Interstellar extinction in the vicinity of the Galactic center

We present J (1.2 mum), H (1.6 mum), K' (2.11 mum), and Bry (2.166 mum) ima ges from four large regions within the central 40 pc of the Galaxy. Localiz ed variations in the extinction, as determined by observations of the stell ar population, are examined using the median H-K' color as a function of po sition within each region. As the value of the derived extinction from the stars is dependent upon the intrinsic magnitude of the assumed stellar type , the J-H versus H-K' diagrams are first used to investigate the distributi on of stellar types in the four regions, We find that there is a distinct O B population, contrary to earlier assumptions, with the ratio of K and M gi ants and supergiants to OB stars approximately twice that of the solar neig hborhood. Although on the scale of similar to1' fluctuations in the extinct ion are on the order of A(V) similar to 2, throughout the entire region the extinction varies from A(V) greater than or similar to 25 to A(V) less tha n or similar to 40. We also examine whether there is any variation in the e xtinction and stellar number density relative to the unusual radio features in these regions and do not find a significant correlation. Spectral imagi ng in Bry 2.166 mum emission shows a strong morphological correspondence be tween the 6 cm radio images and the diffuse Bry emission. By comparing the theoretical Bry flux derived from the radio flux using recombination theory with our measured Bry flux, we obtain a second, independent, estimate of t he extinction. We compare the two data sets and find that the extinction as derived from the stars is consistently greater, sometimes by a factor of 2 , than the value of the extinction derived from the Bry images. The derived extinction in various regions, however, is insufficient for any of these r egions to be located behind the molecular clouds as previously observed in the Galactic center, consistent with the theory that the observed radio emi ssion is produced on the foreground surface of these clouds.