  Using the recent shell model evaluation of stellar weak interaction rates we
have calculated the neutrino spectra arising from electron capture on pf-shell
nuclei under presupernova conditions. We present a simple parametrization of
the spectra which allows for an easy implementation into collapse simulations.
We discuss that the explicit consideration of thermal ensembles in the parent
nucleus broadens the neutrino spectra and results in larger average neutrino
energies. The capture rates and neutrino spectra can be easily modified to
account for phase space blocking by neutrinos which becomes increasingly
important during the final stellar collapse.
