High Energy Cosmic Rays (C.R.) versus Neutrino and Neutralino induced
Air-Shower maybe tested at Horizons by their muons, gamma and Cerenkov blazing
signals. Inclined and Horizontal C.R. Showers (70-90 zenith angle) produce
secondary (gamma, e+, e-) mostly suppressed by high column atmosphere depth.
Earliest shower Cherenkov photons are diluted by large distances and by air
opacity, while secondary penetrating muons and their successive decay into
electrons and gamma, may revive additional Cerenkov lights. GeVs gamma
telescopes at the top of the mountains or in Space may detect at horizons PeVs
up to EeV C.R. and their secondaries. Details on arrival angle and column
depth, shower shape, timing signature of photon flash intensity, may inform us
on the altitude interaction and primary UHECR composition. Below the horizons,
at zenith angle among copious single albedo muons, rare up-going showers traced
by muon bundles would give evidence of rare tau Earth-Skimming neutrinos, at
EeVs energies. Their rate may be comparable with 6.3 PeVs anti-neutrino
electron induced air-shower (mostly hadronic) originated above and also below
horizons, in interposed atmosphere by W resonance at Glashow peak. Additional
and complementary UHE SUSY neutralinos at tens PeVs-EeV energy may blaze, by
its characteristic electromagnetic signature. Their secondary shower blazing
Cerenkov lights and distances might be disentangled from UHECR by Stereoscopic
Telescopes such as Magic ones or Hess array experiment. The horizontal
detection sensitivity of Magic in the present set up (if totally devoted to the
Horizons Shower search) maybe already be comparable to AMANDA underground
neutrino detector at PeVs energies.Comment: 9 pages, 3 figures, International Conference on Frontier Science,
Phys. and Astrophysics in Space, June 200
