  Large volume cosmological simulations succeed in reproducing the large-scale
structure of the Universe. However, they lack resolution and may not take into
account all relevant physical processes to test if the detail properties of
galaxies can be explained by the CDM paradigm. On the other hand, galaxy-scale
simulations could resolve this in a robust way but do not usually include a
realistic cosmological context.
  To study galaxy evolution in cosmological context, we use a new method that
consists in coupling cosmological simulations and galactic scale simulations.
For this, we record merger and gas accretion histories from cosmological
simulations and re-simulate at very high resolution the evolution of baryons
and dark matter within the virial radius of a target galaxy. This allows us for
example to better take into account gas evolution and associated star
formation, to finely study the internal evolution of galaxies and their disks
in a realistic cosmological context.
  We aim at obtaining a statistical view on galaxy evolution from z = 2 to 0,
and we present here the first results of the study: we mainly stress the
importance of taking into account gas accretion along filaments to understand
galaxy evolution.
