Tau Neutrino Astronomy by GZK UHE He

UHECR may be either nucleons or nuclei; in the latter case the Lightest Nuclei, as He4 or He3 , explains the absence of Virgo signals and the crowding of events around CenA bent by galactic magnetic ¯elds.This model agrees with observed mass composition discovered in AUGER. However UHECR nucleons above GZK produce EeV neutrinos while Heavy Nuclei, as Fe UHECR do not produce much. Also UHECR He nuclei at few 1019eV su®er nuclear fragmentation (producing low energetic neutrino at tens PeVs) but it also su®er photo-pion GZK suppression (leading to EeV neutrinos) once above one-few 1020eV . These UHE secondary neutrinos signals may in°uence expected (via GZK nucleon) Tau Neutrino Astronomy in signi¯cant and detectable way; the role of resonant antineutrino electron-electron leading to Tau air-shower may also rise.