The Kinematic Morphology-Density Relation from the SAMI Pilot Survey
  We present the kinematic morphology-density relation in three galaxy
clusters, Abell 85, 168 and 2399, using data from the SAMI Pilot Survey. We
classify the early-type galaxies in our sample as fast or slow rotators
(FRs/SRs) according to a measured proxy for their projected specific stellar
angular momentum. We find each cluster contains both fast and slow rotators
with and average fraction of SRs in the sample of $f_{SR}=0.15\pm$0.04. We
investigate this fraction within each cluster as a function of local projected
galaxy density. For Abell 85 we find that $f_{SR}$ increases at high local
density but for Abell 168 and 2399 this trend is not seen. We find SRs not just
at the centres of our clusters but also on the outskirts and hypothesise that
these SRs may have formed in group environments eventually accreted to the
larger cluster.
