Constraints on low-mass, relic dark matter candidates from a surface-operated SuperCDMS single-charge sensitive detector

被引：105

作者：

Amaral, D. W. ^{[1
]}

Aralis, T. ^{[2
]}

Aramaki, T. ^{[3
]}

Arnquist, I. J. ^{[4
]}

Azadbakht, E. ^{[5
,6
]}

Banik, S. ^{[7
]}

Barker, D. ^{[8
]}

Bathurst, C. ^{[9
]}

Bauer, D. A. ^{[10
]}

Bezerra, L. V. S. ^{[11
,12
]}

Bhattacharyya, R. ^{[5
,6
]}

Binder, T. ^{[13
]}

Bowles, M. A. ^{[14
]}

Brink, P. L. ^{[3
]}

Bunker, R. ^{[4
]}

Cabrera, B. ^{[15
]}

Calkins, R. ^{[16
]}

Cameron, R. A. ^{[3
]}

Cartaro, C. ^{[3
]}

Cerdeno, D. G. ^{[1
,17
]}

Chang, Y-Y ^{[2
]}

Chen, R. ^{[18
]}

Chott, N. ^{[14
]}

Cooley, J. ^{[16
]}

Coombes, H. ^{[9
]}

Corbett, J. ^{[19
]}

Cushman, P. ^{[8
]}

De Brienne, F. ^{[20
]}

di Vacri, M. L. ^{[4
]}

Diamond, M. D. ^{[21
]}

Fascione, E. ^{[12
,19
]}

Figueroa-Feliciano, E. ^{[18
]}

Fink, C. W. ^{[22
]}

Fouts, K. ^{[3
]}

Fritts, M. ^{[8
]}

Gerbier, G. ^{[19
]}

Germond, R. ^{[12
,19
]}

Ghaith, M. ^{[19
]}

Golwala, S. R. ^{[2
]}

Harris, H. R. ^{[5
,6
,23
]}

Herbert, N. ^{[5
,6
]}

Hines, B. A. ^{[24
]}

Hollister, M., I ^{[10
]}

Hong, Z. ^{[18
]}

Hoppe, E. W. ^{[4
]}

Hsu, L. ^{[10
]}

Huber, M. E. ^{[24
,25
]}

Iyer, V ^{[7
]}

Jardin, D. ^{[16
]}

Jastram, A. ^{[5
,6
]}

机构：

[1] Univ Durham, Dept Phys, Durham DH1 3LE, England

[2] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[3] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA

[4] Pacific Northwest Natl Lab, Richland, WA 99352 USA

[5] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[6] Texas A&M Univ, Mitchell Inst Fundamental Phys & Astron, College Stn, TX 77843 USA

[7] HBNI, Natl Inst Sci Educ & Res, Sch Phys Sci, Jatni 752050, India

[8] Univ Minnesota, Sch Phys & Astrorwmy, Minneapolis, MN 55455 USA

[9] Univ Florida, Dept Phys, Gainesville, FL 32611 USA

[10] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[11] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada

[12] TRIUMF, Columbia, BC V6T 2A3, Canada

[13] Univ South Dakota, Dept Phys, Vermillion, SD 57069 USA

[14] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA

[15] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[16] Southern Methodist Univ, Dept Phys, Dallas, TX 75275 USA

[17] Univ Autonoma Madrid, UAM, CSIC, Inst Fis Teor, Madrid 28049, Spain

[18] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA

[19] Queens Univ, Dept Phys, Kingston, ON K7L 3N6, Canada

[20] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada

[21] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada

[22] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[23] Texas A&M Univ, Dept Elect & Comp Engn, College Stn, TX 77843 USA

[24] Univ Colorado, Dept Phys, Denver, CO 80217 USA

[25] Univ Colorado, Dept Elect Engn, Denver, CO 80217 USA

[26] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[27] SNOLAB, Creighton Mine 9,1039 Reg Rd 24, Sudbury, ON P3Y 1N2, Canada

[28] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany

[29] Santa Clara Univ, Dept Phys, Santa Clara, CA 95053 USA

来源：

PHYSICAL REVIEW D | 2020年 / 102卷 / 09期

基金：

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：

OPTICAL-PARAMETERS; INTRINSIC SILICON; ABSORPTION; SI; PHOTOABSORPTION; TRANSMISSION; GERMANIUM; REGION;

D O I：

10.1103/PhysRevD.102.091101

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This article presents an analysis and the resulting limits on light dark matter inelastically scattering off of electrons, and on dark photon and axionlike particle absorption, using a second-generation SuperCDMS high-voltage eV-resolution detector. The 0.93 g Si detector achieved a 3 eV phonon energy resolution; for a detector bias of 100 V, this corresponds to a charge resolution of 3% of a single electron-hole pair. The energy spectrum is reported from a blind analysis with 1.2 g-days of exposure acquired in an above-ground laboratory. With charge carrier trapping and impact ionization effects incorporated into the dark matter signal models, the dark matter-electron cross section (sigma) over bar (e) is constrained for dark matter masses from 0.5 to 10(4) MeV/c(2); in the mass range from 1.2 to 50 eV/c(2) the dark photon kinetic mixing parameter e and the axioelectric coupling constant gae are constrained. The minimum 90% confidence-level upper limits within the above-mentioned mass ranges are (sigma) over bar (e) = 8.7 x 10(-34) cm(2), epsilon = 3.3 x 10(-14), and g(ae) = 1.0 x 10(-9).

引用

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