that the stellar populations at any point in the cluster are clearly mixed and thus information determined from comparing the observations to single-stellar population models should be viewed with caution. With the maturing of NIR stellar models and spectral libraries [e.g. @lancon07; @marmolqueralto08], future population synthesis studies may be able to provide more robust results on the resolved star formation history from this type of data. Lastly, we note that it is possible for thermal emission from warm dust to reduce the strength of the CO absorption. However, the low star formation activity in the NSC indicated by the lack of NIR emission lines suggests that dust emission probably does not play a large role in this cluster.

We now turn to the relation between the stellar populations and the rotation. Figure \[profilefig\] shows the derived velocity, CO line strength, optical color, and disk fraction of the NGC 4244 NSC as function of position in slices along, above, and below the major axis. The slices are each 0.25$\arcsec$ in height, and the plotted lines are the result of averaging the maps (i.e. Fig. \[velfig\] and \[popfig\]) along the vertical direction in each slice at every pixel along the x-direction. The 