Distribution of Slow and Fast Rotators in the Fornax Cluster
  We present integral field spectroscopy of 10 early-type galaxies in the
nearby, low-mass, Fornax cluster, from which we derive spatially resolved
stellar kinematics. Based on the morphologies of their stellar velocity maps we
classify 2/10 galaxies as slow rotators, with the remaining 8 galaxies fast
rotators.
  Supplementing our integral field observations with morphological and
kinematic data from the literature, we analyse the `kinematic' type of all 30
galaxies in the Fornax cluster brighter than M_K = -21.5 mag (M_* ~ 6 x 10^9
M_sun). Our sample's slow rotator fraction within one virial radius is
7(^+4_-6) per cent. 13(^+8_-6} per cent of the early-type galaxies are slow
rotators, consistent with the observed fraction in other galaxy aggregates. The
fraction of slow rotators in Fornax varies with cluster-centric radius, rising
to 16(^+11_-8) per cent of all kinematic types within the central 0.2 virial
radii, from 0 per cent in the cluster outskirts.
  We find that, even in mass-matched samples of slow and fast rotators, slow
rotators are found preferentially at higher projected environmental density
than fast rotators. This demonstrates that dynamical friction alone cannot be
responsible for the differing distributions of slow and fast rotators. For
dynamical friction to play a significant role, slow rotators must reside in
higher mass sub-halos than fast rotators and/or form in the centres of groups
before being accreted on to the cluster.
