TY - JOUR
T1 - Indirect search for dark matter from the Galactic Center and halo with the Super-Kamiokande detector
AU - THE SUPER-KAMIOKANDE COLLABORATION
AU - Abe, K.
AU - Bronner, C.
AU - Haga, Y.
AU - Hayato, Y.
AU - Ikeda, M.
AU - Imaizumi, S.
AU - Ito, H.
AU - Iyogi, K.
AU - Kameda, J.
AU - Kataoka, Y.
AU - Kato, Y.
AU - Kishimoto, Y.
AU - Marti, Ll
AU - Miura, M.
AU - Moriyama, S.
AU - Mochizuki, T.
AU - Nagao, Y.
AU - Nakahata, M.
AU - Nakajima, Y.
AU - Nakajima, T.
AU - Nakayama, S.
AU - Okada, T.
AU - Okamoto, K.
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 - Tomura, T.
AU - Ueno, K.
AU - Yano, T.
AU - Yokozawa, T.
AU - Akutsu, R.
AU - Han, S.
AU - Irvine, T.
AU - Kajita, T.
AU - Kametani, I.
AU - Lee, K. P.
AU - Mclachlan, T.
AU - Okumura, K.
AU - Richard, E.
AU - Hiraki, T.
AU - Ishino, H.
AU - Ito, Shintaro
AU - Koshio, Y.
AU - Sakuda, Makoto
N1 - Funding Information:
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 and the Ministry of Education (2018R1D1A3B07050696, 2018R1D1A1B07049158), the Japan Society for the Promotion of Science, the National Natural Science Foundation of China under Grants No.11235006, the Spanish Ministry of Science, Universities and Innovation (Grant No. PGC2018-099388-B-I00), the Natural Sciences and Engineering Research Council (NSERC) of Canada, the Scinet and Westgrid consortia of Compute Canada, the National Science Centre, Poland (2015/18/E/ST2/00758), the Science and Technology Facilities Council (STFC) and GridPPP, UK, the European Union's H2020-MSCA-RISE-2018 JENNIFER2 Grant Agreement No.822070, and H2020-MSCA-RISE-2019 SK2HK Grant Agreement No.872549.
Funding Information:
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 and the Ministry of Education (2018R1D1A3B07050696, 2018R1D1A1B07049158), the Japan Society for the Promotion of Science, the National Natural Science Foundation of China under Grants No. 11235006, the Spanish Ministry of Science, Universities and Innovation (Grant No. PGC2018-099388-B-I00), the Natural Sciences and Engineering Research Council (NSERC) of Canada, the Scinet and Westgrid consortia of Compute Canada, the National Science Centre, Poland (2015/18/E/ST2/00758), the Science and Technology Facilities Council (STFC) and GridPPP, UK, the European Union’s H2020-MSCA-RISE-2018 JENNIFER2 Grant Agreement No. 822070, and H2020-MSCA-RISE-2019 SK2HK Grant Agreement No. 872549.
Publisher Copyright:
© 2020 authors.
PY - 2020/10
Y1 - 2020/10
N2 - We present a search for an excess of neutrino interactions due to dark matter in the form of weakly interacting massive particles (WIMPs) annihilating in the Galactic center or halo based on the data set of Super-Kamiokande-I, -II, -III and -IV taken from 1996 to 2016. We model the neutrino flux, energy, and flavor distributions assuming WIMP self-annihilation is dominant to νν¯, μ+μ-, bb¯, or W+W-. The excess is in comparison to atmospheric neutrino interactions which are modeled in detail and fit to data. Limits on the self-annihilation cross section σ are derived for WIMP masses in the range 1 GeV to 10 TeV, reaching as low as 9.6×10-23 cm3 s-1 for 5 GeV WIMPs in bb¯ mode and 1.2×10-24 cm3 s-1 for 1 GeV WIMPs in νν¯ mode. The obtained sensitivity of the Super-Kamiokande detector to WIMP masses below several tens of GeV is the best among similar indirect searches to date.
AB - We present a search for an excess of neutrino interactions due to dark matter in the form of weakly interacting massive particles (WIMPs) annihilating in the Galactic center or halo based on the data set of Super-Kamiokande-I, -II, -III and -IV taken from 1996 to 2016. We model the neutrino flux, energy, and flavor distributions assuming WIMP self-annihilation is dominant to νν¯, μ+μ-, bb¯, or W+W-. The excess is in comparison to atmospheric neutrino interactions which are modeled in detail and fit to data. Limits on the self-annihilation cross section σ are derived for WIMP masses in the range 1 GeV to 10 TeV, reaching as low as 9.6×10-23 cm3 s-1 for 5 GeV WIMPs in bb¯ mode and 1.2×10-24 cm3 s-1 for 1 GeV WIMPs in νν¯ mode. The obtained sensitivity of the Super-Kamiokande detector to WIMP masses below several tens of GeV is the best among similar indirect searches to date.
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U2 - 10.1103/PhysRevD.102.072002
DO - 10.1103/PhysRevD.102.072002
M3 - Article
AN - SCOPUS:85096624570
SN - 2470-0010
VL - 102
JO - Physical Review D
JF - Physical Review D
IS - 7
M1 - 072002
ER -