Phys. Rev. Lett.
92,
071301
(2004)
[5 pages]
High Sensitivity Search for ν̅ e’s from the Sun and Other Sources at KamLAND
K. Eguchi et al. KamLAND Collaboration
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K. Eguchi1, S. Enomoto1, K. Furuno1, H. Ikeda1, K. Ikeda1, K. Inoue1, K. Ishihara1,*, T. Iwamoto1,†, T. Kawashima1, Y. Kishimoto1, M. Koga1, Y. Koseki1, T. Maeda1, T. Mitsui1, M. Motoki1, K. Nakajima1, H. Ogawa1, K. Owada1, F. Piquemal1, I. Shimizu1, J. Shirai1, F. Suekane1, A. Suzuki1, K. Tada1, O. Tajima1, T. Takayama1, K. Tamae1, H. Watanabe1, J. Busenitz2, Z. Djurcic2, K. McKinny2, D-M. Mei2, A. Piepke2, E. Yakushev2, B. E. Berger3, Y. D. Chan3, M. P. Decowski3, D. A. Dwyer3, S. J. Freedman3, Y. Fu3, B. K. Fujikawa3, J. Goldman3, K. M. Heeger3, K. T. Lesko3, K.-B. Luk3, H. Murayama3, D. R. Nygren3, C. E. Okada3, A. W. P. Poon3, H. M. Steiner3, L. A. Winslow3, G. A. Horton-Smith4, C. Mauger4, R. D. McKeown4, B. Tipton4, P. Vogel4, C. E. Lane5, T. Miletic5, P. W. Gorham6, G. Guillian6, J. G. Learned6, J. Maricic6, S. Matsuno6, S. Pakvasa6, S. Dazeley7, S. Hatakeyama7, R. Svoboda7, B. D. Dieterle8, M. DiMauro8, J. Detwiler9, G. Gratta9, K. Ishii9, N. Tolich9, Y. Uchida9, M. Batygov10, W. Bugg10, Y. Efremenko10, Y. Kamyshkov10, A. Kozlov10, Y. Nakamura10, C. R. Gould11, H. J. Karwowski11, D. M. Markoff11, J. A. Messimore11, K. Nakamura11, R. M. Rohm11, W. Tornow11, A. R. Young11, M-J. Chen12, and Y-F. Wang12 (KamLAND Collaboration)
1Research Center for Neutrino Science, Tohoku University, Sendai 980-8578, Japan
2Department of Physics and Astronomy, University of Alabama, Tuscaloosa, Alabama 35487, USA
3Physics Department, University of California at Berkeley and Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
4W. K. Kellogg Radiation Laboratory, California Institute of Technology, Pasadena, California 91125, USA
5Physics Department, Drexel University, Philadelphia, Pennsylvania 19104, USA
6Department of Physics and Astronomy, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA
7Department of Physics and Astronomy, Louisiana State University, Baton Rouge, Louisiana 70803, USA
8Physics Department, University of New Mexico, Albuquerque, New Mexico 87131, USA
9Physics Department, Stanford University, Stanford, California 94305, USA
10Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
11Triangle Universities Nuclear Laboratory, Durham, North Carolina 27708, USA Physics Department, Duke University, Durham, North Carolina 27706, USA Physics Department, North Carolina State University, Raleigh, North Carolina 27695, USA Physics Department, University of North Carolina at Chapel Hill, Chapel Hill, North Carolina 27514, USA
12Institute of High Energy Physics, Beijing 100039, People’s Republic of China
Received 22 October 2003; published 20 February 2004
Data corresponding to a KamLAND detector exposure of 0.28 kton yr has been used to search for ν̅ e’s in the energy range 8.3<Eν̅ e<14.8 MeV. No candidates were found for an expected background of 1.1±0.4 events. This result can be used to obtain a limit on ν̅ e fluxes of any origin. Assuming that all ν̅ e flux has its origin in the Sun and has the characteristic 8B solar νe energy spectrum, we obtain an upper limit of 3.7×102 cm-2 s-1 (90% C.L.) on the ν̅ e flux. We interpret this limit, corresponding to 2.8×10-4 of the standard solar model 8B νe flux, in the framework of spin-flavor precession and neutrino decay models.
© 2004 The American Physical Society
URL:
http://link.aps.org/doi/10.1103/PhysRevLett.92.071301
DOI:
10.1103/PhysRevLett.92.071301
PACS:
26.65.+t, 13.35.Hb, 14.60.St
*Present address: Institute for Cosmic Ray Research, University of Tokyo, Tokyo, Japan. †Present address: International Center for Elementary Particle Physics, University of Tokyo, Tokyo, Japan.
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