Abstract
The observed clustering of galaxies and the cross-correlation of galaxies and
mass (a measure of galaxy-galaxy lensing) provide important constraints on both
cosmology and models of galaxy formation. Even though the dissipation, and more
importantly the feedback processes associated with galaxy formation are thought
to affect the distribution of matter, essentially all models used to predict
clustering data are based on dark matter only simulations. Here, we use large
hydrodynamical simulations to investigate how galaxy formation affects the
autocorrelation functions of galaxies, subhaloes, as well as their
cross-correlation with matter. We show that the changes due to the inclusion of
baryons are not limited to small scales and are even present in samples
selected by subhalo mass. Samples selected by subhalo mass cluster ~10% more
strongly in a baryonic run on scales r ~ 1Mpc/h or larger, and this difference
increases for smaller separations. While the inclusion of baryons boosts the
clustering at fixed subhalo mass on all scales, the sign of the effect on the
cross-correlation of subhaloes with matter can vary with radius. By linking
subhaloes between simulations, we show that the large-scale effects are due to
the change in subhalo mass caused by the strong feedback associated with galaxy
formation and may therefore not affect samples selected by number density.
However, on scales r < r_vir significant differences remain after accounting
for the change in subhalo mass. We conclude that predictions for galaxy-galaxy
and galaxy-mass clustering from models based on dark matter only simulations
will have errors greater than 10% on sub-Mpc scales, unless the simulation
results are modified to correctly account for the effects of baryons on the
distributions of mass and satellites.
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