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Search for Supernova Neutrino Bursts at Super-Kamiokande

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M. Ikeda1, A. Takeda2, Y. Fukuda3, M. R. Vagins4, K. Abe2, T. Iida2, K. Ishihara2, J. Kameda2, Y. Koshio2, A. Minamino2, C. Mitsuda2, M. Miura2, S. Moriyama2, M. Nakahata2, Y. Obayashi2, H. Ogawa2, H. Sekiya2, M. Shiozawa2, Y. Suzuki2, Y. Takeuchi2, K. Ueshima2, H. Watanabe2, S. Yamada2, I. Higuchi5, C. Ishihara5, M. Ishitsuka5, T. Kajita5, K. Kaneyuki5, G. Mitsuka5, S. Nakayama5, H. Nishino5, K. Okumura5, C. Saji5, Y. Takenaga5, S. Clark6, S. Desai6,7, F. Dufour6, E. Kearns6, S. Likhoded6, M. Litos6, J. L. Raaf6, J. L. Stone6, L. R. Sulak6, W. Wang6, M. Goldhaber8, D. Casper4, J. P. Cravens4, J. Dunmore4, W. R. Kropp4, D. W. Liu4, S. Mine4, C. Regis4, M. B. Smy4, H. W. Sobel4, K. S. Ganezer9, J. Hill9, W. E. Keig9, J. S. Jang10, J. Y. Kim10, I. T. Lim10, K. Scholberg11, N. Tanimoto11, C. W. Walter11, R. Wendell11, R. W. Ellsworth12, S. Tasaka13, G. Guillian14, J. G. Learned14, S. Matsuno14, M. D. Messier15, Y. Hayato2,16, A. K. Ichikawa16, T. Ishida16, T. Ishii16, T. Iwashita16, T. Kobayashi16, T. Nakadaira16, K. Nakamura16, K. Nitta16, Y. Oyama16, Y. Totsuka2,16, A. T. Suzuki17, M. Hasegawa18, K. Hiraide18, H. Maesaka18, T. Nakaya18, K. Nishikawa16, T. Sasaki18, S. Yamamoto18, M. Yokoyama18, T. J. Haines4,19, S. Dazeley20, S. Hatakeyama20, R. Svoboda20, G. W. Sullivan21, D. Turcan21, A. Habig22, T. Sato3, Y. Itow23, T. Koike23, T. Tanaka23, C. K. Jung24, T. Kato24, K. Kobayashi24, M. Malek24, C. McGrew24, A. Sarrat24, R. Terri24, C. Yanagisawa24, N. Tamura25, Y. Idehara1, M. Sakuda1, M. Sugihara1, Y. Kuno26, M. Yoshida26, S. B. Kim27, B. S. Yang27, J. Yoo27, T. Ishizuka28, H. Okazawa29, Y. Choi30, H. K. Seo30, Y. Gando31, T. Hasegawa31, K. Inoue31, Y. Furuse32, H. Ishii32, K. Nishijima32, H. Ishino33, Y. Watanabe33, M. Koshiba34, S. Chen35, Z. Deng35, Y. Liu35, D. Kielczewska4,36, J. Zalipska36, H. Berns37, R. Gran22,37, K. K. Shiraishi37, A. Stachyra37, E. Thrane37, K. Washburn37 and R. J. Wilkes37 (The Super-Kamiokande Collaboration)

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We report the results of a search for neutrino bursts from supernova explosions using the Super-Kamiokande detector. Super-Kamiokande is sensitive to core-collapse supernova explosions via observation of their neutrino emissions. The expected number of events comprising such a burst is ~104, and the average energy of the neutrinos is in the range of a few tens of MeV for a core-collapse supernova explosion at a typical distance in our galaxy (10 kpc); this strong signal means that the detection efficiency anywhere within our galaxy and well past the Magellanic Clouds should be 100%. We examined a data set taken from 1996 May to 2001 July, and from 2002 December to 2005 October, corresponding to 2589.2 live days. However, there is no evidence of such a supernova explosion during the data-taking period. The 90% C.L. upper limit on the rate of core-collapse supernova explosions out to distances of 100 kpc is found to be 0.32 SN yr-1.


Subject headings

galaxies: individual (Milky Way, LMC, SMC); neutrinos; supernovae: general


Dates

Issue 1 (2007 November 1)

Received 2007 May 14, accepted for publication 2007 July 10



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