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is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1674-1137/ad83aa">10.1088/1674-1137/ad83aa <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prediction of Energy Resolution in the JUNO Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Adamowicz%2C+K">Kai Adamowicz</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">Marco Beretta</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Bick%2C+D">Daniel Bick</a> , et al. (629 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.17860v2-abstract-short" style="display: inline;"> This paper presents an energy resolution study of the JUNO experiment, incorporating the latest knowledge acquired during the detector construction phase. The determination of neutrino mass ordering in JUNO requires an exceptional energy resolution better than 3\% at 1~MeV. To achieve this ambitious goal, significant efforts have been undertaken in the design and production of the key components o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17860v2-abstract-full').style.display = 'inline'; document.getElementById('2405.17860v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17860v2-abstract-full" style="display: none;"> This paper presents an energy resolution study of the JUNO experiment, incorporating the latest knowledge acquired during the detector construction phase. The determination of neutrino mass ordering in JUNO requires an exceptional energy resolution better than 3\% at 1~MeV. To achieve this ambitious goal, significant efforts have been undertaken in the design and production of the key components of the JUNO detector. Various factors affecting the detection of inverse beta decay signals have an impact on the energy resolution, extending beyond the statistical fluctuations of the detected number of photons, such as the properties of the liquid scintillator, performance of photomultiplier tubes, and the energy reconstruction algorithm. To account for these effects, a full JUNO simulation and reconstruction approach is employed. This enables the modeling of all relevant effects and the evaluation of associated inputs to accurately estimate the energy resolution. The results of study reveal an energy resolution of 2.95\% at 1~MeV. Furthermore, this study assesses the contribution of major effects to the overall energy resolution budget. This analysis serves as a reference for interpreting future measurements of energy resolution during JUNO data collection. Moreover, it provides a guideline for comprehending the energy resolution characteristics of liquid scintillator-based detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17860v2-abstract-full').style.display = 'none'; document.getElementById('2405.17860v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Chinese Phys. C 49 013003 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.05172">arXiv:2303.05172</a> <span> [<a href="https://arxiv.org/pdf/2303.05172">pdf</a>, <a href="https://arxiv.org/format/2303.05172">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2023.168680">10.1016/j.nima.2023.168680 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The JUNO experiment Top Tracker </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/physics?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a> , et al. (592 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.05172v1-abstract-short" style="display: inline;"> The main task of the Top Tracker detector of the neutrino reactor experiment Jiangmen Underground Neutrino Observatory (JUNO) is to reconstruct and extrapolate atmospheric muon tracks down to the central detector. This muon tracker will help to evaluate the contribution of the cosmogenic background to the signal. The Top Tracker is located above JUNO's water Cherenkov Detector and Central Detector… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.05172v1-abstract-full').style.display = 'inline'; document.getElementById('2303.05172v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.05172v1-abstract-full" style="display: none;"> The main task of the Top Tracker detector of the neutrino reactor experiment Jiangmen Underground Neutrino Observatory (JUNO) is to reconstruct and extrapolate atmospheric muon tracks down to the central detector. This muon tracker will help to evaluate the contribution of the cosmogenic background to the signal. The Top Tracker is located above JUNO's water Cherenkov Detector and Central Detector, covering about 60% of the surface above them. The JUNO Top Tracker is constituted by the decommissioned OPERA experiment Target Tracker modules. The technology used consists in walls of two planes of plastic scintillator strips, one per transverse direction. Wavelength shifting fibres collect the light signal emitted by the scintillator strips and guide it to both ends where it is read by multianode photomultiplier tubes. Compared to the OPERA Target Tracker, the JUNO Top Tracker uses new electronics able to cope with the high rate produced by the high rock radioactivity compared to the one in Gran Sasso underground laboratory. This paper will present the new electronics and mechanical structure developed for the Top Tracker of JUNO along with its expected performance based on the current detector simulation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.05172v1-abstract-full').style.display = 'none'; document.getElementById('2303.05172v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Instrum.Meth.A 1057 (2023) 168680 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.03910">arXiv:2303.03910</a> <span> [<a href="https://arxiv.org/pdf/2303.03910">pdf</a>, <a href="https://arxiv.org/format/2303.03910">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> JUNO sensitivity to $^7$Be, $pep$, and CNO solar neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/physics?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">Marco Beretta</a> , et al. (592 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.03910v1-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO), the first multi-kton liquid scintillator detector, which is under construction in China, will have a unique potential to perform a real-time measurement of solar neutrinos well below the few MeV threshold typical for Water Cherenkov detectors. JUNO's large target mass and excellent energy resolution are prerequisites for reaching unprecedented… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03910v1-abstract-full').style.display = 'inline'; document.getElementById('2303.03910v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.03910v1-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO), the first multi-kton liquid scintillator detector, which is under construction in China, will have a unique potential to perform a real-time measurement of solar neutrinos well below the few MeV threshold typical for Water Cherenkov detectors. JUNO's large target mass and excellent energy resolution are prerequisites for reaching unprecedented levels of precision. In this paper, we provide estimation of the JUNO sensitivity to 7Be, pep, and CNO solar neutrinos that can be obtained via a spectral analysis above the 0.45 MeV threshold. This study is performed assuming different scenarios of the liquid scintillator radiopurity, ranging from the most opti mistic one corresponding to the radiopurity levels obtained by the Borexino experiment, up to the minimum requirements needed to perform the neutrino mass ordering determination with reactor antineutrinos - the main goal of JUNO. Our study shows that in most scenarios, JUNO will be able to improve the current best measurements on 7Be, pep, and CNO solar neutrino fluxes. We also perform a study on the JUNO capability to detect periodical time variations in the solar neutrino flux, such as the day-night modulation induced by neutrino flavor regeneration in Earth, and the modulations induced by temperature changes driven by helioseismic waves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03910v1-abstract-full').style.display = 'none'; document.getElementById('2303.03910v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.08830">arXiv:2205.08830</a> <span> [<a href="https://arxiv.org/pdf/2205.08830">pdf</a>, <a href="https://arxiv.org/format/2205.08830">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2022/10/033">10.1088/1475-7516/2022/10/033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for Detecting the Diffuse Supernova Neutrino Background with JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a>, <a href="/search/physics?searchtype=author&query=Blin%2C+S">Sylvie Blin</a> , et al. (577 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.08830v2-abstract-short" style="display: inline;"> We present the detection potential for the diffuse supernova neutrino background (DSNB) at the Jiangmen Underground Neutrino Observatory (JUNO), using the inverse-beta-decay (IBD) detection channel on free protons. We employ the latest information on the DSNB flux predictions, and investigate in detail the background and its reduction for the DSNB search at JUNO. The atmospheric neutrino induced n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08830v2-abstract-full').style.display = 'inline'; document.getElementById('2205.08830v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.08830v2-abstract-full" style="display: none;"> We present the detection potential for the diffuse supernova neutrino background (DSNB) at the Jiangmen Underground Neutrino Observatory (JUNO), using the inverse-beta-decay (IBD) detection channel on free protons. We employ the latest information on the DSNB flux predictions, and investigate in detail the background and its reduction for the DSNB search at JUNO. The atmospheric neutrino induced neutral current (NC) background turns out to be the most critical background, whose uncertainty is carefully evaluated from both the spread of model predictions and an envisaged \textit{in situ} measurement. We also make a careful study on the background suppression with the pulse shape discrimination (PSD) and triple coincidence (TC) cuts. With latest DSNB signal predictions, more realistic background evaluation and PSD efficiency optimization, and additional TC cut, JUNO can reach the significance of 3$蟽$ for 3 years of data taking, and achieve better than 5$蟽$ after 10 years for a reference DSNB model. In the pessimistic scenario of non-observation, JUNO would strongly improve the limits and exclude a significant region of the model parameter space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08830v2-abstract-full').style.display = 'none'; document.getElementById('2205.08830v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 11 figures, final published version in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 10 (2022) 033 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.08629">arXiv:2205.08629</a> <span> [<a href="https://arxiv.org/pdf/2205.08629">pdf</a>, <a href="https://arxiv.org/format/2205.08629">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-022-11002-8">10.1140/epjc/s10052-022-11002-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mass Testing and Characterization of 20-inch PMTs for JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/physics?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andre%2C+J+P+A+M">Joao Pedro Athayde Marcondes de Andre</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/physics?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a> , et al. (541 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.08629v2-abstract-short" style="display: inline;"> Main goal of the JUNO experiment is to determine the neutrino mass ordering using a 20kt liquid-scintillator detector. Its key feature is an excellent energy resolution of at least 3 % at 1 MeV, for which its instruments need to meet a certain quality and thus have to be fully characterized. More than 20,000 20-inch PMTs have been received and assessed by JUNO after a detailed testing program whic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08629v2-abstract-full').style.display = 'inline'; document.getElementById('2205.08629v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.08629v2-abstract-full" style="display: none;"> Main goal of the JUNO experiment is to determine the neutrino mass ordering using a 20kt liquid-scintillator detector. Its key feature is an excellent energy resolution of at least 3 % at 1 MeV, for which its instruments need to meet a certain quality and thus have to be fully characterized. More than 20,000 20-inch PMTs have been received and assessed by JUNO after a detailed testing program which began in 2017 and elapsed for about four years. Based on this mass characterization and a set of specific requirements, a good quality of all accepted PMTs could be ascertained. This paper presents the performed testing procedure with the designed testing systems as well as the statistical characteristics of all 20-inch PMTs intended to be used in the JUNO experiment, covering more than fifteen performance parameters including the photocathode uniformity. This constitutes the largest sample of 20-inch PMTs ever produced and studied in detail to date, i.e. 15,000 of the newly developed 20-inch MCP-PMTs from Northern Night Vision Technology Co. (NNVT) and 5,000 of dynode PMTs from Hamamatsu Photonics K. K.(HPK). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08629v2-abstract-full').style.display = 'none'; document.getElementById('2205.08629v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.03669">arXiv:2107.03669</a> <span> [<a href="https://arxiv.org/pdf/2107.03669">pdf</a>, <a href="https://arxiv.org/format/2107.03669">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/JHEP11(2021)102">10.1007/JHEP11(2021)102 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radioactivity control strategy for the JUNO detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+collaboration"> JUNO collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Babic%2C+A">Andrej Babic</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a>, <a href="/search/physics?searchtype=author&query=Blin%2C+S">Sylvie Blin</a> , et al. (578 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.03669v2-abstract-short" style="display: inline;"> JUNO is a massive liquid scintillator detector with a primary scientific goal of determining the neutrino mass ordering by studying the oscillated anti-neutrino flux coming from two nuclear power plants at 53 km distance. The expected signal anti-neutrino interaction rate is only 60 counts per day, therefore a careful control of the background sources due to radioactivity is critical. In particula… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03669v2-abstract-full').style.display = 'inline'; document.getElementById('2107.03669v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.03669v2-abstract-full" style="display: none;"> JUNO is a massive liquid scintillator detector with a primary scientific goal of determining the neutrino mass ordering by studying the oscillated anti-neutrino flux coming from two nuclear power plants at 53 km distance. The expected signal anti-neutrino interaction rate is only 60 counts per day, therefore a careful control of the background sources due to radioactivity is critical. In particular, natural radioactivity present in all materials and in the environment represents a serious issue that could impair the sensitivity of the experiment if appropriate countermeasures were not foreseen. In this paper we discuss the background reduction strategies undertaken by the JUNO collaboration to reduce at minimum the impact of natural radioactivity. We describe our efforts for an optimized experimental design, a careful material screening and accurate detector production handling, and a constant control of the expected results through a meticulous Monte Carlo simulation program. We show that all these actions should allow us to keep the background count rate safely below the target value of 10 Hz in the default fiducial volume, above an energy threshold of 0.7 MeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03669v2-abstract-full').style.display = 'none'; document.getElementById('2107.03669v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 12 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/2103.16900">arXiv:2103.16900</a> <span> [<a href="https://arxiv.org/pdf/2103.16900">pdf</a>, <a href="https://arxiv.org/format/2103.16900">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> The Design and Sensitivity of JUNO's scintillator radiopurity pre-detector OSIRIS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+G">Guangpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Babic%2C+A">Andrej Babic</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a> , 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="2103.16900v1-abstract-short" style="display: inline;"> The OSIRIS detector is a subsystem of the liquid scintillator fillling chain of the JUNO reactor neutrino experiment. Its purpose is to validate the radiopurity of the scintillator to assure that all components of the JUNO scintillator system work to specifications and only neutrino-grade scintillator is filled into the JUNO Central Detector. The aspired sensitivity level of $10^{-16}$ g/g of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.16900v1-abstract-full').style.display = 'inline'; document.getElementById('2103.16900v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.16900v1-abstract-full" style="display: none;"> The OSIRIS detector is a subsystem of the liquid scintillator fillling chain of the JUNO reactor neutrino experiment. Its purpose is to validate the radiopurity of the scintillator to assure that all components of the JUNO scintillator system work to specifications and only neutrino-grade scintillator is filled into the JUNO Central Detector. The aspired sensitivity level of $10^{-16}$ g/g of $^{238}$U and $^{232}$Th requires a large ($\sim$20 m$^3$) detection volume and ultralow background levels. The present paper reports on the design and major components of the OSIRIS detector, the detector simulation as well as the measuring strategies foreseen and the sensitivity levels to U/Th that can be reached in this setup. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.16900v1-abstract-full').style.display = 'none'; document.getElementById('2103.16900v1-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">32 pages, 22 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/2011.06405">arXiv:2011.06405</a> <span> [<a href="https://arxiv.org/pdf/2011.06405">pdf</a>, <a href="https://arxiv.org/format/2011.06405">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/10.1007/JHEP03(2021)004">10.1007/JHEP03(2021)004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration Strategy of the JUNO Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+collaboration"> JUNO collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+G">Guangpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Babic%2C+A">Andrej Babic</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Bernieri%2C+E">Enrico Bernieri</a>, <a href="/search/physics?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a> , et al. (571 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="2011.06405v3-abstract-short" style="display: inline;"> We present the calibration strategy for the 20 kton liquid scintillator central detector of the Jiangmen Underground Neutrino Observatory (JUNO). By utilizing a comprehensive multiple-source and multiple-positional calibration program, in combination with a novel dual calorimetry technique exploiting two independent photosensors and readout systems, we demonstrate that the JUNO central detector ca… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06405v3-abstract-full').style.display = 'inline'; document.getElementById('2011.06405v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.06405v3-abstract-full" style="display: none;"> We present the calibration strategy for the 20 kton liquid scintillator central detector of the Jiangmen Underground Neutrino Observatory (JUNO). By utilizing a comprehensive multiple-source and multiple-positional calibration program, in combination with a novel dual calorimetry technique exploiting two independent photosensors and readout systems, we demonstrate that the JUNO central detector can achieve a better than 1% energy linearity and a 3% effective energy resolution, required by the neutrino mass ordering determination. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06405v3-abstract-full').style.display = 'none'; document.getElementById('2011.06405v3-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.00314">arXiv:2007.00314</a> <span> [<a href="https://arxiv.org/pdf/2007.00314">pdf</a>, <a href="https://arxiv.org/format/2007.00314">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"> Optimization of the JUNO liquid scintillator composition using a Daya Bay antineutrino detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bay%2C+D">Daya Bay</a>, <a href="/search/physics?searchtype=author&query=collaborations%2C+J">JUNO collaborations</a>, <a href="/search/physics?searchtype=author&query=%3A"> :</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">A. Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">T. Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">S. Ahmad</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">M. Akram</a>, <a href="/search/physics?searchtype=author&query=Ali%2C+N">N. Ali</a>, <a href="/search/physics?searchtype=author&query=An%2C+F+P">F. P. An</a>, <a href="/search/physics?searchtype=author&query=An%2C+G+P">G. P. An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">N. Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">T. Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">B. Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">J. P. A. M. de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Babic%2C+A">A. Babic</a>, <a href="/search/physics?searchtype=author&query=Balantekin%2C+A+B">A. B. Balantekin</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">W. Baldini</a>, <a href="/search/physics?searchtype=author&query=Baldoncini%2C+M">M. Baldoncini</a>, <a href="/search/physics?searchtype=author&query=Band%2C+H+R">H. R. Band</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">E. Baussan</a> , et al. (642 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.00314v1-abstract-short" style="display: inline;"> To maximize the light yield of the liquid scintillator (LS) for the Jiangmen Underground Neutrino Observatory (JUNO), a 20 t LS sample was produced in a pilot plant at Daya Bay. The optical properties of the new LS in various compositions were studied by replacing the gadolinium-loaded LS in one antineutrino detector. The concentrations of the fluor, PPO, and the wavelength shifter, bis-MSB, were… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.00314v1-abstract-full').style.display = 'inline'; document.getElementById('2007.00314v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.00314v1-abstract-full" style="display: none;"> To maximize the light yield of the liquid scintillator (LS) for the Jiangmen Underground Neutrino Observatory (JUNO), a 20 t LS sample was produced in a pilot plant at Daya Bay. The optical properties of the new LS in various compositions were studied by replacing the gadolinium-loaded LS in one antineutrino detector. The concentrations of the fluor, PPO, and the wavelength shifter, bis-MSB, were increased in 12 steps from 0.5 g/L and <0.01 mg/L to 4 g/L and 13 mg/L, respectively. The numbers of total detected photoelectrons suggest that, with the optically purified solvent, the bis-MSB concentration does not need to be more than 4 mg/L. To bridge the one order of magnitude in the detector size difference between Daya Bay and JUNO, the Daya Bay data were used to tune the parameters of a newly developed optical model. Then, the model and tuned parameters were used in the JUNO simulation. This enabled to determine the optimal composition for the JUNO LS: purified solvent LAB with 2.5 g/L PPO, and 1 to 4 mg/L bis-MSB. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.00314v1-abstract-full').style.display = 'none'; document.getElementById('2007.00314v1-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.11760">arXiv:2006.11760</a> <span> [<a href="https://arxiv.org/pdf/2006.11760">pdf</a>, <a href="https://arxiv.org/format/2006.11760">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Feasibility and physics potential of detecting $^8$B solar neutrinos at JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+collaboration"> JUNO collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=Ali%2C+N">Nawab Ali</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+G">Guangpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Babic%2C+A">Andrej Babic</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Bernieri%2C+E">Enrico Bernieri</a>, <a href="/search/physics?searchtype=author&query=Biare%2C+D">David Biare</a> , et al. (572 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="2006.11760v1-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory~(JUNO) features a 20~kt multi-purpose underground liquid scintillator sphere as its main detector. Some of JUNO's features make it an excellent experiment for $^8$B solar neutrino measurements, such as its low-energy threshold, its high energy resolution compared to water Cherenkov detectors, and its much large target mass compared to previous liquid s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.11760v1-abstract-full').style.display = 'inline'; document.getElementById('2006.11760v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.11760v1-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory~(JUNO) features a 20~kt multi-purpose underground liquid scintillator sphere as its main detector. Some of JUNO's features make it an excellent experiment for $^8$B solar neutrino measurements, such as its low-energy threshold, its high energy resolution compared to water Cherenkov detectors, and its much large target mass compared to previous liquid scintillator detectors. In this paper we present a comprehensive assessment of JUNO's potential for detecting $^8$B solar neutrinos via the neutrino-electron elastic scattering process. A reduced 2~MeV threshold on the recoil electron energy is found to be achievable assuming the intrinsic radioactive background $^{238}$U and $^{232}$Th in the liquid scintillator can be controlled to 10$^{-17}$~g/g. With ten years of data taking, about 60,000 signal and 30,000 background events are expected. This large sample will enable an examination of the distortion of the recoil electron spectrum that is dominated by the neutrino flavor transformation in the dense solar matter, which will shed new light on the tension between the measured electron spectra and the predictions of the standard three-flavor neutrino oscillation framework. If $螖m^{2}_{21}=4.8\times10^{-5}~(7.5\times10^{-5})$~eV$^{2}$, JUNO can provide evidence of neutrino oscillation in the Earth at the about 3$蟽$~(2$蟽$) level by measuring the non-zero signal rate variation with respect to the solar zenith angle. Moveover, JUNO can simultaneously measure $螖m^2_{21}$ using $^8$B solar neutrinos to a precision of 20\% or better depending on the central value and to sub-percent precision using reactor antineutrinos. A comparison of these two measurements from the same detector will help elucidate the current tension between the value of $螖m^2_{21}$ reported by solar neutrino experiments and the KamLAND experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.11760v1-abstract-full').style.display = 'none'; document.getElementById('2006.11760v1-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 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">29 pages, 14 plots, 7 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/2005.08745">arXiv:2005.08745</a> <span> [<a href="https://arxiv.org/pdf/2005.08745">pdf</a>, <a href="https://arxiv.org/format/2005.08745">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> TAO Conceptual Design Report: A Precision Measurement of the Reactor Antineutrino Spectrum with Sub-percent Energy Resolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/physics?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/physics?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/physics?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/physics?searchtype=author&query=Ali%2C+N">Nawab Ali</a>, <a href="/search/physics?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+G">Guangpeng An</a>, <a href="/search/physics?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/physics?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/physics?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/physics?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/physics?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/physics?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/physics?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/physics?searchtype=author&query=Babic%2C+A">Andrej Babic</a>, <a href="/search/physics?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/physics?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/physics?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/physics?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/physics?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/physics?searchtype=author&query=Bernieri%2C+E">Enrico Bernieri</a>, <a href="/search/physics?searchtype=author&query=Biare%2C+D">David Biare</a> , et al. (568 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="2005.08745v1-abstract-short" style="display: inline;"> The Taishan Antineutrino Observatory (TAO, also known as JUNO-TAO) is a satellite experiment of the Jiangmen Underground Neutrino Observatory (JUNO). A ton-level liquid scintillator detector will be placed at about 30 m from a core of the Taishan Nuclear Power Plant. The reactor antineutrino spectrum will be measured with sub-percent energy resolution, to provide a reference spectrum for future re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.08745v1-abstract-full').style.display = 'inline'; document.getElementById('2005.08745v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.08745v1-abstract-full" style="display: none;"> The Taishan Antineutrino Observatory (TAO, also known as JUNO-TAO) is a satellite experiment of the Jiangmen Underground Neutrino Observatory (JUNO). A ton-level liquid scintillator detector will be placed at about 30 m from a core of the Taishan Nuclear Power Plant. The reactor antineutrino spectrum will be measured with sub-percent energy resolution, to provide a reference spectrum for future reactor neutrino experiments, and to provide a benchmark measurement to test nuclear databases. A spherical acrylic vessel containing 2.8 ton gadolinium-doped liquid scintillator will be viewed by 10 m^2 Silicon Photomultipliers (SiPMs) of >50% photon detection efficiency with almost full coverage. The photoelectron yield is about 4500 per MeV, an order higher than any existing large-scale liquid scintillator detectors. The detector operates at -50 degree C to lower the dark noise of SiPMs to an acceptable level. The detector will measure about 2000 reactor antineutrinos per day, and is designed to be well shielded from cosmogenic backgrounds and ambient radioactivities to have about 10% background-to-signal ratio. The experiment is expected to start operation in 2022. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.08745v1-abstract-full').style.display = 'none'; document.getElementById('2005.08745v1-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 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">134 pages, 114 figures</span> </p> </li> </ol> <div class="is-hidden-tablet"> <!-- feedback for mobile only --> <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a> </span> </div> </div> </main> <footer> <div class="columns is-desktop" 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