Large-scale mapping and high-spectral-resolution profile measurements of the vibrational H2 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 H2 line profiles at certain locations within the outflow possess high-velocity wings which extend to beyond 100 km/s from the DR 21 rest velocity. It is argued that the jets, which shock the surrounding molecular cloud medium and produce the bright H2-line emission, are composed primarily of hot atomic gas which is confined by the thermal pressure of the ambient cloud medium.
No takes yet. Share an insight, caveat, or question.
Garden et al. (1991) studied this question.