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High-Energy Neutrino Astronomy from AMANDA to Icecube
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University of Wisconsin - Madison MADPH-03-1347
September 2003
High-Energy Neutrino Astronomy:
From AMANDA to IceCube?
Francis Halzen
Department of Physics, University of Wisconsin, Madison, WI 53706
Abstract
Kilometer-scale neutrino detectors such as IceCube are discovery instru-
ments covering nuclear and particle physics, cosmology and astronomy. Exam-
ples of their multidisciplinary missions include the search for the particle nature
of dark matter and for additional small dimensions of space. In the end, their
conceptual design is very much anchored to the observational fact that Nature
accelerates protons and photons to energies in excess of 1020 and 1013 eV, re-
spectively. The cosmic ray connection sets the scale of cosmic neutrino fluxes.
In this context, we discuss the first results of the completed AMANDA detector
and the reach of its extension, IceCube.
1 Neutrinos Associated with the Highest Energy
Cosmic Rays
The flux of cosmic rays is summarized in Fig. 1a,b[1]. The energy spectrum follows a
broken power law. The two power laws are separated by a feature referred to as the
“knee”; see Fig. 1a. There is evidence that cosmic rays, up to several EeV, originate
in galactic sources. This correlation disappears in the vicinity of a second feature
in the spectrum dubbed the “ankle”. Above the ankle, the gyroradius of a proton
exceeds the size of the galaxy and it is generally assumed that we are witnessing the
onset of an extragalactic component in the spectrum that extends to energies beyond
100EeV. Experiments indicate that the highest energy cosmic rays are predominantly
protons. Above a threshold of 50 EeV these protons interact with CMBR photons
and therefore lose their energy to pions before reaching our detectors. This limits
their sources to tens of Mpc, the so-called Greissen-Zatsepin-Kuzmin cutoff.
Models for the origin of the highest energy cosmic rays fall into two categories,
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