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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 | 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 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 | Services: | Forum | Review | PDF | Favorites |
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