Search for Neutrinos in Super-Kamiokande associated with the GW170817 neutron-star merger
Creators: name: Abe, K.
name: Bronner, C.
name: Hayato, Y.
name: Ikeda, M.
name: Iyogi, K.
name: Kameda, J.
name: Kato, Y.
name: Kishimoto, Y.
name: Marti, Ll.
name: Miura, M.
name: Moriyama, S.
name: Nakahata, M.
name: Nakajima, Y.
name: Nakano, Y.
name: Nakayama, S.
name: Orii, A.
name: Pronost, G.
name: Sekiya, H.
name: Shiozawa, M.
name: Sonoda, Y.
name: Takeda, A.
name: Takenaka, A.
name: Tanaka, H.
name: Tasaka, S.
name: Yano, T.
name: Akutsu, R.
name: Kajita, T.
name: Nishimura, Y.
name: Okumura, K.
name: Tsui, K. M.
name: Labarga, L.
name: Fernandez, P.
name: Blaszczyk, F. d. M.
name: Kachulis, C.
name: Kearns, E.
name: Raaf, J. L.
name: Stone, J. L.
name: Sulak, L. R.
name: Berkman, S.
name: Tobayama, S.
name: Bian, J.
name: Elnimr, M.
name: Kropp, W. R.
name: Locke, S.
name: Mine, S.
name: Weatherly, P.
name: Smy, M. B.
name: Sobel, H. W.
name: Takhistov, V.
name: Ganezer, K. S.
name: Hill, J.
name: Kim, J. Y.
name: Lim, I. T.
name: Park, R. G.
name: Li, Z.
name: O'Sullivan, E.
name: Scholberg, K.
name: Walter, C. W.
name: Gonin, M.
name: Imber, J.
name: Mueller, Th. A.
name: Ishizuka, T.
name: Nakamura, T.
name: Jang, J. S.
name: Choi, K.
name: Learned, J. G.
name: Matsuno, S.
name: Amey, J.
name: Litchfield, R. P.
name: Ma, W. Y.
name: Uchida, Y.
name: Wascko, M. O.
name: Catanesi, M. G.
name: Intonti, R. A.
name: Radicioni, E.
name: De Rosa, G.
name: Ali, A.
name: Collazuol, G.
name: Ludovici, L.
name: Cao, S.
name: Friend, M.
name: Hasegawa, T.
name: Ishida, T.
name: Ishii, T.
name: Kobayashi, T.
name: Nakadaira, T.
name: Nakamura, K.
name: Oyama, Y.
name: Sakashita, K.
name: Sekiguchi, T.
name: Tsukamoto, T.
name: Abe, KE.
name: Hasegawa, M.
name: Suzuki, A. T.
name: Takeuchi, Y.
name: Hayashino, T.
name: Hirota, S.
name: Jiang, M.
name: Mori, M.
name: Nakamura, KE.
name: Nakaya, T.
name: Wendell, R. A.
name: Anthony, L. H. V.
name: McCauley, N.
name: Pritchard, A.
name: Fukuda, Y.
name: Itow, Y.
name: Murase, M.
name: Muto, F.
name: Mijakowski, P.
name: Frankiewicz, K.
name: Jung, C. K.
name: Li, X.
name: Palomino, J. L.
name: Santucci, G.
name: Viela, C.
name: Wilking, M. J.
name: Yanagisawa, C.
name: Fukuda, D.
name: Ishino, H.
name: Ito, S.
name: Kibayashi, A.
name: Koshio, Y.
name: Nagata, H.
name: Sakuda, M.
name: Xu, C.
name: Kuno, Y.
name: Wark, D.
name: Di Lodovico, F.
name: Richards, B.
name: Sedgwick, S. Molina
name: Tacik, R.
name: Kim, S. B.
name: Cole, A.
name: Thompson, L.
name: Okazawa, H.
name: Choi, Y.
name: Ito, K.
name: Nishijima, K.
name: Koshiba, M.
name: Suda, Y.
name: Yokoyama, M.
name: Calland, R. G.
name: Hartz, M.
name: Martens, K.
name: Murdoch, M.
name: Quilain, B.
name: Simpson, C.
name: Suzuki, Y.
name: Vagins, M. R.
name: Hamabe, D.
name: Kuze, M.
name: Okajima, Y.
name: Yoshida, T.
name: Ishitsuka, M.
name: Martin, J. F.
name: Nantais, C. M.
name: Tanaka, H. A.
name: Towstego, T.
name: Konaka, A.
name: Chen, S.
name: Wan, L.
name: Minamino, A.
Publisher: name: arXiv
Year: 2018
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We report the results of a neutrino search in Super-Kamiokande for coincident signals with the first detected gravitational wave 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 $\sim$100 PeV, in a time window $\pm$500 seconds 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-going-muon events in the energy region above 1.6 GeV, the neutrino fluence limit is $16.0^{+0.7}_{-0.6}$ ($21.3^{+1.1}_{-0.8}$) cm$^{-2}$ for muon neutrinos (muon antineutrinos), with an error range of $\pm5^{\circ}$ 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 $6.6 \times 10^7$ cm$^{-2}$ for anti-electron neutrinos under the assumption of a Fermi-Dirac spectrum with average energy of 20 MeV.
description: 8 pages, 4 figures