Measurement of the 8B solar neutrino flux in SNO plus with very low backgrounds

被引：31

作者：

Anderson, M. ^{[1
]}

Andringa, S. ^{[2
]}

Asahi, S. ^{[1
]}

Askins, M. ^{[3
,5
]}

Auty, D. J. ^{[6
]}

Barros, N. ^{[7
]}

Bartlett, D. ^{[1
]}

Barao, F. ^{[2
,8
]}

Bayes, R. ^{[9
]}

Beier, E. W. ^{[7
]}

Bialek, A. ^{[1
,6
,10
,11
]}

Biller, S. D. ^{[11
]}

Blucher, E. ^{[12
,13
]}

Bonventre, R. ^{[4
,5
]}

Boulay, M. ^{[1
]}

Caden, E. ^{[9
,10
]}

Callaghan, E. J. ^{[5
]}

Caravaca, J. ^{[5
]}

Chauhan, D. ^{[10
]}

Chen, M. ^{[1
]}

Chkvorets, O. ^{[9
]}

Cleveland, B. ^{[9
,10
]}

Connors, C. ^{[9
]}

Coulter, I. T. ^{[7
]}

Depatie, M. M. ^{[9
]}

Di Lodovico, F. ^{[14
]}

Duncan, F. ^{[9
,10
]}

Dunger, J. ^{[11
]}

Falk, E. ^{[15
]}

Fischer, V. ^{[3
]}

Fletcher, E. ^{[1
]}

Ford, R. ^{[9
,10
]}

Gagnon, N. ^{[10
]}

Gilje, K. ^{[6
]}

Grant, C. ^{[16
]}

Grove, J. ^{[9
]}

Hallin, A. L. ^{[6
]}

Hallman, D. ^{[9
]}

Hans, S. ^{[17
]}

Hartnell, J. ^{[15
]}

Heintzelman, W. J. ^{[7
]}

Helmer, R. L. ^{[18
]}

Hernandez-Hernandez, J. L. ^{[9
,19
]}

Hreljac, B. ^{[1
]}

Hu, J. ^{[6
]}

Inacio, A. S. ^{[2
,20
]}

Jillings, C. J. ^{[9
,10
]}

Kaptanoglu, T. ^{[7
]}

Khaghani, P. ^{[9
]}

Klein, J. R. ^{[7
]}

机构：

[1] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada

[2] Lab Instrumentacao & Fis Expt Particulas LIP, Ave Prof Gama Pinto 2, P-1649003 Lisbon, Portugal

[3] Univ Calif Davis, 1 Shields Ave, Davis, CA 95616 USA

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

[5] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

[6] Univ Alberta, Dept Phys, 4-181 CCIS, Edmonton, AB T6G 2E1, Canada

[7] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA

[8] Univ Lisbon, Inst Super Tecn, Dept Fis, Ave Rovisco Pais, P-1049001 Lisbon, Portugal

[9] Laurentian Univ, Dept Phys, 935 Ramsey Lake Rd, Sudbury, ON P3E 2C6, Canada

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

[11] Univ Oxford, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[12] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA

[13] Univ Chicago, Dept Phys, Chicago, IL 60637 USA

[14] Queen Mary Univ London, Sch Phys & Astron, 327 Mile End Rd, London E1 4NS, England

[15] Univ Sussex, Phys & Astron, Pevensey 2, Brighton BN1 9QH, E Sussex, England

[16] Boston Univ, Dept Phys, 590 Commonwealth Ave, Boston, MA 02215 USA

[17] Brookhaven Natl Lab, Dept Chem, Bldg 555,POB 5000, Upton, NY 11973 USA

[18] TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada

[19] Univ Nacl Autonoma Mexico, Inst Fis, Apartado Postal 20-364, Mexico City 01000, DF, Mexico

[20] Univ Lisbon, Fac Ciencias FCUL, Dept Fis, Edificio C8, P-1749016 Lisbon, Portugal

[21] Norwich Univ, 158 Harmon Dr, Northfield, VT 05663 USA

[22] Univ Lancaster, Phys Dept, Lancaster LA1 4YB, England

[23] Univ Liverpool, Dept Phys, Liverpool L69 3BX, Merseyside, England

[24] Tech Univ Dresden, Inst Kern & Teilchenphys, Zellescher Weg 19, D-01069 Dresden, Germany

[25] Univ Alberta, Dept Chem, 1-001 CCIS, Edmonton, AB T6G 2E9, Canada

[26] Tech Univ Dresden, Fac Chem & Food Chem, D-01062 Dresden, Germany

[27] MTA Atomki, H-4001 Debrecen, Hungary

来源：

PHYSICAL REVIEW D | 2019年 / 99卷 / 01期

基金：

加拿大自然科学与工程研究理事会; 加拿大创新基金会; 美国国家科学基金会; 英国科学技术设施理事会; 欧洲研究理事会;

关键词：

D O I：

10.1103/PhysRevD.99.012012

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A measurement of the B-8 solar neutrino flux has been made using a 69.2 kt-day dataset acquired with the SNO+ detector during its water commissioning phase. At energies above 6 MeV the dataset is an extremely pure sample of solar neutrino elastic scattering events, owing primarily to the detector's deep location, allowing an accurate measurement with relatively little exposure. In that energy region the best tit background rate is 0.25(-0.07)(+0.09) events/kt-day, significantly lower than the measured solar neutrino event rate in that energy range, which is 1.03(-0.12)(+0.13) events/kt-day. Also using data below this threshold, don to 5 MeV, fits of the solar neutrino event direction yielded an observed flux of 2.51(-0.28)(+0.31)(stat)(-0.10)(+0.13)(syst) x 10(6) cm(-2) s(-1), assuming no neutrino oscillations. This rate is consistent with matter enhanced neutrino oscillations and measurements from other experiments.

引用

页数：7

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