the nucleus. Assuming a Keplerian disk, this rotation suggests a mass of 1.7$\times$10$^6$ solar masses enclosed within the central 8 pc. Beyond this radius, there is some suggestion the velocity may drop, however due to the low S/N at large radii this result is not robust.

Based on the morphological results presented in the previous section, the NSC dominates the mass in the center of NGC 4244, and thus is likely to be kinematically distinct from the rotation of the overall galaxy disk. @olling96 has presented a study of the HI rotation curve of NGC 4244 with resolution as high as 10$\arcsec
\times$20$\arcsec$. The HI gas rotates in the same direction as the NGC 4244 NSC. The innermost point in their derived rotation curve is at 24$\arcsec$ where the galaxy rotation is 35 kms$^{-1}$, increasing to 60 kms$^{-1}$ at 47$\arcsec$. Given that we observe rotation of $\sim$30 kms$^{-1}$ within the central half-arcsecond, this suggests that the rotation of the NSC is distinct from the gas component of the galaxy disk. It would be interesting to compare the NSC rotation to the stellar rotation in the galaxy disk, however, this would require relatively deep long-slit spectroscopy [e.g. @yoachim08a] since the surface 