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We present a comparison between the observed color distribution, number andmass density of massive galaxies at 1.5 < z < 3 and a model by Hopkins et al.that relates the quasar and galaxy population on the basis of gas-rich mergers.In order to test the hypothesis that quiescent red galaxies are formed after agas-rich merger involving quasar activity, we confront photometry of massive (M> 4x10^10 Msun) galaxies extracted from the FIRES, GOODS-South, and MUSYCsurveys, together spanning an area of 496 arcmin^2, with synthetic photometryfrom hydrodynamical merger simulations. As in the Hopkins et al. (2006b) model,we use the observed quasar luminosity function to estimate the merger rate. Wefind that the synthetic U-V and V-J colors of galaxies that had a quasar phasein their past match the colors of observed galaxies that are best characterizedby a quiescent stellar population. At z ~ 2.6, the observed number and massdensity of quiescent red galaxies with M > 4x10^10 Msun is consistent with themodel in which every quiescent massive galaxy underwent a quasar phase in thepast. At z ~ 1.9, 2.8 times less quiescent galaxies are observed than predictedby the model as descendants of higher redshift quasars. The merger model alsopredicts a large number of galaxies undergoing merger-driven star formation. Wefind that the predicted number and mass density accounts for 30-50% of theobserved massive star-forming galaxies. However, their colors do not matchthose of observed star-forming galaxies. In particular, the colors of dusty redgalaxies are not reproduced by the simulations. Several possible origins ofthis discrepancy are discussed. The observational constraints on the validityof the model are currently limited by cosmic variance and uncertainties instellar population synthesis and radiative transfer.

Color Distributions, Number and Mass Densities of Massive Galaxies at 1.5 < z < 3: Comparing Observations with Merger Simulations