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We investigate the stellar populations of galaxies in clusters at differentdynamical stages, aiming to identify possible effects of the relaxation stateof the cluster or subcluster on the star formation histories of its galaxies.We have developed and applied a code for kinematic substructure detection to asample of 412 galaxy clusters drawn from the \citet[]{tempel2012} catalogue,finding a frequency of substructures of 45\%. We have extracted mean stellarages with the {\sc{starlight}} spectral synthesis code applied to SDSS-IIIspectra of the sample galaxies. We found lower mean stellar ages in unrelaxedclusters relative to relaxed clusters. For unrelaxed clusters, we separatedprimary and secondary subhalos and found that, while relaxed clusters andprimaries present similar masses and age distributions, secondaries presentyounger stellar populations, mainly due to low-mass galaxies ($\logM_\star/M_\odot \lesssim 11$\,dex). An age-clustercentric radius relation isseen for all subhalos irrespective of the presence of substructures. We alsoobserve relations between the mean stellar age and mass of relaxed andunrelaxed clusters, massive systems presenting higher mean ages. The locus ofthese relations is distinct between relaxed and unrelaxed clusters, but becomeindistinguishable when separating primaries and secondaries. Our resultssuggest that differences between relaxed and unrelaxed clusters are mainlydriven by low-mass systems in the clusters outskirts, and that, whilepre-processing can be seen in the subcomponents of dynamically young clusters,some evolution in the stellar populations must occur during the clustersrelaxation.

The dynamic stage of clusters and its influence on the stellar populations of galaxies