represent upper limits. It is unclear whether the increased dispersion we see in the center is a result of unresolved rotation or a genuinely hot component.

The use of the templates from NIFS and GNIRS give very similar results for both the velocities and dispersions. The GNIRS templates selected for fitting the spectra are primarily at spectral types close to those (K-M giants) represented by the 3 NIFS spectra. For almost all the spectra, our measured non-Gaussian $h3$ and $h4$ components of the LOSVD were consistent with zero. However, due to our low S/N and resolution, we would not expect to be able to detect any non-Gaussian signatures [@cappellari04].

Stellar Populations and Connection to Kinematics
------------------------------------------------

From the optical data described in Paper I, the NGC 4244 NSC has two distinct stellar populations – a bluer population dominates in the midplane with a redder population dominating above and below the plane. This is clearly seen in the HST based color-map shown in the top panel of Fig. \[popfig\]. We would expect the NIFS data to resolve these different populations despite the 2$\times$ lower resolution. If we make a map of the CO line strength (bottom panel of Fig. \[popfig\]), the 