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

We re-evaluate the event rate expected in km-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 γ-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 γ-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-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 eV. The GC neutrino signal should also produce a detectable signal from neutrino showering and resonant W− production by νe’s in the volume of a km-scale detector. Subject headings: cosmic-rays — elementary particles — Galaxy: center — neutrinos — radiation mechanisms: nonthermal — supernova remnants