Numerical Simulations in Cosmology II: Spatial and Velocity Biases

We give a summary of recent results on spatial and velocity biases in cosmological models. Progress in numerical techniques made it possible to simulate halos in large volumes with a such accuracy that halos survive in dense environments of groups and clusters of galaxies. Halos in simulations look like real galaxies, and, thus, can be used to study the biases – differences between galaxies and the dark matter. The biases depend on scale, redshift, and circular velocities of selected halos. Two processes seem to define the evolution of the spatial bias: (1) statistical bias and (2) merger bias (merging of galaxies, which happens preferentially in groups, reduces the number of galaxies, but does not affect the clustering of the dark matter). There are two kinds of velocity bias. The pair-wise velocity bias is b12 = 0.6 − 0.8 at r < 5h −1Mpc, z = 0. This bias mostly reflects the spatial bias and provides almost no information on the relative velocities of the galaxies and the dark matter. One-point velocity bias is a better measure of the velocities. Inside clusters the galaxies should move slightly faster (bv = 1.1 − 1.3) than the dark matter. Qualitatively this result can be understood using the Jeans equations of the stellar dynamics. For the standard LCDM model we find that the correlation function and the power spectrum of galaxy-size halos at z = 0 are antibiased on scales r < 5h−1Mpc and k ≈ (0.15 − 30)hMpc−1. Subject headings: cosmology: theory large-scale structure of the universe