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We examine the kinematic morphology of early-type galaxies (ETGs) in threegalaxy clusters Abell 85, 168 and 2399. Using data from the Sydney-AAOMulti-object Integral field spectrograph (SAMI) we measured spatially-resolvedkinematics for 79 ETGs in these clusters. We calculate $\lambda_{R}$, a proxyfor the projected specific stellar angular momentum, for each galaxy andclassify the 79 ETGs in our samples as fast or slow rotators. We calculate thefraction of slow rotators in the ETG populations ($f_{SR}$) of the clusters tobe $0.21\pm0.08$, $0.08\pm0.08$ and $0.12\pm0.06$ for Abell 85, 168 and 2399respectively, with an overall fraction of $0.15\pm0.04$. These numbers arebroadly consistent with the values found in the literature, confirming recentwork asserting that the fraction of slow rotators in the ETG population isconstant across many orders of magnitude in global environment.  We examine the distribution of kinematic classes in each cluster as afunction of environment using the projected density of galaxies: the kinematicmorphology-density relation. We find that in Abell 85 $f_{SR}$ increases inhigher density regions but in Abell 168 and Abell 2399 this trend is not seen.We examine the differences between the individual clusters to explain this. Inaddition, we find slow rotators on the outskirts of two of the clustersstudied, Abell 85 and 2399. These galaxies reside in intermediate to lowdensity regions and have clearly not formed at the centre of a clusterenvironment. We hypothesise that they formed at the centres of groups and arefalling into the clusters for the first time.

The SAMI Pilot Survey: The Kinematic Morphology-Density Relation in Abell 85, Abell 168 and Abell 2399