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Y. Kuno

Bio: Y. Kuno is an academic researcher from Osaka University. The author has contributed to research in topics: Neutrino & Muon. The author has an hindex of 44, co-authored 158 publications receiving 7659 citations. Previous affiliations of Y. Kuno include Illinois Institute of Technology.


Papers
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Journal ArticleDOI
Y. Ashie1, J. Hosaka1, K. Ishihara1, Yoshitaka Itow1, J. Kameda1, Yusuke Koshio1, A. Minamino1, C. Mitsuda1, M. Miura1, Shigetaka Moriyama1, Masayuki Nakahata1, Toshio Namba1, R. Nambu1, Y. Obayashi1, Masato Shiozawa1, Yoshihiro Suzuki1, Y. Takeuchi1, K. Taki1, Shinya Yamada1, M. Ishitsuka1, Takaaki Kajita1, K. Kaneyuki1, Shoei Nakayama1, A. Okada1, Ko Okumura1, C. Saji1, Y. Takenaga1, S. Clark2, Shantanu Desai2, E. Kearns2, S. Likhoded2, J. L. Stone2, L. R. Sulak2, W. Wang2, M. Goldhaber3, David William Casper4, J. P. Cravens4, W. Gajewski4, W. R. Kropp4, D. W. Liu4, S. Mine4, Michael B. Smy4, Henry W. Sobel4, C. W. Sterner4, Mark R. Vagins4, K. S. Ganezer5, John Hill5, W. E. Keig5, J. S. Jang6, J. Y. Kim6, I. T. Lim6, Kate Scholberg7, C. W. Walter7, R. W. Ellsworth8, S. Tasaka9, G. Guillian, A. Kibayashi, John G. Learned, S. Matsuno, D. Takemori, M. D. Messier10, Y. Hayato, A. K. Ichikawa, T. Ishida, T. Ishii, T. Iwashita, Takashi Kobayashi, T. Maruyama11, Koji Nakamura, K. Nitta, Yuichi Oyama, Makoto Sakuda12, Y. Totsuka, Atsumu Suzuki13, Masaya Hasegawa14, K. Hayashi14, I. Kato14, H. Maesaka14, Taichi Morita14, Tsuyoshi Nakaya14, K. Nishikawa14, T. Sasaki14, S. Ueda14, Shoji Yamamoto14, Todd Haines15, Todd Haines4, S. Dazeley16, S. Hatakeyama16, R. Svoboda16, E. Blaufuss17, J. A. Goodman17, G. W. Sullivan17, D. Turcan17, Alec Habig18, Y. Fukuda19, C. K. Jung20, T. Kato20, Katsuhiro Kobayashi20, Magdalena Malek20, C. Mauger20, C. McGrew20, A. Sarrat20, E. Sharkey20, C. Yanagisawa20, T. Toshito21, Kazumasa Miyano22, N. Tamura22, J. Ishii23, Y. Kuno23, Minoru Yoshida23, S. B. Kim24, J. Yoo24, H. Okazawa, T. Ishizuka25, Y. Choi26, H. Seo26, Y. Gando27, Takehisa Hasegawa27, Kunio Inoue27, J. Shirai27, A. Suzuki27, Masatoshi Koshiba1, Y. Nakajima28, Kyoshi Nishijima28, T. Harada29, Hirokazu Ishino29, Y. Watanabe29, D. Kielczewska30, D. Kielczewska4, J. Zalipska30, H. G. Berns31, R. Gran31, K. K. Shiraishi31, A. L. Stachyra31, K. Washburn31, R. J. Wilkes31 
TL;DR: In this article, a combined analysis of fully-contained, partially-contained and upward-going muon atmospheric neutrino data from a 1489 d exposure of the Super-Kamiokande detector is presented.
Abstract: We present a combined analysis of fully-contained, partially-contained and upward-going muon atmospheric neutrino data from a 1489 d exposure of the Super-Kamiokande detector. The data samples span roughly five decades in neutrino energy, from 100 MeV to 10 TeV. A detailed Monte Carlo comparison is described and presented. The data is fit to the Monte Carlo expectation, and is found to be consistent with neutrino oscillations of {nu}{sub {mu}}{r_reversible}{nu}{sub {tau}} with sin{sup 2}2{theta}>0.92 and 1.5x10{sup -3}<{delta}m{sup 2}<3.4x10{sup -3} eV{sup 2} at 90% confidence level.

701 citations

Journal ArticleDOI
Y. Ashie1, J. Hosaka1, K. Ishihara1, Yoshitaka Itow1, J. Kameda1, Yusuke Koshio1, A. Minamino1, C. Mitsuda1, M. Miura1, Shigetaka Moriyama1, Masayuki Nakahata1, Toshio Namba1, R. Nambu1, Y. Obayashi1, Masato Shiozawa1, Yasunari Suzuki1, Y. Takeuchi1, K. Taki1, Shinya Yamada1, Masaki Ishitsuka1, Takaaki Kajita1, K. Kaneyuki1, Shoei Nakayama1, A. Okada1, Ko Okumura1, T. Ooyabu1, C. Saji1, Y. Takenaga1, Shantanu Desai2, E. Kearns2, S. Likhoded2, J. L. Stone2, L. R. Sulak2, C. W. Walter2, W. Wang2, M. Goldhaber3, David William Casper4, J. P. Cravens4, W. Gajewski4, W. R. Kropp4, D. W. Liu4, S. Mine4, Michael B. Smy4, H. W. Sobel4, C. W. Sterner4, Mark R. Vagins4, K. S. Ganezer5, John Hill5, W. E. Keig5, J. S. Jang6, J. Y. Kim6, I. T. Lim6, R. W. Ellsworth7, S. Tasaka8, G. Guillian, A. Kibayashi, John G. Learned, S. Matsuno, D. Takemori, M. D. Messier9, Y. Hayato, A. K. Ichikawa, T. Ishida, T. Ishii, T. Iwashita, T. Kobayashi, Tomoyuki Maruyama, K. Nakamura, K. Nitta, Yuichi Oyama, Makoto Sakuda, Y. Totsuka, Atsumu Suzuki10, Masaya Hasegawa11, K. Hayashi11, T. Inagaki11, I. Kato11, H. Maesaka11, Taichi Morita11, Tsuyoshi Nakaya11, K. Nishikawa11, T. Sasaki11, S. Ueda11, Shoji Yamamoto11, Todd Haines4, Todd Haines12, S. Dazeley13, S. Hatakeyama13, R. Svoboda13, E. Blaufuss14, J. A. Goodman14, G. W. Sullivan14, D. Turcan14, Kate Scholberg15, Alec Habig16, Y. Fukuda17, C. K. Jung18, T. Kato18, Katsuhiro Kobayashi18, Magdalena Malek18, C. Mauger18, C. McGrew18, A. Sarrat18, E. Sharkey18, C. Yanagisawa18, T. Toshito19, Kazumasa Miyano20, N. Tamura20, J. Ishii21, Y. Kuno21, Y. Nagashima21, M. Takita21, Minoru Yoshida21, S. B. Kim22, J. Yoo22, H. Okazawa, T. Ishizuka23, Y. Choi24, H. Seo24, Y. Gando25, Takehisa Hasegawa25, Kunio Inoue25, J. Shirai25, A. Suzuki25, Masatoshi Koshiba1, Y. Nakajima26, Kyoshi Nishijima26, T. Harada27, Hirokazu Ishino27, R. Nishimura27, Y. Watanabe27, D. Kielczewska28, D. Kielczewska4, J. Zalipska28, H. G. Berns29, R. Gran29, K. K. Shiraishi29, A. L. Stachyra29, K. Washburn29, R. J. Wilkes29 
TL;DR: A dip in the L/E distribution was observed in the data, as predicted from the sinusoidal flavor transition probability of neutrino oscillation, which constrained nu(micro)<-->nu(tau) neutrinos oscillation parameters.
Abstract: Muon neutrino disappearance probability as a function of neutrino flight length $L$ over neutrino energy $E$ was studied. A dip in the $L/E$ distribution was observed in the data, as predicted from the sinusoidal flavor transition probability of neutrino oscillation. The observed $L/E$ distribution constrained ${\ensuremath{ u}}_{\ensuremath{\mu}}\ensuremath{\leftrightarrow}{\ensuremath{ u}}_{\ensuremath{\tau}}$ neutrino oscillation parameters; $1.9\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}l\ensuremath{\Delta}{m}^{2}l3.0\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}\text{ }\text{ }{\mathrm{e}\mathrm{V}}^{2}$ and ${sin }^{2}2\ensuremath{\theta}g0.90$ at 90% confidence level.

522 citations

Journal ArticleDOI
J. P. Cravens1, K. Abe2, T. Iida2, K. Ishihara2  +147 moreInstitutions (34)
TL;DR: The results of the second phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first phase in this paper, showing no evidence of systematic tendencies between the first and second phases.
Abstract: The results of the second phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first phase. The solar neutrino flux spectrum and time variation as well as oscillation results are statistically consistent with the first phase and do not show spectral distortion. The time-dependent flux measurement of the combined first and second phases coincides with the full period of solar cycle 23 and shows no correlation with solar activity. The measured {sup 8}B total flux is (2.38{+-}0.05(stat.){sub -0.15}{sup +0.16}(sys.))x10{sup 6} cm{sup -2} s{sup -1} and the day-night difference is found to be (-6.3{+-}4.2(stat.){+-}3.7(sys.))%. There is no evidence of systematic tendencies between the first and second phases.

439 citations

Journal ArticleDOI
K. Abe1, Y. Hayato1, T. Iida1, M. Ikeda1, M. Ikeda2, C. Ishihara1, K. Iyogi1, J. Kameda1, Ken-ichiro Kobayashi1, Yusuke Koshio1, Y. Kozuma1, M. Miura1, S. Moriyama1, Masayuki Nakahata1, S. Nakayama1, Y. Obayashi1, H. Ogawa1, Hiroyuki Sekiya1, Masato Shiozawa1, Yasunari Suzuki1, Atsushi Takeda1, Y. Takenaga1, Koh Ueno1, K. Ueshima, Hiroshi Watanabe, S. Yamada1, T. Yokozawa1, S. Hazama1, H. Kaji1, Takaaki Kajita1, K. Kaneyuki1, T. McLachlan1, Ko Okumura1, Y. Shimizu1, N. Tanimoto1, M. R. Vagins1, M. R. Vagins3, L. Labarga4, L. M. Magro4, Frédéric Dufour5, E. Kearns5, E. Kearns1, Michael Litos5, J. L. Raaf5, J. L. Stone5, J. L. Stone1, L. R. Sulak5, W. Wang5, W. Wang6, M. Goldhaber7, K. Bays3, David William Casper3, J. P. Cravens3, W. R. Kropp3, S. Mine3, C. Regis3, A. L. Renshaw3, M. B. Smy1, M. B. Smy3, H. W. Sobel1, H. W. Sobel3, K. S. Ganezer8, John Hill8, W. E. Keig8, J. S. Jang9, J. Y. Kim9, I. T. Lim9, Justin Albert10, R. A. Wendell10, T. Wongjirad10, Kate Scholberg10, Kate Scholberg1, C. W. Walter1, C. W. Walter10, T. Ishizuka11, S. Tasaka12, John G. Learned, S. Matsuno, Y. Watanabe13, Takehisa Hasegawa, T. Ishida, T. Ishii, T. Kobayashi, T. Nakadaira, Koji Nakamura1, K. Nishikawa, H. Nishino, Yuichi Oyama, Ken Sakashita, T. Sekiguchi, T. Tsukamoto, A. T. Suzuki14, Y. Takeuchi14, Y. Takeuchi1, A. Minamino2, Tsuyoshi Nakaya2, Tsuyoshi Nakaya1, Y. Fukuda15, Yoshitaka Itow16, G. Mitsuka16, T. Tanaka16, C. K. Jung17, G. D. Lopez17, C. McGrew17, R. Terri17, C. Yanagisawa17, N. Tamura18, Hirokazu Ishino19, A. Kibayashi19, S. Mino19, Takaaki Mori19, Makoto Sakuda19, H. Toyota19, Y. Kuno20, Minoru Yoshida20, S. B. Kim21, B. S. Yang21, H. Okazawa22, Y. Choi23, K. Nishijima24, Y. Yokosawa24, M. Koshiba1, Y. Totsuka1, Masashi Yokoyama1, Song Chen25, Y. Heng25, Zishuo Yang25, Haoxiong Zhang25, D. Kielczewska26, P. Mijakowski26, K. Connolly27, M. Dziomba27, E. Thrane28, E. Thrane27, R. J. Wilkes27 
TL;DR: The results of the third phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first and second phase results in this article, where improved detector calibrations, a full detector simulation, and improved analysis methods are estimated to be approximately 2.1%, which is about two thirds of the systematic uncertainty for the first phase.
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 $\ifmmode\pm\else\textpm\fi{}2.1%$, which is about two thirds of the systematic uncertainty for the first phase of Super-Kamiokande. The observed $^{8}\mathrm{B}$ solar flux in the 5.0 to 20 MeV total electron energy region is $2.32\ifmmode\pm\else\textpm\fi{}0.04(\mathrm{stat})\ifmmode\pm\else\textpm\fi{}0.05(\mathrm{sys})\ifmmode\times\else\texttimes\fi{}{10}^{6}\text{ }\text{ }{\mathrm{cm}}^{\ensuremath{-}2}\text{ }{\mathrm{sec}}^{\ensuremath{-}1}$ 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 ${sin }^{2}{\ensuremath{\theta}}_{12}={0.30}_{\ensuremath{-}0.01}^{+0.02}({tan }^{2}{\ensuremath{\theta}}_{12}={0.42}_{\ensuremath{-}0.02}^{+0.04})$ and $\ensuremath{\Delta}{m}_{21}^{2}={6.2}_{\ensuremath{-}1.9}^{+1.1}\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}5}\text{ }\text{ }{\mathrm{eV}}^{2}$. Combined with KamLAND results, the best-fit oscillation parameters are found to be ${sin }^{2}{\ensuremath{\theta}}_{12}=0.31\ifmmode\pm\else\textpm\fi{}0.01({tan }^{2}{\ensuremath{\theta}}_{12}=0.44\ifmmode\pm\else\textpm\fi{}0.03)$ and $\ensuremath{\Delta}{m}_{21}^{2}=7.6\ifmmode\pm\else\textpm\fi{}0.2\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}5}\text{ }\text{ }{\mathrm{eV}}^{2}$. The $^{8}\mathrm{B}$ neutrino flux obtained from global solar neutrino experiments is $5.3\ifmmode\pm\else\textpm\fi{}0.2(\mathrm{stat}+\mathrm{sys})\ifmmode\times\else\texttimes\fi{}{10}^{6}\text{ }\text{ }{\mathrm{cm}}^{\ensuremath{-}2}\text{ }{\mathrm{s}}^{\ensuremath{-}1}$, while the $^{8}\mathrm{B}$ flux becomes $5.1\ifmmode\pm\else\textpm\fi{}0.1(\mathrm{stat}+\mathrm{sys})\ifmmode\times\else\texttimes\fi{}{10}^{6}\text{ }\text{ }{\mathrm{cm}}^{\ensuremath{-}2}\text{ }{\mathrm{s}}^{\ensuremath{-}1}$ by adding KamLAND results. In a three-flavor analysis combining all solar neutrino experiments, the upper limit of ${sin }^{2}{\ensuremath{\theta}}_{13}$ is 0.060 at 95% C.L.. After combination with KamLAND results, the upper limit of ${sin }^{2}{\ensuremath{\theta}}_{13}$ is found to be 0.059 at 95% C.L.

404 citations

Journal ArticleDOI
K. Choi1, K. Abe2, K. Abe3, Yoshinori Haga3, Y. Hayato2, Y. Hayato3, K. Iyogi3, J. Kameda2, J. Kameda3, Yasuhiro Kishimoto2, Yasuhiro Kishimoto3, M. Miura3, M. Miura2, S. Moriyama3, S. Moriyama2, Masayuki Nakahata3, Masayuki Nakahata2, Yuuki Nakano3, S. Nakayama3, S. Nakayama2, Hiroyuki Sekiya2, Hiroyuki Sekiya3, Masato Shiozawa3, Masato Shiozawa2, Yasunari Suzuki3, Yasunari Suzuki2, Atsushi Takeda2, Atsushi Takeda3, T. Tomura3, T. Tomura2, R. A. Wendell3, R. A. Wendell2, T. J. Irvine3, Takaaki Kajita2, Takaaki Kajita3, I. Kametani3, K. Kaneyuki2, K. Kaneyuki3, K. P. Lee3, Y. Nishimura3, Kimihiro Okumura3, Kimihiro Okumura2, T. McLachlan3, L. Labarga, E. Kearns4, E. Kearns2, J. L. Raaf4, J. L. Stone2, J. L. Stone4, L. R. Sulak4, S. Berkman5, H.A. Tanaka5, S. Tobayama5, M. Goldhaber6, G. Carminati7, W. R. Kropp7, S. Mine7, A. L. Renshaw7, M. B. Smy7, M. B. Smy2, H. W. Sobel2, H. W. Sobel7, K. S. Ganezer8, John Hill8, N. Hong9, J. Y. Kim9, I. T. Lim9, T. Akiri10, A. Himmel10, Kate Scholberg2, Kate Scholberg10, C. W. Walter10, C. W. Walter2, T. Wongjirad10, T. Ishizuka11, Shigeki Tasaka12, J. S. Jang13, J. G. Learned14, S. Matsuno14, S. N. Smith14, T. Hasegawa15, T. Ishida15, T. Ishii15, T. Kobayashi15, T. Nakadaira15, K. Nakamura15, K. Nakamura2, Yuichi Oyama15, K. Sakashita15, T. Sekiguchi15, T. Tsukamoto15, A. T. Suzuki16, Y. Takeuchi16, C. Bronner17, Seiko Hirota17, K. Huang17, K. Ieki17, M. Ikeda17, T. Kikawa17, A. Minamino17, Tsuyoshi Nakaya2, Tsuyoshi Nakaya17, Kazuhiro Suzuki17, Susumu Takahashi17, Y. Fukuda18, Yoshitaka Itow1, G. Mitsuka1, P. Mijakowski, Joshua Hignight19, J. Imber19, C. K. Jung19, C. Yanagisawa19, Hirokazu Ishino20, A. Kibayashi20, Yusuke Koshio20, Takaaki Mori20, Makoto Sakuda20, T. Yano20, Y. Kuno21, R. Tacik22, R. Tacik23, S. B. Kim24, H. Okazawa25, Y. Choi26, K. Nishijima27, M. Koshiba3, Y. Totsuka3, Masashi Yokoyama2, Masashi Yokoyama3, K. Martens2, Ll. Marti2, M. R. Vagins7, M. R. Vagins2, J. F. Martin28, P. de Perio28, A. Konaka23, M. J. Wilking23, Song Chen29, Yejin Zhang29, R. J. Wilkes30 
TL;DR: In this article, the authors considered neutrino events with interaction vertices in the SK detector in addition to upward-going muons produced in the surrounding rock and found no significant excess over expected atmospheric-neutrino background and interpreted the result in terms of upper limits on WIMP-nucleon elastic scattering cross sections under different assumptions about the annihilation channel.
Abstract: Super-Kamiokande (SK) can search for weakly interacting massive particles (WIMPs) by detecting neutrinos produced from WIMP annihilations occurring inside the Sun. In this analysis, we include neutrino events with interaction vertices in the detector in addition to upward-going muons produced in the surrounding rock. Compared to the previous result, which used the upward-going muons only, the signal acceptances for light (few-GeV/c^{2}-200-GeV/c^{2}) WIMPs are significantly increased. We fit 3903 days of SK data to search for the contribution of neutrinos from WIMP annihilation in the Sun. We found no significant excess over expected atmospheric-neutrino background and the result is interpreted in terms of upper limits on WIMP-nucleon elastic scattering cross sections under different assumptions about the annihilation channel. We set the current best limits on the spin-dependent WIMP-proton cross section for WIMP masses below 200 GeV/c^{2} (at 10 GeV/c^{2}, 1.49×10^{-39} cm^{2} for χχ→bb[over ¯] and 1.31×10^{-40} cm^{2} for χχ→τ^{+}τ^{-} annihilation channels), also ruling out some fraction of WIMP candidates with spin-independent coupling in the few-GeV/c^{2} mass range.

297 citations


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TL;DR: In this paper, the authors review the present status of QCD corrections to weak decays beyond the leading-logarithmic approximation, including particle-antiparticle mixing and rare and $\mathrm{CP}$-violating decays.
Abstract: We review the present status of QCD corrections to weak decays beyond the leading-logarithmic approximation, including particle-antiparticle mixing and rare and $\mathrm{CP}$-violating decays. After presenting the basic formalism for these calculations we discuss in detail the effective Hamiltonians of all decays for which the next-to-leading-order corrections are known. Subsequently, we present the phenomenological implications of these calculations. The values of various parameters are updated, in particular the mass of the newly discovered top quark. One of the central issues in this review are the theoretical uncertainties related to renormalization-scale ambiguities, which are substantially reduced by including next-to-leading-order corrections. The impact of this theoretical improvement on the determination of the Cabibbo-Kobayashi-Maskawa matrix is then illustrated. [S0034-6861(96)00304-2]

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TL;DR: In this paper, the authors employed a matrix-based power spectrum estimation method using pseudo-Karhunen-Loeve eigenmodes, producing uncorrelated minimum-variance measurements in 20 k-bands of both the clustering power and its anisotropy due to redshift-space distortions.
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