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@article{Abe:2020:10.1103/PhysRevD.102.072002,
author = {Abe, K and Bronner, C and Haga, Y and Hayato, Y and Ikeda, M and Imaizumi, S and Ito, H and Iyogi, K and Kameda, J and Kataoka, Y and Kato, Y and Kishimoto, Y and Marti, L and Miura, M and Moriyama, S and Mochizuki, T and Nagao, Y and Nakahata, M and Nakajima, Y and Nakajima, T and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Takeda, A and Takenaka, A and Tanaka, H and Tasaka, S and Tomura, T and Ueno, K and Yano, T and Yokozawa, T and Akutsu, R and Han, S and Irvine, T and Kajita, T and Kametani, I and Lee, KP and McLachlan, T and Okumura, K and Richard, E and Tashiro, T and Wang, R and Xia, J and Bravo-Berguno, D and Labarga, L and Fernandez, P and Blaszczyk, FDM and Gustafson, J and Kachulis, C and Kearns, E and Raaf, JL and Stone, JL and Sulak, LR and Sussman, S and Wan, L and Wester, T and Berkman, S and Tobayama, S and Bian, J and Carminati, G and Elnimr, M and Griskevich, NJ and Kropp, WR and Locke, S and Mine},
doi = {10.1103/PhysRevD.102.072002},
journal = {Physical Review D: Particles, Fields, Gravitation and Cosmology},
pages = {072002  1--072002  14},
title = {Indirect search for dark matter from the Galactic Center and halo with the Super-Kamiokande detector},
url = {http://dx.doi.org/10.1103/PhysRevD.102.072002},
volume = {102},
year = {2020}
}

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TY  - JOUR
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 ν¯ν, μ+μ−, b¯b, 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 σAV 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 b¯b mode and 1.2×10−24  cm3 s−1 for 1 GeV WIMPs in ν¯ν 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.
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,L
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,KP
AU  - McLachlan,T
AU  - Okumura,K
AU  - Richard,E
AU  - Tashiro,T
AU  - Wang,R
AU  - Xia,J
AU  - Bravo-Berguno,D
AU  - Labarga,L
AU  - Fernandez,P
AU  - Blaszczyk,FDM
AU  - Gustafson,J
AU  - Kachulis,C
AU  - Kearns,E
AU  - Raaf,JL
AU  - Stone,JL
AU  - Sulak,LR
AU  - Sussman,S
AU  - Wan,L
AU  - Wester,T
AU  - Berkman,S
AU  - Tobayama,S
AU  - Bian,J
AU  - Carminati,G
AU  - Elnimr,M
AU  - Griskevich,NJ
AU  - Kropp,WR
AU  - Locke,S
AU  - Mine,S
AU  - Renshaw,A
AU  - Smy,MB
AU  - Sobel,HW
AU  - Takhistov,V
AU  - Weatherly,P
AU  - Hartfiel,BL
AU  - Hill,J
AU  - Keig,WE
AU  - Hong,N
AU  - Kim,JY
AU  - Lim,IT
AU  - Park,RG
AU  - Akiri,T
AU  - Bodur,B
AU  - Himmel,A
AU  - Li,Z
AU  - O'Sullivan,E
AU  - Scholberg,K
AU  - Walter,CW
AU  - Wongjirad,T
AU  - Coffani,A
AU  - Drapier,O
AU  - El,Hedri S
AU  - Giampaolo,A
AU  - Gonin,M
AU  - Imber,J
AU  - Mueller,TA
AU  - Paganini,P
AU  - Quilain,B
AU  - Ishizuka,T
AU  - Nakamura,T
AU  - Jang,JS
AU  - Choi,K
AU  - Learned,JG
AU  - Matsuno,S
AU  - Smith,SN
AU  - Amey,J
AU  - Anthony,LH
AU  - Litchfield,RP
AU  - Sztuc,AA
AU  - Uchida,Y
AU  - Wascko,MO
AU  - Berardi,V
AU  - Catanesi,MG
AU  - Intonti,RA
AU  - Radicioni,E
AU  - Calabria,NF
AU  - Machado,LN
AU  - De,Rosa G
AU  - Collazuol,G
AU  - Iacob,F
AU  - Lamoureux,M
AU  - Ospina,N
AU  - Ludovici,L
AU  - Boschi,T
AU  - Di,Lodovico F
AU  - Sedgwick,SM
AU  - Zsoldos,S
AU  - Nishimura,Y
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
AU  - Hasegawa,M
AU  - Isobe,Y
AU  - Miyabe,H
AU  - Nakano,Y
AU  - Shiozawa,T
AU  - Sugimoto,T
AU  - Suzuki,AT
AU  - Takeuchi,Y
AU  - Yamamoto,S
AU  - Ali,A
AU  - Ashida,Y
AU  - Hayashino,T
AU  - Hiraki,T
AU  - Hirota,S
AU  - Huang,K
AU  - Ieki,K
AU  - Jiang,M
AU  - Kikawa,T
AU  - Mori,M
AU  - Murakami,A
AU  - Nakamura,KE
AU  - Nakaya,T
AU  - Patel,ND
AU  - Suzuki,K
AU  - Takahashi,S
AU  - Tateishi,K
AU  - Wendell,RA
AU  - McCauley,N
AU  - Mehta,P
AU  - Pritchard,A
AU  - Tsui,KM
AU  - Fukuda,Y
AU  - Itow,Y
AU  - Menjo,H
AU  - Mitsuka,G
AU  - Murase,M
AU  - Muto,F
AU  - Niwa,T
AU  - Sato,K
AU  - Suzuki,T
AU  - Taani,M
AU  - Tsukada,M
AU  - Mijakowski,P
AU  - Frankiewicz,K
AU  - Hignight,J
AU  - Jung,CK
AU  - Li
DO  - 10.1103/PhysRevD.102.072002
EP  - 1
PY  - 2020///
SN  - 1550-2368
SP  - 072002
TI  - Indirect search for dark matter from the Galactic Center and halo with the Super-Kamiokande detector
T2  - Physical Review D: Particles, Fields, Gravitation and Cosmology
UR  - http://dx.doi.org/10.1103/PhysRevD.102.072002
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000576601100001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - https://journals.aps.org/prd/abstract/10.1103/PhysRevD.102.072002
UR  - http://hdl.handle.net/10044/1/84547
VL  - 102
ER  -

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