Table 5
Ratios W(DIB, 5797 Å)/W(DIB, 5780 Å).
| LOS | W(DIB, 5780 Å) (mÅ) | W(DIB, 5797 Å) (mÅ) | Ratio |
|---|---|---|---|
| BD+31°643 | 314 ± 4 | 96.0 ± 4 | 0.31 ± 0.01 |
| Cyg OB2 3 | 841 ± 4 | 177 ± 5 | 0.210 ± 0.006 |
| Cyg OB2 5 | 731 ± 5 | 185 ± 6 | 0.253 ± 0.008 |
| HD 23180 | 93 ± 2 | 63 ± 3 | 0.68 ± 0.03 |
| HD 24432 | 352 ± 3 | 112 ± 4 | 0.32 ± 0.01 |
| HD 37022 | 76 ± 2 | ≤3.1 ± 0.5 | ≤0.041 ± 0.007 |
| HD 41690 | 325 ± 4 | 98 ± 4 | 0.30 ± 0.01 |
| HD 183143 | 736 ± 3 | 189 ± 5 | 0.257 ± 0.007 |
Notes. Present ratios are in agreement with those derived from equivalent widths reported by Friedman et al. (2011) and Fan et al. (2017) in spectra of Cyg OB2 5, HD 23180, HD 37022, and HD 183143; by Désert et al. (1995) in those of BD+31°643 and HD 183143; by Snow et al. (1994) and Galazutdinov et al. (2011) for BD+31°643, as HD 281159 in the latter study; and by Smoker et al. (2023) for HD 183143. We remark that ratios derived with equivalent widths reported by Thorburn et al. (2003) for BD+31°643 (as HD 281159), Cyg OB2 5, HD 23180, and HD 183143 are about 20–50% greater than ours. Finally, ratios are in agreement with those derived from equivalent widths reported by Sonnentrucker et al. (1997) for Cyg OB2 5 (as BD+40°4220) and HD 183143, whereas they differ for HD 23180 and HD 37022, though they show the same trend.
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