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The observed clustering of galaxies and the cross-correlation of galaxies andmass provide important constraints on both cosmology and models of galaxyformation. Even though the dissipation and feedback processes associated withgalaxy formation are thought to affect the distribution of matter, essentiallyall models used to predict clustering data are based on collisionlesssimulations. Here, we use large hydrodynamical simulations to investigate howgalaxy formation affects the autocorrelation functions of galaxies andsubhaloes, as well as their cross-correlation with matter. We show that thechanges due to the inclusion of baryons are not limited to small scales and areeven present in samples selected by subhalo mass. Samples selected by subhalomass cluster ~10% more strongly in a baryonic run on scales r > 1Mpc/h, andthis difference increases for smaller separations. While the inclusion ofbaryons boosts the clustering at fixed subhalo mass on all scales, the sign ofthe effect on the cross-correlation of subhaloes with matter can vary withradius. We show that the large-scale effects are due to the change in subhalomass caused by the strong feedback associated with galaxy formation and maytherefore not affect samples selected by number density. However, on scales r <r_vir significant differences remain after accounting for the change in subhalomass. We conclude that predictions for galaxy-galaxy and galaxy-mass clusteringfrom models based on collisionless simulations will have errors greater than10% on sub-Mpc scales, unless the simulation results are modified to correctlyaccount for the effects of baryons on the distributions of mass and satellites.

The impact of baryonic processes on the two-point correlation functions of galaxies, subhaloes and matter