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is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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="2405.17792v1-abstract-short" style="display: inline;"> We explore the bound neutrons decay into invisible particles (e.g., $n\rightarrow 3 谓$ or $nn \rightarrow 2 谓$) in the JUNO liquid scintillator detector. 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 mode… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17792v1-abstract-full').style.display = 'inline'; document.getElementById('2405.17792v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17792v1-abstract-full" style="display: none;"> We explore the bound neutrons decay into invisible particles (e.g., $n\rightarrow 3 谓$ or $nn \rightarrow 2 谓$) in the JUNO liquid scintillator detector. 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('2405.17792v1-abstract-full').style.display = 'none'; document.getElementById('2405.17792v1-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, 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">28 pages, 7 figures, 4 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/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/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/2303.05172">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/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/2205.08830">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/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/2104.02565">arXiv:2104.02565</a> <span> [<a href="https://arxiv.org/pdf/2104.02565">pdf</a>, <a href="https://arxiv.org/format/2104.02565">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/10.1016/j.ppnp.2021.103927">10.1016/j.ppnp.2021.103927 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JUNO Physics and Detector </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+G">Guangpeng 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=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=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=Bernieri%2C+E">Enrico Bernieri</a>, <a href="/search/hep-ex?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a> , et al. (591 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="2104.02565v2-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a 20 kton LS detector at 700-m underground. An excellent energy resolution and a large fiducial volume offer exciting opportunities for addressing many important topics in neutrino and astro-particle physics. With 6 years of data, the neutrino mass ordering can be determined at 3-4 sigma and three oscillation parameters can be measured to a p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02565v2-abstract-full').style.display = 'inline'; document.getElementById('2104.02565v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.02565v2-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO) is a 20 kton LS detector at 700-m underground. An excellent energy resolution and a large fiducial volume offer exciting opportunities for addressing many important topics in neutrino and astro-particle physics. With 6 years of data, the neutrino mass ordering can be determined at 3-4 sigma and three oscillation parameters can be measured to a precision of 0.6% or better by detecting reactor antineutrinos. With 10 years of data, DSNB could be observed at 3-sigma; a lower limit of the proton lifetime of 8.34e33 years (90% C.L.) can be set by searching for p->nu_bar K^+; detection of solar neutrinos would shed new light on the solar metallicity problem and examine the vacuum-matter transition region. A core-collapse supernova at 10 kpc would lead to ~5000 IBD and ~2000 (300) all-flavor neutrino-proton (electron) scattering events. Geo-neutrinos can be detected with a rate of ~400 events/year. We also summarize the final design of the JUNO detector and the key R&D achievements. All 20-inch PMTs have been tested. The average photon detection efficiency is 28.9% for the 15,000 MCP PMTs and 28.1% for the 5,000 dynode PMTs, higher than the JUNO requirement of 27%. Together with the >20 m attenuation length of LS, we expect a yield of 1345 p.e. per MeV and an effective energy resolution of 3.02%/\sqrt{E (MeV)}$ in simulations. The underwater electronics is designed to have a loss rate <0.5% in 6 years. With degassing membranes and a micro-bubble system, the radon concentration in the 35-kton water pool could be lowered to <10 mBq/m^3. Acrylic panels of radiopurity <0.5 ppt U/Th are produced. The 20-kton LS will be purified onsite. Singles in the fiducial volume can be controlled to ~10 Hz. The JUNO experiment also features a double calorimeter system with 25,600 3-inch PMTs, a LS testing facility OSIRIS, and a near detector TAO. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02565v2-abstract-full').style.display = 'none'; document.getElementById('2104.02565v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">A review paper with 78 pages and 32 figures. v2: minor revision. Final version to appear in Progress in Particle and Nuclear Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.09908">arXiv:2103.09908</a> <span> [<a href="https://arxiv.org/pdf/2103.09908">pdf</a>, <a href="https://arxiv.org/format/2103.09908">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/10.1140/epjc/s10052-021-09565-z">10.1140/epjc/s10052-021-09565-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JUNO sensitivity to low energy atmospheric neutrino spectra </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+G">Guangpeng 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=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=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=Bernieri%2C+E">Enrico Bernieri</a>, <a href="/search/hep-ex?searchtype=author&query=Birkenfeld%2C+T">Thilo Birkenfeld</a> , et al. (588 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="2103.09908v3-abstract-short" style="display: inline;"> Atmospheric neutrinos are one of the most relevant natural neutrino sources that can be exploited to infer properties about cosmic rays and neutrino oscillations. The Jiangmen Underground Neutrino Observatory (JUNO) experiment, a 20 kton liquid scintillator detector with excellent energy resolution is currently under construction in China. JUNO will be able to detect several atmospheric neutrinos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.09908v3-abstract-full').style.display = 'inline'; document.getElementById('2103.09908v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.09908v3-abstract-full" style="display: none;"> Atmospheric neutrinos are one of the most relevant natural neutrino sources that can be exploited to infer properties about cosmic rays and neutrino oscillations. The Jiangmen Underground Neutrino Observatory (JUNO) experiment, a 20 kton liquid scintillator detector with excellent energy resolution is currently under construction in China. JUNO will be able to detect several atmospheric neutrinos per day given the large volume. A study on the JUNO detection and reconstruction capabilities of atmospheric $谓_e$ and $谓_渭$ fluxes is presented in this paper. In this study, a sample of atmospheric neutrino Monte Carlo events has been generated, starting from theoretical models, and then processed by the detector simulation. The excellent timing resolution of the 3'' PMT light detection system of JUNO detector and the much higher light yield for scintillation over Cherenkov allow to measure the time structure of the scintillation light with very high precision. Since $谓_e$ and $谓_渭$ interactions produce a slightly different light pattern, the different time evolution of light allows to discriminate the flavor of primary neutrinos. A probabilistic unfolding method has been used, in order to infer the primary neutrino energy spectrum from the detector experimental observables. The simulated spectrum has been reconstructed between 100 MeV and 10 GeV, showing a great potential of the detector in the atmospheric low energy region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.09908v3-abstract-full').style.display = 'none'; document.getElementById('2103.09908v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">25 pages, 9 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, 81 10 (2021) 887 </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/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+G">Guangpeng 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=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=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=Bernieri%2C+E">Enrico Bernieri</a>, <a href="/search/hep-ex?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/hep-ex?searchtype=author&query=Bay%2C+D">Daya Bay</a>, <a href="/search/hep-ex?searchtype=author&query=collaborations%2C+J">JUNO collaborations</a>, <a href="/search/hep-ex?searchtype=author&query=%3A"> :</a>, <a href="/search/hep-ex?searchtype=author&query=Abusleme%2C+A">A. Abusleme</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">T. Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Ahmad%2C+S">S. Ahmad</a>, <a href="/search/hep-ex?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/hep-ex?searchtype=author&query=Akram%2C+M">M. Akram</a>, <a href="/search/hep-ex?searchtype=author&query=Ali%2C+N">N. Ali</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F+P">F. P. An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+G+P">G. P. An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ex?searchtype=author&query=Andronico%2C+G">G. Andronico</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">N. Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Antoshkina%2C+T">T. Antoshkina</a>, <a href="/search/hep-ex?searchtype=author&query=Asavapibhop%2C+B">B. Asavapibhop</a>, <a href="/search/hep-ex?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">J. P. A. M. de Andr茅</a>, <a href="/search/hep-ex?searchtype=author&query=Babic%2C+A">A. Babic</a>, <a href="/search/hep-ex?searchtype=author&query=Balantekin%2C+A+B">A. B. Balantekin</a>, <a href="/search/hep-ex?searchtype=author&query=Baldini%2C+W">W. Baldini</a>, <a href="/search/hep-ex?searchtype=author&query=Baldoncini%2C+M">M. Baldoncini</a>, <a href="/search/hep-ex?searchtype=author&query=Band%2C+H+R">H. R. Band</a>, <a href="/search/hep-ex?searchtype=author&query=Barresi%2C+A">A. Barresi</a>, <a href="/search/hep-ex?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/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=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=Ali%2C+N">Nawab Ali</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+G">Guangpeng 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=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=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=Bernieri%2C+E">Enrico Bernieri</a>, <a href="/search/hep-ex?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/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=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=Ali%2C+N">Nawab Ali</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+G">Guangpeng 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=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=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=Bernieri%2C+E">Enrico Bernieri</a>, <a href="/search/hep-ex?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> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.07166">arXiv:1508.07166</a> <span> [<a href="https://arxiv.org/pdf/1508.07166">pdf</a>, <a href="https://arxiv.org/format/1508.07166">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"> JUNO Conceptual Design Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">T. Adam</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+F">F. An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+G">G. An</a>, <a href="/search/hep-ex?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ex?searchtype=author&query=Anfimov%2C+N">N. Anfimov</a>, <a href="/search/hep-ex?searchtype=author&query=Antonelli%2C+V">V. Antonelli</a>, <a href="/search/hep-ex?searchtype=author&query=Baccolo%2C+G">G. Baccolo</a>, <a href="/search/hep-ex?searchtype=author&query=Baldoncini%2C+M">M. Baldoncini</a>, <a href="/search/hep-ex?searchtype=author&query=Baussan%2C+E">E. Baussan</a>, <a href="/search/hep-ex?searchtype=author&query=Bellato%2C+M">M. Bellato</a>, <a href="/search/hep-ex?searchtype=author&query=Bezrukov%2C+L">L. Bezrukov</a>, <a href="/search/hep-ex?searchtype=author&query=Bick%2C+D">D. Bick</a>, <a href="/search/hep-ex?searchtype=author&query=Blyth%2C+S">S. Blyth</a>, <a href="/search/hep-ex?searchtype=author&query=Boarin%2C+S">S. Boarin</a>, <a href="/search/hep-ex?searchtype=author&query=Brigatti%2C+A">A. Brigatti</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/hep-ex?searchtype=author&query=Avanzini%2C+M+B">M. Buizza Avanzini</a>, <a href="/search/hep-ex?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/hep-ex?searchtype=author&query=Cabrera%2C+A">A. Cabrera</a>, <a href="/search/hep-ex?searchtype=author&query=Cai%2C+H">H. Cai</a>, <a href="/search/hep-ex?searchtype=author&query=Cai%2C+X">X. Cai</a>, <a href="/search/hep-ex?searchtype=author&query=Cammi%2C+A">A. Cammi</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+D">D. Cao</a>, <a href="/search/hep-ex?searchtype=author&query=Cao%2C+G">G. Cao</a> , et al. (372 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1508.07166v2-abstract-short" style="display: inline;"> The Jiangmen Underground Neutrino Observatory (JUNO) is proposed to determine the neutrino mass hierarchy using an underground liquid scintillator detector. It is located 53 km away from both Yangjiang and Taishan Nuclear Power Plants in Guangdong, China. The experimental hall, spanning more than 50 meters, is under a granite mountain of over 700 m overburden. Within six years of running, the dete… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.07166v2-abstract-full').style.display = 'inline'; document.getElementById('1508.07166v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.07166v2-abstract-full" style="display: none;"> The Jiangmen Underground Neutrino Observatory (JUNO) is proposed to determine the neutrino mass hierarchy using an underground liquid scintillator detector. It is located 53 km away from both Yangjiang and Taishan Nuclear Power Plants in Guangdong, China. The experimental hall, spanning more than 50 meters, is under a granite mountain of over 700 m overburden. Within six years of running, the detection of reactor antineutrinos can resolve the neutrino mass hierarchy at a confidence level of 3-4$蟽$, and determine neutrino oscillation parameters $\sin^2胃_{12}$, $螖m^2_{21}$, and $|螖m^2_{ee}|$ to an accuracy of better than 1%. The JUNO detector can be also used to study terrestrial and extra-terrestrial neutrinos and new physics beyond the Standard Model. The central detector contains 20,000 tons liquid scintillator with an acrylic sphere of 35 m in diameter. $\sim$17,000 508-mm diameter PMTs with high quantum efficiency provide $\sim$75% optical coverage. The current choice of the liquid scintillator is: linear alkyl benzene (LAB) as the solvent, plus PPO as the scintillation fluor and a wavelength-shifter (Bis-MSB). The number of detected photoelectrons per MeV is larger than 1,100 and the energy resolution is expected to be 3% at 1 MeV. The calibration system is designed to deploy multiple sources to cover the entire energy range of reactor antineutrinos, and to achieve a full-volume position coverage inside the detector. The veto system is used for muon detection, muon induced background study and reduction. It consists of a Water Cherenkov detector and a Top Tracker system. The readout system, the detector control system and the offline system insure efficient and stable data acquisition and processing. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.07166v2-abstract-full').style.display = 'none'; document.getElementById('1508.07166v2-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">328 pages, 211 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/1212.1276">arXiv:1212.1276</a> <span> [<a href="https://arxiv.org/pdf/1212.1276">pdf</a>, <a href="https://arxiv.org/ps/1212.1276">ps</a>, <a href="https://arxiv.org/format/1212.1276">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/JHEP01(2013)153">10.1007/JHEP01(2013)153 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the neutrino velocity with the OPERA detector in the CNGS beam using the 2012 dedicated data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+OPERA+Collaboration"> The OPERA Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">T. Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Agafonova%2C+N">N. Agafonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aleksandrov%2C+A">A. Aleksandrov</a>, <a href="/search/hep-ex?searchtype=author&query=Anokhina%2C+A">A. Anokhina</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+T">T. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Autiero%2C+D">D. Autiero</a>, <a href="/search/hep-ex?searchtype=author&query=Badertscher%2C+A">A. Badertscher</a>, <a href="/search/hep-ex?searchtype=author&query=Dhahbi%2C+A+B">A. Ben Dhahbi</a>, <a href="/search/hep-ex?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/hep-ex?searchtype=author&query=Bertolin%2C+A">A. Bertolin</a>, <a href="/search/hep-ex?searchtype=author&query=Bozza%2C+C">C. Bozza</a>, <a href="/search/hep-ex?searchtype=author&query=Brugi%C3%A8re%2C+T">T. Brugi猫re</a>, <a href="/search/hep-ex?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/hep-ex?searchtype=author&query=Brunet%2C+F">F. Brunet</a>, <a href="/search/hep-ex?searchtype=author&query=Brunetti%2C+G">G. Brunetti</a>, <a href="/search/hep-ex?searchtype=author&query=Buettner%2C+B">B. Buettner</a>, <a href="/search/hep-ex?searchtype=author&query=Buontempo%2C+S">S. Buontempo</a>, <a href="/search/hep-ex?searchtype=author&query=Carlus%2C+B">B. Carlus</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/hep-ex?searchtype=author&query=Chaussard%2C+L">L. Chaussard</a>, <a href="/search/hep-ex?searchtype=author&query=Chernyavsky%2C+M">M. Chernyavsky</a> , et al. (146 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1212.1276v2-abstract-short" style="display: inline;"> In spring 2012 CERN provided two weeks of a short bunch proton beam dedicated to the neutrino velocity measurement over a distance of 730 km. The OPERA neutrino experiment at the underground Gran Sasso Laboratory used an upgraded setup compared to the 2011 measurements, improving the measurement time accuracy. An independent timing system based on the Resistive Plate Chambers was exploited providi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.1276v2-abstract-full').style.display = 'inline'; document.getElementById('1212.1276v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1212.1276v2-abstract-full" style="display: none;"> In spring 2012 CERN provided two weeks of a short bunch proton beam dedicated to the neutrino velocity measurement over a distance of 730 km. The OPERA neutrino experiment at the underground Gran Sasso Laboratory used an upgraded setup compared to the 2011 measurements, improving the measurement time accuracy. An independent timing system based on the Resistive Plate Chambers was exploited providing a time accuracy of $\sim$1 ns. Neutrino and anti-neutrino contributions were separated using the information provided by the OPERA magnetic spectrometers. The new analysis profited from the precision geodesy measurements of the neutrino baseline and of the CNGS/LNGS clock synchronization. The neutrino arrival time with respect to the one computed assuming the speed of light in vacuum is found to be $未t_谓\equiv TOF_c - TOF_谓= (0.6 \pm 0.4\ (stat.) \pm 3.0\ (syst.))$ ns and $未t_{\bar谓} \equiv TOF_c - TOF_{\bar谓} = (1.7 \pm 1.4\ (stat.) \pm 3.1\ (syst.))$ ns for $谓_渭$ and $\bar谓_渭$, respectively. This corresponds to a limit on the muon neutrino velocity with respect to the speed of light of $-1.8 \times 10^{-6} < (v_谓-c)/c < 2.3 \times 10^{-6}$ at 90% C.L. This new measurement confirms with higher accuracy the revised OPERA result. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.1276v2-abstract-full').style.display = 'none'; document.getElementById('1212.1276v2-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 December, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 December, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1109.4897">arXiv:1109.4897</a> <span> [<a href="https://arxiv.org/pdf/1109.4897">pdf</a>, <a href="https://arxiv.org/format/1109.4897">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/JHEP10(2012)093">10.1007/JHEP10(2012)093 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the neutrino velocity with the OPERA detector in the CNGS beam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ex?searchtype=author&query=The+OPERA+Collaboration"> The OPERA Collaboration</a>, <a href="/search/hep-ex?searchtype=author&query=Adam%2C+T">T. Adam</a>, <a href="/search/hep-ex?searchtype=author&query=Agafonova%2C+N">N. Agafonova</a>, <a href="/search/hep-ex?searchtype=author&query=Aleksandrov%2C+A">A. Aleksandrov</a>, <a href="/search/hep-ex?searchtype=author&query=Altinok%2C+O">O. Altinok</a>, <a href="/search/hep-ex?searchtype=author&query=Sanchez%2C+P+A">P. Alvarez Sanchez</a>, <a href="/search/hep-ex?searchtype=author&query=Anokhina%2C+A">A. Anokhina</a>, <a href="/search/hep-ex?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Ariga%2C+T">T. Ariga</a>, <a href="/search/hep-ex?searchtype=author&query=Autiero%2C+D">D. Autiero</a>, <a href="/search/hep-ex?searchtype=author&query=Badertscher%2C+A">A. Badertscher</a>, <a href="/search/hep-ex?searchtype=author&query=Dhahbi%2C+A+B">A. Ben Dhahbi</a>, <a href="/search/hep-ex?searchtype=author&query=Bertolin%2C+A">A. Bertolin</a>, <a href="/search/hep-ex?searchtype=author&query=Bozza%2C+C">C. Bozza</a>, <a href="/search/hep-ex?searchtype=author&query=Brugiere%2C+T">T. Brugiere</a>, <a href="/search/hep-ex?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/hep-ex?searchtype=author&query=Brunet%2C+F">F. Brunet</a>, <a href="/search/hep-ex?searchtype=author&query=Brunetti%2C+G">G. Brunetti</a>, <a href="/search/hep-ex?searchtype=author&query=Buontempo%2C+S">S. Buontempo</a>, <a href="/search/hep-ex?searchtype=author&query=Carlus%2C+B">B. Carlus</a>, <a href="/search/hep-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/hep-ex?searchtype=author&query=Cazes%2C+A">A. Cazes</a>, <a href="/search/hep-ex?searchtype=author&query=Chaussard%2C+L">L. Chaussard</a>, <a href="/search/hep-ex?searchtype=author&query=Chernyavsky%2C+M">M. Chernyavsky</a> , et al. (166 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="1109.4897v4-abstract-short" style="display: inline;"> The OPERA neutrino experiment at the underground Gran Sasso Laboratory has measured the velocity of neutrinos from the CERN CNGS beam over a baseline of about 730 km. The measurement is based on data taken by OPERA in the years 2009, 2010 and 2011. Dedicated upgrades of the CNGS timing system and of the OPERA detector, as well as a high precision geodesy campaign for the measurement of the neutrin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.4897v4-abstract-full').style.display = 'inline'; document.getElementById('1109.4897v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1109.4897v4-abstract-full" style="display: none;"> The OPERA neutrino experiment at the underground Gran Sasso Laboratory has measured the velocity of neutrinos from the CERN CNGS beam over a baseline of about 730 km. The measurement is based on data taken by OPERA in the years 2009, 2010 and 2011. Dedicated upgrades of the CNGS timing system and of the OPERA detector, as well as a high precision geodesy campaign for the measurement of the neutrino baseline, allowed reaching comparable systematic and statistical accuracies. An arrival time of CNGS muon neutrinos with respect to the one computed assuming the speed of light in vacuum of (6.5 +/- 7.4(stat.)((+8.3)(-8.0)sys.))ns was measured corresponding to a relative difference of the muon neutrino velocity with respect to the speed of light (v-c)/c =(2.7 +/-3.1(stat.)((+3.4)(-3.3)(sys.))x10^(-6). The above result, obtained by comparing the time distributions of neutrino interactions and of protons hitting the CNGS target in 10.5 microseconds long extractions, was confirmed by a test performed at the end of 2011 using a short bunch beam allowing to measure the neutrino time of flight at the single interaction level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.4897v4-abstract-full').style.display = 'none'; document.getElementById('1109.4897v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 September, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">34 pages, 22 figures This version replaces all previous ones</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 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