Search for a Light Sterile Neutrino at Daya Bay

An, Fengpeng; Balantekin, A. B.; Band, H. R.; Beriguete, W.; Bishai, M.; Blyth, S.; Butorov, Ilya; Cao, G. F.; Cao, Junpeng; Chan, Y. L.; Chang, J. F.; Chang, Ling-Hua; Chang, Yun Hsuan; Chasman, C.; Chen, H.; Chen, Q. Y.; Chen, S. M.; Chen, X.; Chen, Y. X.; Chen, Y.; Cheng, Yaping; Cherwinka, J. J.; Chu, M. C.; Cummings, J. P.; Arcos, J. de; Deng, Z. Y.; Ding, Yayun; Diwan, M. V.; Draeger, E.; Du, X. F.; Dwyer, D. A.; Edwards, W. R.; Ely, S.; Fu, J.; Ge, Liangquan; Gill, R. L.; Gonchar, M.; Gong, Guanghua; Gong, H.; Grassi, M.; Gu, W.; Guan, Mengyun; Guo, Xin-Heng; Hackenburg, R.; Han, G. H.; Hans, S.; He, M.; Heeger, K. M.; Heng, Y. K.; Hinrichs, P.; Hor, YuenKeung; Hsiung, Y.; Hu, Bei-Zhen; Hu, Liangming; Hu, Li; Hu, T.; Hu, Wayne; Huang, E.-C.; Huang, Hanxiong; Huang, X. T.; Huber, Patrick; Hussain, G.; Isvan, Z.; Jaffe, D. E.; Jaffke, P.; Jen, K. L.; Jetter, S.; Ji, X.; Ji, X. L.; Jiang, Hao; Jiao, J. B.; Johnson, R. A.; Li, Kang; Kettell, S. H.; Krämer, M.; Kwan, K. K.; Kwok, M. W.; Kwok, T.; Lai, Wanchang; Lau, K.; Lebanowski, L.; Lee, J.; Lei, Ruiting; Leitner, R.; Leung, A.Y.T.; Leung, J. K. C.; Lewis, C. A.; Li, D. J.; Li, F.; Li, G. S.; Li, Q. J.; Li, W. D.; Li, X. N.; Li, X. Q.; Li, Y. F.; Li, Z. B.; Liu, Han; Lin, C. J.; Lin, Guey-Lin; Lin, P. Y.; Lin, S.; Lin, Y. C.; Ling, Jiajie; Link, J. M.; Littenberg, L.; Littlejohn, B. R.; Liu, D. W.; Liu, H.; Liu, J. L.; Liu, J. C.; Liu, S. S.; Liu, Y. B.; Lü, C.; Lu, Haoqi; Luk, K. B.; M., Q.; Y., X.; B., X.; Q., Y.; McDonald, Kirk T.; McFarlane, M. C.; McKeown, R. D.; Meng, Y.; Mitchell, I.V.; Kebwaro, Jeremiah Monari; Nakajima, Yasuhiro; Napolitano, J.; Naumov, D.; Наумова, Э.; Nemchenok, I.; Ngai, H. Y.; Ning, Z.; Ochoa-Ricoux, J. P.; Olshevski, A. G.; Patton, S.; Pec, V.; Peng, J. C.; Piilonen, L. E.; Pinsky, L.; Pun, C. S. J.; Qi, F. Z.; Qi, M.; Qian, X.; Raper, N.; Ren, Biying; Ren, Jie; Rosero, R.; Roskovec, B.; Ruan, X. C.; Shao, B.; Steiner, H.; Sun, G. X.; Sun, Jian; Tam, Y. H.; Tang, Xiao; Themann, H.; Tsang, K. V.; Tsang, R.; Tull, C. E.; Tung, Y. C.; Viren, B.; Vorobel, V.; Wang, C. H.; Wang, L. S.; Wang, L. Y.; Wang, M.; Wang, N. Y.; Wang, R. G.; Wang, W.; Wang, W. W.; Wang, X.; Wang, Y. F.; Wang, Z.; Wang, Z. M.; Webber, D.M.; Wei, H.; Wei, Yadong; Wen, L.; Whisnant, K.; White, C.; Whitehead, L.; Wise, T.; Wong, H. L. H.; Wong, Steven Chan-Fai; Worcester, E.; Wu, Qun; Xia, Dongmei; Xia, J. K.; Xia, X. M.; Xing, Zhi-zhong; Xu, Jilei; Jinsong, Xu; Xu, Jilei; Xu, Y.; Xue, T.; Yan, Jurang; Yang, Changgen; Yang, Lei; Yang, M. S.; Yang, M. T.; Ye, M.; Yeh, M.; Yeh, Y. S.; Young, Ben; Yu, G. Y.; Yu, Jiguo; Yu, Zezhong; Zang, S. L.; Zeng, Bin; Zhan, Liang; Zhang, C.; Zhang, F. H.; Zhang, J. W.; Zhang, Q. M.; Zhang, Q.; Zhang, S. H.; Zhang, Y. C.; Zhang, Y. M.; Zhang, Y. H.; Zhang, Y. X.; Zhang, Z. J.; Zhang, Z. Y.; Zhang, Z. P.; Zhao, J.; Zhao, Q.; Zhao, Yushan; Zhao, Yue; Zheng, Lei; Zhong, Weili; Li, Zhou; Zhou, Z. Y.; Zhuang, H. L.; Zou, J. H.

doi:10.1103/physrevlett.113.141802

Cited by 95 publications

(62 citation statements)

References 62 publications

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“…This effective mixing angle is the same as θ 14 under the choice of PMNS parameterisation in this work. Based on [56], we assume θ 14 ≤ 13 • at 95% C.L. Slightly tighter constraints are available from the BUGEY experiment; but at 90% C.L.…”

Section: Simulation Proceduresmentioning

confidence: 99%

Capabilities of long-baseline experiments in the presence of a sterile neutrino

Dutta

Gandhi

Kayser

et al. 2016

J. High Energ. Phys.

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Assuming that there is a sterile neutrino, we ask what then is the ability of long-baseline experiments to i) establish that neutrino oscillation violates CP, ii) determine the three-neutrino mass ordering, and iii) determine which CP-violating phase or phases are the cause of any CP violation that may be observed. We find that the ability to establish CP violation and to determine the mass ordering could be very substantial. However, the effects of the sterile neutrino could be quite large, and it might prove very difficult to determine which phase is responsible for an observed CP violation. We explain why a sterile neutrino changes the long-baseline sensitivities to CP violation and to the mass ordering in the ways that it does. We note that long-baseline experiments can probe the presence of sterile neutrinos in a way that is different from, and complementary to, the probes of short-baseline experiments. We explore the question of how large sterile-active mixing angles need to be before long-baseline experiments can detect their effects, or how small they need to be before the interpretation of these experiments can safely disregard the possible existence of sterile neutrinos.

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Section: Simulation Proceduresmentioning

confidence: 99%

Capabilities of long-baseline experiments in the presence of a sterile neutrino

Dutta

Gandhi

Kayser

et al. 2016

J. High Energ. Phys.

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show abstract

“…For other relevant studies of sterile neutrinos, see, e.g., Refs. [20][21][22][23][24][25][26][27][28][29][30]. Thus, to relieve the tensions in cosmological observations, a natural choice is to consider the model with light sterile neutrinos.…”

Section: Introductionmentioning

confidence: 99%

A search for sterile neutrinos with the latest cosmological observations

Lü

Zhang

2017

Eur. Phys. J. C

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We report the result of a search for sterile neutrinos with the latest cosmological observations. Both cases of massless and massive sterile neutrinos are considered in the CDM cosmology. The cosmological observations used in this work include the Planck 2015 temperature and polarization data, the baryon acoustic oscillation data, the Hubble constant direct measurement data, the Planck SunyaevZeldovich cluster counts data, the Planck lensing data, and the cosmic shear data. We find that the current observational data give a hint of the existence of massless sterile neutrino (as dark radiation) at the 1.44σ level, and the consideration of an extra massless sterile neutrino can indeed relieve the tension between observations and improve the cosmological fit. For the case of massive sterile neutrino, the observations give a rather tight upper limit on the mass, which implies that actually a massless sterile neutrino is more favored. Our result is consistent with the recent result of neutrino oscillation experiment done by the Daya Bay and MINOS collaborations, as well as the recent result of cosmic ray experiment done by the IceCube collaboration.

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“…New data from reactor and other short-and long-baseline neutrino experiments (such as MINOS [14][15][16][17][18][19][20][21][22][23][24][25], Daya Bay [25][26][27][28][29][30][31][32], Bugey [33], etc.) and their analyses considering the active-sterile neutrino oscillation have given new bounds on active-sterile mixing angles and Δm 2 .…”

Section: Introductionmentioning

confidence: 99%

Probing a four flavor vis-a-vis three flavor neutrino mixing for ultrahigh energy neutrino signals at a 1 km2 detector

2018

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We consider a four-flavor scenario for the neutrinos where an extra sterile neutrino is introduced to the three families of active neutrinos and study the deviation from the three-flavor scenario in the ultrahighenergy (UHE) regime. We calculate the possible muon and shower yields at a 1 km 2 detector such as IceCube for these neutrinos from distant UHE sources, e.g., gamma-ray bursts, etc. Similar estimations for muon and shower yields are also obtained for the three-flavor case. Comparing the two results, we find considerable differences between the yields for these two cases. This can be useful for probing the existence of a fourth sterile component using UHE neutrino flux.

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Search for a Light Sterile Neutrino at Daya Bay

Cited by 95 publications

References 62 publications

Capabilities of long-baseline experiments in the presence of a sterile neutrino

Capabilities of long-baseline experiments in the presence of a sterile neutrino

A search for sterile neutrinos with the latest cosmological observations

Probing a four flavor vis-a-vis three flavor neutrino mixing for ultrahigh energy neutrino signals at a 1 km2 detector

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