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Using $\sim 100$ X-ray selected clusters in the Dark Energy Survey ScienceVerification data, we constrain the luminosity function (LF) of cluster redsequence galaxies as a function of redshift. This is the first homogeneousoptical/X-ray sample large enough to constrain the evolution of the luminosityfunction simultaneously in redshift ($0.1<z<1.05$) and cluster mass ($13.5 \le\rm{log_{10}}(M_{200crit}) \sim< 15.0$). We pay particular attention tocompleteness issues and the detection limit of the galaxy sample. We then applya hierarchical Bayesian model to fit the cluster galaxy LFs via a Schecterfunction, including its characteristic break ($m^*$) to a faint end power-lawslope ($\alpha$). Our method enables us to avoid known issues in similaranalyses based on stacking or binning the clusters. We find weak andstatistically insignificant ($\sim 1.9 \sigma$) evolution in the faint endslope $\alpha$ versus redshift. We also find no dependence in $\alpha$ or $m^*$with the X-ray inferred cluster masses. However, the amplitude of the LF as afunction of cluster mass is constrained to $\sim 20\%$ precision. As aby-product of our algorithm, we utilize the correlation between the LF andcluster mass to provide an improved estimate of the individual cluster massesas well as the scatter in true mass given the X-ray inferred masses. Thistechnique can be applied to a larger sample of X-ray or optically selectedclusters from the Dark Energy Survey, significantly improving the sensitivityof the analysis.

Galaxies in X-ray Selected Clusters and Groups in Dark Energy Survey  Data II: Hierarchical Bayesian Modeling of the Red-Sequence Galaxy Luminosity  Function