High angular resolution J,H,K, and L ^ { \prime } images are used to investigate the stellar content within 6 arcsec of SgrA* .
The data , which are complete to K \sim 16 , are the deepest multicolor observations of this region published to date .
The mean locus of the ( K,H - K ) CMD varies across the field , a result that is attributed to differential reddening with amplitude \Delta A _ { V } \sim 15 mag .
The reddening variations within 3 arcsec of SgrA* are significantly smaller than this , and the resolved members of the compact star cluster immediately surrounding SgrA* have photometric properties that are not significantly different from objects at larger radii .
We find that sources in our field with published 2 \mu m spectra showing either line emission or CO absorption occupy different sequences on the ( K,J - K ) CMD .
The emission line stars , which fall along the most richly populated sequence , have redder J - K colors than stars in the Magellanic Clouds with similar spectroscopic characteristics , and evidence is presented that this is due to excess infrared emission in the spectrum of the GC sources .

The photometric properties of the giant branch , which is defined by stars showing CO absorption , are similar to those of the giant branch in Baade ’ s Window ( BW ) .
The mean J - K color and peak K brightness of the red giant branch are both consistent with a metal-rich population having an age \sim 10 Gyr , while the width of the giant branch on the ( K,J - K ) CMD is indicative of an age spread \Delta log ( t ) \leq 1 dex .
Therefore , if the inner bulge contains an underlying population of stars with ages in excess of \sim 10 Gyr , as is the case in BW , then the region within a few arcsec of SgrA* can not contain a large population of giant branch stars younger than 1 Gyr .
We also report the detection of a modest population of faint , blue sources with K \geq 14 .
We speculate that these are bright main sequence stars at the distance of the GC , although spectra will be required to confirm this interpretation .
Nevertheless , the photometric properties of the largely unresolved compact knot of stars immediately surrounding SgrA* provide indirect evidence to support the presence of a large population of faint blue stars .
In particular , we confirm previous studies that measure a relatively blue color for this cluster .