|AUTHORS: Frank Varosi1, Daniel Y. Gezari2, Charles Telesco1, Eli Dwek2|
INSTITUTIONS: 1. Astronomy, University of Florida, Gainesville, FL, United States. 2. Astronomy, NASA Goddard Space Flight Center, Greenbelt, MD, United States.
We analyze multi-wavelength images of the central parsec of the Galactic Center using a Line-Of-Sight (LOS) radiative transfer model to infer the dust temperatures and column densities at each pixel of the images, giving maps of temperatures and opacities of the warm, cool, and dark dust components. The data consists of images at seven wavelengths in the mid-infrared (N-band and Q-band) from the T-ReCS instrument at Gemini South, and also 31.5 um and 37.7 um images from the KWIC instrument on the KAO. The results of the LOS modeling indicate that the extinction optical depth is quite large and varies substantially over the FOV. The LOS distribution of cool dust relative to warm dust is also inferred from the modelling. We propose that most of the extinction is near the galactic center, and the large column densities of dust and gas together with clumpiness suggest that the region has or will form many stars. The two temperatures of emitting dust produce high Luminosities, and simple modelling shows that the heating is produced by the embedded stars and distributed HeI stars. We also compare the distribution of dust temperatures, opacities and Luminosities with previous studies.