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BibTex format

@inproceedings{Giampaolo:2022,
author = {Giampaolo, A and El, Hedri S 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 Giampolo, 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 and Cao, S and},
title = {Diffuse Supernova Neutrino Background search at Super-Kamiokande with neutron tagging},
year = {2022}
}

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TY  - CPAPER
AB  - Detecting the Diffuse Supernova Neutrino Background at Super-Kamiokande requires designing state-of-the-art background removal technique to reject radioactivity induced by cosmic muon spallation, and identify atmospheric neutrino interactions. Identifying the neutron produced by the interaction of DSNB antineutrinos would allow to remove most of these backgrounds, but is particularly challenging in pure water. With the advent of the SK-Gd era, with Gadolinium being dissolved in the SK water, the efficiency of the neutron tagging procedure will increase dramatically, and the SK experiment will make significant gains in its sensitivity to the DSNB. I will present the role of neutron tagging and the challenges it provides, as well as discuss the impact of the SK-Gd project.
AU  - Giampaolo,A
AU  - El,Hedri S
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  - Giampolo,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
AU  - Sakashita,K
PY  - 2022///
TI  - Diffuse Supernova Neutrino Background search at Super-Kamiokande with neutron tagging
ER  -

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Professor Yoshi Uchida

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