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We have updated the Munich galaxy formation model to the Planck first-yearcosmology, while modifying the treatment of baryonic processes to reproducerecent data on the abundance and passive fractions of galaxies from z= 3 downto z=0. Matching these more extensive and more precise observational resultsrequires us to delay the reincorporation of wind ejecta, to lower the surfacedensity threshold for turning cold gas into stars, to eliminate ram-pressurestripping in haloes less massive than ~10^14 Msun, and to modify our model forradio mode feedback. These changes cure the most obvious failings of ourprevious models, namely the overly early formation of low-mass galaxies and theoverly large fraction of them that are passive at late times. The new model iscalibrated to reproduce the observed evolution both of the stellar massfunction and of the distribution of star formation rate at each stellar mass.Massive galaxies (M>10^11 [Msun]) assemble most of their mass before z=1 andare predominantly old and passive at z=0, while lower mass galaxies assemblelater and, for M<10^9.5 (Msun), are still predominantly blue and star formingat z=0. This phenomenological but physically based model allows theobservations to be interpreted in terms of the efficiency of the variousprocesses that control the formation and evolution of galaxies as a function oftheir stellar mass, gas content, environment and time.

Galaxy formation in the Planck Cosmology - I. Matching the observed evolution of star formation rates, colours and stellar masses