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We establish correlations between equivalent widths of eight diffuseinterstellar bands (DIBs), and examine their correlations with atomic hydrogen,molecular hydrogen, and EB-V . The DIBs are centered at \lambda\lambda 5780.5,6204.5, 6283.8, 6196.0, 6613.6, 5705.1, 5797.1, and 5487.7, in decreasing orderof Pearson\^as correlation coefficient with N(H) (here defined as the columndensity of neutral hydrogen), ranging from 0.96 to 0.82. We find the equivalentwidth of \lambda 5780.5 is better correlated with column densities of H thanwith E(B-V) or H2, confirming earlier results based on smaller datasets. Weshow the same is true for six of the seven other DIBs presented here. Despitethis similarity, the eight strong DIBs chosen are not well enough correlatedwith each other to suggest they come from the same carrier. We further concludethat these eight DIBs are more likely to be associated with H than with H2, andhence are not preferentially located in the densest, most UV shielded parts ofinterstellar clouds. We suggest they arise from different molecules found indiffuse H regions with very little H (molecular fraction f<0.01). Of the 133stars with available data in our study, there are three with significantlyweaker \lambda 5780.5 than our mean H-5780.5 relationship, all of which are inregions of high radiation fields, as previously noted by Herbig. Thecorrelations will be useful in deriving interstellar parameters when directmethods are not available. For instance, with care, the value of N(H) can bederived from W{\lambda}(5780.5).

Studies of Diffuse Interstellar Bands. V. Pairwise Correlations of Eight Strong DIBs and Neutral Hydrogen, Molecular Hydrogen, and Color Excess