Aprile E, Abe K, Agostini F, Ahmed Maouloud S, Althueser L, Andrieu B, Angelino E, Angevaare J R, Antochi V C, Antón Martin D, Arneodo F, Baudis L, Baxter A L, Bazyk M, Bellagamba L, Biondi R, Bismark A, Brookes E J, Brown A, Bruenner S, Bruno G, Budnik R, Bui T K, Cai C, Cardoso J M R, Cichon D, Cimental Chavez A P, Colijn A P, Conrad J, Cuenca-García J J, Cussonneau J P, D'Andrea V, Decowski M P, Di Gangi P, Di Pede S, Diglio S, Eitel K, Elykov A, Farrell S, Ferella A D, Ferrari C, Fischer H, Flierman M, Fulgione W, Fuselli C, Gaemers P, Gaior R, Gallo Rosso A, Galloway M, Gao F, Glade-Beucke R, Grandi L, Grigat J, Guan H, Guida M, Hammann R, Higuera A, Hils C, Hoetzsch L, Hood N F, Howlett J, Iacovacci M, Itow Y, Jakob J, Joerg F, Joy A, Kato N, Kara M, Kavrigin P, Kazama S, Kobayashi M, Koltman G, Kopec A, Kuger F, Landsman H, Lang R F, Levinson L, Li I, Li S, Liang S, Lindemann S, Lindner M, Liu K, Loizeau J, Lombardi F, Long J, Lopes J A M, Ma Y, Macolino C, Mahlstedt J, Mancuso A, Manenti L, Marignetti F, Marrodán Undagoitia T, Martens K, Masbou J, Masson D, Masson E, Mastroianni S, Messina M, Miuchi K, Mizukoshi K, Molinario A, Moriyama S, Morå K, Mosbacher Y, Murra M, Müller J, Ni K, Oberlack U, Paetsch B, Palacio J, Peres R, Peters C, Pienaar J, Pierre M, Pizzella V, Plante G, Qi J, Qin J, Ramírez García D, Singh R, Sanchez L, Dos Santos J M F, Sarnoff I, Sartorelli G, Schreiner J, Schulte D, Schulte P, Schulze Eißing H, Schumann M, Scotto Lavina L, Selvi M, Semeria F, Shagin P, Shi S, Shockley E, Silva M, Simgen H, Takeda A, Tan P-L, Terliuk A, Thers D, Toschi F, Trinchero G, Tunnell C, Tönnies F, Valerius K, Volta G, Weinheimer C, Weiss M, Wenz D, Wittweg C, Wolf T, Wu V H S, Xing Y, Xu D, Xu Z, Yamashita M, Yang L, Ye J, Yuan L, Zavattini G, Zhong M, Zhu T
Physics Department, Columbia University, New York, New York 10027, USA.
Kamioka Observatory, Institute for Cosmic Ray Research, and Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu 506-1205, Japan.
Phys Rev Lett. 2023 Jul 28;131(4):041003. doi: 10.1103/PhysRevLett.131.041003.
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 ton. During the (1.09±0.03) ton yr exposure used for this search, the intrinsic ^{85}Kr and ^{222}Rn concentrations in the liquid target are reduced to unprecedentedly low levels, giving an electronic recoil background rate of (15.8±1.3) events/ton yr keV in the region of interest. A blind analysis of nuclear recoil events with energies between 3.3 and 60.5 keV finds no significant excess. This leads to a minimum upper limit on the spin-independent WIMP-nucleon cross section of 2.58×10^{-47} cm^{2} for a WIMP mass of 28 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.
我们报告了利用XENONnT实验首次对弱相互作用大质量粒子（WIMP）形式的暗物质产生的核反冲进行的搜索，该实验基于一个两相时间投影室，其灵敏的液态氙质量为5.9吨。在此次搜索所使用的（1.09±0.03）吨·年的曝光期间，液态靶材中固有的(^{85}Kr)和(^{222}Rn)浓度被降低到了前所未有的低水平，在感兴趣区域给出了（15.8±1.3）次事件/吨·年·keV的电子反冲本底率。对能量在3.3至60.5keV之间的核反冲事件进行的盲分析未发现显著过量。这导致在90%置信水平下，对于质量为28GeV/(c^{2})的WIMP，自旋无关的WIMP-核子截面的最小上限为(2.58×10^{-47}) (cm^{2})。还提供了自旋相关相互作用的限制。此处分析的整个WIMP质量范围内的限制和灵敏度都比之前使用XENON1T实验在相同曝光量下获得的结果有所提高。
