velocity and CO measurements were made using the Voronoi binned data; the symbols in these panels show the light-weighted positions of the bins coded by which slice they fell in.

The top panel of Figure \[profilefig\] shows that the rotation is not confined to the midplane, but is present $\sim$0.25$\arcsec$ above and below the midplane as well. The bottom three panels show that the slices above and below the plane are clearly sampling a different component/stellar population from the midplane. The CO lines are less deep away from the plane, while the optical color is redder. The disk fraction in the bottom panel is based on the results of our morphological descomposition from §3.1. We calculated the fraction of disk light along our slices from the best-fitting Sérsic$+$Disk model after convolving each component with the PSF. For the area above and below the major axis, only 10-20% of the light in our NIFS observations appear to be coming from the disk. Taken together, [*these plots show that the whole cluster is rotating, not just the bluer, younger disk component.*]{} This finding places strong constraints on the formation of this NSC as detailed in the following section.

Discussion & Conclusions
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