Seeding Black Holes in Cosmological Simulations
  We present a new model for the formation of black holes in cosmological
simulations, motivated by the first star formation. Black holes form from high
density peaks of primordial gas, and grow via both gas accretion and mergers.
Massive black holes heat the surrounding material, suppressing star formation
at the centres of galaxies, and driving galactic winds. We perform an
investigation into the physical effects of the model parameters, and obtain a
`best' set of these parameters by comparing the outcome of simulations to
observations. With this best set, we successfully reproduce the cosmic star
formation rate history, black hole mass -- velocity dispersion relation, and
the size -- velocity dispersion relation of galaxies. The black hole seed mass
is 10^3Msun, which is orders of magnitude smaller than has been used in
previous cosmological simulations with active galactic nuclei, but suggests
that the origin of the seed black holes is the death of Population III stars.
