Projected sensitivity of the SuperCDMS SNOLAB experiment

被引:205
作者
Agnese, R. [24 ]
Anderson, A. J. [5 ]
Aramaki, T. [11 ]
Arnquist, I. [8 ]
Baker, W. [15 ,16 ]
Barker, D. [25 ]
Thakur, R. Basu [3 ,28 ]
Bauer, D. A. [3 ]
Borgland, A. [11 ]
Bowles, M. A. [12 ]
Brink, P. L. [11 ]
Bunker, R. [8 ]
Cabrera, B.
Caldwell, D. O. [22 ]
Calkins, R. [13 ]
Cartaro, C. [11 ]
Cerdeno, D. G. [2 ,17 ]
Chagani, H. [25 ]
Chen, Y. [14 ]
Cooley, J. [13 ]
Cornell, B. [1 ]
Cushman, P. [25 ]
Daal, M. [19 ]
Di Stefano, P. C. F. [9 ]
Doughty, T. [19 ]
Esteban, L. [17 ]
Fallows, S. [25 ]
Figueroa-Feliciano, E. [7 ]
Fritts, M. [25 ]
Gerbier, G. [9 ]
Ghaith, M. [9 ]
Godfrey, G. L. [11 ]
Golwala, S. R.
Hall, J. [8 ]
Harris, H. R. [15 ,16 ]
Hofer, T. [25 ]
Holmgren, D. [3 ]
Hong, Z. [7 ]
Hoppe, E. [8 ]
Hsu, L. [3 ]
Huber, M. E. [20 ,21 ]
Iyer, V. [6 ]
Jardin, D. [13 ]
Jastram, A. [15 ,16 ]
Kelsey, M. H. [11 ]
Kennedy, A. [25 ]
Kubik, A. [15 ,16 ]
Kurinsky, N. A. [11 ]
Leder, A. [5 ]
Loer, B. [8 ]
机构
[1] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA
[2] Univ Durham, Dept Phys, Durham DH1 3LE, England
[3] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA
[4] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA
[5] MIT, Dept Phys, Cambridge, MA 02139 USA
[6] HBNI, Natl Inst Sci Educ & Res, Sch Phys Sci, Jatni 752050, India
[7] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA
[8] Pacific Northwest Natl Lab, Richland, WA 99352 USA
[9] Queens Univ, Dept Phys, Kingston, ON K7L 3N6, Canada
[10] Santa Clara Univ, Dept Phys, Santa Clara, CA 95053 USA
[11] Kavli Inst Particle Astrophys & Cosmol, Natl Accelerator Lab, SLAC, Menlo Pk, CA 94025 USA
[12] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD USA
[13] Southern Methodist Univ, Dept Phys, Dallas, TX 75275 USA
[14] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA
[15] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA
[16] Texas A&M Univ, Mitchell Inst Fundamental Phys & Astron, College Stn, TX 77843 USA
[17] Univ Autonoma Madrid, Inst Fis Teor, UAM, CSIC, E-28049 Madrid, Spain
[18] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada
[19] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[20] Univ Colorado Denver, Dept Phys, Denver, CO 80217 USA
[21] Univ Colorado Denver, Dept Elect Engn, Denver, CO 80217 USA
[22] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[23] Univ Evansville, Dept Phys, Evansville, IN 47722 USA
[24] Univ Florida, Dept Phys, Gainesville, FL 32611 USA
[25] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA
[26] Univ South Dakota, Dept Phys, Vermillion, SD 57069 USA
[27] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada
[28] Univ Illinois, Dept Phys, Urbana, IL 61801 USA
基金
美国能源部; 美国国家科学基金会; 加拿大自然科学与工程研究理事会;
关键词
NUCLEAR RECOILS; IONIZATION; SILICON;
D O I
10.1103/PhysRevD.95.082002
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
SuperCDMS SNOLAB will be a next-generation experiment aimed at directly detecting low-mass particles (with masses <= 10 GeV=c(2)) that may constitute dark matter by using cryogenic detectors of two types (HV and iZIP) and two target materials (germanium and silicon). The experiment is being designed with an initial sensitivity to nuclear recoil cross sections similar to 1 x 10(-43) cm(2) for a dark matter particle mass of 1 GeV= c(2), and with capacity to continue exploration to both smaller masses and better sensitivities. The phonon sensitivity of the HV detectors will be sufficient to detect nuclear recoils from sub-GeV dark matter. A detailed calibration of the detector response to low-energy recoils will be needed to optimize running conditions of the HV detectors and to interpret their data for dark matter searches. Low-activity shielding, and the depth of SNOLAB, will reduce most backgrounds, but cosmogenically produced 3H and naturally occurring 32Si will be present in the detectors at some level. Even if these backgrounds are 10 times higher than expected, the science reach of the HV detectors would be over 3 orders of magnitude beyond current results for a dark matter mass of 1 GeV= c(2). The iZIP detectors are relatively insensitive to variations in detector response and backgrounds, and will provide better sensitivity for dark matter particles with masses. less than or similar to 5 GeV= c(2). The mix of detector types (HV and iZIP), and targets (germanium and silicon), planned for the experiment, as well as flexibility in how the detectors are operated, will allow us to maximize the low-mass reach, and understand the backgrounds that the experiment will encounter. Upgrades to the experiment, perhaps with a variety of ultra-low-background cryogenic detectors, will extend dark matter sensitivity down to the "neutrino floor,"where coherent scatters of solar neutrinos become a limiting background.
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