Ram pressure profiles in galaxy groups and clusters
  Using a hybrid method which combines non-radiative hydrodynamical simulations
with a semi-analytic model of galaxy formation, we determine the ram pressure
as a function of halocentric distance experienced by galaxies in haloes with
virial masses 12.5 <= log (M_200 h/M_Sun) < 15.35, for redshifts 0 <= z <= 3.
The ram pressure is calculated with a self-consistent method which uses the
simulation gas particles to obtain the properties of the intergalactic medium.
The ram pressure profiles obtained can be well described by beta profile
models, with parameters that depend on redshift and halo virial mass in a
simple fashion. The fitting formulae provided here will prove useful to include
ram pressure effects into semi-analytic models based on methods which lack gas
physics, such as dark matter-only simulations or the Press-Schechter formalism.
