brightness of the galaxy beyond the nuclear star cluster is quite low.

The line-of-sight velocity dispersion is a somewhat more difficult quantity to measure accurately due to the low dispersion of the cluster as a whole. Our spectra have 2.1Å/28 kms$^{-1}$ pixels and 4.1Å/53 kms$^{-1}$ resolution (FWHM), while the dispersions of NSCs in late-type galaxies are typically $\sim$25 kms$^{-1}$ [@walcher05]. Nonetheless, we are able to make an accurate measurement of the central dispersion of the cluster, $\sigma =
28\pm2$ kms$^{-1}$. Convolution of the templates with this dispersion substantially (by a factor of 2) improves the $\chi^2$ of their fit to the central spectrum of the cluster, giving a reduced $\chi^2$ of 0.9 and 1.1 using the GNIRS and NIFS templates respectively. The bottom panel of Fig. \[velfig\] shows a map after clipping data with S/N$<$15 or errors in the dispersion $>$10 kms$^{-1}$. The velocity dispersion drops along the major axis to to values of 10-20 kms$^{-1}$ at precisely the area where rotation is seen most strongly indicating that we are indeed seeing a relatively cold rotating disk. This dispersion is close to the limit of what we can reliably recover from our relatively low resolution observations, thus these values may 