Abstract
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-going-muon events in the energy region above 1.6 GeV, the neutrino fluence limit is () cm-2 for muon neutrinos (muon antineutrinos), with an error range of ±5around 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 × 107 cm-2 for anti-electron neutrinos under the assumption of a Fermi-Dirac spectrum with average energy of 20 MeV.
| Original language | English |
|---|---|
| Article number | L4 |
| Journal | Astrophysical Journal Letters |
| Volume | 857 |
| Issue number | 1 |
| DOIs | |
| Publication status | Published - Apr 10 2018 |
Keywords
- astroparticle physics
- gravitational waves
- neutrinos
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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Search for Neutrinos in Super-Kamiokande Associated with the GW170817 Neutron-star Merger. / Abe, K.; Bronner, C.; Hayato, Y.; Ikeda, M.; Iyogi, K.; Kameda, J.; Kato, Y.; Kishimoto, Y.; Marti, Ll; Miura, M.; Moriyama, S.; Nakahata, M.; Nakajima, Y.; Nakano, Y.; Nakayama, S.; Orii, A.; Pronost, G.; Sekiya, H.; Shiozawa, M.; Sonoda, Y.; Takeda, A.; Takenaka, A.; Tanaka, H.; Tasaka, S.; Yano, T.; Akutsu, R.; Kajita, T.; Nishimura, Y.; Okumura, K.; Tsui, K. M.; Labarga, L.; Fernandez, P.; Blaszczyk, F. D.M.; Kachulis, C.; Kearns, E.; Raaf, J. L.; Stone, J. L.; Sulak, L. R.; Berkman, S.; Tobayama, S.; Bian, J.; Elnimr, M.; Kropp, W. R.; Locke, S.; Mine, S.; Weatherly, P.; Smy, M. B.; Sobel, H. W.; Takhistov, V.; Ganezer, K. S.; Hill, J.; Kim, J. Y.; Lim, I. T.; Park, R. G.; Li, Z.; O'Sullivan, E.; Scholberg, K.; Walter, C. W.; Gonin, M.; Imber, J.; Mueller, Th A.; Ishizuka, T.; Nakamura, T.; Jang, J. S.; Choi, K.; Learned, J. G.; Matsuno, S.; Amey, J.; Litchfield, R. P.; Ma, W. Y.; Uchida, Y.; Wascko, M. O.; Catanesi, M. G.; Intonti, R. A.; Radicioni, E.; Rosa, G. De; Ali, A.; Collazuol, G.; Ludovici, L.; Cao, S.; Friend, M.; Hasegawa, T.; Ishida, T.; Ishii, T.; Kobayashi, T.; Nakadaira, T.; Nakamura, K.; Oyama, Y.; Sakashita, K.; Sekiguchi, T.; Tsukamoto, T.; Abe, K. E.; Hasegawa, M.; Suzuki, A. T.; Takeuchi, Y.; Hayashino, T.; Hirota, S.; Jiang, M.; Mori, M.; Nakamura, K. E.; Nakaya, T.; Wendell, R. A.; Anthony, L. H.V.; McCauley, N.; Pritchard, A.; Fukuda, Y.; Itow, Y.; Murase, M.; Muto, F.; Mijakowski, P.; Frankiewicz, K.; Jung, C. K.; Li, X.; Palomino, J. L.; Santucci, G.; Viela, C.; Wilking, M. J.; Yanagisawa, C.; Fukuda, D.; Ishino, H.; Ito, Shintaro; Kibayashi, A.; Koshio, Y.; Nagata, H.; Sakuda, Makoto; Xu, C.; Kuno, Y.; Wark, D.; Lodovico, F. Di; Richards, B.; Sedgwick, S. Molina; Tacik, R.; Kim, S. B.; Cole, A.; Thompson, L.; Okazawa, H.; Choi, Y.; Ito, K.; Nishijima, K.; Koshiba, M.; Suda, Y.; Yokoyama, M.; Calland, R. G.; Hartz, M.; Martens, K.; Murdoch, M.; Quilain, B.; Simpson, C.; Suzuki, Y.; Vagins, M. R.; Hamabe, D.; Kuze, M.; Okajima, Y.; Yoshida, T.; Ishitsuka, M.; Martin, J. F.; Nantais, C. M.; Tanaka, H. A.; Towstego, T.; Konaka, A.; Chen, S.; Wan, L.; Minamino, A.
In: Astrophysical Journal Letters, Vol. 857, No. 1, L4, 10.04.2018.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - Search for Neutrinos in Super-Kamiokande Associated with the GW170817 Neutron-star Merger
AU - Abe, K.
AU - Bronner, C.
AU - Hayato, Y.
AU - Ikeda, M.
AU - Iyogi, K.
AU - Kameda, J.
AU - Kato, Y.
AU - Kishimoto, Y.
AU - Marti, Ll
AU - Miura, M.
AU - Moriyama, S.
AU - Nakahata, M.
AU - Nakajima, Y.
AU - Nakano, Y.
AU - Nakayama, S.
AU - Orii, A.
AU - Pronost, G.
AU - Sekiya, H.
AU - Shiozawa, M.
AU - Sonoda, Y.
AU - Takeda, A.
AU - Takenaka, A.
AU - Tanaka, H.
AU - Tasaka, S.
AU - Yano, T.
AU - Akutsu, R.
AU - Kajita, T.
AU - Nishimura, Y.
AU - Okumura, K.
AU - Tsui, K. M.
AU - Labarga, L.
AU - Fernandez, P.
AU - Blaszczyk, F. D.M.
AU - Kachulis, C.
AU - Kearns, E.
AU - Raaf, J. L.
AU - Stone, J. L.
AU - Sulak, L. R.
AU - Berkman, S.
AU - Tobayama, S.
AU - Bian, J.
AU - Elnimr, M.
AU - Kropp, W. R.
AU - Locke, S.
AU - Mine, S.
AU - Weatherly, P.
AU - Smy, M. B.
AU - Sobel, H. W.
AU - Takhistov, V.
AU - Ganezer, K. S.
AU - Hill, J.
AU - Kim, J. Y.
AU - Lim, I. T.
AU - Park, R. G.
AU - Li, Z.
AU - O'Sullivan, E.
AU - Scholberg, K.
AU - Walter, C. W.
AU - Gonin, M.
AU - Imber, J.
AU - Mueller, Th A.
AU - Ishizuka, T.
AU - Nakamura, T.
AU - Jang, J. S.
AU - Choi, K.
AU - Learned, J. G.
AU - Matsuno, S.
AU - Amey, J.
AU - Litchfield, R. P.
AU - Ma, W. Y.
AU - Uchida, Y.
AU - Wascko, M. O.
AU - Catanesi, M. G.
AU - Intonti, R. A.
AU - Radicioni, E.
AU - Rosa, G. De
AU - Ali, A.
AU - Collazuol, G.
AU - Ludovici, L.
AU - Cao, S.
AU - Friend, M.
AU - Hasegawa, T.
AU - Ishida, T.
AU - Ishii, T.
AU - Kobayashi, T.
AU - Nakadaira, T.
AU - Nakamura, K.
AU - Oyama, Y.
AU - Sakashita, K.
AU - Sekiguchi, T.
AU - Tsukamoto, T.
AU - Abe, K. E.
AU - Hasegawa, M.
AU - Suzuki, A. T.
AU - Takeuchi, Y.
AU - Hayashino, T.
AU - Hirota, S.
AU - Jiang, M.
AU - Mori, M.
AU - Nakamura, K. E.
AU - Nakaya, T.
AU - Wendell, R. A.
AU - Anthony, L. H.V.
AU - McCauley, N.
AU - Pritchard, A.
AU - Fukuda, Y.
AU - Itow, Y.
AU - Murase, M.
AU - Muto, F.
AU - Mijakowski, P.
AU - Frankiewicz, K.
AU - Jung, C. K.
AU - Li, X.
AU - Palomino, J. L.
AU - Santucci, G.
AU - Viela, C.
AU - Wilking, M. J.
AU - Yanagisawa, C.
AU - Fukuda, D.
AU - Ishino, H.
AU - Ito, Shintaro
AU - Kibayashi, A.
AU - Koshio, Y.
AU - Nagata, H.
AU - Sakuda, Makoto
AU - Xu, C.
AU - Kuno, Y.
AU - Wark, D.
AU - Lodovico, F. Di
AU - Richards, B.
AU - Sedgwick, S. Molina
AU - Tacik, R.
AU - Kim, S. B.
AU - Cole, A.
AU - Thompson, L.
AU - Okazawa, H.
AU - Choi, Y.
AU - Ito, K.
AU - Nishijima, K.
AU - Koshiba, M.
AU - Suda, Y.
AU - Yokoyama, M.
AU - Calland, R. G.
AU - Hartz, M.
AU - Martens, K.
AU - Murdoch, M.
AU - Quilain, B.
AU - Simpson, C.
AU - Suzuki, Y.
AU - Vagins, M. R.
AU - Hamabe, D.
AU - Kuze, M.
AU - Okajima, Y.
AU - Yoshida, T.
AU - Ishitsuka, M.
AU - Martin, J. F.
AU - Nantais, C. M.
AU - Tanaka, H. A.
AU - Towstego, T.
AU - Konaka, A.
AU - Chen, S.
AU - Wan, L.
AU - Minamino, A.
N1 - Funding Information: In the high-energy data sample, three neutrino interaction categories are considered: FC, PC, and UPMU. No neutrino candidate was found in the ±500-s window. The number of candidates in a 14-day time window in the entire sky, as well as We gratefully acknowledge the cooperation of the Kamioka Mining and Smelting Company. The Super-Kamiokande experiment has been built and operated from funding by the Japanese Ministry of Education, Culture, Sports, Science and Technology, the U.S. Department of Energy, and the U.S. National Science Foundation. Some of us have been supported by funds from the National Research Foundation of Korea NRF-2009-0083526 (KNRC) funded by the Ministry of Science, ICT, and Future Planning, the European Union H2020 RISE-GA641540-SKPLUS, the Japan Society for the Promotion of Science, the National Natural Science Foundation of China under grants No. 11235006, the National Science and Engineering Research Council (NSERC) of Canada, the Scinet and Westgrid Consortia of Compute Canada, and the National Science Centre, Poland (2015/17/N/ST2/04064, 2015/18/ E/ST2/00758). Publisher Copyright: © 2018. The American Astronomical Society. All rights reserved.
PY - 2018/4/10
Y1 - 2018/4/10
N2 - 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-going-muon events in the energy region above 1.6 GeV, the neutrino fluence limit is () cm-2 for muon neutrinos (muon antineutrinos), with an error range of ±5around 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 × 107 cm-2 for anti-electron neutrinos under the assumption of a Fermi-Dirac spectrum with average energy of 20 MeV.
AB - 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-going-muon events in the energy region above 1.6 GeV, the neutrino fluence limit is () cm-2 for muon neutrinos (muon antineutrinos), with an error range of ±5around 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 × 107 cm-2 for anti-electron neutrinos under the assumption of a Fermi-Dirac spectrum with average energy of 20 MeV.
KW - astroparticle physics
KW - gravitational waves
KW - neutrinos
UR - http://www.scopus.com/inward/record.url?scp=85045853820&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85045853820&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/aabaca
DO - 10.3847/2041-8213/aabaca
M3 - Article
AN - SCOPUS:85045853820
VL - 857
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 1
M1 - L4
ER -