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R. Indebetouw (University of Virginia), Y. Shirley (University of Arizona), B A Whitney (Space Science Institute), B. Babler, M. Meade (University of Wisconsin), C Watson (Manchester College), M. Wolfire (University of Maryland), M. Wolff (Space Science Institute)
Massive stars dominate the evolution of galaxies and their interstellar matter, yet their formation is poorly understood. High-mass protostellar objects (HMPOs) are heavily embedded and short-lived, so extensive observational investigation has had to wait for technology to enable efficient infrared surveys.
We analyze a sample of HMPOs with multiwavelength imaging: NIR from the 2MASS survey, 3-8um from the Galactic Lecacy Infrared MidPlane Survey Extraordinaire (GLIMPSE), and 450 and 850um using SCUBA. Spherical models with fairly large radial density gradients (power-law indices >2) have previously been used to model submm radial intensity profiles and the submm part of the SED. 1-D models are inadequate at shorter wavelengths at which disk geometry and scattered light can have significant effects on the emergent radiation. We have recently used 3D models with clumpy envelopes and fairly flat average radial density profiles to model SEDs of embedded high-mass stars (Indebetouw et al ApJ in press). Here, we use our 3D clumpy models to fit both the SED and multiwavelength spatial intensity profiles.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.