to that seen in the models of @maraston05, which also include contributions from thermally pulsing AGB stars, but differs from earlier models that don’t include this phase and thus are lacking the second peak in CO depth [e.g. @leitherer99].

We can use these models to qualitatively analyze the variations in stellar population seen across the cluster in Figs. \[popfig\] and \[profilefig\]. The extinction is not well known, however spectroscopic fits suggest an $A_V \sim 0.5$ corresponding to a reddening of $\sim$0.2 magnitudes in the F606W-F814W color. For the youngest stars, we expect a metallicity of Z$\sim$0.008 based on the 100 kms$^{-1}$ circular velocity of NGC 4244 [@garnett02]. However, the combination of the red color and low CO values above and below the midplane of the cluster suggest an old ($\gtrsim$1 Gyr), more metal-poor population. Along the major axis there is a slight reddening in the optical color along with an increase in the CO line strength. One possible explanation for this is an age gradient within the disk; for instance if the center had an age of $\sim$100 Myr years then the redder colors and deeper CO could result from slightly older or younger populations at 5-10 pc. We caution 