  We study the dependence of satellite star formation rate and morphology on
group dynamics for a sample of SDSS groups. We classify the group dynamical
state and study satellite properties for populations of galaxies at small and
large group-centric radii. For galaxies at large radii we find no differences
in the star-forming or disc fraction for those in Gaussian groups compared to
those in non-Gaussian groups. By comparing the star-forming and disc fractions
of infalling galaxies to field galaxies we find evidence for the pre-processing
of both star formation rate and morphology. The strength of pre-processing
increases with halo mass and is highest for low-mass galaxies infalling onto
high-mass haloes. We show that the star formation rate of galaxies at small
radii correlates with group dynamical state, with galaxies in non- Gaussian
groups showing enhanced star-forming fractions compared to galaxies in Gaussian
groups. Similar correlations are not seen for the disc fractions of galaxies at
small radii. This seems to suggest that either the mechanisms driving star
formation quenching at small halo-centric radii are more efficient in
dynamically relaxed groups, or that non-Gaussian groups have assembled more
recently and therefore satellites of the groups will have been exposed to these
transforming mechanisms for less time.
