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The Sloan Digital Sky Survey pipeline photometry underestimates thebrightnesses of the most luminous galaxies. This is mainly because (i) the SDSSoverestimates the sky background and (ii) single or two-component Sersic-basedmodels better fit the surface brightness profile of galaxies, especially athigh luminosities, than does the de Vaucouleurs model used by the SDSSpipeline. We use the PyMorph photometric reductions to isolate effect (ii) andshow that it is the same in the full sample as in small group environments, andfor satellites in the most massive clusters as well. None of these are expectedto be significantly affected by intracluster light (ICL). We only see anadditional effect for centrals in the most massive halos, but we argue thateven this is not dominated by ICL. Hence, for the vast majority of galaxies,the differences between PyMorph and SDSS pipeline photometry cannot be ascribedto the semantics of whether or not one includes the ICL when describing thestellar mass of massive galaxies. Rather, they likely reflect differences instar formation or assembly histories. Failure to account for the SDSSunderestimate has significantly biased most previous estimates of the SDSSluminosity and stellar mass functions, and therefore Halo Model estimates ofthe z ~ 0.1 relation between the mass of a halo and that of the galaxy at itscenter. We also show that when one studies correlations, at fixed group mass,with a quantity which was not used to define the groups, then selection effectsappear. We show why such effects arise, and should not be mistaken for physicaleffects.

Comparing PyMorph and SDSS photometry. II. The differences are more than semantics and are not dominated by intracluster light