M. E. C. Swanson et al. 2006 ApJ 652 206 doi:10.1086/507983
M. E. C. Swanson1, K. Abe2, J. Hosaka2, T. Iida2, K. Ishihara2, J. Kameda2, Y. Koshio2, A. Minamino2, C. Mitsuda2, M. Miura2, S. Moriyama2, M. Nakahata2, Y. Obayashi2, H. Ogawa2, M. Shiozawa2, Y. Suzuki2, A. Takeda2, Y. Takeuchi2, K. Ueshima2, I. Higuchi3, C. Ishihara3, M. Ishitsuka3, T. Kajita3, K. Kaneyuki3, G. Mitsuka3, S. Nakayama3, H. Nishino3, A. Okada3, K. Okumura3, C. Saji3, Y. Takenaga3, S. Clark4, S. Desai4,5, F. Dufour4, E. Kearns4, S. Likhoded4, M. Litos4, J. L. Raaf4, J. L. Stone4, L. R. Sulak4, W. Wang4, M. Goldhaber6, D. Casper7, J. P. Cravens7, J. Dunmore7, W. R. Kropp7, D. W. Liu7, S. Mine7, C. Regis7, M. B. Smy7, H. W. Sobel7, M. R. Vagins7, K. S. Ganezer8, J. E. Hill8, W. E. Keig8, J. S. Jang9, J. Y. Kim9, I. T. Lim9, K. Scholberg1,10, N. Tanimoto10, C. W. Walter10, R. Wendell10, R. W. Ellsworth11, S. Tasaka12, G. Guillian13, J. G. Learned13, S. Matsuno13, M. D. Messier14, Y. Hayato15,16, A. K. Ichikawa15, T. Ishida15, T. Ishii15, T. Iwashita15, T. Kobayashi15, T. Nakadaira15, K. Nakamura15, K. Nitta15, Y. Oyama15, Y. Totsuka15,17, A. T. Suzuki18, M. Hasegawa19, K. Hiraide19, I. Kato19,20, H. Maesaka19, T. Nakaya19, K. Nishikawa19, T. Sasaki19, H. Sato19, S. Yamamoto19, M. Yokoyama19, T. J. Haines7,21, S. Dazeley22, S. Hatakeyama22, R. Svoboda22, G. W. Sullivan23, D. Turcan23, J. Cooley1,24, K. B. M. Mahn1,25, A. Habig26, Y. Fukuda27, T. Sato27, Y. Itow28, T. Koike28, C. K. Jung29, T. Kato29, K. Kobayashi29, M. Malek29, C. McGrew29, A. Sarrat29, R. Terri29, C. Yanagisawa29, N. Tamura30, M. Sakuda31, M. Sugihara31, Y. Kuno32, M. Yoshida32, S. B. Kim33, B. S. Yang33, J. Yoo33, T. Ishizuka34, H. Okazawa35, Y. Choi36, H. K. Seo36, Y. Gando37, T. Hasegawa37, K. Inoue37, H. Ishii38, K. Nishijima38, H. Ishino39, Y. Watanabe39, M. Koshiba40, D. Kielczewska7,41, J. Zalipska41, H. G. Berns42, R. Gran26,42, K. K. Shiraishi42, A. Stachyra42, E. Thrane42, K. Washburn42, R. J. Wilkes42 and (The Super-Kamiokande Collaboration)
Show affiliationsMany astrophysical models predict a diffuse flux of high-energy neutrinos from active galactic nuclei and other extragalactic sources. At muon energies above 1 TeV, the upward-going muon flux induced by neutrinos from active galactic nuclei is expected to exceed the flux due to atmospheric neutrinos. We have performed a search for this astrophysical neutrino flux by looking for upward-going muons in the highest energy data sample from the Super-Kamiokande detector using 1679.6 live days of data. We found one extremely high energy upward-going muon event, compared with an expected atmospheric neutrino background of 0.46 ± 0.23 events. Using this result, we set an upper limit on the diffuse flux of upward-going muons due to neutrinos from astrophysical sources in the muon energy range 3.16-100 TeV.
Issue 1 (2006 November 20)
Received 2006 June 6, accepted for publication 2006 July 26
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K. Abe et al. 2006 ApJ 652 198
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