BibTex format
@inproceedings{Harada:2024,
author = {Harada, M and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Tanaka, H and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang, X and Yoshida, S and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Lee, SH and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Beauchêne, A and Drapier, O and Giampaolo, A and Mueller, TA and Santos, AD and Paganini, P and Quilain, B and},
title = {First result of a search for Diffuse Supernova Neutrino Background in SK-Gd experiment},
year = {2024}
}
RIS format (EndNote, RefMan)
TY - CPAPER
AB - Since 2020, Super-Kamiokande (SK) detector has been updated by loading gadolinium (Gd) as a new experimental phase, ‘SK-Gd.’ In the SK-Gd experiment, we can search low-energy electron antineutrinos via inverse-beta decay with efficient neutron identification thanks to high cross-section and high-energy gamma-ray emission of thermal neutron capture on Gd. Until July 2022, the observation is operated with the 0.01% Gd mass concentration. The neutron capture fraction on Gd is about 50% in this situation. In this paper, the first search result for the flux of astrophysical electron antineutrinos for the energy range of O(10) MeV in SK-Gd with a 22.5 × 552 kton·day exposure at 0.01% Gd mass concentration of the initial stage of SK-Gd is reported.
AU - Harada,M
AU - Abe,K
AU - Bronner,C
AU - Hayato,Y
AU - Hiraide,K
AU - Hosokawa,K
AU - Ieki,K
AU - Ikeda,M
AU - Kameda,J
AU - Kanemura,Y
AU - Kaneshima,R
AU - Kashiwagi,Y
AU - Kataoka,Y
AU - Miki,S
AU - Mine,S
AU - Miura,M
AU - Moriyama,S
AU - Nakano,Y
AU - Nakahata,M
AU - Nakayama,S
AU - Noguchi,Y
AU - Sato,K
AU - Sekiya,H
AU - Shiba,H
AU - Shimizu,K
AU - Shiozawa,M
AU - Sonoda,Y
AU - Suzuki,Y
AU - Takeda,A
AU - Takemoto,Y
AU - Tanaka,H
AU - Yano,T
AU - Han,S
AU - Kajita,T
AU - Okumura,K
AU - Tashiro,T
AU - Tomiya,T
AU - Wang,X
AU - Yoshida,S
AU - Fernandez,P
AU - Labarga,L
AU - Ospina,N
AU - Zaldivar,B
AU - Pointon,BW
AU - Kearns,E
AU - Raaf,JL
AU - Wan,L
AU - Wester,T
AU - Bian,J
AU - Griskevich,NJ
AU - Locke,S
AU - Smy,MB
AU - Sobel,HW
AU - Takhistov,V
AU - Yankelevich,A
AU - Hill,J
AU - Lee,SH
AU - Moon,DH
AU - Park,RG
AU - Bodur,B
AU - Scholberg,K
AU - Walter,CW
AU - Beauchêne,A
AU - Drapier,O
AU - Giampaolo,A
AU - Mueller,TA
AU - Santos,AD
AU - Paganini,P
AU - Quilain,B
AU - Nakamura,T
AU - Jang,JS
AU - Machado,LN
AU - Learned,JG
AU - Choi,K
AU - Iovine,N
AU - Cao,S
AU - Anthony,LHV
AU - Martin,D
AU - Prouse,NW
AU - Scott,M
AU - Sztuc,AA
AU - Uchida,Y
AU - Berardi,V
AU - Catanesi,MG
AU - Radicioni,E
AU - Calabria,NF
AU - Langella,A
AU - De,Rosa G
AU - Collazuol,G
AU - Iacob,F
AU - Mattiazzi,M
AU - Ludovici,L
AU - Gonin,M
AU - Pronost,G
AU - Fujisawa,C
AU - Maekawa,Y
AU - Nishimura,Y
AU - Okazaki,R
AU - Akutsu,R
AU - Friend,M
PY - 2024///
TI - First result of a search for Diffuse Supernova Neutrino Background in SK-Gd experiment
ER -