Abstract
Large-scale mapping and high-spectral resolution profile measurements of the vibrational H 2 v = 1-0 S(1) line are used to investigate the morphology and kinematic structure of the hot, shocked gas associated with the ultraluminous DR 21 young-stellar outflow. It is found that the H 2 line profiles at certain locations within the outflow possess high-velocity wings which extend to beyond 100 km s -1 from the DR 21 rest velocity. It is argued that the jets, which shock the surrounding molecular cloud medium and produce the bright H 2 line emission, are composed primarily of hot atomic gas which is confined by the thermal pressure of the ambient cloud medium.
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