An analysis of OH excited state absorption lines in DR 21 and K3-50

Details An analysis of OH excited state absorption lines in DR 21 and K3-50 An analysis of OH excited state absorption lines in DR 21 and K3-50

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...264..220j&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 264, no. 1, p. 220-228.

Astronomy and Astrophysics

Astrophysics

6

Absorption Spectra, H Ii Regions, Hydroxyl Radicals, Molecular Clouds, Molecular Excitation, Astronomical Spectroscopy, Emission Spectra, Molecular Energy Levels, Molecular Rotation, Turbulence Effects

Scientific paper

We present an analysis of the OH absorption line zones observed toward the compact H II regions DR 21 and K3-50. Using as parameters the kinetic and dust temperatures, the H2 number density and the ratio of OH-H2 number densities to the velocity gradient, the model quantitatively reproduces the absorption line data for the six main line transitions in 2 Pi3/2 J = 5/2, 7/2, and 9/2. Observed upper limits for the absorption or emission in the satellite lines of 2 Pi3/2 J = 5/2 are crucial in constraining the range of derived parameters. Physical conditions derived for DR 21 show that the kinetic temperature centers around 140 K, the H2 number density around 10 exp 7/cu cm, and that the OH column density in the excited state absorption zone lies between 1 x 10 exp 15/sq cm and 2 x 10 exp 15/sq cm. Including contributions from a J = 3/2 absorption zone, the total OH column density is more than a factor of 2 lower than estimates based upon LTE (Walmsley et al., 1986). The OH absorption zone in K3-50 tends toward higher density and displays a larger column density, while the kinetic temperature is similar. For both sources, the dust temperature is found to be significantly lower than the kinetic temperature.

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