  High-resolution N-body re-simulations of 15 massive (10^{14}-10^{15} Msun)
dark matter haloes have been combined with the hybrid galaxy formation model
GalICS (Hatton et al. 2003), to study the formation and evolution of galaxies
in clusters, within the framework of the hierarchical merging scenario. New
features in GalICS include a better description of galaxy positioning within
dark matter haloes, a more reliable computation of the temperature of the
inter-galactic medium as a function of redshift, and a description of the ram
pressure stripping process. We focus on the luminosity functions, morphological
fractions and colour distributions of galaxies in clusters and in cluster
outskirts, at z=0. No systematic dependency on cluster richness is found either
for the galaxy luminosity functions, morphological mixes, or colour
distributions. Moving from higher density (cluster cores), to lower density
environments (cluster outskirts), we detect a progressive flattening of the
luminosity functions, an increase of the fraction of spirals and a decrease of
that of ellipticals and S0s, and the progressive emergence of a bluer tail in
the distributions of galaxy colours, especially for spirals. As compared to
cluster spirals, early-type galaxies show a flatter luminosity function, and
more homogeneous and redder colours. An overall good agreement is found between
our results and the observations, particularly in terms of the cluster
luminosity functions and morphological mixes. However, some discrepancies are
also apparent, with too faint magnitudes of the brightest cluster members,
especially in the B band, and galaxy colours tendentially too red (or not blue
enough) in the model, with respect to the observations. Finally, ram pressure
stripping appears to affect very little our results.
