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 Å .
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 ATLAS ^ { \mathrm { 3 D } } survey , finding the slow rotator fraction is \sim 50 per cent larger in the core of the Coma cluster than in the volume-limited ATLAS ^ { \mathrm { 3 D } } sample , 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 .