  Neutrinos emitted during stellar core collapse up to their trapping phase
carry information about the stage from which the Supernova explosion process
initiates. The dominant $\nu_e$ emission mechanism is by electron capture on
free protons and f-p shell nuclei and the spectrum of these neutrinos is a
function of the ambient physical conditions within the core as well as the
nuclear equation of state. The number of collapse phase $\nu_e$ which can be
detected by Super-Kamioka and Sudbury Neutrino Observatory from a Supernova
within 1 kpc, and their generic energy spectra are given.
