Position of the peak corresponding to for the full (filled circles) and red (filled diamonds) samples as function of redshift. Error bars are derived from the nearest data point to the peak. We compare our results with measurements in SDSS (Zehavi et al. 2011), in COSMOS (Leauthaud et al. 2012b) and in the NEWFIRM Medium Band Survey (NMBS, Wake et al. 2011). We convert M₂₀₀ halo masses (corresponding to a sphere with overdensity 200 times the background density) into virial masses M_vir (our definition) using the method described in Appendix C of Hu & Kravtsov (2003). We also display numerical predictions based on abundance-matching method from Behroozi et al. (2010) and Moster et al. (2010), where the shaded region shows the 1 − σ uncertainty.