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High mass proto-stars create Ultra-Compact Hii regions (UCHII) at the stageof evolution when most of the accretion is finished but the star is stillheavily embedded in molecular material. The morphologies of UCHII regionsreflect the interactions of stellar winds, stellar motions, and densitystructure in the molecular cloud; they are complex and it has been verydifficult to interpret them. We here present data obtained with TEXES on theNASA IRTF of the [NeII] emission line in the proto-cluster of young OB stars inW33 Main. The data cube has a spatial resolution of ~ 1.4 arcsec and truevelocity resolution ~ 5 km/s; with A ~ 0.02Av it is relatively unaffected byextinction. We have run 3D hydrodynamic and line profile simulations, usingPLUTO and RADMC-3D, of the gas structures created by multiple windy starsmoving relative to each other through the ambient cloud. By iterativecomparison of the data cube and the simulations, we arrive at models thatreproduce the different morphology and kinematic structure of each UCHII regionin W33 Main. The results indicate that each sub-source probably holds multipleexciting stars, permitting an improved view of the stellar population, andfinds the stellar trajectories, which may determine the dynamical developmentof the proto-cluster.

Kinematics and Structure of Ionized Gas in the UCHII Regions of W33 Main