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We have compared the observed distribution of galaxies in the plane ofspecific star formation rate versus stellar mass with the predictions of theGarching semi-analytic model at redshifts 0, 1 and 2. The goal is to testwhether the implementation of radio mode AGN feedback, which is responsible forterminating the formation of stars in high mass galaxies, provides an adequatematch to current high-redshift observations. The fraction of quenched galaxiesas a function of stellar mass in the models is in good agreement with data atz=0 and z=1. By z=2, there are too few quenched galaxies with low stellarmasses in the models. At z=2, the population of galaxies with no ongoing starformation is clearly separated from the `main sequence' of star-forminggalaxies in the data. This is not found in the models, because z=2 galaxieswith stellar masses less than 10^11 solar masses are predicted to host blackholes with relatively low masses (less than 10^8 solar masses). The currentimplementation of radio mode feedback from such black holes reduces the coolingrates from the surrounding halo, but does not generate sufficient energy tostop star formation entirely. We suggest that the models may be brought intobetter agreement with the data if black hole growth is triggered by discinstabilities in addition to major mergers, and if feedback mechanismsassociated with the formation of galactic bulges act to quench star formationin galaxies.

On the Evolution of the Bi-Modal Distribution of Galaxies in the Plane of Specific Star Formation Rate versus Stellar Mass