structures in the disk plane difficult to detect. And very few galaxies have the pc-scale quality of kinematic data that we have here. However, where this data exists there is evidence for nuclear structures similar to those presented here.

The Milky Way hosts a nuclear star cluster centered on Sgr A$^*$, first noted by @becklin68. The luminosity profile of the inner $\sim$100 pc of the Milky Way is distinct from the underlying bulge and disk profiles [e.g. @serabyn96]. This component is clearly flattened along the galactic plane [axial ratio of 0.45; @catchpole90], but less so in the central 30 pc, which led @launhardt02 to propose the existence of two components, a 3$\times$10$^7$ Msol NSC dominating the central 30 pc (with $r_{eff} \sim 10$ pc) and a more massive nuclear stellar disk extending out to 100-200 pc. Numerous young OH/IR stars are found, primarily within the central 40 pc and these have a flattened distribution with rotation of $>$100 kms$^{-1}$ [@lindqvist92]. Based on integrated K-band spectra, @mcginn89 find that the central dispersion is $\sim$125 kms$^{-1}$ and drops quickly with increasing radius, while the rotation increases outwards equalling the rotation at a radius of $\sim$3 pc, the edge of their study. Compared 