BibTex format
@inproceedings{El:2022,
author = {El, Hedri S and Ashida, Y and Giampaolo, A and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okamoto, K and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Xia, J and Megias, GD and Labarga, L and Marti, L 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 Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Gimpaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG },
title = {Diffuse Supernova Neutrino Background Search at Super-Kamiokande},
year = {2022}
}
RIS format (EndNote, RefMan)
TY - CPAPER
AB - We present the results of a search for the Diffuse Supernova Neutrino Background (DSNB) at Super-Kamiokande (SK) that incorporates 22.5 × 2970 kton.days of data from its fourth data-taking phase. Two analyses, with different energy regimes covering the 9.3−81.3 MeV antineutrino energy range, have been developed based on previous SK searches, with substantially improved background modeling and data reduction techniques. Moreover, a combined analysis of nearly 20 years of SK data (1996-2018) has been performed, with a 90% C.L. sensitivity to the DSNB flux comparable to various DSNB predictions. No significant evidence for a DSNB signal has been observed, and both analyses set world-leading limits on the DSNB flux that can reach about 2.7ν<inf>e</inf>.cm<sup>−2</sup>.s<sup>−1</sup> for a wide range of models.
AU - El,Hedri S
AU - Ashida,Y
AU - Giampaolo,A
AU - Abe,K
AU - Bronner,C
AU - Hayato,Y
AU - Hiraide,K
AU - Ikeda,M
AU - Kameda,J
AU - Kanemura,Y
AU - Kataoka,Y
AU - Miki,S
AU - Miura,M
AU - Moriyama,S
AU - Nagao,Y
AU - Nakahata,M
AU - Nakayama,S
AU - Okamoto,K
AU - Pronost,G
AU - Sekiya,H
AU - Shiozawa,M
AU - Sonoda,Y
AU - Suzuki,Y
AU - Takeda,A
AU - Takemoto,Y
AU - Takenaka,A
AU - Tanaka,H
AU - Watanabe,S
AU - Yano,T
AU - Han,S
AU - Kajita,T
AU - Okumura,K
AU - Tashiro,T
AU - Xia,J
AU - Megias,GD
AU - Labarga,L
AU - Marti,L
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 - Kropp,WR
AU - Locke,S
AU - Mine,S
AU - Smy,MB
AU - Sobel,HW
AU - Takhistov,V
AU - Hill,J
AU - Kim,JY
AU - Lim,IT
AU - Park,RG
AU - Bodur,B
AU - Scholberg,K
AU - Walter,CW
AU - Bernard,L
AU - Coffani,A
AU - Drapier,O
AU - Gimpaolo,A
AU - Gonin,M
AU - Mueller,TA
AU - Paganini,P
AU - Quilain,B
AU - Ishizuka,T
AU - Nakamura,T
AU - Jang,JS
AU - Learned,JG
AU - Cao,S
AU - Anthony,LHV
AU - Martin,D
AU - Scott,M
AU - Sztuc,AA
AU - Uchida,Y
AU - Berardi,V
AU - Catanesi,MG
AU - Radicioni,E
AU - Calabria,NF
AU - Machado,LN
AU - De,Rosa G
AU - Collazuol,G
AU - Iacob,F
AU - Lamoureux,M
AU - Mattiazzi,M
AU - Ospina,N
AU - Ludovici,L
AU - Maekawa,Y
AU - Nishimura,Y
AU - Friend,M
AU - Hasegawa,T
AU - Ishida,T
AU - Kobayashi,T
AU - Jakkapu,M
AU - Matsubara,T
AU - Nakadaira,T
AU - Nakamura,K
AU - Oyama,Y
PY - 2022///
TI - Diffuse Supernova Neutrino Background Search at Super-Kamiokande
ER -