On the conversion of carbon monoxide intensities to molecular hydrogen abundances

Details On the conversion of carbon monoxide intensities to molecular hydrogen abundances On the conversion of carbon monoxide intensities to molecular hydrogen abundances

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...291..188k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 1, 1985, p. 188-201. Research supported by the Dudley Observator

Statistics

Computation

74

Abundance, Carbon Monoxide, Hydrogen Clouds, Interstellar Gas, Molecular Clouds, Astronomical Models, Computational Astrophysics, Gas Temperature, Line Spectra, Milky Way Galaxy, Spectral Energy Distribution, Temperature Dependence, Virial Theorem

Scientific paper

The study of interstellar molecular clouds involves frequently the problem of a determination of the molecular hydrogen (H2) content of various clouds. However, H2 is generally not observable from the ground. For this reason, information on H2 is commonly obtained on the basis of an observation of trace molecules, such as carbon monoxide (CO), and a conversion of the CO data into H2 data. Difficulties of such an approach are related to the necessity of an establishment of appropriate conversion factors. To date all studies regarding the CO to H2 conversion are empirical in approach. The present investigation provides results of theoretical cloud modelling with the objective to furnish a basis for guiding empirical decisions on the conversion of CO to H2. A cloud model with known input parameters is used to simulate CO and (C-13)O observations.

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