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We examine galaxy groups from the present epoch to z = 1 to explore theimpact of group dynamics on galaxy evolution. We use group catalagues from theSloan Digital Sky Survey (SDSS), the Group Environment and EvolutionCollaboration (GEEC) and the high redshift GEEC2 sample to study how theobserved member properties depend on galaxy stellar mass, group dynamical massand dynamical state of the host group. We find a strong correlation between thefraction of non-star-forming (quiescent) galaxies and galaxy stellar mass, butdo not detect a significant difference in the quiescent fraction with groupdynamical mass, within our sample halo mass range of 10^13-10^14.5 M_sun, orwith dynamical sate. However, at a redshift of approximately 0.4 we do see someevidence that the quiescent fraction in low mass galaxies (log(M_star/M_sun) <10.5) is lower in groups with substructure. Additionally, our results show thatthe fraction of groups with non-Gaussian velocity distributions increases withredshift to roughly z = 0.4, while the amount of detected substructure remainsconstant to z = 1. Based on these results, we conclude that for massivegalaxies (log(M_star/M_sun_ > 10.5), evolution is most strongly correlated tothe stellar mass of a galaxy with little or no additional effect related toeither the group dynamical mass or dynamical state. For low mass galaxies, wedo see some evidence of a correlation between the quiescent fraction and theamount of detected substructure, highlighting the need to probe further downthe stellar mass function to elucidate the role of the environment in galaxyevolution.

Do group dynamics play a role in the evolution of member galaxies?