Determining the Neutrino Mass Ordering and Oscillation Parameters with KM3NeT/ORCA
S. Aiello, A. Albert, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, J. Aubl… 展开作者
S. Aiello, A. Albert, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Biagi, M. Bissinger, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, M. Bouwhuis, C. Bozza, H. Brânzaş, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, D. Calvo, A. Capone, V. Carretero, P. Castaldi, S. Celli, M. Chabab, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Molla, R. Coniglione, P. Coyle, A. Creusot, A. Cruz, G. Cuttone, R. Dallier, B. De Martino, M. De Palma, M. Di Marino, I. Di Palma, A. F. Díaz, D. Diego-Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, D. Elsaesser, A. Enzenhöfer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, L. A. Fusco, T. Gal, A. Garcia Soto, F. Garufi, Y. Gatelet, N. Geisselbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, D. Grasso, G. Grella, D. Guderian, C. Guidi, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, J. J. Hernández-Rey, J. Hofestädt, F. Huang, W. Idrissi Ibnsalih, G. Illuminati, C. W. James, M. de Jong, P. de Jong, B. J. Jung, M. Kadler, P. Kalaczyński, O. Kalekin, U. F. Katz, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, M. Kreter, V. Kulikovskiy, R. Lahmann, M. Lamoureux, G. Larosa, C. Lastoria, R. Le Breton, S. Le Stum, O. Leonardi, F. Leone, E. Leonora, N. Lessing, G. Levi, M. Lincetto, M. Lindsey Clark, T. Lipreau, F. Longhitano, D. Lopez-Coto, L. Maderer, J. Mańczak, K. Mannheim, A. Margiotta, A. Marinelli, C. Markou, L. Martin, J. A. Martínez-Mora, A. Martini, F. Marzaioli, S. Mastroianni, K. W. Melis, G. Miele, P. Migliozzi, E. Migneco, P. Mijakowski, L. S. Miranda, C. M. Mollo, M. Morganti, M. Moser, A. Moussa, R. Muller, M. Musumeci, L. Nauta, S. Navas, C. A. Nicolau, B. Ó Fearraigh, M. O'Sullivan, M. Organokov, A. Orlando, J. Palacios González, G. Papalashvili, R. Papaleo, C. Pastore, A. M. Păun, G. E. Păvălaş, C. Pellegrino, M. Perrin-Terrin, V. Pestel, P. Piattelli, C. Pieterse, K. Pikounis, O. Pisanti, C. Poirè, V. Popa, T. Pradier, G. Pühlhofer, S. Pulvirenti, O. Rabyang, F. Raffaelli, N. Randazzo, S. Razzaque, D. Real, S. Reck, G. Riccobene, A. Romanov, A. Rovelli, F. Salesa Greus, D. F. E. Samtleben, A. Sánchez Losa, M. Sanguineti, A. Santangelo, D. Santonocito, P. Sapienza, J. Schnabel, M. F. Schneider, J. Schumann, H. M. Schutte, J. Seneca, I. Sgura, R. Shanidze, A. Sharma, A. Sinopoulou, B. Spisso, M. Spurio, D. Stavropoulos, S. M. Stellacci, M. Taiuti, Y. Tayalati, E. Tenllado, H. Thiersen, S. Tingay, V. Tsourapis, E. Tzamariudaki, D. Tzanetatos, V. Van Elewyck, G. Vasileiadis, F. Versari, D. Vivolo, G. de Wasseige, J. Wilms, R. Wojaczyński, E. de Wolf, T. Yousfi, S. Zavatarelli, A. Zegarelli, D. Zito, J. D. Zornoza, J. Zúñiga, N. Zywucka
地中海的下一代水切伦科夫中微子望远镜正在法国（KM 3 NeT/ORCA）和西西里岛（KM 3 NeT/ARCA）近海建造。KM 3 NeT/ORCA探测器具有能量探测阈值，可以收集大气中微子以研究味道振荡。本文报道了KM 3 NeT/ORCA对这种现象的敏感性。描述了事件的重建、选择和分类。的灵敏度，以确定中微子质量排序进行了评估，发现是4.4 $σ$，如果真正的顺序是正常的和2.3 $σ$，如果倒置，经过三年的数据采集。对正常中微子质量序的测量精度为$85\cdot10^{-6}$ eV $^2$和$θ_{23}$，对倒序的测量精度为$75\cdot10^{-6}$ eV $^2$和$(^{+2.0}_{-7.0})^{\circ}$。最后，描述了通过测量τ中微子的速率来检验轻子混合矩阵的么正性。发现3年的数据采集足以排除$3σ$水平下$ν_τ$和$\barν_τ$事件发生率变化大于20%的情况。
英文摘要：
The next generation of water Cherenkov neutrino telescopes in the Mediterranean Sea are under construction offshore France (KM3NeT/ORCA) and Sicily (KM3NeT/ARCA). The KM3NeT/ORCA detector features an energy detection threshold which allows to collect atmospheric neutrinos to study flavour oscillation. This paper reports the KM3NeT/ORCA sensitivity to this phenomenon. The event reconstruction, selection and classification are described. The sensitivity to determine the neutrino mass ordering was evaluated and found to be 4.4 $σ$ if the true ordering is normal and 2.3 $σ$ if inverted, after three years of data taking. The precision to measure $Δm^2_{32}$ and $θ_{23}$ were also estimated and found to be $85\cdot10^{-6}$ eV$^2$ and $(^{+1.9}_{-3.1})^{\circ}$ for normal neutrino mass ordering and, $75\cdot10^{-6}$ eV$^2$ and $(^{+2.0}_{-7.0})^{\circ}$ for inverted ordering. Finally, a unitarity test of the leptonic mixing matrix by measuring the rate of tau neutrinos is described. Three years of data taking were found to be sufficient to exclude $ν_τ$ and $\barν_τ$ event rate variations larger than 20% at $3σ$ level.
Neutrino Oscillations and Non-standard Interactions with KM3NeT-ORCA
ORCA（Oscillations Research with Cosmics in the Abyss）是位于地中海的下一代水下切伦科夫中微子探测器KM 3 NeT的低能节点。KM 3 NeT-ORCA的主要目标是确定中微子质量排序（NMO）。在几个GeV的能量阈值和几个Mton的有效质量下，KM 3 NeT-ORCA也可以对大气振荡参数进行精确测量。此外，它可以获得广泛的能量和基线，这使得它最适合发现标准模型之外的奇异物理，如中微子的非标准相互作用（NSI）。探测器的中微子质量排序的灵敏度，以及其潜在的确定大气振荡参数。据观察，KM 3 NeT-ORCA将在三年的数据采集后将NSI参数的当前上限提高一个数量级。
Neutrino oscillation tomography of the Earth with KM3NeT-ORCA
KM 3 NeT-ORCA是一个水切伦科夫中微子探测器，设计用于研究大气中微子振荡，主要目标是测量中微子质量有序。穿过地球的大气中微子受到物质效应的影响，改变了它们的味道振荡模式。因此，对ORCA中中微子事件的角度和能量分布的研究可以提供关于地球内部的层析成像信息，这是对标准地球物理学方法的补充。基于探测器响应的完整蒙特卡罗模拟的初步估计表明，经过十年的运行，电子密度可以在地幔中以3-5%的精度测量，在外核中以7-10%的精度测量-取决于质量排序。
Determining Neutrino Mass Ordering with NOvA and Upcoming JUNO Measurements
Erciyes University（埃尔西耶斯大学）；Universidad del Atlantico（大西洋大学）；University of Mississippi（密西西比大学）；Fermi National Accelerator Laboratory（费米国家加速器实验室）；Joint Institute for Nuclear Research（苏联联合核研究所）；Universidad del Magdalena（马格达莱纳大学）；University of Sussex（萨塞克斯大学）；University of Cincinnati（辛辛那提大学）；University of Hyderabad（海德拉巴大学）；University of California at Irvine（加州大学尔湾分校）；University of Minnesota Twin Cities（明尼苏达大学双城分校）
Improved precision on 2-3 oscillation parameters using the synergy between DUNE and T2HK
Institute of Physics（印度物理研究所）；Homi Bhabha National Institute（霍米·巴巴国立学院）；Department of Physics & Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin, Madison（威斯康星大学麦迪逊分校物理系与威斯康星冰立方粒子天体物理中心）；Department of Physics, Utkal University（乌塔卡尔大学物理系）
