J = 2-1 CO observations of molecular clouds with high-velocity gas - Evidence for clumpy outflows

Details J = 2-1 CO observations of molecular clouds with high-velocity gas - Evidence for clumpy outflows J = 2-1 CO observations of molecular clouds with high-velocity gas - Evidence for clumpy outflows

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...266..321p&link_type=abstract

Astrophysical Journal, Part 1, vol. 266, Mar. 1, 1983, p. 321-330.

Astronomy and Astrophysics

Astrophysics

68

Carbon Monoxide, Electron Transitions, Interstellar Gas, Molecular Clouds, Molecular Spectra, Nebulae, Brightness Temperature, Early Stars, Line Spectra, Molecular Excitation, Vibrational Spectra

Scientific paper

Spectra are presented of the J = 2-1 and J = 1-0 transitions of (C-12)O toward seven regions where high-velocity molecular gas and vibrationally excited H2 emissions are seen. The two CO lines were observed with similar telescope beamwidths, so that the 2-1 and 1-0 transitions probe the same volume of gas. In all the sources, including Orion, the data indicate that the 2-1 CO lines are optically thick even in the high-velocity gas. In order to account for the low CO antenna temperatures observed in the line wings, the high-velocity gas can fill only a small fraction of the telescope beam. Since many of the regions of high-velocity gas are known to be extended relative to the beam, the CO emission must arise from numerous small, high-velocity condensations. This result provides possible observational support for the 'interstellar bullet' models of Norman and Silk, (1979), or for Chevalier's (1980) clumpy outflow model of Orion.

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