Neutrinos as a diagnostic of cosmic ray galactic-extragalactic transition
- Deutsches Elektronen-Synchrotron DESY, Hamburg (Germany)
- Department of Physics, Northeastern University, Boston, Massachusetts 02115 (United States)
- Department of Physics, University of Wisconsin, Madison Wisconsin 53706 (United States)
- Department of Physics and Astronomy, Vanderbilt University, Nashville Tennessee 37235 (United States)
Motivated by a recent change in viewing the onset of the extragalactic component in the cosmic ray spectrum, we have fitted the observed data down to 10{sup 8.6} GeV and have obtained the corresponding power emissivity. This transition energy is well below the threshold for resonant p{gamma} absorption on the cosmic microwave background, and thus source evolution is an essential ingredient in the fitting procedure. Two-parameter fits in the spectral and redshift evolution indices show that a standard Fermi E{sub i}{sup -2} source spectrum is excluded at larger than 95% confidence level (CL). Armed with the primordial emissivity, we follow Waxman and Bahcall to derive the associated neutrino flux on the basis of optically thin sources. For pp interactions as the generating mechanism, the neutrino flux exceeds the AMANDA-B10 90% CL upper limits. In the case of p{gamma} dominance, the flux is consistent with AMANDA-B10 data. In the new scenario the source neutrino flux is considerably enhanced, especially below 10{sup 9} GeV. Should data from AMANDA-II prove consistent with the model, we show that IceCube can measure the characteristic power law of the neutrino spectrum, and thus provide a window on the source dynamics.
- OSTI ID:
- 20711099
- Journal Information:
- Physical Review. D, Particles Fields, Vol. 72, Issue 2; Other Information: DOI: 10.1103/PhysRevD.72.023001; (c) 2005 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); ISSN 0556-2821
- Country of Publication:
- United States
- Language:
- English
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