Revised time-dependent models of the ion-molecule chemistry of dense interstellar clouds (Graedel, Langer, and Frerking, 1982) are used to calculate the abundances of key observational species used to interpret cloud properties and study interstellar chemistry. Consideration is given to nitrogen-, oxygen-, and carbon-bearing molecules and isotopic ratios over a hydrogen density range of 1,000-50,000/cu cm and a temperature range of 10-40 K. The results for over 15 species, including C-13 variants, are presented in tables and graphs. The results are compared to abundance observations in TMC-1 and other interstellar clouds, showing that most observed abundances can be predicted by the models.
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Langer et al. (1989) studied this question.