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@article{Simpson:2019:1538-4357/ab4883,
author = {Simpson, C and Abe, K and Bronner, C and Hayato, Y and Ikeda, M 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 Nakahata, M and Nakajima, Y 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 Yano, T and Akutsu, R and Kajita, T and Okumura, K and Wang, R and Xia, J and Bravo-Berguno, D and Labarga, L and Fernandez, P and Blaszczyk, FDM and Kachulis, C and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Sussman, S and Berkman, S and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Ganezer, KS and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Coffani, A and Drapier, O and Gonin, M and Imber, J and Mueller, TA and Paganini, P and Ishizuka, },
doi = {1538-4357/ab4883},
journal = {The Astrophysical Journal: an international review of astronomy and astronomical physics},
pages = {1--14},
title = {Sensitivity of super-kamiokande with gadolinium to low energy antineutrinos from pre-supernova emission},
url = {http://dx.doi.org/10.3847/1538-4357/ab4883},
volume = {885},
year = {2019}
}

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TY  - JOUR
AB  - Supernova detection is a major objective of the Super-Kamiokande (SK) experiment. In the next stage of SK (SK-Gd), gadolinium (Gd) sulfate will be added to the detector, which will improve the ability of the detector to identify neutrons. A core-collapse supernova (CCSN) will be preceded by an increasing flux of neutrinos and antineutrinos, from thermal and weak nuclear processes in the star, over a timescale of hours; some of which may be detected at SK-Gd. This could provide an early warning of an imminent CCSN, hours earlier than the detection of the neutrinos from core collapse. Electron antineutrino detection will rely on inverse beta decay events below the usual analysis energy threshold of SK, so Gd loading is vital to reduce backgrounds while maximizing detection efficiency. Assuming normal neutrino mass ordering, more than 200 events could be detected in the final 12 hr before core collapse for a 15–25 solar mass star at around 200 pc, which is representative of the nearest red supergiant to Earth, α-Ori (Betelgeuse). At a statistical false alarm rate of 1 per century, detection could be up to 10 hr before core collapse, and a pre-supernova star could be detected by SK-Gd up to 600 pc away. A pre-supernova alert could be provided to the astrophysics community following gadolinium loading.
AU  - Simpson,C
AU  - Abe,K
AU  - Bronner,C
AU  - Hayato,Y
AU  - Ikeda,M
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  - Nakahata,M
AU  - Nakajima,Y
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  - Yano,T
AU  - Akutsu,R
AU  - Kajita,T
AU  - Okumura,K
AU  - Wang,R
AU  - Xia,J
AU  - Bravo-Berguno,D
AU  - Labarga,L
AU  - Fernandez,P
AU  - Blaszczyk,FDM
AU  - Kachulis,C
AU  - Kearns,E
AU  - Raaf,JL
AU  - Stone,JL
AU  - Wan,L
AU  - Wester,T
AU  - Sussman,S
AU  - Berkman,S
AU  - Bian,J
AU  - Griskevich,NJ
AU  - Kropp,WR
AU  - Locke,S
AU  - Mine,S
AU  - Smy,MB
AU  - Sobel,HW
AU  - Takhistov,V
AU  - Weatherly,P
AU  - Ganezer,KS
AU  - Hill,J
AU  - Kim,JY
AU  - Lim,IT
AU  - Park,RG
AU  - Bodur,B
AU  - Scholberg,K
AU  - Walter,CW
AU  - Coffani,A
AU  - Drapier,O
AU  - Gonin,M
AU  - Imber,J
AU  - Mueller,TA
AU  - Paganini,P
AU  - Ishizuka,T
AU  - Nakamura,T
AU  - Jang,JS
AU  - Choi,K
AU  - Learned,JG
AU  - Matsuno,S
AU  - Litchfield,RP
AU  - Sztuc,AA
AU  - Uchida,Y
AU  - Wascko,MO
AU  - Berardi,V
AU  - Calabria,NF
AU  - Catanesi,MG
AU  - Intonti,RA
AU  - Radicioni,E
AU  - De,Rosa G
AU  - Collazuol,G
AU  - Iacob,F
AU  - Ludovici,L
AU  - Nishimura,Y
AU  - Cao,S
AU  - Friend,M
AU  - Hasegawa,T
AU  - Ishida,T
AU  - Kobayashi,T
AU  - Nakadaira,T
AU  - Nakamura,K
AU  - Oyama,Y
AU  - Sakashita,K
AU  - Sekiguchi,T
AU  - Tsukamoto,T
AU  - Abe,KE
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  - Ali,A
AU  - Ashida,Y
AU  - Hayashino,T
AU  - Hirota,S
AU  - Jiang,M
AU  - Kikawa,T
AU  - Mori,M
AU  - Nakamura,KE
AU  - Nakaya,T
AU  - Wendell,RA
AU  - Anthony,LH
AU  - McCauley,N
AU  - Pritchard,A
AU  - Tsui,KM
AU  - Fukuda,Y
AU  - Itow,Y
AU  - Murrase,M
AU  - Niwa,T
AU  - Taani,M
AU  - Tsukada,M
AU  - Mijakowski,P
AU  - Frankiewicz,K
AU  - Jung,CK
AU  - Li,X
AU  - Palomino,JL
AU  - Santucci,G
AU  - Vilela,C
AU  - Wilking,MJ
AU  - Yanagisawa,C
AU  - Fukuda,D
AU  - Harada,M
AU  - Hagiwara,K
AU  - Horai,T
AU  - Ishino,H
AU  - Ito,S
AU  - Koshio,Y
AU  - Sakuda,M
AU  - Takahira,Y
AU  - Xu,C
AU  - Kuno,Y
AU  - Cook,L
AU  - Wark,D
AU  - Di,Lodovico F
AU  - Sedgwick,SM
AU  - Richards,B
AU  - Zsoldos,S
AU  - Kim,SB
AU  - Tacik,R
AU  - Thiesse,M
AU  - Thompson,L
AU  - Okazawa,H
AU  - Choi,Y
AU  - Nishijima,K
AU  - Koshiba,M
AU  - Yokoyama,M
AU  - Goldsack,A
AU  - Martens,K
AU  - Murdoch,M
AU  - Quilain,B
AU  - Suzuki,Y
AU  - Vagins,MR
AU  - Kuze,M
AU  - Okajima,Y
AU  - Tanaka,M
AU  - Yoshida,T
AU  - Ishitsuka,M
AU  - Matsumoto,R
AU  - Ohta,K
AU  - Martin,JF
AU  - Nantais,CM
AU  - Tanaka,HA
AU  - Towstego,T
AU  - Hartz,M
AU  - Konaka,A
AU  - de,Perio P
AU  - Chen,S
AU  - Jamieson,B
AU  - Walker,J
AU  - Minamino,A
DO  - 1538-4357/ab4883
EP  - 14
PY  - 2019///
SN  - 0004-637X
SP  - 1
TI  - Sensitivity of super-kamiokande with gadolinium to low energy antineutrinos from pre-supernova emission
T2  - The Astrophysical Journal: an international review of astronomy and astronomical physics
UR  - http://dx.doi.org/10.3847/1538-4357/ab4883
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000499869600001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - https://iopscience.iop.org/article/10.3847/1538-4357/ab4883
UR  - http://hdl.handle.net/10044/1/76628
VL  - 885
ER  -

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