CLOUD STRUCTURE AND PHYSICAL CONDITIONS IN STAR-FORMING REGIONS FROM OPTICAL OBSERVATIONS. II. ANALYSIS

To complement the optical absorption line survey of diffuse molecular gas in Paper I, we obtained and analyzed far-ultraviolet H2 and CO data on lines of sight toward stars in Cep OB2 and Cep OB3. Possible correlations between column densities of different species for individual velocity components, not total columns along a line of sight as in the past, were examined and were interpreted in terms of cloud structure. The analysis reveals that there are two kinds of CH in diffuse molecular gas: CN-like CH and CH+-like CH. Evidence is provided that CO is also associated with CN in diffuse molecular clouds. Different species are distributed according to gas density in the diffuse molecular gas. Both calcium and potassium may be depleted onto grains in high-density gas, but with dif-ferent dependencies on local gas density. Gas densities for components where CNwas detected were inferred from a chemical model. Analysis of cloud structure indicates that our data are generally consistent with the large-scale structure suggested by maps of CO millimeter-wave emission. On small scales, the gas density is seen to vary by factors greater than 5.0 over scales of10,000 AU. The relationships between column densities of CO and CHwith that of H2 along a line of sight show similar slopes for the gas toward Cep OB2 and Cep OB3, but the CO/H2 and CH/H2 ratios tend to differ, which we ascribe to variation in average density along the line of sight