A spectroscopic study of the DR 21 outflow source. II. The vibrational H2 line emission

Journal Article · Tue Jan 01 00:00:00 EST 1991 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/169582· OSTI ID:5995292

Garden, R P; Geballe, T R; Gatley, I; Nadeau, D ^[1]

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1. California Univ., Irvine (USA) Joint Astronomy Center, Hilo, HI (USA) National Optical Astronomy Observatories, Tucson, AZ (USA) Montreal Universite, Montreal (Canada)

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. 37 refs.

• OSTI ID: 5995292
• Journal Information: Astrophysical Journal; (USA), Vol. 366; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
PROTOSTARS
MASS TRANSFER
ATOMS
COSMIC GASES
EMISSION SPECTRA
GAS FLOW
INTERSTELLAR SPACE
MAPS
MOLECULES
MORPHOLOGY
NEBULAE
PARTICLE KINEMATICS
SPECTROSCOPY
VELOCITY
FLUID FLOW
FLUIDS
GASES
SPACE
SPECTRA
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources