A comparative study of H2CO, OH, and H I in the dark Taurus dust cloud

Details A comparative study of H2CO, OH, and H I in the dark Taurus dust cloud A comparative study of H2CO, OH, and H I in the dark Taurus dust cloud

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...199..361h&link_type=abstract

Astrophysical Journal, vol. 199, July 15, 1975, pt. 1, p. 361-378. NSF-supported research.

Astronomy and Astrophysics

Astrophysics

30

Cosmic Dust, Emission Spectra, Interstellar Matter, Nebulae, Radio Emission, Radio Spectra, Abundance, Astronomical Spectroscopy, Formaldehyde, Graphs (Charts), Hydrogen Atoms, Hydroxyl Emission, Line Spectra, Molecular Excitation, Molecular Spectra, Spectral Line Width, Spectrum Analysis, Taurus Constellation, Velocity Distribution

Scientific paper

Results are reported for analysis of high-sensitivity radio-emission spectra of H2CO, OH, and H I obtained with the same angular resolution in the dark dust cloud in Taurus. Three velocity components are determined at some positions, and the correlation between the H I and molecular profiles suggests that much of the H I lies outside the region containing the molecules. Two extreme interpretations are considered for the widely varying relative intensities of the molecular lines: a constant H2CO excitation temperature within the cloud and a constant value for the OH/H2CO density ratio. The former interpretation is shown to lead to large variations of the OH/H2CO density ratio at different points within the cloud, while the latter results in a correlation of the OH and H2CO excitation temperatures, which is a natural result of collisional excitation of both molecules. Only one case is found of an anomalous OH line-intensity ratio, but this is attributed to either erroneous observational data, a very high kinetic temperature in this region, or a weak OH maser.

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