- Main
Search for electron-antineutrinos associated with gravitational-wave events GW150914, GW151012, GW151226, GW170104, GW170608, GW170814, and GW170817 at Daya Bay * *Daya Bay is supported in part by the Ministry of Science and Technology of China, the U.S. Department of Energy, the Chinese Academy of Sciences, the CAS Center for Excellence in Particle Physics, the National Natural Science Foundation of China, the Guangdong provincial government, the Shenzhen municipal government, the China General Nuclear Power Group, Key Laboratory of Particle and Radiation Imaging (Tsinghua University), the Ministry of Education, Key Laboratory of Particle Physics and Particle Irradiation (Shandong University), the Ministry of Education, Shanghai Laboratory for Particle Physics and Cosmology, the Research Grants Council of the Hong Kong Special Administrative Region of China, the University Development Fund of the University of Hong Kong, the MOE program for Research of Excellence at National Taiwan University, National Chia
- An, FP;
- Balantekin, AB;
- Band, HR;
- Bishai, M;
- Blyth, S;
- Cao, GF;
- Cao, J;
- Chang, JF;
- Chang, Y;
- Chen, HS;
- Chen, SM;
- Chen, Y;
- Chen, YX;
- Cheng, J;
- Cheng, ZK;
- Cherwinka, JJ;
- Chu, MC;
- Cummings, JP;
- Dalager, O;
- Deng, FS;
- Ding, YY;
- Diwan, MV;
- Dohnal, T;
- Dove, J;
- Dvořák, M;
- Dwyer, DA;
- Gallo, JP;
- Gonchar, M;
- Gong, GH;
- Gong, H;
- Gu, WQ;
- Guo, JY;
- Guo, L;
- Guo, XH;
- Guo, YH;
- Guo, Z;
- Hackenburg, RW;
- Hans, S;
- He, M;
- Heeger, KM;
- Heng, YK;
- Higuera, A;
- Hor, YK;
- Hsiung, YB;
- Hu, BZ;
- Hu, JR;
- Hu, T;
- Hu, ZJ;
- Huang, HX;
- Huang, XT;
- Huang, YB;
- Huber, P;
- Jaffe, DE;
- Jen, KL;
- Ji, XL;
- Ji, XP;
- Johnson, RA;
- Jones, D;
- Kang, L;
- Kettell, SH;
- Kohn, S;
- Kramer, M;
- Langford, TJ;
- Lee, J;
- Lee, JHC;
- Lei, RT;
- Leitner, R;
- Leung, JKC;
- Li, F;
- Li, JJ;
- Li, QJ;
- Li, S;
- Li, SC;
- Li, WD;
- Li, XN;
- Li, XQ;
- Li, YF;
- Li, ZB;
- Liang, H;
- Lin, CJ;
- Lin, GL;
- Lin, S;
- Ling, JJ;
- Link, JM;
- Littenberg, L;
- Littlejohn, BR;
- Liu, JC;
- Liu, JL;
- Lu, C;
- Lu, HQ;
- Lu, JS;
- Luk, KB;
- B., X;
- Y., X;
- Q., Y;
- Marshall, C;
- Caicedo, DA Martinez;
- McDonald, KT;
- McKeown, RD;
- Meng, Y;
- Napolitano, J;
- Naumov, D;
- Naumova, E;
- Ochoa-Ricoux, JP;
- Olshevskiy, A;
- Pan, H-R;
- Park, J;
- Patton, S;
- Peng, JC;
- Pun, CSJ;
- Qi, FZ;
- Qi, M;
- Qian, X;
- Raper, N;
- Ren, J;
- Reveco, C Morales;
- Rosero, R;
- Roskovec, B;
- Ruan, XC;
- Steiner, H;
- Sun, JL;
- Tmej, T;
- Treskov, K;
- Tse, W-H;
- Tull, CE;
- Viren, B;
- Vorobel, V;
- Wang, CH;
- Wang, J;
- Wang, M;
- Wang, NY;
- Wang, RG;
- Wang, W;
- Wang, W;
- Wang, X;
- Wang, Y;
- Wang, YF;
- Wang, Z;
- Wang, Z;
- Wang, ZM;
- Wei, HY;
- Wei, LH;
- Wen, LJ;
- Whisnant, K;
- White, CG;
- Wong, HLH;
- Worcester, E;
- Wu, DR;
- Wu, FL;
- Wu, Q;
- Wu, WJ;
- Xia, DM;
- Xie, ZQ;
- Xing, ZZ;
- Xu, JL;
- Xu, T;
- Xue, T;
- Yang, CG;
- Yang, L;
- Yang, YZ;
- Yao, HF;
- Ye, M;
- Yeh, M;
- Young, BL;
- Yu, HZ;
- Yu, ZY;
- Yue, BB;
- Zeng, S;
- Zeng, Y;
- Zhan, L;
- Zhang, C;
- Zhang, FY;
- Zhang, HH;
- Zhang, JW;
- Zhang, QM;
- Zhang, XT;
- Zhang, YM;
- Zhang, YX;
- Zhang, YY;
- Zhang, ZJ;
- Zhang, ZP;
- Zhang, ZY;
- Zhao, J;
- Zhou, L;
- Zhuang, HL;
- Zou, JH
- et al.
Published Web Location
https://doi.org/10.1088/1674-1137/abe84bAbstract
The establishment of a possible connection between neutrino emission and gravitational-wave (GW) bursts is important to our understanding of the physical processes that occur when black holes or neutron stars merge. In the Daya Bay experiment, using the data collected from December 2011 to August 2017, a search was performed for electron-Antineutrino signals that coincided with detected GW events, including GW150914, GW151012, GW151226, GW170104, GW170608, GW170814, and GW170817. We used three time windows of 10, 500, and 1000 s relative to the occurrence of the GW events and a neutrino energy range of 1.8 to 100 MeV to search for correlated neutrino candidates. The detected electron-Antineutrino candidates were consistent with the expected background rates for all the three time windows. Assuming monochromatic spectra, we found upper limits (90% confidence level) of the electron-Antineutrino fluence of (1.13-2.44)×1011 cm-2 at 5 MeV to 8.0×107 cm-2 at 100 MeV for the three time windows. Under the assumption of a Fermi-Dirac spectrum, the upper limits were found to be (5.4-7.0)×109 cm-2 for the three time windows.
Many UC-authored scholarly publications are freely available on this site because of the UC's open access policies. Let us know how this access is important for you.
Main Content
Enter the password to open this PDF file:
-
-
-
-
-
-
-
-
-
-
-
-
-
-