Virial Scaling of Galaxies in Clusters: Bright to Faint is Cool to Hot

By combining galaxy tracers from high-resolution N -body and hydrodynamical simulations, we present a consistent picture of the behavior of galaxy velocities in massive clusters. In haloes above ∼10M , the brightest satellite galaxies are slightly cooler compared to the dark matter, while fainter satellites are hotter. Within the virial radius of a cluster, the mean velocity dispersion based on the 100 brightest galaxies is a factor of 1.046 ± 0.008 (stat) ± 0.010 (sys) higher than that of the dark matter (corresponding to a ∼ 10 − 15 per cent bias in the dynamical mass estimate) while that based on only the 5 brightest galaxies is 0.86± 0.040 (stat) ± 0.030 (sys). These trends are approximately independent of redshift. The velocity structure is sensitive to the modeling of galaxies in clusters, indicative of the complex interplay of tidal stripping, dynamical friction, and merging. Velocity dispersions derived from instantaneous subhalo properties are larger than those employing either peak subhalo properties or hydrodynamical galaxy tracers. The latter two methods are consistent, implying that stacked spectroscopic analysis of cluster samples should, after correction for projection, show a trend toward slightly higher velocities when fainter galaxies are included, with an unbiased measure of dark matter velocity dispersion coming from approximately 30 galaxies per cluster. We show evidence that the velocity distribution function of bright galaxies near the cluster center has a low-velocity tail due to strong dynamical friction.