Search for an Excess of Events in the Super-Kamiokande Detector in the Directions of the Astrophysical Neutrinos Reported by the IceCube Collaboration

Abe, K.; Bronner, C.; Pronost, G.; Hayato, Y.; Ikeda, M.; Iyogi, K.; Kameda, J.; Kato, Y.; Kishimoto, Y.; Marti, Ll.; Miura, M.; Moriyama, S.; Nakahata, M.; Nakano, Y.; Nakayama, S.; Okajima, Y.; Orii, A.; Sekiya, H.; Shiozawa, M.; Sonoda, Y.; Takeda, Atsushi; Takenaka, A.; Tasaka, S.; Tomura, T.; Akutsu, R.; Kajita, T.; Kaneyuki, K.; Nishimura, Y.; Okumura, K.; Tsui, K. M.; Labarga, L.; Fernández, P.; Blaszczyk, F. d. M.; Gustafson, J.; Kachulis, C.; Kearns, E.; Raaf, J. L.; Stone, James L.; Sulak, L.; Berkman, S.; Tobayama, S.; Goldhaber, M.; Elnimr, M.; Kropp, W. R.; Mine, S.; Locke, S.; Weatherly, P.; Smy, M. B.; Sobel, H. W.; Takhistov, Volodymyr; Ganezer, K. S.; Hill, J.; Kim, J. Y.; Lim, I. T.; Park, R. G.; Himmel, A.; Li, Z.; O’Sullivan, Erin; Scholberg, K.; Walter, C. W.; Ishizuka, T.; Nakamura, T.; Jang, J. S.; Choi, Koun; Learned, J. G.; Matsuno, S.; Smith, S. N.; Amey, Jake Lewis; Litchfield, R. P.; Y., W.; Uchida, Y.; Wascko, M. O.; Friend, M.; Hasegawa, T.; Ishida, Toru; Ishii, T.; Kobayashi, T.; Nakadaira, T.; Nakamura, K.; Oyama, Y.; Sakashita, K.; Sekiguchi, Toyokazu; Tsukamoto, T.; Abe, K.; Hasegawa, M.; Suzuki, A.; Takeuchi, Y.; Yano, T.; Cao, S.; Hayashino, T.; Hiraki, T.; Hirota, S.; Huang, K.; Jiang, M.; Minamino, A.; Nakamura, K.; Nakaya, T.; Quilain, B.; Patel, N. D.; Wendell, R.; Anthony, L. H. V.; McCauley, N.; Pritchard, A.; Fukuda, Y.; Itow, Y.; Murase, M.; Muto, Fumihito; Mijakowski, P.; Frankiewicz, K.; Jung, C. K.; Li, X.; Palomino, J. L.; Santucci, G.; Vilela, C.; Wilking, M. J.; Yanagisawa, C.; Ito, S.; Fukuda, Daisuke; Ishino, H.; Kibayashi, A.; Koshio, Y.; Nagata, Hiroshi; Sakuda, M.; Xu, Chenyuan; Kuno, Y.; Wark, D.; Lodovico, F. Di; Richards, B.; Tacik, R.; Kim, S. B.; Cole, A. A.; Thompson, L. F.; Okazawa, H.; Choi, Y.; Ito, K.; Nishijima, K.; Koshiba, M.; Totsuka, Y.; Suda, Y.; Yokoyama, M.; Calland, R. G.; Hartz, M.; Martens, K.; Simpson, C.; Suzuki, Y.; Vagins, M. R.; Hamabe, D.; Kuze, M.; Yoshida, Tadashi; Ishitsuka, M.; Martin, J. F.; Nantais, C.; Tanaka, Hirohisa; Konaka, A.; Chen, S.; Wan, L.; Zhang, Y.; Wilkes, R. J.

doi:10.3847/1538-4357/aa951b

Cited by 10 publications

(10 citation statements)

References 17 publications

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“…The following reduction cuts are first applied to remove spurious events and entering backgrounds [18,34]. First, a trigger cut is applied to remove calibration events and events that trigger the OD, which are most likely to be a cosmic-ray muon.…”

Section: First Reductionmentioning

confidence: 99%

Measurement of the neutrino-oxygen neutral-current quasielastic cross section using atmospheric neutrinos at Super-Kamiokande

Wan¹,

Bronner²,

Hayato³

et al. 2019

Phys. Rev. D

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Neutral current (NC) interactions of atmospheric neutrinos on oxygen form one of the major backgrounds in the search for supernova relic neutrinos with water-based Cherenkov detectors. The NC channel is dominated by neutrino quasielastic (NCQE) scattering off nucleons inside 16 O nuclei. In this paper we report the first measurement of NCQE cross section using atmospheric neutrinos at Super-Kamiokande (SK). The measurement used 2,778 live days of SK-IV data with a fiducial volume of 22.5 kiloton water. Within the visible energy window of 7.5-29.5 MeV, we observed 117 events compared to the expected 71.9 NCQE signal and 53.1 background events. Weighted by the atmospheric neutrino spectrum from 160 MeV to 10 GeV, the flux averaged NCQE cross section is measured to be ð1.01 AE 0.17ðstat:Þ þ0.78 −0.30 ðsys:ÞÞ × 10 −38 cm 2 .

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Section: First Reductionmentioning

confidence: 99%

Measurement of the neutrino-oxygen neutral-current quasielastic cross section using atmospheric neutrinos at Super-Kamiokande

Wan¹,

Bronner²,

Hayato³

et al. 2019

Phys. Rev. D

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“…Because the direction of NGC4993 is well known Abbott et al (2017c);Coulter et al (2017), for UPMU data, for which the angular resolution is better than for the other two samples, we concentrated on a ±5°cone around NGC4993 for the event search in the subsequent 14 days. This method was previously used in SK to search for neutrino signals associated with astrophysical objects (Abe et al 2017). The ±5°constraint was not used for the ±500 s search in Table 1 because no event was observed in all sky during this window, and unlike the 14-day-window case, the zenith angle change of NGC4993 in ±500 s can be ignored.…”

Section: High-energy Data Samplementioning

confidence: 99%

Search for Neutrinos in Super-Kamiokande Associated with the GW170817 Neutron-star Merger

Bronner¹,

Hayato²,

Ikeda³

et al. 2018

ApJL

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We report the results of a neutrino search in Super-Kamiokande (SK) for coincident signals with the first detected gravitational wave (GW) produced by a binary neutron-star merger, GW170817, which was followed by a short gamma-ray burst, GRB170817A, and a kilonova/macronova. We searched for coincident neutrino events in the range from 3.5MeV to ∼100 PeV, in a time window ±500 s around the gravitational wave detection time, as well as during a 14-day period after the detection. No significant neutrino signal was observed for either time window. We calculated 90% confidence level upper limits on the neutrino fluence for GW170817. From the upward-goingmuon events in the energy region above 1.6 GeV, the neutrino fluence limit is -+ 16.0 0.6 0.7 ( -+ 21.3 0.8 1.1 ) cm −2 for muon neutrinos (muon antineutrinos), with an error range of ±5°around the zenith angle of NGC4993, and the energy spectrum is under the assumption of an index of −2. The fluence limit for neutrino energies less than 100MeV, for which the emission mechanism would be different than for higher-energy neutrinos, is also calculated. It is 6.6×10 7 cm −2 for anti-electron neutrinos under the assumption of a Fermi-Dirac spectrum with average energy of 20 MeV.

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“…It would be interesting to see if SuperK can improve this limit with data already collected. SuperKamiokande has also searched for matter disintegration caused by n −n transition inside nuclear matter, and has set a limit of τ > 1.89×10 32 yrs [14], which would correspond to Λ nn > 10 5 GeV, with a larger uncertainty resulting from the relevant nuclear matrix element. An experiment carried out at ILL with free neutrons has set a limit on the n −n oscillation time of τ (n −n) > 0.86 × 10 8 sec [15], which would also yield comparable limit, Λ nn > 10 5 GeV.…”

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confidence: 99%

Determining Majorana nature of neutrino from nucleon decays andn−n¯oscillations

Babu¹,

Mohapatra²

2015

Phys. Rev. D

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We show that discovery of baryon number violation in two processes with at least one obeying the selection rule ∆(B − L) = ±2 can determine the Majorana character of neutrinos. Thus observing p → e + π 0 and n → e − π 0 decays, or p → e + π 0 and n − n oscillations, or n → e − π + and n − n oscillations would establish that neutrinos are Majorana particles. We discuss this in a model-independent effective operator approach.

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Search for an Excess of Events in the Super-Kamiokande Detector in the Directions of the Astrophysical Neutrinos Reported by the IceCube Collaboration

Cited by 10 publications

References 17 publications

Measurement of the neutrino-oxygen neutral-current quasielastic cross section using atmospheric neutrinos at Super-Kamiokande

Measurement of the neutrino-oxygen neutral-current quasielastic cross section using atmospheric neutrinos at Super-Kamiokande

Search for Neutrinos in Super-Kamiokande Associated with the GW170817 Neutron-star Merger

Determining Majorana nature of neutrino from nucleon decays andn−n¯oscillations

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