First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment
XENON Collaboration, E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, … 展开作者
XENON Collaboration, E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, M. Bazyk, L. Bellagamba, R. Biondi, A. Bismark, E. J. Brookes, A. Brown, S. Bruenner, G. Bruno, R. Budnik, T. K. Bui, C. Cai, J. M. R. Cardoso, D. Cichon, A. P. Cimental Chavez, A. P. Colijn, J. Conrad, J. J. Cuenca-García, J. P. Cussonneau, V. D'Andrea, M. P. Decowski, P. Di Gangi, S. Di Pede, S. Diglio, K. Eitel, A. Elykov, S. Farrell, A. D. Ferella, C. Ferrari, H. Fischer, M. Flierman, W. Fulgione, C. Fuselli, P. Gaemers, R. Gaior, A. Gallo Rosso, M. Galloway, F. Gao, R. Glade-Beucke, L. Grandi, J. Grigat, H. Guan, M. Guida, R. Hammann, A. Higuera, C. Hils, L. Hoetzsch, N. F. Hood, J. Howlett, M. Iacovacci, Y. Itow, J. Jakob, F. Joerg, A. Joy, N. Kato, M. Kara, P. Kavrigin, S. Kazama, M. Kobayashi, G. Koltman, A. Kopec, F. Kuger, H. Landsman, R. F. Lang, L. Levinson, I. Li, S. Li, S. Liang, S. Lindemann, M. Lindner, K. Liu, J. Loizeau, F. Lombardi, J. Long, J. A. M. Lopes, Y. Ma, C. Macolino, J. Mahlstedt, A. Mancuso, L. Manenti, F. Marignetti, T. Marrodán Undagoitia, K. Martens, J. Masbou, D. Masson, E. Masson, S. Mastroianni, M. Messina, K. Miuchi, K. Mizukoshi, A. Molinario, S. Moriyama, K. Morå, Y. Mosbacher, M. Murra, J. Müller, K. Ni, U. Oberlack, B. Paetsch, J. Palacio, R. Peres, C. Peters, J. Pienaar, M. Pierre, V. Pizzella, G. Plante, J. Qi, J. Qin, D. Ramírez García, R. Singh, L. Sanchez, J. M. F. dos Santos, I. Sarnoff, G. Sartorelli, J. Schreiner, D. Schulte, P. Schulte, H. Schulze Eißing, M. Schumann, L. Scotto Lavina, M. Selvi, F. Semeria, P. Shagin, S. Shi, E. Shockley, M. Silva, H. Simgen, A. Takeda, P. -L. Tan, A. Terliuk, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, F. Tönnies, K. Valerius, G. Volta, C. Weinheimer, M. Weiss, D. Wenz, C. Wittweg, T. Wolf, V. H. S. Wu, Y. Xing, D. Xu, Z. Xu, M. Yamashita, L. Yang, J. Ye, L. Yuan, G. Zavattini, M. Zhong, T. Zhu
我们报告了XENONnT实验首次对以弱相互作用大质量粒子（WIMPs）形式存在的暗物质核反冲进行的搜寻。该实验基于一个两相时间投影室，灵敏液氙质量为5.9吨。在本次搜寻所用的大约1.1吨·年曝光量期间，液态靶中的本征$^{85}$Kr和$^{222}$Rn浓度被降低至前所未有的低水平，使得感兴趣区内的电子反冲本底率为$(15.8\pm1.3)~\mathrm{events}/(\mathrm{t\cdot y \cdot keV})$。对能量在3.3 keV至60.5 keV之间的核反冲事件进行盲分析，未发现显著超出。由此得到在90%置信水平下，WIMP质量为$28~\mathrm{GeV}/c^2$时自旋无关WIMP-核子散射截面的最小上限为$2.58\times 10^{-47}~\mathrm{cm}^2$。同时给出了自旋相关相互作用的上限。对于本文分析的全部WIMP质量范围，其上限和灵敏度在相同曝光量下均优于此前XENON1T实验所获得的结果。
英文摘要：
We report on the first search for nuclear recoils from dark matter in the form of weakly interacting massive particles (WIMPs) with the XENONnT experiment which is based on a two-phase time projection chamber with a sensitive liquid xenon mass of $5.9$ t. During the approximately 1.1 tonne-year exposure used for this search, the intrinsic $^{85}$Kr and $^{222}$Rn concentrations in the liquid target were reduced to unprecedentedly low levels, giving an electronic recoil background rate of $(15.8\pm1.3)~\mathrm{events}/(\mathrm{t\cdot y \cdot keV})$ in the region of interest. A blind analysis of nuclear recoil events with energies between $3.3$ keV and $60.5$ keV finds no significant excess. This leads to a minimum upper limit on the spin-independent WIMP-nucleon cross section of $2.58\times 10^{-47}~\mathrm{cm}^2$ for a WIMP mass of $28~\mathrm{GeV}/c^2$ at $90\%$ confidence level. Limits for spin-dependent interactions are also provided. Both the limit and the sensitivity for the full range of WIMP masses analyzed here improve on previous results obtained with the XENON1T experiment for the same exposure.
Direct detection of solar chameleons with electron recoil data from XENONnT
University of Trento（特伦托大学）；Trento Institute for Fundamental Physics and Applications (TIFPA)-INFN（特伦托基础物理与应用研究所（TIFPA）-意大利国家核物理研究所）；University of Cambridge（剑桥大学）；Kavli Institute for Cosmology (KICC), University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Universidad de Zaragoza（萨拉戈萨大学）；Centro de Astropartículas y Física de Altas Energías, Universidad de Zaragoza（萨拉戈萨大学高能天体粒子物理中心）；University of Salerno（萨莱诺大学）；INFN Sezione di Napoli, Gruppo Collegato di Salerno（意大利国家核物理研究所那不勒斯分部萨莱诺协作组）；Technische Universität Dortmund（多特蒙德工业大学）
Low-Energy Nuclear Recoil Calibration of XENONnT with a $^{88}$YBe Photoneutron Source
Columbia University（哥伦比亚大学）；Nikhef and the University of Groningen, Van Swinderen Institute（荷兰核物理研究所与格罗宁根大学范斯温德伦研究所）；Kamioka Observatory, Institute for Cosmic Ray Research, and Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学宇宙射线研究所神冈观测站及武利宇宙物理学数学研究所）；LPNHE, Sorbonne Université, CNRS/IN2P3（索邦大学国家科学研究中心/法国原子能和替代能源委员会高能物理实验室）；Institut für Kernphysik, University of Münster（明斯特大学核物理研究所）；INAF-Astrophysical Observatory of Torino, Department of Physics, University of Torino and INFN-Torino（都灵大学物理系、意大利国家天体物理研究所都灵天文台及意大利国家核物理研究所都灵分部）；INFN-Laboratori Nazionali del Gran Sasso and Gran Sasso Science Institute（意大利国家核物理研究所格兰萨索国家实验室及格兰萨索科学研究所）；Department of Physics, Enrico Fermi Institute & Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学恩里科·费米研究所、卡弗里宇宙物理学研究所及物理系）；New York University Abu Dhabi - Center for Astro, Particle and Planetary Physics（纽约大学阿布扎比分校天体、粒子与行星物理中心）；Physik-Institut, University of Zürich（苏黎世大学物理研究所）；SUBATECH, IMT Atlantique, CNRS/IN2P3, Nantes Université（南特大学IMT大西洋学院国家科学研究中心/法国原子能和替代能源委员会亚原子与技术研究实验室）；Department of Physics and Astronomy, University of Bologna and INFN-Bologna（博洛尼亚大学物理与天文学系及意大利国家核物理研究所博洛尼亚分部）
Light Dark Matter Search with 7.8 Tonne-Year of Ionization-Only Data in XENONnT
Columbia University（哥伦比亚大学）；Nikhef and the University of Groningen, Van Swinderen Institute（荷兰核粒子物理研究所和格罗宁根大学范斯温德伦研究所）；Kamioka Observatory, Institute for Cosmic Ray Research, and Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京宇宙线研究所神冈观测站及汤川理论物理数学研究所（WPI），东京大学）；University of Zürich（苏黎世大学）；LPNHE, Sorbonne Université, CNRS/IN2P3（巴黎大索邦大学、法国国家科学研究中心/欧洲核子研究组织粒子与高能物理实验室）；University of Münster（明斯特大学）；INFN-Laboratori Nazionali del Gran Sasso and Gran Sasso Science Institute（意大利国家核物理研究所格兰萨索国家实验室及格兰萨索科学研究所）；University of Chicago（芝加哥大学）；Max-Planck-Institut für Kernphysik（马克斯·普朗克核物理研究所）；New York University Abu Dhabi - Center for Astro, Particle and Planetary Physics（纽约大学阿布扎比分校天体、粒子和行星物理中心）；SUBATECH, IMT Atlantique, CNRS/IN2P3, Nantes Université（南特大学、大西洋高等矿业学院、法国国家科学研究中心/欧洲核子研究组织亚原子技术与高能物理实验室）
First Indication of Solar $^8$B Neutrinos via Coherent Elastic Neutrino-Nucleus Scattering with XENONnT
Columbia University（哥伦比亚大学）；Nikhef and the University of Groningen, Van Swinderen Institute（NIKHEF与格罗宁根大学范斯温德伦研究所）；Kamioka Observatory, Institute for Cosmic Ray Research, and Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学神冈观测站、宇宙线研究所及Kavli宇宙物理数学研究所（WPI））；LPNHE, Sorbonne Université, CNRS/IN2P3（索邦大学LPNHE实验室，CNRS/IN2P3）；Institut für Kernphysik, University of Münster（明斯特大学核物理研究所）；INAF-Astrophysical Observatory of Torino, Department of Physics, University of Torino and INFN-Torino（都灵大学天体物理研究所INFAS、物理系及INFN-都灵分部）；INFN-Laboratori Nazionali del Gran Sasso and Gran Sasso Science Institute（INFN大萨索国家实验室与大萨索科学研究所）；Department of Physics, Enrico Fermi Institute & Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学物理系、恩里科·费米研究所及Kavli宇宙物理研究所）；New York University Abu Dhabi - Center for Astro, Particle and Planetary Physics（纽约大学阿布扎比分校天文、粒子与行星物理中心）；Physik-Institut, University of Zürich（苏黎世大学物理研究所）；SUBATECH, IMT Atlantique, CNRS/IN2P3, Université de Nantes（南特大学SUBATECH实验室，IMT大西洋学院，CNRS/IN2P3）；Department of Physics and Astronomy, University of Bologna and INFN-Bologna（博洛尼亚大学物理与天文学系及INFN-博洛尼部分部）
