We discuss images of the star clusters GLIMPSE C01 ( GC01 ) and GLIMPSE C02 ( GC02 ) that were recorded with the Subaru IRCS .
Distortions in the wavefront were corrected with the RAVEN adaptive optics ( AO ) science demonstrator , allowing individual stars in the central regions of both clusters – where the fractional contamination from non-cluster objects is lowest – to be imaged .
In addition to J,H, and K ^ { \prime } images , both clusters were observed through a narrow-band filter centered near 3.05 \mu m ; GC01 was also observed through two other narrow-band filters that sample longer wavelengths .
Stars in the narrow-band images have a FWHM that is close to the telescope diffraction limit , demonstrating that open loop AO systems like RAVEN can deliver exceptional image quality .
The near-infrared color magnitude diagram of GC01 is smeared by non-uniform extinction with a 1 \sigma dispersion \Delta A _ { K } = \pm 0.13 magnitudes .
Spatial variations in A _ { K } are not related in a systematic way to location in the field .
The Red Clump is identified in the K luminosity function ( LF ) of GC01 , and a distance modulus of 13.6 is found .
The K LF of GC01 is consistent with a system that is dominated by stars with an age > 1 Gyr .
As for GC02 , the K LF is flat for K > 16 , and the absence of a sub-giant branch argues against an old age if the cluster is at a distance of \sim 7 kpc .
Archival SPITZER [ 3.6 ] and [ 4.5 ] images of the clusters are also examined , and the red giant branch-tip is identified .
It is demonstrated in the Appendix that the [ 3.6 ] surface brightness profiles of both clusters can be traced out to radii of at least 100 arcsec .