clusters distributed in a spheroidal distribution no rotation would be expected. Thus the primary formation mechanism must be through episodic accretion of material from the disk of the galaxy, either gas or young star clusters. Distinguishing between gas and star cluster accretion may be possible through comparison of our kinematic data with simulations. Direct evidence of gas accretion into the central $\sim$10 parsecs is seen in a couple nearby nuclear star clusters using CO observations [@schinnerer03; @schinnerer06].

There is substantial evidence that the structure we see in NGC 4244 is not unique, and in fact may be typical for NSCs in spiral galaxies. In Paper I, 5/9 NSCs in edge-on spirals were significantly flattened along the major axis of the galaxy disk, with three showing clear composite morphologies. NGC 4244 is the nearest of these galaxies and thus presents the clearest view of these structures. There is also evidence for similar structures in earlier type galaxies; @balcells07 find a number of disky “nuclear extended components” with scale lengths as small as 5 pc in a sample of early-type spirals and elliptical galaxies. Previous studies of nuclei in large samples of spirals [@boker02; @carollo02] have focused on face-on galaxies making the 