Conversion from /C-12/O integrated intensity at 2.6 millimeter wavelength to hydrogen column density

Details Conversion from /C-12/O integrated intensity at 2.6 millimeter wavelength to hydrogen column density Conversion from /C-12/O integrated intensity at 2.6 millimeter wavelength to hydrogen column density

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...262..198l&link_type=abstract

Astrophysical Journal, Part 1, vol. 262, Nov. 1, 1982, p. 198-200.

Astronomy and Astrophysics

Astrophysics

48

Carbon Monoxide, Interstellar Matter, Interstellar Radiation, Microwave Spectra, Molecular Clouds, Molecular Spectra, Carbon 12, Milky Way Galaxy, Millimeter Waves, Proton Density (Concentration)

Scientific paper

The principal defect of CO as a probe of the interstellar medium is the uncertainty which arises in converting the observed antenna temperatures to column densities of hydrogen nuclei N(H). The full potential of carbon monoxide as a diagnostic tool can, therefore, only be realized if a better approach is found for converting the observed spectral-line parameters into quantities of H nuclei. The present investigation considers details regarding various kinds of clouds in which the (C-12)O (j=1-0) line has been observed. Diffuse clouds are considered, taking into account the line of sight toward Zeta Ophiuchi. Attention is given to 'giant molecular cloud complexes' and local dark clouds, clouds in the inner galaxy, the line of sight toward OMC-1, and extragalactic CO lines. A rule of thumb for determining N(H) is considered. In many cases this rule should provide about as good an estimate for N(H) as can be obtained, without the need for an elaborate justification of the many steps often used in a reconstruction procedure.

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