The non-gaussian terms [$h3$ and $h4$, see @vandermarel93] in the LOSVD are penalized, thus the solution typically converges to a Gaussian LOSVD at low S/N. The method also compensates for any low-frequency differences between the template and galaxy spectral shape using Legendre polynomials. We fit the area of the spectrum from 22900Å to 24000Å, which is dominated by strong CO lines. We calculated errors on the LOSVD parameters using Monte Carlo tests that consisted of adding noise to the spectrum based on the measured S/N and remeasuring the LOSVD 250 times without penalizing non-Gaussian distributions. The typical standard deviation on the velocity and dispersion for pixels with S/N$\sim$25 is $\sim$3 kms$^{-1}$. When using GNIRS templates, we convolve the template spectra by a Gaussian with $\sigma=13$ kms$^{-1}$ to correct for the slightly higher resolution of the GNIRS data.

We show the radial velocity map derived using PPXF on each spectral bin in the top panel of Figure \[velfig\]. We show only data with reliable measurements by clipping bins with S/N$<$10 or errors on the velocity above 15 kms$^{-1}$. [*The radial velocity map shows strong rotation in the NGC 4244 NSC.*]{} The rotation velocities reach an amplitude of 30 kms$^{-1}$ $\sim$0.4$\arcsec$ from 