Low-mass dark matter search with CDMSlite
Low-mass dark matter search with CDMSlite
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DOI：
10.1103/physrevd.97.022002
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发表时间：
2017-07
影响因子：
5
通讯作者：
R. Agnese;A. Anderson;T. Aralis;T. Aramaki;I. Arnquist;W. Baker;D. Balakishiyeva;D. Barker;
中科院分区：
文献类型：
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作者：
R. Agnese;A. Anderson;T. Aralis;T. Aramaki;I. Arnquist;W. Baker;D. Balakishiyeva;D. Barker;
作者：Agnese， R；安德森,AJ;Aralis T;Aramaki T;Arnquist IJ;贝克,W;Balakishiyeva D;巴克,D;巴苏·塔库尔，R；鲍尔达;粘结剂、T;鲍尔斯,马;边缘,PL;地堡,R;卡布瑞拉,B;考德威尔;卡尔金斯,R;Cartaro C;Cerdeno DG;常,Y;Chagani H;陈,Y;地中海,J;康奈尔,B;Cushman P;女土,M;迪·斯特凡诺，PCF；勇敢的,T;埃斯特万,L;Fascione E;Figueroa-Feliciano E;Fritts, M;Gerbier G;吉斯,M;戈弗雷,GL;Golwala老;大厅,J。哈里斯,人力资源;在香港,Z;霍普,电子战;许,L;胡贝尔,我;艾耶V;查顿D;Jastram,;耶拿,C;凯尔西,MH;肯尼迪;Kubik,;Kurinsky NA;一个分类账;爱人,B;洛佩兹·阿萨玛，E；luken P;Macdonell D;塔,R;Mandic V;桅杆,N;米勒,嗯;Mirabolfathi N;莫法,类风湿性关节炎;莫汉蒂,B;莫拉莱斯·门多萨，法学博士；纳尔逊,J;Orrell表示,杰;奥泽,SM;页面中,K;页面,佤邦;鹧鸪,R;Pepin, M;Penalver Martinez， M；菲普斯,一个;Poudel年代;派尔,M;秋,H;劳,W;Redl P;Reisetter,;雷诺兹,T;罗伯茨,;罗宾逊,AE;罗杰斯,他;萨博,T;Sadoulet, B;摘要：©2018美国物理学会。超级cdms实验旨在直接探测可能构成银河系暗物质的弱相互作用大质量粒子（wimp）。在苏丹地下实验室运行期间，锗探测器在CDMSlite模式下运行，专门收集质量为10gev /c2的wimp的灵敏度数据集。在这种模式下，一个较高的探测器偏置电压被应用于放大由漂移电荷产生的声子信号。本文介绍了实验噪声及其对可实现能量阈值的影响，该阈值可低至56 eVee（电子当量能量）。详细描述了探测器偏置配置，并对电压变化进行了几个百分点的分析校正。对电场几何结构的详细研究，以及由此产生的基准参数的成功开发，消除了测量不良的事件，产生的能量分辨率范围从0 keV的~ 9 eee到~ 10 keee的101 eee。与WIMP搜索极限相关的天体物理不确定性得到了新的结果，特别是研究了它们如何受到最可能的WIMP速度和银河系逃逸速度变化的影响。这些变化对于质量低于10 GeV/c2的WIMP更为重要。最后，推导了自旋依赖的低质量WIMP-核子相互作用的新极限，排除了WIMP质量< 3 GeV/c2的新参数空间。
Author(s): Agnese, R; Anderson, AJ; Aralis, T; Aramaki, T; Arnquist, IJ; Baker, W; Balakishiyeva, D; Barker, D; Basu Thakur, R; Bauer, DA; Binder, T; Bowles, MA; Brink, PL; Bunker, R; Cabrera, B; Caldwell, DO; Calkins, R; Cartaro, C; Cerdeno, DG; Chang, Y; Chagani, H; Chen, Y; Cooley, J; Cornell, B; Cushman, P; Daal, M; Di Stefano, PCF; Doughty, T; Esteban, L; Fascione, E; Figueroa-Feliciano, E; Fritts, M; Gerbier, G; Ghaith, M; Godfrey, GL; Golwala, SR; Hall, J; Harris, HR; Hong, Z; Hoppe, EW; Hsu, L; Huber, ME; Iyer, V; Jardin, D; Jastram, A; Jena, C; Kelsey, MH; Kennedy, A; Kubik, A; Kurinsky, NA; Leder, A; Loer, B; Lopez Asamar, E; Lukens, P; Macdonell, D; Mahapatra, R; Mandic, V; Mast, N; Miller, EH; Mirabolfathi, N; Moffatt, RA; Mohanty, B; Morales Mendoza, JD; Nelson, J; Orrell, JL; Oser, SM; Page, K; Page, WA; Partridge, R; Pepin, M; Penalver Martinez, M; Phipps, A; Poudel, S; Pyle, M; Qiu, H; Rau, W; Redl, P; Reisetter, A; Reynolds, T; Roberts, A; Robinson, AE; Rogers, HE; Saab, T; Sadoulet, B; Sander, J | Abstract: © 2018 American Physical Society. The SuperCDMS experiment is designed to directly detect weakly interacting massive particles (WIMPs) that may constitute the dark matter in our Galaxy. During its operation at the Soudan Underground Laboratory, germanium detectors were run in the CDMSlite mode to gather data sets with sensitivity specifically for WIMPs with masses l10 GeV/c2. In this mode, a higher detector-bias voltage is applied to amplify the phonon signals produced by drifting charges. This paper presents studies of the experimental noise and its effect on the achievable energy threshold, which is demonstrated to be as low as 56 eVee (electron equivalent energy). The detector-biasing configuration is described in detail, with analysis corrections for voltage variations to the level of a few percent. Detailed studies of the electric-field geometry, and the resulting successful development of a fiducial parameter, eliminate poorly measured events, yielding an energy resolution ranging from ∼9 eVee at 0 keV to 101 eVee at ∼10 keVee. New results are derived for astrophysical uncertainties relevant to the WIMP-search limits, specifically examining how they are affected by variations in the most probable WIMP velocity and the Galactic escape velocity. These variations become more important for WIMP masses below 10 GeV/c2. Finally, new limits on spin-dependent low-mass WIMP-nucleon interactions are derived, with new parameter space excluded for WIMP masses ≲3 GeV/c2.