Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...271..175b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 271, Aug. 1, 1983, p. 175-182. Research supported by the Alfred P. Sloan Fo
Astronomy and Astrophysics
Astrophysics
15
Hydrogen Clouds, Interstellar Gas, Molecular Clouds, Orion Nebula, Shock Waves, Gas Temperature, Interstellar Extinction, Spatial Distribution
Scientific paper
Observations of the spatial distribution of extinction and excitation temperature toward the molecular hydrogen emission in the Orion molecular cloud OMC-1 are presented. Most, although not all, of the observed structure in the near-infrared line intensities results from variations in the column density of vibrationally excited H2 and is not due to variable extinction or temperature. The extinction toward the center of the emission region is between 1 and 2 mag at 4712/cm, the frequency of the v = 1-0 S(1) line, but increases toward the edges. The lack of emission from the eastern part of the nebula may result from increased extinction in that direction. Variations in the extinction temperature are less than the observational uncertainties of + or - 200 K at all but one position observed. Therefore, the excitation temperature of the hydrogen molecules is probably not a strong function of either the shock velocity or the density of the gas. Observations of the v = 3-2 S(3) line in the direction of strongest emission indicate the presence of gas temperatures about 2700 K and place constraints on the column density of gas which is at higher temperature.
Beck Sara C.
Beckwith Steve
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