Search for Neutrinos in Super-Kamiokande Associated With Gravitational-Wave Events Gw150914 and Gw151226

Abe, K.; Haga, Kazuo; Hayato, Y.; Ikeda, M.; Iyogi, K.; Kameda, J.; Kishimoto, Y.; Miura, Makoto; Moriyama, S.; Nakahata, M.; Nakajima, Tetsuo; Nakano, Y.; Nakayama, S.; Orii, A.; Sekiya, H.; Shiozawa, M.; Takeda, Atsushi; Tanaka, H.; Tasaka, S.; Tomura, T.; Akutsu, R.; Kajita, T.; Kaneyuki, K.; Nishimura, Y.; Richard, E.; Okumura, K.; Labarga, L.; Fernández, P.; Blaszczyk, F. d. M.; Gustafson, J.; Kachulis, C.; Kearns, E.; Raaf, J. L.; Stone, James L.; Sulak, L.; Berkman, S.; Nantais, C.; Tobayama, S.; Goldhaber, M.; Kropp, W. R.; Mine, S.; Weatherly, P.; Smy, M. B.; Sobel, H. W.; Takhistov, Volodymyr; Ganezer, K. S.; Hartfiel, B. L.; Hill, J.; Hồng, Nguyễn Thị; 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.; Friend, M.; Hasegawa, T.; Ishida, Toru; Ishii, T.; Kobayashi, T.; Nakadaira, T.; Nakamura, K.; Oyama, Y.; Sakashita, K.; Sekiguchi, T.; Tsukamoto, T.; Suzuki, A.; Takeuchi, Y.; Yano, T.; Cao, S.; Hiraki, T.; Hirota, S.; Huang, K.; Jiang, M.; Minamino, A.; Nakaya, T.; Patel, N. D.; Wendell, R.; Suzuki, K.; Fukuda, Y.; Itow, Y.; Suzuki, T.; Mijakowski, P.; Frankiewicz, K.; Hignight, J.; Imber, J.; Jung, C. K.; Li, X.; Palomino, J. L.; Santucci, G.; Wilking, M. J.; Yanagisawa, C.; Fukuda, Daisuke; Ishino, H.; Kayano, T.; Kibayashi, A.; Koshio, Y.; Mori, Takaaki; Sakuda, M.; Xu, Chenyuan; Kuno, Y.; Tacik, R.; Kim, S. B.; Okazawa, H.; Choi, Y.; Nishijima, K.; Koshiba, M.; Totsuka, Y.; Suda, Y.; Yokoyama, M.; Bronner, C.; Calland, R. G.; Hartz, M.; Martens, K.; Marti, Ll.; Suzuki, Y.; Vagins, M. R.; Martin, J. F.; Tanaka, Hirohisa; Konaka, A.; Chen, S.; Wan, L.; Zhang, Y.; Wilkes, R. J.

doi:10.3847/2041-8205/830/1/l11

Cited by 36 publications

(23 citation statements)

References 21 publications

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“…In this paper, we neglect background contamination because of the small expected background rate in the fiducial volume for energies over 5 MeV. More specifically, for electrons and positrons, the measured background rate above 5 MeV of kinetic energy at SK was 150 per day at the time of GW150914 (Abe et al 2016a), which corresponds to 0.17 events during 100 s in the 22.5 kton detector volume. This property helps to determine the time of the last event.…”

Section: Summary and Discussionmentioning

confidence: 99%

“…It should also be noted that this background estimate already takes into account reduction cuts (for details, see Abe et al 2016b). At energies above 5 MeV, the dominant background is expected to be from spallation products (Abe et al 2016a), whose rate can be estimated from measurements at SK (Zhang et al 2016) as roughly 2.5 events in 100 s, without the reduction cuts. Roughly speaking, the reduction cuts reduce the back-ground level significantly (about a factor of 10), but also reduce the neutrino signal by ∼20% (Abe et al 2016b).…”

Section: Summary and Discussionmentioning

confidence: 99%

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Observing Supernova Neutrino Light Curves with Super-Kamiokande: Expected Event Number over 10 s

Suwa

Sumiyoshi

Nakazato

et al. 2019

ApJ

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Supernova neutrinos are crucially important to probe the final phases of massive star evolution. As is well known from observations of SN 1987A, neutrinos provide information on the physical conditions responsible for neutron star formation and on the supernova explosion mechanism. However, there is still no complete understanding of the long-term evolution of neutrino emission in supernova explosions, although there are a number of modern simulations of neutrino radiation hydrodynamics, which study neutrino emission at times less than one second after the bounce. In the present work we systematically calculate the number of neutrinos that can be observed in Super-Kamiokande over periods longer than ten seconds using the database of Nakazato et al. (2013) anticipating that neutrinos from a Galactic supernova can be detected for several tens of seconds. We find that for a supernova at a distance of 10 kpc, neutrinos remain observable for longer than 30 s for a low-mass neutron star (1.20M ⊙ gravitational mass) and even longer than 100 s for a high-mass neutron star (2.05M ⊙ ). These scenarios are much longer than the observations of SN 1987A and longer than the duration of existing numerical simulations. We propose a new analysis method based on the cumulative neutrino event distribution as a function of reverse time from the last observed event, as a useful probe of the neutron star mass. Our result demonstrates the importance of complete modeling of neutrino light curves in order to extract physical quantities essential for understanding supernova explosion mechanisms, such as the mass and radius of the resulting neutron star.

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Section: Summary and Discussionmentioning

confidence: 99%

Section: Summary and Discussionmentioning

confidence: 99%

Observing Supernova Neutrino Light Curves with Super-Kamiokande: Expected Event Number over 10 s

Suwa

Sumiyoshi

Nakazato

et al. 2019

ApJ

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“…The detection of SRNs via inverse beta decay (IBD, ν e þ p → n þ e þ ) is a goal of current and future large neutrino detectors [3]. In water Cherenkov detectors such as Super-Kamiokande (SK), where e=γ discrimination is feasible but still challenging, NCQE interactions of atmospheric neutrinos with oxygen form a significant background to SRN searches as well as other rare signal searches [4][5][6][7].…”

Section: Introductionmentioning

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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“…The analysis method is similar to that for the previous neutrino search in SK for GW150914 and GW151226 (Abe et al 2016a). SK is a water Cherenkov detector with 50-kton water mass and 22.5-kton fiducial volume.…”

Section: Introductionmentioning

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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Search for Neutrinos in Super-Kamiokande Associated With Gravitational-Wave Events Gw150914 and Gw151226

Cited by 36 publications

References 21 publications

Observing Supernova Neutrino Light Curves with Super-Kamiokande: Expected Event Number over 10 s

Observing Supernova Neutrino Light Curves with Super-Kamiokande: Expected Event Number over 10 s

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

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