Using Gemini QuickStart infrared observations of the central 22 ^ { \prime \prime } of M33 , we analyze the stellar populations in this controversial region .
Based on the slope of the giant branch we estimate the mean metallicity to be -0.26 \pm 0.27 , and from the luminosities of the most luminous stars , we estimate that there were two bursts of star formation \sim 2 and \sim 0.5 Gyr ago .
We show that the stellar luminosity function not only has a different bright end cutoff , but also a significantly different slope than that of the Galactic bulge , and suggest that this difference is due to the young stellar component in M33 .
We combine our infrared Gemini data with optical HST-WFPC2 measurements revealing a CMD populated with young , intermediate , and old age stellar populations .
Using surface brightness profiles from 0.1 ^ { \prime \prime } to 18 ^ { \prime } , we perform simple decompositions and show that the data are best fit by a three-component , core + bulge + disk model .
Finally , we find no evidence for radial variations of the stellar populations in the inner 3 - 10 ^ { \prime \prime } of M33 based on a spatial analysis of the color-magnitude diagrams and luminosity functions .