BibTex format
@inproceedings{Nakano:2024,
author = {Nakano, Y and Tada, T and Kitagawa, H and Koshio, Y 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 San},
title = {Measurement of the charge ratio and polarization of cosmic-ray muon using the tagged decay-e events in Super-Kamiokande},
year = {2024}
}
RIS format (EndNote, RefMan)
TY - CPAPER
AB - Neutrinos and muons from cosmic-ray interactions in the atmosphere originate from mesons, such as pions and kaons, in air-showers. An accuracy of the absolute atmospheric neutrino flux and its flavor ratio are limited due to the uncertainty of meson productions in hadronic interaction models. In order to reduce such uncertainty, measurements of the charge ratio and the polarization of cosmic-ray muons are important as new inputs to theoretical models which simulate the atmospheric neutrino flux. In this proceedings, we present the results of the charge ratio (R) and polarization (P<sup>μ</sup><inf>0</inf>) of cosmic-ray muon measurements using the decay electrons collected from 2008 September to 2022 June by the Super-Kamiokande (SK) detector. We measured muon charge ratio to be R = 1.32±0.02 (stat.+syst.) and the muon polarization at the production location to be P<sup>μ</sup><inf>0</inf> = 0.52±0.01 (stat.+syst.). The SK detector uniquely measured the polarization of cosmic-ray muons with energies more than 1 TeV at sea-level because of its underground location.
AU - Nakano,Y
AU - Tada,T
AU - Kitagawa,H
AU - Koshio,Y
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
PY - 2024///
TI - Measurement of the charge ratio and polarization of cosmic-ray muon using the tagged decay-e events in Super-Kamiokande
ER -