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The high end of the stellar mass function of galaxies is observed to havelittle evolution since z~1. This represents a stringent constraint formerger--based models, aimed at explaining the evolution of the most massivegalaxies in the concordance LambdaCDM cosmology. In this Letter we show that itis possible to remove the tension between the above observations and modelpredictions by allowing a fraction of stars to be scattered to the DiffuseStellar Component (DSC) of galaxy clusters at each galaxy merger, as recentlysuggested by the analysis of N-body hydrodynamical simulations. To thispurpose, we use the MORGANA model of galaxy formation in a minimal version, inwhich gas cooling and star formation are switched off after z=1. In this way,any predicted evolution of the galaxy stellar mass function is purely driven bymergers. We show that, even in this extreme case, the predicted degree ofevolution of the high end of the stellar mass function is larger than thatsuggested by data. Assuming instead that a significant fraction, ~30 per cent,of stars are scattered in the DSC at each merger event, leads to a significantsuppression of the predicted evolution, in better agreement with observationalconstraints, while providing a total amount of DSC in clusters which isconsistent with recent observational determinations.Comment: 5 pages, figures included; ApJ Letters, in press. Revision: reference  adde

Diffuse Stellar Component in Galaxy Clusters and the Evolution of the Most Massive Galaxies at [FORMULA][F]z≲1[/F][/FORMULA]