to the NGC 4244 NSC, the Milky Way appears quite similar, but scaled up by $\sim$10$\times$ in mass and $\sim$3$\times$ in size, rotation, and dispersion as would be expected for a more massive galaxy. The very center ($<$1 pc) of the MW NSC has been intensively studied and shows complex dynamics with striking differences between older stars and very young ($<$10 Myr) stars. The latter show ordered rotation (and counter rotation!) and provide evidence for processes 2 [@genzel03] and 3 [e.g. @maillard04; @lu05] described above.

There is also evidence for flattening and rotation in the M33 NSC. This cluster is elongated along the major axis of the galaxy with an axial ratio of $\sim$0.85 [@lauer98; @matthews01]. At a radius of $\sim$1$\arcsec$ (4 pc), the rotation is $\sim$8 kms$^{-1}$ and dispersion is 27 kms$^{-1}$ [@gebhardt01]. Even considering that the orientation is likely not edge-on, it appears that the rotation does not dominate in the M33 NSC to the same extent as in NGC 4244.

In conclusion, we have shown above that the nuclear star cluster in NGC 4244 is rotating. The rotation is seen in both the young disk and older spheroid components, suggesting that accretion of gas or star clusters 