How robust are predictions of galaxy clustering?

Abstract

We use the Millennium Simulation data base to compare how different versions of the Durham and Munich semi-analytical galaxy formation models populate dark matter haloes with galaxies. The models follow the same physical processes but differ in how these are implemented. All of the models we consider use the Millennium N-body Simulation; however, theDurham and Munich groups use independent algorithms to construct halo merger histories from the simulation output.We compare the predicted halo occupation distributions (HODs) and correlation functions for galaxy samples defined by stellar mass, cold gas mass and star formation rate. The model predictions for the HOD are remarkably similar for samples ranked by stellar mass. The predicted bias averaged over pair separations in the range 5-25 h-1 Mpc is consistent between models to within 10 per cent. At small pair separations there is a clear difference in the predicted clustering. This arises because the Durham models allow some satellite galaxies to merge with the central galaxy in a halo when they are still associated with resolved dark matter subhaloes. The agreement between the models is less good for samples definedby cold gas mass or star formation rate, with the spread in predicted galaxy bias reaching 20 per cent and the small-scale clustering differing by an order of magnitude, reflecting the uncertainty in the modelling of star formation. The model predictions in these cases are nevertheless qualitatively similar, with a markedly shallower slope for the correlation function than is found for stellar mass selected samples and with the HOD displaying an asymmetric peak for central galaxies. We provide illustrative parametric fits to the HODs predicted by the models. Our results reveal the currentlimitations on how well we can predict galaxy bias in a fixed cosmology, which has implications for the interpretation of constraints on the physics of galaxy formation from galaxy clustering measurements and the ability of future galaxy surveys to measure dark energy. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.