Solar neutrino results in Super-Kamiokande-III

K. Abe; Y. Hayato; T. Iida; M. Ikeda; C. Ishihara; K. Iyogi; J. Kameda; K. Kobayashi; Y. Koshio; Y. Kozuma; M. Miura; S. Moriyama; M. Nakahata; S. Nakayama; Y. Obayashi; H. Ogawa; H. Sekiya; M. Shiozawa; Y. Suzuki; A. Takeda; Y. Takenaga; K. Ueno; K. Ueshima; H. Watanabe; S. Yamada; T. Yokozawa; S. Hazama; H. Kaji; T. Kajita; K. Kaneyuki; T. McLachlan; K. Okumura; Y. Shimizu; N. Tanimoto; M. R. Vagins; L. Labarga; L. M. Magro; F. Dufour; E. Kearns; M. Litos; J. L. Raaf; J. L. Stone; L. R. Sulak; W. Wang; M. Goldhaber; K. Bays; D. Casper; J. P. Cravens; W. R. Kropp; S. Mine; C. Regis; A. Renshaw; M. B. Smy; H. W. Sobel; K. S. Ganezer; J. Hill; W. E. Keig; J. S. Jang; J. Y. Kim; I. T. Lim; J. Albert; R. Wendell; T. Wongjirad; K. Scholberg; C. W. Walter; T. Ishizuka; S. Tasaka; J. G. Learned; S. Matsuno; Y. Watanabe; T. Hasegawa; T. Ishida; T. Ishii; T. Kobayashi; T. Nakadaira; K. Nakamura; K. Nishikawa; H. Nishino; Y. Oyama; K. Sakashita; T. Sekiguchi; T. Tsukamoto; A. T. Suzuki; Y. Takeuchi; A. Minamino; T. Nakaya; Y. Fukuda; Y. Itow; G. Mitsuka; T. Tanaka; C. K. Jung; G. Lopez; C. McGrew; R. Terri; C. Yanagisawa; N. Tamura; H. Ishino; A. Kibayashi; S. Mino; T. Mori; Makoto Sakuda; H. Toyota; Y. Kuno; M. Yoshida; S. B. Kim; B. S. Yang; T. Ishizuka; H. Okazawa; Y. Choi; K. Nishijima; Y. Yokosawa; M. Koshiba; Y. Totsuka; M. Yokoyama; S. Chen; Y. Heng; Z. Yang; H. Zhang; D. Kielczewska; P. Mijakowski; K. Connolly; M. Dziomba; E. Thrane; R. J. Wilkes

doi:10.1103/PhysRevD.83.052010

Solar neutrino results in Super-Kamiokande-III

K. Abe, Y. Hayato, T. Iida, M. Ikeda, C. Ishihara, K. Iyogi, J. Kameda, K. Kobayashi, Y. Koshio, Y. Kozuma, M. Miura, S. Moriyama, M. Nakahata, S. Nakayama, Y. Obayashi, H. Ogawa, H. Sekiya, M. Shiozawa, Y. Suzuki, A. TakedaY. Takenaga, K. Ueno, K. Ueshima, H. Watanabe, S. Yamada, T. Yokozawa, S. Hazama, H. Kaji, T. Kajita, K. Kaneyuki, T. McLachlan, K. Okumura, Y. Shimizu, N. Tanimoto, M. R. Vagins, L. Labarga, L. M. Magro, F. Dufour, E. Kearns, M. Litos, J. L. Raaf, J. L. Stone, L. R. Sulak, W. Wang, M. Goldhaber, K. Bays, D. Casper, J. P. Cravens, W. R. Kropp, S. Mine, C. Regis, A. Renshaw, M. B. Smy, H. W. Sobel, K. S. Ganezer, J. Hill, W. E. Keig, J. S. Jang, J. Y. Kim, I. T. Lim, J. Albert, R. Wendell, T. Wongjirad, K. Scholberg, C. W. Walter, T. Ishizuka, S. Tasaka, J. G. Learned, S. Matsuno, Y. Watanabe, T. Hasegawa, T. Ishida, T. Ishii, T. Kobayashi, T. Nakadaira, K. Nakamura, K. Nishikawa, H. Nishino, Y. Oyama, K. Sakashita, T. Sekiguchi, T. Tsukamoto, A. T. Suzuki, Y. Takeuchi, A. Minamino, T. Nakaya, Y. Fukuda, Y. Itow, G. Mitsuka, T. Tanaka, C. K. Jung, G. Lopez, C. McGrew, R. Terri, C. Yanagisawa, N. Tamura, H. Ishino, A. Kibayashi, S. Mino, T. Mori, Makoto Sakuda, H. Toyota, Y. Kuno, M. Yoshida, S. B. Kim, B. S. Yang, T. Ishizuka, H. Okazawa, Y. Choi, K. Nishijima, Y. Yokosawa, M. Koshiba, Y. Totsuka, M. Yokoyama, S. Chen, Y. Heng, Z. Yang, H. Zhang, D. Kielczewska, P. Mijakowski, K. Connolly, M. Dziomba, E. Thrane, R. J. Wilkes

研究成果 › 査読

325 被引用数 (Scopus)

抄録

The results of the third phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first and second phase results. With improved detector calibrations, a full detector simulation, and improved analysis methods, the systematic uncertainty on the total neutrino flux is estimated to be ±2.1%, which is about two thirds of the systematic uncertainty for the first phase of Super-Kamiokande. The observed B8 solar flux in the 5.0 to 20 MeV total electron energy region is 2.32±0.04(stat) ±0.05(sys)×106cm^-2sec^-1 under the assumption of pure electron-flavor content, in agreement with previous measurements. A combined oscillation analysis is carried out using SK-I, II, and III data, and the results are also combined with the results of other solar neutrino experiments. The best-fit oscillation parameters are obtained to be ^sin2θ₁₂=0.30-0.01+0.02(^tan2θ ₁₂=0.42-0.02+0.04) and Δm212=6.2-1.9+1.1×10 ^-5eV2. Combined with KamLAND results, the best-fit oscillation parameters are found to be ^sin2θ₁₂=0.31±0. 01(^tan2θ₁₂=0.44±0.03) and Δm212=7.6±0.2×10^-5eV2. The B8 neutrino flux obtained from global solar neutrino experiments is 5.3±0.2(stat+sys) ×106cm^-2s^-1, while the B8 flux becomes 5.1±0.1(stat+sys)×106cm^-2s^-1 by adding KamLAND results. In a three-flavor analysis combining all solar neutrino experiments, the upper limit of ^sin2θ₁₃ is 0.060 at 95% C.L.. After combination with KamLAND results, the upper limit of ^sin2θ₁₃ is found to be 0.059 at 95% C.L.

本文言語	English
論文番号	052010
ジャーナル	Physical Review D - Particles, Fields, Gravitation and Cosmology
巻	83
号	5
DOI	https://doi.org/10.1103/PhysRevD.83.052010
出版ステータス	Published - 3月 24 2011

ASJC Scopus subject areas

核物理学および高エネルギー物理学
物理学および天文学（その他）

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10.1103/PhysRevD.83.052010

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引用スタイル

Abe, K., Hayato, Y., Iida, T., Ikeda, M., Ishihara, C., Iyogi, K., Kameda, J., Kobayashi, K., Koshio, Y., Kozuma, Y., Miura, M., Moriyama, S., Nakahata, M., Nakayama, S., Obayashi, Y., Ogawa, H., Sekiya, H., Shiozawa, M., Suzuki, Y., ... Wilkes, R. J. (2011). Solar neutrino results in Super-Kamiokande-III. Physical Review D - Particles, Fields, Gravitation and Cosmology, 83(5), [052010]. https://doi.org/10.1103/PhysRevD.83.052010

Abe, K, Hayato, Y, Iida, T, Ikeda, M, Ishihara, C, Iyogi, K, Kameda, J, Kobayashi, K, Koshio, Y, Kozuma, Y, Miura, M, Moriyama, S, Nakahata, M, Nakayama, S, Obayashi, Y, Ogawa, H, Sekiya, H, Shiozawa, M, Suzuki, Y, Takeda, A, Takenaga, Y, Ueno, K, Ueshima, K, Watanabe, H, Yamada, S, Yokozawa, T, Hazama, S, Kaji, H, Kajita, T, Kaneyuki, K, McLachlan, T, Okumura, K, Shimizu, Y, Tanimoto, N, Vagins, MR, Labarga, L, Magro, LM, Dufour, F, Kearns, E, Litos, M, Raaf, JL, Stone, JL, Sulak, LR, Wang, W, Goldhaber, M, Bays, K, Casper, D, Cravens, JP, Kropp, WR, Mine, S, Regis, C, Renshaw, A, Smy, MB, Sobel, HW, Ganezer, KS, Hill, J, Keig, WE, Jang, JS, Kim, JY, Lim, IT, Albert, J, Wendell, R, Wongjirad, T, Scholberg, K, Walter, CW, Ishizuka, T, Tasaka, S, Learned, JG, Matsuno, S, Watanabe, Y, Hasegawa, T, Ishida, T, Ishii, T, Kobayashi, T, Nakadaira, T, Nakamura, K, Nishikawa, K, Nishino, H, Oyama, Y, Sakashita, K, Sekiguchi, T, Tsukamoto, T, Suzuki, AT, Takeuchi, Y, Minamino, A, Nakaya, T, Fukuda, Y, Itow, Y, Mitsuka, G, Tanaka, T, Jung, CK, Lopez, G, McGrew, C, Terri, R, Yanagisawa, C, Tamura, N, Ishino, H, Kibayashi, A, Mino, S, Mori, T, Sakuda, M, Toyota, H, Kuno, Y, Yoshida, M, Kim, SB, Yang, BS, Ishizuka, T, Okazawa, H, Choi, Y, Nishijima, K, Yokosawa, Y, Koshiba, M, Totsuka, Y, Yokoyama, M, Chen, S, Heng, Y, Yang, Z, Zhang, H, Kielczewska, D, Mijakowski, P, Connolly, K, Dziomba, M, Thrane, E & Wilkes, RJ 2011, 'Solar neutrino results in Super-Kamiokande-III', Physical Review D - Particles, Fields, Gravitation and Cosmology, vol. 83, no. 5, 052010. https://doi.org/10.1103/PhysRevD.83.052010

@article{d79570135d5f42d4ac81d3d1654a526f,

title = "Solar neutrino results in Super-Kamiokande-III",

abstract = "The results of the third phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first and second phase results. With improved detector calibrations, a full detector simulation, and improved analysis methods, the systematic uncertainty on the total neutrino flux is estimated to be ±2.1%, which is about two thirds of the systematic uncertainty for the first phase of Super-Kamiokande. The observed B8 solar flux in the 5.0 to 20 MeV total electron energy region is 2.32±0.04(stat) ±0.05(sys)×106cm-2sec-1 under the assumption of pure electron-flavor content, in agreement with previous measurements. A combined oscillation analysis is carried out using SK-I, II, and III data, and the results are also combined with the results of other solar neutrino experiments. The best-fit oscillation parameters are obtained to be sin2θ12=0.30-0.01+0.02(tan2θ 12=0.42-0.02+0.04) and Δm212=6.2-1.9+1.1×10 -5eV2. Combined with KamLAND results, the best-fit oscillation parameters are found to be sin2θ12=0.31±0. 01(tan2θ12=0.44±0.03) and Δm212=7.6±0.2×10-5eV2. The B8 neutrino flux obtained from global solar neutrino experiments is 5.3±0.2(stat+sys) ×106cm-2s-1, while the B8 flux becomes 5.1±0.1(stat+sys)×106cm-2s-1 by adding KamLAND results. In a three-flavor analysis combining all solar neutrino experiments, the upper limit of sin2θ13 is 0.060 at 95% C.L.. After combination with KamLAND results, the upper limit of sin2θ13 is found to be 0.059 at 95% C.L.",

author = "K. Abe and Y. Hayato and T. Iida and M. Ikeda and C. Ishihara and K. Iyogi and J. Kameda and K. Kobayashi and Y. Koshio and Y. Kozuma and M. Miura and S. Moriyama and M. Nakahata and S. Nakayama and Y. Obayashi and H. Ogawa and H. Sekiya and M. Shiozawa and Y. Suzuki and A. Takeda and Y. Takenaga and K. Ueno and K. Ueshima and H. Watanabe and S. Yamada and T. Yokozawa and S. Hazama and H. Kaji and T. Kajita and K. Kaneyuki and T. McLachlan and K. Okumura and Y. Shimizu and N. Tanimoto and Vagins, {M. R.} and L. Labarga and Magro, {L. M.} and F. Dufour and E. Kearns and M. Litos and Raaf, {J. L.} and Stone, {J. L.} and Sulak, {L. R.} and W. Wang and M. Goldhaber and K. Bays and D. Casper and Cravens, {J. P.} and Kropp, {W. R.} and S. Mine and C. Regis and A. Renshaw and Smy, {M. B.} and Sobel, {H. W.} and Ganezer, {K. S.} and J. Hill and Keig, {W. E.} and Jang, {J. S.} and Kim, {J. Y.} and Lim, {I. T.} and J. Albert and R. Wendell and T. Wongjirad and K. Scholberg and Walter, {C. W.} and T. Ishizuka and S. Tasaka and Learned, {J. G.} and S. Matsuno and Y. Watanabe and T. Hasegawa and T. Ishida and T. Ishii and T. Kobayashi and T. Nakadaira and K. Nakamura and K. Nishikawa and H. Nishino and Y. Oyama and K. Sakashita and T. Sekiguchi and T. Tsukamoto and Suzuki, {A. T.} and Y. Takeuchi and A. Minamino and T. Nakaya and Y. Fukuda and Y. Itow and G. Mitsuka and T. Tanaka and Jung, {C. K.} and G. Lopez and C. McGrew and R. Terri and C. Yanagisawa and N. Tamura and H. Ishino and A. Kibayashi and S. Mino and T. Mori and Makoto Sakuda and H. Toyota and Y. Kuno and M. Yoshida and Kim, {S. B.} and Yang, {B. S.} and T. Ishizuka and H. Okazawa and Y. Choi and K. Nishijima and Y. Yokosawa and M. Koshiba and Y. Totsuka and M. Yokoyama and S. Chen and Y. Heng and Z. Yang and H. Zhang and D. Kielczewska and P. Mijakowski and K. Connolly and M. Dziomba and E. Thrane and Wilkes, {R. J.}",

year = "2011",

month = mar,

day = "24",

doi = "10.1103/PhysRevD.83.052010",

language = "English",

volume = "83",

journal = "Physical Review D",

issn = "0556-2821",

number = "5",

}

TY - JOUR

T1 - Solar neutrino results in Super-Kamiokande-III

AU - Abe, K.

AU - Hayato, Y.

AU - Iida, T.

AU - Ikeda, M.

AU - Ishihara, C.

AU - Iyogi, K.

AU - Kameda, J.

AU - Kobayashi, K.

AU - Koshio, Y.

AU - Kozuma, Y.

AU - Miura, M.

AU - Moriyama, S.

AU - Nakahata, M.

AU - Nakayama, S.

AU - Obayashi, Y.

AU - Ogawa, H.

AU - Sekiya, H.

AU - Shiozawa, M.

AU - Suzuki, Y.

AU - Takeda, A.

AU - Takenaga, Y.

AU - Ueno, K.

AU - Ueshima, K.

AU - Watanabe, H.

AU - Yamada, S.

AU - Yokozawa, T.

AU - Hazama, S.

AU - Kaji, H.

AU - Kajita, T.

AU - Kaneyuki, K.

AU - McLachlan, T.

AU - Okumura, K.

AU - Shimizu, Y.

AU - Tanimoto, N.

AU - Vagins, M. R.

AU - Labarga, L.

AU - Magro, L. M.

AU - Dufour, F.

AU - Kearns, E.

AU - Litos, M.

AU - Raaf, J. L.

AU - Stone, J. L.

AU - Sulak, L. R.

AU - Wang, W.

AU - Goldhaber, M.

AU - Bays, K.

AU - Casper, D.

AU - Cravens, J. P.

AU - Kropp, W. R.

AU - Mine, S.

AU - Regis, C.

AU - Renshaw, A.

AU - Smy, M. B.

AU - Sobel, H. W.

AU - Ganezer, K. S.

AU - Hill, J.

AU - Keig, W. E.

AU - Jang, J. S.

AU - Kim, J. Y.

AU - Lim, I. T.

AU - Albert, J.

AU - Wendell, R.

AU - Wongjirad, T.

AU - Scholberg, K.

AU - Walter, C. W.

AU - Ishizuka, T.

AU - Tasaka, S.

AU - Learned, J. G.

AU - Matsuno, S.

AU - Watanabe, Y.

AU - Hasegawa, T.

AU - Ishida, T.

AU - Ishii, T.

AU - Kobayashi, T.

AU - Nakadaira, T.

AU - Nakamura, K.

AU - Nishikawa, K.

AU - Nishino, H.

AU - Oyama, Y.

AU - Sakashita, K.

AU - Sekiguchi, T.

AU - Tsukamoto, T.

AU - Suzuki, A. T.

AU - Takeuchi, Y.

AU - Minamino, A.

AU - Nakaya, T.

AU - Fukuda, Y.

AU - Itow, Y.

AU - Mitsuka, G.

AU - Tanaka, T.

AU - Jung, C. K.

AU - Lopez, G.

AU - McGrew, C.

AU - Terri, R.

AU - Yanagisawa, C.

AU - Tamura, N.

AU - Ishino, H.

AU - Kibayashi, A.

AU - Mino, S.

AU - Mori, T.

AU - Sakuda, Makoto

AU - Toyota, H.

AU - Kuno, Y.

AU - Yoshida, M.

AU - Kim, S. B.

AU - Yang, B. S.

AU - Ishizuka, T.

AU - Okazawa, H.

AU - Choi, Y.

AU - Nishijima, K.

AU - Yokosawa, Y.

AU - Koshiba, M.

AU - Totsuka, Y.

AU - Yokoyama, M.

AU - Chen, S.

AU - Heng, Y.

AU - Yang, Z.

AU - Zhang, H.

AU - Kielczewska, D.

AU - Mijakowski, P.

AU - Connolly, K.

AU - Dziomba, M.

AU - Thrane, E.

AU - Wilkes, R. J.

PY - 2011/3/24

Y1 - 2011/3/24

N2 - The results of the third phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first and second phase results. With improved detector calibrations, a full detector simulation, and improved analysis methods, the systematic uncertainty on the total neutrino flux is estimated to be ±2.1%, which is about two thirds of the systematic uncertainty for the first phase of Super-Kamiokande. The observed B8 solar flux in the 5.0 to 20 MeV total electron energy region is 2.32±0.04(stat) ±0.05(sys)×106cm-2sec-1 under the assumption of pure electron-flavor content, in agreement with previous measurements. A combined oscillation analysis is carried out using SK-I, II, and III data, and the results are also combined with the results of other solar neutrino experiments. The best-fit oscillation parameters are obtained to be sin2θ12=0.30-0.01+0.02(tan2θ 12=0.42-0.02+0.04) and Δm212=6.2-1.9+1.1×10 -5eV2. Combined with KamLAND results, the best-fit oscillation parameters are found to be sin2θ12=0.31±0. 01(tan2θ12=0.44±0.03) and Δm212=7.6±0.2×10-5eV2. The B8 neutrino flux obtained from global solar neutrino experiments is 5.3±0.2(stat+sys) ×106cm-2s-1, while the B8 flux becomes 5.1±0.1(stat+sys)×106cm-2s-1 by adding KamLAND results. In a three-flavor analysis combining all solar neutrino experiments, the upper limit of sin2θ13 is 0.060 at 95% C.L.. After combination with KamLAND results, the upper limit of sin2θ13 is found to be 0.059 at 95% C.L.

AB - The results of the third phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first and second phase results. With improved detector calibrations, a full detector simulation, and improved analysis methods, the systematic uncertainty on the total neutrino flux is estimated to be ±2.1%, which is about two thirds of the systematic uncertainty for the first phase of Super-Kamiokande. The observed B8 solar flux in the 5.0 to 20 MeV total electron energy region is 2.32±0.04(stat) ±0.05(sys)×106cm-2sec-1 under the assumption of pure electron-flavor content, in agreement with previous measurements. A combined oscillation analysis is carried out using SK-I, II, and III data, and the results are also combined with the results of other solar neutrino experiments. The best-fit oscillation parameters are obtained to be sin2θ12=0.30-0.01+0.02(tan2θ 12=0.42-0.02+0.04) and Δm212=6.2-1.9+1.1×10 -5eV2. Combined with KamLAND results, the best-fit oscillation parameters are found to be sin2θ12=0.31±0. 01(tan2θ12=0.44±0.03) and Δm212=7.6±0.2×10-5eV2. The B8 neutrino flux obtained from global solar neutrino experiments is 5.3±0.2(stat+sys) ×106cm-2s-1, while the B8 flux becomes 5.1±0.1(stat+sys)×106cm-2s-1 by adding KamLAND results. In a three-flavor analysis combining all solar neutrino experiments, the upper limit of sin2θ13 is 0.060 at 95% C.L.. After combination with KamLAND results, the upper limit of sin2θ13 is found to be 0.059 at 95% C.L.

UR - http://www.scopus.com/inward/record.url?scp=79960768333&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=79960768333&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.83.052010

DO - 10.1103/PhysRevD.83.052010

M3 - Article

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SN - 0556-2821

VL - 83

JO - Physical Review D

JF - Physical Review D

IS - 5

M1 - 052010

ER -

Solar neutrino results in Super-Kamiokande-III

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