The DCO/+/ to HCO/+/ abundance ratio and the electron density in cool interstellar clouds

Details The DCO/+/ to HCO/+/ abundance ratio and the electron density in cool interstellar clouds The DCO/+/ to HCO/+/ abundance ratio and the electron density in cool interstellar clouds

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...222l.145w&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 222, June 15, 1978, p. L145-L147.

Astronomy and Astrophysics

Astrophysics

45

Abundance, Deuterium Compounds, Electron Density (Concentration), Hydrogen Compounds, Interstellar Gas, Molecular Ions, Carbon Monoxide, Emission Spectra, Gas Temperature, Interstellar Chemistry, Line Spectra, Nebulae, Stellar Evolution

Scientific paper

The J = 1-0 transition of H(C-13)O(+) has been detected in L134 at one-third the level (integrated antenna temperatures) of D(C-12)O(+). Scaling of the DCO(+)/H(C-13)O(+) abundance ratio and high-resolution studies of line profiles provide more reliable information than previously available about the abundance of DCO(+) and H12CO(+) in the representative dark cloud L134. These data imply that low relative abundances for electrons, CO, and N2 do in fact occur, though the present more firm upper limits are somewhat higher than those derived by certain previous investigators. Since the H(C-13)O(+) intensity is also one-seventh the level of H(C-12)O(+) and the actual C-13/C-12 abundance ratio is quite unlikely to be so large, emission by the more abundant species is apparently reduced by optical-depth effects. This casts doubt on the general validity of the premise that the DCO(+)H(C-12)O(+) abundance ratio in cool interstellar clouds can be derived by assuming that it is essentially the same as that which would be derived in the optically thin case.

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