Neutrinos from the Galactic Center in the Light of its Gamma-Ray Detection at TeV Energy

Details Neutrinos from the Galactic Center in the Light of its Gamma-Ray Detection at TeV Energy Neutrinos from the Galactic Center in the Light of its Gamma-Ray Detection at TeV Energy

2004-11-16

arxiv.org/abs/astro-ph/0411471v4

Astrophys.J. 622 (2005) L37-L40

Astronomy and Astrophysics

Astrophysics

12 pages, 1 figure. Version accepted to ApJ Letters. Minor amendments

Scientific paper

10.1086/429539

We re-evaluate the event rate expected in km^3-scale detectors for neutrinos from the direction of the Galactic Center (GC) in light of recent spectral measurements obtained by the HESS instrument for ~TeV gamma-radiation from this direction. In the most plausible scenario the re-evaluated event rate is smaller than that previously calculated--and here re-calculated--on the basis of EGRET data. However, the GC TeV gamma-ray detections by the Whipple, CANGAROO, and HESS instruments, together with the strong indications for an overabundance of cosmic rays coming from the GC at EeV energies, strengthen the expectation for a detectable, TeV-PeV GC neutrino signal from proton-proton interactions in that region. If the TeV gamma-ray--EeV cosmic ray anisotropy connection is correct, this signal will be detectable within a year and half for km^3-scale neutrino detectors in the Northern Hemisphere at super-TeV energies and, significantly, should also be detectable in 1.6 years by the South Polar IceCube detector at energies > 10^14 eV. The GC neutrino signal should also produce a detectable signal from neutrino showering and resonant W^- production by anti-electron-neutrinos in the volume of a km^3-scale detector.

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