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Cosmological simulations of galaxies have typically produced too many starsat early times. We study the global and morphological effects of radiationpressure (RP) in eight pairs of high-resolution cosmological galaxy formationsimulations. We find that the additional feedback suppresses star formationglobally by a factor of ~2. Despite this reduction, the simulations stilloverproduce stars by a factor of ~2 with respect to the predictions provided byabundance matching methods for halos more massive than 5E11 Msun/h (Behroozi,Wechsler & Conroy 2013).  We also study the morphological impact of radiation pressure on oursimulations. In simulations with RP the average number of low mass clumps fallsdramatically. Only clumps with stellar masses Mclump/Mdisk <= 5% are impactedby the inclusion of RP, and RP and no-RP clump counts above this range arecomparable. The inclusion of RP depresses the contrast ratios of clumps byfactors of a few for clump masses less than 5% of the disk masses. For moremassive clumps, the differences between and RP and no-RP simulations diminish.We note however, that the simulations analyzed have disk stellar masses belowabout 2E10 Msun/h.  By creating mock Hubble Space Telescope observations we find that the numberof clumps is slightly reduced in simulations with RP. However, since massiveclumps survive the inclusion of RP and are found in our mock observations, wedo not find a disagreement between simulations of our clumpy galaxies andobservations of clumpy galaxies. We demonstrate that clumps found in any singlegas, stellar, or mock observation image are not necessarily clumps found inanother map, and that there are few clumps common to multiple maps.

Star Formation and Clumps in Cosmological Galaxy Simulations with Radiation Pressure Feedback