The impact of galaxy formation on the total mass, mass profile and
  abundance of haloes
  We use cosmological hydrodynamical simulations to investigate how the
inclusion of physical processes relevant to galaxy formation (star formation,
metal-line cooling, stellar winds, supernovae and feedback from Active Galactic
Nuclei, AGN) change the properties of haloes, over four orders of magnitude in
mass. We find that gas expulsion and the associated dark matter (DM) expansion
induced by supernova-driven winds are important for haloes with masses M200 <
10^13 Msun, lowering their masses by up to 20% relative to a DM-only model. AGN
feedback, which is required to prevent overcooling, has a significant impact on
halo masses all the way up to cluster scales (M200 ~ 10^15 Msun). Baryonic
physics changes the total mass profiles of haloes out to several times the
virial radius, a modification that cannot be captured by a change in the halo
concentration. The decrease in the total halo mass causes a decrease in the
halo mass function of about 20%. This effect can have important consequences
for abundance matching technique as well as for most semi-analytic models of
galaxy formation. We provide analytic fitting formulae, derived from
simulations that reproduce the observed baryon fractions, to correct halo
masses and mass functions from DM-only simulations. The effect of baryonic
physics (AGN feedback in particular) on cluster number counts is about as large
as changing the cosmology from WMAP7 to Planck, even when a moderately high
mass limit of M500 ~ 10^14 Msun is adopted. Thus, for precision cosmology the
effects of baryons must be accounted for.
