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Y. L. Shirley (Bok Fellow, University of Arizona), D. Johnstone (Herzberg Institute of Astrophysics)
Our understanding of the structure of high-mass and intermediate-mass (M > 25 solar masses) star-forming cores has been hampered by the complexity of these regions: turbulent gas linewidths, poor angular resolution due to large distances, and regions forming more than one star within a dense core. Submillimeter dust continuum is a powerful probe of the temperature, density, and dust opacity structure in the envelope of star-forming cores. We present a detailed comparison of observations of a sample of high-mass protostellar cores (HMPCs) that have been observed with SCUBA at 850 and 450 microns and SHARC (Mueller et al. 2002) and SHARCII at 350 microns. We model the long wavelength SEDs (> 70 microns) and submillimeter intensity profiles simultaneously using a 1D radiative transfer code. The robustness of the models are tested and the submillimeter properties of the HMPCs are compared to recent molecular line mapping surveys of dense gas. Modeling at three submillimeter wavelengths uniquely constrains the large scale structure of HMPCs and provides an important input for 3D models.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.