric models, we show the muon flux to be positively correlated with the atmospheric temperature and measure the effective temperature coefficient $伪_\mathrm{T} = 0.90 \pm 0.02$. The origin of cosmic muons from pion and kaon decays in the atmosphere allows to interpret the effective temperature coefficient as an indirect measurement of the atmospheric kaon-to-pion production ratio $r_{\mathrm{K}/蟺} = 0.11^{+0.11}_{-0.07}$ for primary energies above $18\,\mathrm{TeV}$. We find evidence for a long-term modulation of the muon flux with a period of $\sim 3000\,\mathrm{d}$ and a maximum in June 2012 that is not present in the atmospheric temperature data. A possible correlation between this modulation and the solar activity is investigated. The cosmogenic neutron production rate is found to show a seasonal modulation in phase with the cosmic muon flux but with an increased amplitude of $(2.6 \pm 0.4)\%$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.04207v3-abstract-full').style.display = 'none'; document.getElementById('1808.04207v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 16 figures, proofreading for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.11125">arXiv:1805.11125</a> <span> [<a href="https://arxiv.org/pdf/1805.11125">pdf</a>, <a href="https://arxiv.org/format/1805.11125">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/1342/1/012115">10.1088/1742-6596/1342/1/012115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Speeding up complex multivariate data analysis in Borexino with parallel computing based on Graphics Processing Unit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a> , et al. (82 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1805.11125v1-abstract-short" style="display: inline;"> A spectral fitter based on the graphics processor unit (GPU) has been developed for Borexino solar neutrino analysis. It is able to shorten the fitting time to a superior level compared to the CPU fitting procedure. In Borexino solar neutrino spectral analysis, fitting usually requires around one hour to converge since it includes time-consuming convolutions in order to account for the detector re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11125v1-abstract-full').style.display = 'inline'; document.getElementById('1805.11125v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.11125v1-abstract-full" style="display: none;"> A spectral fitter based on the graphics processor unit (GPU) has been developed for Borexino solar neutrino analysis. It is able to shorten the fitting time to a superior level compared to the CPU fitting procedure. In Borexino solar neutrino spectral analysis, fitting usually requires around one hour to converge since it includes time-consuming convolutions in order to account for the detector response and pile-up effects. Moreover, the convergence time increases to more than two days when including extra computations for the discrimination of $^{11}$C and external $纬$s. In sharp contrast, with the GPU-based fitter it takes less than 10 seconds and less than four minutes, respectively. This fitter is developed utilizing the GooFit project with customized likelihoods, pdfs and infrastructures supporting certain analysis methods. In this proceeding the design of the package, developed features and the comparison with the original CPU fitter are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11125v1-abstract-full').style.display = 'none'; document.getElementById('1805.11125v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures, proceeding for TAUP 2017 XV International Conference on Topics in Astroparticle and Underground Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> 1342 no. 012115 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Physics: Conference Series (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.00756">arXiv:1709.00756</a> <span> [<a href="https://arxiv.org/pdf/1709.00756">pdf</a>, <a href="https://arxiv.org/format/1709.00756">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.101.062001">10.1103/PhysRevD.101.062001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved measurement of $^8$B solar neutrinos with 1.5 kt y of Borexino exposure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+Borexino+Collaboration"> The Borexino Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Giacinto%2C+A">A. Di Giacinto</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Marcello%2C+V">V. Di Marcello</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a> , et al. (73 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1709.00756v2-abstract-short" style="display: inline;"> We report on an improved measurement of the $^8$B solar neutrino interaction rate with the Borexino experiment at the Laboratori Nazionali del Gran Sasso. Neutrinos are detected via their elastic scattering on electrons in a large volume of liquid scintillator. The measured rate of scattered electrons above 3 MeV of energy is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.00756v2-abstract-full').style.display = 'inline'; document.getElementById('1709.00756v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.00756v2-abstract-full" style="display: none;"> We report on an improved measurement of the $^8$B solar neutrino interaction rate with the Borexino experiment at the Laboratori Nazionali del Gran Sasso. Neutrinos are detected via their elastic scattering on electrons in a large volume of liquid scintillator. The measured rate of scattered electrons above 3 MeV of energy is $0.223\substack{+0.015 \\ -0.016}\,(stat)\,\substack{+0.006 \\ -0.006}\,(syst)$ cpd/100 t, which corresponds to an observed solar neutrino flux assuming no neutrino flavor conversion of $桅\substack{\rm ES \\ ^8\rm B}=2.57\substack{+0.17 \\ -0.18}(stat)\substack{+0.07\\ -0.07}(syst)\times$10$^6$ cm$^{-2}\,$s$^{-1}$. This measurement exploits the active volume of the detector in almost its entirety for the first time, and takes advantage of a reduced radioactive background following the 2011 scintillator purification campaign and of novel analysis tools providing a more precise modeling of the background. Additionally, we set a new limit on the interaction rate of solar $hep$ neutrinos, searched via their elastic scattering on electrons as well as their neutral current-mediated inelastic scattering on carbon, $^{12}$C($谓,谓'$)$^{12}$C* ($E_纬$= 15.1 MeV). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.00756v2-abstract-full').style.display = 'none'; document.getElementById('1709.00756v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 13 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 062001 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.09355">arXiv:1707.09355</a> <span> [<a href="https://arxiv.org/pdf/1707.09355">pdf</a>, <a href="https://arxiv.org/format/1707.09355">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.96.091103">10.1103/PhysRevD.96.091103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limiting neutrino magnetic moments with Borexino Phase-II solar neutrino data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a> , et al. (82 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.09355v3-abstract-short" style="display: inline;"> A search for the solar neutrino effective magnetic moment has been performed using data from 1291.5 days exposure during the second phase of the Borexino experiment. No significant deviations from the expected shape of the electron recoil spectrum from solar neutrinos have been found, and a new upper limit on the effective neutrino magnetic moment of $渭_谓^{eff}$ $<$ 2.8$\cdot$10$^{-11}$ $渭_{B}$ at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09355v3-abstract-full').style.display = 'inline'; document.getElementById('1707.09355v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.09355v3-abstract-full" style="display: none;"> A search for the solar neutrino effective magnetic moment has been performed using data from 1291.5 days exposure during the second phase of the Borexino experiment. No significant deviations from the expected shape of the electron recoil spectrum from solar neutrinos have been found, and a new upper limit on the effective neutrino magnetic moment of $渭_谓^{eff}$ $<$ 2.8$\cdot$10$^{-11}$ $渭_{B}$ at 90\% c.l. has been set using constraints on the sum of the solar neutrino fluxes implied by the radiochemical gallium experiments.Using the limit for the effective neutrino moment, new limits for the magnetic moments of the neutrino flavor states, and for the elements of the neutrino magnetic moments matrix for Dirac and Majorana neutrinos, are derived. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09355v3-abstract-full').style.display = 'none'; document.getElementById('1707.09355v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 96, 091103 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.09279">arXiv:1707.09279</a> <span> [<a href="https://arxiv.org/pdf/1707.09279">pdf</a>, <a href="https://arxiv.org/format/1707.09279">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.100.082004">10.1103/PhysRevD.100.082004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simultaneous Precision Spectroscopy of $pp$, $^7$Be, and $pep$ Solar Neutrinos with Borexino Phase-II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=Collica%2C+L">L. Collica</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a> , et al. (82 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.09279v3-abstract-short" style="display: inline;"> We present the first simultaneous measurement of the interaction rates of $pp$, $^7$Be, and $pep$ solar neutrinos performed with a global fit to the Borexino data in an extended energy range (0.19-2.93)$\,$MeV. This result was obtained by analyzing 1291.51$\,$days of Borexino Phase-II data, collected between December 2011 and May 2016 after an extensive scintillator purification campaign. We find:… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09279v3-abstract-full').style.display = 'inline'; document.getElementById('1707.09279v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.09279v3-abstract-full" style="display: none;"> We present the first simultaneous measurement of the interaction rates of $pp$, $^7$Be, and $pep$ solar neutrinos performed with a global fit to the Borexino data in an extended energy range (0.19-2.93)$\,$MeV. This result was obtained by analyzing 1291.51$\,$days of Borexino Phase-II data, collected between December 2011 and May 2016 after an extensive scintillator purification campaign. We find: rate($pp$)$\,$=$\,$$134$$\,$$\pm$$\,$$10$$\,$($stat$)$\,$$^{\rm +6}_{\rm -10}$$\,$($sys$)$\,$cpd/100$\,$t, rate($^7$Be)$\,$=$\,$$48.3$$\,$$\pm$$\,$$1.1$$\,$($stat$)$\,$$^{\rm +0.4}_{\rm -0.7}$$\,$($sys$)$\,$cpd/100$\,$t, and rate($pep$)$\,$=$\,$$2.43$$\pm$$\,$$0.36$$\,$($stat$)$^{+0.15}_{-0.22}$$\,$($sys$)$\,$cpd/100$\,$t. These numbers are in agreement with and improve the precision of our previous measurements. In particular, the interaction rate of $^7$Be $谓$'s is measured with an unprecedented precision of 2.7%, showing that discriminating between the high and low metallicity solar models is now largely dominated by theoretical uncertainties. The absence of $pep$ neutrinos is rejected for the first time at more than 5$\,$$蟽$. An upper limit of $8.1$$\,$cpd/100$\,$t (95%$\,$C.L.) on the CNO neutrino rate is obtained by setting an additional constraint on the ratio between the $pp$ and $pep$ neutrino rates in the fit. This limit has the same significance as that obtained by the Borexino Phase-I (currently providing the tightest bound on this component), but is obtained by applying a less stringent constraint on the $pep$ $谓$ flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.09279v3-abstract-full').style.display = 'none'; document.getElementById('1707.09279v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 100, 082004 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.10176">arXiv:1706.10176</a> <span> [<a href="https://arxiv.org/pdf/1706.10176">pdf</a>, <a href="https://arxiv.org/ps/1706.10176">ps</a>, <a href="https://arxiv.org/format/1706.10176">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aa9521">10.3847/1538-4357/aa9521 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for low-energy neutrinos correlated with gravitational wave events GW150914, GW151226 and GW170104 with the Borexino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Ludovico%2C+A">A. Di Ludovico</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a> , et al. (77 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1706.10176v1-abstract-short" style="display: inline;"> We present the results of a low-energy neutrino search using the Borexino detector in coincidence with the gravitational wave (GW) events GW150914, GW151226 and GW170104. We searched for correlated neutrino events with energies greater than 250 keV within a time window of $\pm500$ s centered around the GW detection time. A total of five candidates were found for all three GW150914, GW151226 and GW… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.10176v1-abstract-full').style.display = 'inline'; document.getElementById('1706.10176v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.10176v1-abstract-full" style="display: none;"> We present the results of a low-energy neutrino search using the Borexino detector in coincidence with the gravitational wave (GW) events GW150914, GW151226 and GW170104. We searched for correlated neutrino events with energies greater than 250 keV within a time window of $\pm500$ s centered around the GW detection time. A total of five candidates were found for all three GW150914, GW151226 and GW170104. This is consistent with the number of expected solar neutrino and background events. As a result, we have obtained the best current upper limits on the GW event neutrino fluence of all flavors ($谓_e, 谓_渭, 谓_蟿$) in the energy range $(0.5 - 5.0)$ MeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.10176v1-abstract-full').style.display = 'none'; document.getElementById('1706.10176v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2017 Astrophys. J. 850 21 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1704.02291">arXiv:1704.02291</a> <span> [<a href="https://arxiv.org/pdf/1704.02291">pdf</a>, <a href="https://arxiv.org/format/1704.02291">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2017.10.003">10.1016/j.astropartphys.2017.10.003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Monte Carlo simulation of the Borexino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Bagdasarian%2C+Z">Z. Bagdasarian</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Borodikhina%2C+L">L. Borodikhina</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a> , et al. (75 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1704.02291v1-abstract-short" style="display: inline;"> We describe the Monte Carlo (MC) simulation package of the Borexino detector and discuss the agreement of its output with data. The Borexino MC 'ab initio' simulates the energy loss of particles in all detector components and generates the resulting scintillation photons and their propagation within the liquid scintillator volume. The simulation accounts for absorption, reemission, and scattering… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.02291v1-abstract-full').style.display = 'inline'; document.getElementById('1704.02291v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.02291v1-abstract-full" style="display: none;"> We describe the Monte Carlo (MC) simulation package of the Borexino detector and discuss the agreement of its output with data. The Borexino MC 'ab initio' simulates the energy loss of particles in all detector components and generates the resulting scintillation photons and their propagation within the liquid scintillator volume. The simulation accounts for absorption, reemission, and scattering of the optical photons and tracks them until they either are absorbed or reach the photocathode of one of the photomultiplier tubes. Photon detection is followed by a comprehensive simulation of the readout electronics response. The algorithm proceeds with a detailed simulation of the electronics chain. The MC is tuned using data collected with radioactive calibration sources deployed inside and around the scintillator volume. The simulation reproduces the energy response of the detector, its uniformity within the fiducial scintillator volume relevant to neutrino physics, and the time distribution of detected photons to better than 1% between 100 keV and several MeV. The techniques developed to simulate the Borexino detector and their level of refinement are of possible interest to the neutrino community, especially for current and future large-volume liquid scintillator experiments such as Kamland-Zen, SNO+, and Juno. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.02291v1-abstract-full').style.display = 'none'; document.getElementById('1704.02291v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.07970">arXiv:1701.07970</a> <span> [<a href="https://arxiv.org/pdf/1701.07970">pdf</a>, <a href="https://arxiv.org/format/1701.07970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2017.04.004">10.1016/j.astropartphys.2017.04.004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Seasonal Modulation of the $^7$Be Solar Neutrino Rate in Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Agostini%2C+M">M. Agostini</a>, <a href="/search/hep-ex?searchtype=author&query=Altenmuller%2C+K">K. Altenmuller</a>, <a href="/search/hep-ex?searchtype=author&query=Appel%2C+S">S. Appel</a>, <a href="/search/hep-ex?searchtype=author&query=Atroshchenko%2C+V">V. Atroshchenko</a>, <a href="/search/hep-ex?searchtype=author&query=Basilico%2C+D">D. Basilico</a>, <a href="/search/hep-ex?searchtype=author&query=Bellini%2C+G">G. Bellini</a>, <a href="/search/hep-ex?searchtype=author&query=Benziger%2C+J">J. Benziger</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Bonfini%2C+G">G. Bonfini</a>, <a href="/search/hep-ex?searchtype=author&query=Borodikhina%2C+L">L. Borodikhina</a>, <a href="/search/hep-ex?searchtype=author&query=Bravo%2C+D">D. Bravo</a>, <a href="/search/hep-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/hep-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/hep-ex?searchtype=author&query=Caminata%2C+A">A. Caminata</a>, <a href="/search/hep-ex?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/hep-ex?searchtype=author&query=Carlini%2C+M">M. Carlini</a>, <a href="/search/hep-ex?searchtype=author&query=Cavalcante%2C+P">P. Cavalcante</a>, <a href="/search/hep-ex?searchtype=author&query=Chepurnov%2C+A">A. Chepurnov</a>, <a href="/search/hep-ex?searchtype=author&query=Choi%2C+K">K. Choi</a>, <a href="/search/hep-ex?searchtype=author&query=D%27Angelo%2C+D">D. D'Angelo</a>, <a href="/search/hep-ex?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/hep-ex?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/hep-ex?searchtype=author&query=Ding%2C+X+F">X. F. Ding</a>, <a href="/search/hep-ex?searchtype=author&query=Di+Noto%2C+L">L. Di Noto</a>, <a href="/search/hep-ex?searchtype=author&query=Drachnev%2C+I">I. Drachnev</a> , et al. (77 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1701.07970v2-abstract-short" style="display: inline;"> We detected the seasonal modulation of the $^7$Be neutrino interaction rate with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. The period, amplitude, and phase of the observed time evolution of the signal are consistent with its solar origin, and the absence of an annual modulation is rejected at 99.99\% C.L. The data are analyzed using three methods: the sinusoidal fi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.07970v2-abstract-full').style.display = 'inline'; document.getElementById('1701.07970v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.07970v2-abstract-full" style="display: none;"> We detected the seasonal modulation of the $^7$Be neutrino interaction rate with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. The period, amplitude, and phase of the observed time evolution of the signal are consistent with its solar origin, and the absence of an annual modulation is rejected at 99.99\% C.L. The data are analyzed using three methods: the sinusoidal fit, the Lomb-Scargle and the Empirical Mode Decomposition techniques, which all yield results in excellent agreement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.07970v2-abstract-full').style.display = 'none'; document.getElementById('1701.07970v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 palese, 13 figures</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: 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