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29 March 2024
 
  » arxiv » 1010.0118

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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 ; M. 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 ;
Date 1 Oct 2010
AbstractThe 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 8B solar flux in the 5.0 to 20 MeV total electron energy region is 2.32+/-0.04 (stat.)+/-0.05 (sys.) *10^6 cm^-2sec^-1, 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 sin^2 { heta}12 = 0.30+0.02-0.01(tan^2 { heta}12 = 0.42+0.04 -0.02) and {Delta}m2_21 = 6.2+1.1-1.9 *10^-5eV^2. Combined with KamLAND results, the best-fit oscillation parameters are found to be sin^2 { heta}12 = 0.31+/-0.01(tan^2 { heta}12 = 0.44+/-0.03) and {Delta}m2_21 = 7.6?0.2*10^-5eV^2 . The 8B neutrino flux obtained from global solar neutrino experiments is 5.3+/-0.2(stat.+sys.)*10^6cm^-2s^-1, while the 8B flux becomes 5.1+/-0.1(stat.+sys.)*10^6cm^-2s^-1 by adding KamLAND result. In a three-flavor analysis combining all solar neutrino experiments, the upper limit of sin^2 { heta}13 is 0.060 at 95% C.L.. After combination with KamLAND results, the upper limit of sin^2 { heta}13 is found to be 0.059 at 95% C.L..
Source arXiv, 1010.0118
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