Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment
Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment
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DOI：
10.1103/physrevd.101.052002
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发表时间：
2018-02
影响因子：
5
通讯作者：
D. Akerib;C. Akerlof;S. Alsum;H. Araújo;M. Arthurs;X. Bai;A. Bailey;J. Balajthy;S. Balashov-S.-Balasho
中科院分区：
文献类型：
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作者：
D. Akerib;C. Akerlof;S. Alsum;H. Araújo;M. Arthurs;X. Bai;A. Bailey;J. Balajthy;S. Balashov-S.-Balasho
作者：Akerib， DS；阿克尔洛夫,连续波;Alsum SK;Araujo,嗯;阿瑟M;巴姨,X;贝利,AJ;Balajthy J;Balashov年代;鲍尔,D;美女,J;Beltrame P;本森,T;伯纳德,EP;Biesiadzinski TP;自夸,客;拳击手,B;胸罩,P;巴克利,JH;Bugaev VV;Burdin年代;Busenitz JK;卡尔,C;Carlsmith DL;卡尔森,B;Carmona-Benitez MC;陈,C;Cherwinka JJ;科尔,;卡特,一个;克拉多克,WW;Currie,;刀,我;达尔,CE;De Viveiros， L；Dobi,;多布森杰特;Druszkiewicz E;Edberg TK;爱德华兹,或者说是;一个风扇;律师法,年代;或者是,年代;Fruth T;盖茨克尔,RJ;Genovesi J;对方C;MGD Gilchriese;Van Der Grinten， MGD；大厅、铬;汉斯,年代;Hanzel K;Haselschwardt SJ;赫特尔,SA);Hillbrand年代;Hjemfelt C;霍夫博士;何珥JYK;黄,DQ;Ignarra厘米;霁,W;Kaboth交流;Kamdin K;Keefner J;Khaitan D;Khazov,;金码;Kocher CD;Korolkova,电动汽车;克劳斯,H;克雷布斯HJ;Kreczko L;Krikler, B;弗吉尼亚州Kudryavtsev;Kyre年代;李,J。BG Lenardo;伦纳德,DS;莱斯科,KT;Levy, C;李,J;廖,J;廖,英国《金融时报》;林,J;摘要：©2020美国物理学会。LUX-ZEPLIN （LZ）是下一代暗物质直接探测实验，将在美国南达科他州铅市桑福德地下研究设施（SURF）的地下4850英尺处运行。LZ将使用一个活跃质量为7吨的两相氙探测器，主要搜索与弱相互作用大质量粒子（wimp）的低能相互作用，这些粒子被假设构成了我们银河系晕中的暗物质。在本文中，基于最新的背景估计和探测器的模拟，给出了LZ的预测WIMP灵敏度。使用5.6吨的基准质量进行1000天的运行，预计LZ将在90%的置信水平上排除40 GeV/c2质量的WIMP中超过1.4×10-48 cm2的自旋无关的核子横截面。此外，预测了5σ的发现潜力，达到了低于最近实验排除极限的截面。对于自旋相关的WIMP-中子（-质子）散射，对于40 GeV/c2质量的WIMP，预计灵敏度为2.3×10-43 cm2 （7.1×10-42 cm2）。随着地下安装的顺利进行，LZ将于2020年在SURF进行调试。
Author(s): Akerib, DS; Akerlof, CW; Alsum, SK; Araujo, HM; Arthurs, M; Bai, X; Bailey, AJ; Balajthy, J; Balashov, S; Bauer, D; Belle, J; Beltrame, P; Benson, T; Bernard, EP; Biesiadzinski, TP; Boast, KE; Boxer, B; Bras, P; Buckley, JH; Bugaev, VV; Burdin, S; Busenitz, JK; Carels, C; Carlsmith, DL; Carlson, B; Carmona-Benitez, MC; Chan, C; Cherwinka, JJ; Cole, A; Cottle, A; Craddock, WW; Currie, A; Cutter, JE; Dahl, CE; De Viveiros, L; Dobi, A; Dobson, JEY; Druszkiewicz, E; Edberg, TK; Edwards, WR; Fan, A; Fayer, S; Fiorucci, S; Fruth, T; Gaitskell, RJ; Genovesi, J; Ghag, C; Gilchriese, MGD; Van Der Grinten, MGD; Hall, CR; Hans, S; Hanzel, K; Haselschwardt, SJ; Hertel, SA; Hillbrand, S; Hjemfelt, C; Hoff, MD; Hor, JYK; Huang, DQ; Ignarra, CM; Ji, W; Kaboth, AC; Kamdin, K; Keefner, J; Khaitan, D; Khazov, A; Kim, YD; Kocher, CD; Korolkova, EV; Kraus, H; Krebs, HJ; Kreczko, L; Krikler, B; Kudryavtsev, VA; Kyre, S; Lee, J; Lenardo, BG; Leonard, DS; Lesko, KT; Levy, C; Li, J; Liao, J; Liao, FT; Lin, J; Lindote, A | Abstract: © 2020 American Physical Society. LUX-ZEPLIN (LZ) is a next-generation dark matter direct detection experiment that will operate 4850 feet underground at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, USA. Using a two-phase xenon detector with an active mass of 7 tonnes, LZ will search primarily for low-energy interactions with weakly interacting massive particles (WIMPs), which are hypothesized to make up the dark matter in our galactic halo. In this paper, the projected WIMP sensitivity of LZ is presented based on the latest background estimates and simulations of the detector. For a 1000 live day run using a 5.6-tonne fiducial mass, LZ is projected to exclude at 90% confidence level spin-independent WIMP-nucleon cross sections above 1.4×10-48 cm2 for a 40 GeV/c2 mass WIMP. Additionally, a 5σ discovery potential is projected, reaching cross sections below the exclusion limits of recent experiments. For spin-dependent WIMP-neutron(-proton) scattering, a sensitivity of 2.3×10-43 cm2 (7.1×10-42 cm2) for a 40 GeV/c2 mass WIMP is expected. With underground installation well underway, LZ is on track for commissioning at SURF in 2020.