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Table A.1

Properties of APO sight-lines.

Star E(B-V) fH2 Ndet %deta Rζσb$\[\mathrm{R}_{\zeta \sigma}^{b}\]$ Typec δd N2σe %2σf
HD20041 0.72 0.42 351 63% 0.33 σ +0.5 14 4%
Cernis52 0.90 >0.78 121 21% 0.91 ζ +0.5 6 5%
HD23180 0.31 0.55 279 50% 0.63 ζ +0.5 11 4%
HD281159 0.85 0.50 369 26% 0.35 σ −0.5 0 0%
HD23512 0.36 0.62 118 21% 0.29 σ -0.7 19 16%
HD24534 0.59 0.76 226 40% 0.75 ζ 0.0 14 6%
HD24912 0.33 0.38 300 53% 0.23 σ +0.5 18 6%
HD28482 0.48 0.66 146 26% 0.26 σ +0.5 12 8%
HD37061 0.52 0.02 144 25% 0.11 σ −0.5 3 2%
HD37903 0.35 0.53 164 29% 0.15 σ 0.0 15 9%
HD43384 0.58 0.44 365 65% 0.32 σ +0.5 6 2%
HD147084 0.73 0.59 109 19% 0.42 σ +0.5 2 2%
HD147889 1.07 0.45 376 67% 0.47 ζσ 0.0 27 7%
HD148579 0.34 0.45 143 25% 0.42 σ +0.5 43 30%
HD166734 1.39 0.39 498 89% 0.42 σ 0.0 30 6%
HD168625 1.48 0.33 351 63% 0.29 σ +0.3 12 3%
HD175156 0.31 0.31 290 52% 0.57 ζ +0.3 79 27%
HD183143 1.27 0.31 472 84% 0.30 σ +0.3 9 2%
HD190603 0.72 0.16 321 57% 0.29 σ +0.5 10 3%
HD194279 1.20 0.30 343 61% 0.35 σ 0.0 2 1%
VICyg 5 1.99 0.47 469 84% 0.32 σ −0.5 2 1%
VICyg 12 3.31 >0.48 439 78% 0.37 σ −0.5 2 1%
HD204827 1.11 0.67 491 88% 0.76 ζ +0.3 30 6%
HD206267 0.53 0.42 374 67% 0.36 σ +0.3 16 4%
HD223385 0.67 0.12 275 49% 0.25 σ +0.3 14 5%

a. Percentage of detection of the 559 APO DIBs in the considered line of sight.

b. Ratio of the equivalent widths of λ5797 to λ5780 DIBs in the line of sight, that is believed to correlate well with the amount of UV radiation (e.g. Ensor et al. 2017).

c. UV-type of the sight line, inferred from the ratio Rζσ, following the definition of Fan et al. (2019), putting the limit between the σ and ζ types at Rζσ ~ 0.5. Type “ζσ” denotes a sight line intermediate between ζ and σ, as defined by Fan et al. (2022).

d. Reduced shift of the central approximate Gaussian distribution from ENav (Section 5.1 and Fig. A.1).

e. Number of DIBs whose EN exceeds the centre of the approximate Gaussian distribution by more than 2σEN.

f. Percentage of DIBs whose EN exceeds the centre of the approximate Gaussian distribution by more than 2σEN.

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