  The progenitors of core-collapse supernovae are stars with an initial mass
greater than about 8M(sun). Understanding the evolution of these stars is
necessary to comprehend the evolution and differences between supernovae.
  We have constructed new and unique opacity tables to increase model accuracy
during the latest stages of stellar evolution. We have investigated how initial
mass, initial composition and mass loss affects the progenitors and their
populations. There are many prescriptions for mass loss. Different research
groups use their preferred rates. We have compared 12 different prescriptions
and determined which provides the best fit to observations. We use our
preferred mass-loss scheme to make suggestions as to the source of the
differences between supernova types from our progenitor models.
  Binary evolution is considered in order to search for low luminosity SN
progenitors and progenitor types not possible from single stars. Removal of the
hydrogen envelope is more common and we find quite different hydrogen deficient
SN progenitors. We discuss the implications of our binary models for
ultra-luminous X-ray sources and gamma-ray bursts. We present an estimation of
the mass distribution for black holes at various metallcities showing that
massive black holes are not formed until very low metallicities. Finally we
combine the single star and binary results to determine their relative
populations and compare to observations. However it is not possible to draw
many firm conclusions because of the uncertainty in observations to date.
