is done using flux ratioed spectra. In order to achieve a reasonable S/N for analysis of the outer parts of the cluster, the data were spatially binned using the Voronoi tesselation method described in [@cappellari03]. The S/N of each pixel was determined empirically using a relatively featureless portion of the spectra between 22140 and 22866Å. Individual pixels near the center of the image have S/N$>$50 per pixel. We binned pixels together in order to obtain a S/N$\sim$25 in each bin, so near the center, the ’bins’ consisted of a single pixel. We found that the S/N did not increase as expected with binning (at least in part due to spectral rebinning during the initial reduction), thus the outer bins have S/N of $<$10.

We also reconstructed a calibrated K-band image of the nuclear star cluster for the morphological analysis presented in §3.1. To do this, we first multiplied the spectra by a 9500K black body to correct for the division by the A0 telluric calibrator, and then multiplied this spectrum by the 2MASS $K_s$ filter response curve before collapsing the data cube to an image. We then calibrated the zeropoint of this image by comparing the flux from the best 