  As a demonstration of the capabilities of the new Oxford SWIFT integral field
spectrograph, we present first observations for a set of 14 early-type galaxies
in the core of the Coma cluster. Our data consist of I- and z-band spatially
resolved spectroscopy obtained with the Oxford SWIFT spectrograph, combined
with r-band photometry from the SDSS archive for 14 early- type galaxies. We
derive spatially resolved kinematics for all objects from observations of the
calcium triplet absorption features at \sim 8500 {AA} . Using this kinematic
information we classify galaxies as either Fast Rotators or Slow Rotators. We
compare the fraction of fast and slow rotators in our sample, representing the
densest environment in the nearby Universe, to results from the ATLAS3D survey,
finding the slow rotator fraction is \sim 50 per cent larger in the core of the
Coma cluster than in the Virgo cluster or field, a 1.2 {\sigma} increase given
our selection criteria. Comparing our sample to the Virgo cluster core only
(which is 24 times less dense than the Coma core) we find no evidence of an
increase in the slow rotator fraction. Combining measurements of the effective
velocity dispersion {\sigma_e} with the photometric data we determine the
Fundamental Plane for our sample of galaxies. We find the use of the average
velocity dispersion within 1 effective radius, {\sigma_e}, reduces the
residuals by 13 per cent with respect to comparable studies using central
velocity dispersions, consistent with other recent integral field Fundamental
Plane determinations.
