Notes. The provided interstellar extinction A_V^† (integrated up to the median distance) is obtained from the 1.25-kpc extinction map from Edenhofer et al. (2024), and thus provides only limited information about the extinction along the line of sight towards more distant stars – such cases are marked with an asterisk. The same extinction map was also used to provide a lower estimate for the number of prominent foreground clouds. We define small (0), intermediate (1), and large (2) FWHM values using the ranges of med(FWHM) ≤ 19.5 km s⁻¹, 19.5 km s⁻¹ < med(FWHM) < 26.0 km s⁻¹, and med(FWHM) ≥ 26.0 km s⁻¹, respectively. We consider the variation of the FWHM within an area in the sky to be small if std(FWHM) < 1.0 km s⁻¹, and minimal if also the number of observed targets is ≥ 5. Atomic (K I, Na I) or molecular (CH^*) line is considered to be splitting if the number of distinguished (no significant blending) kinematic components is two, or higher. An apparent gradient in the FWHM across the sky is noted when the object, either alone or in combination with other objects in the region, exhibits this characteristic. The line of sight classification is based on the prototype cases: USco (intermediate FWHM, no clear line splitting), Perseus (small FWHM, typically no splitting), and Eagle (typically intermediate-to-large FWHM, distinguished splitting). In case of NGC 6475, the variation decreases if two outlying measurements are excluded from the calculation. HD 110432 and stars in the direction of Chamaeleon at distances > 1 kpc show signs of splitting, although the measured DIB profile widths are as narrow as in the case of Perseus (except for HD 109867). Three of the targets (HD 92607, HD 93222, and HD 303135) in the Carina Nebula (S) show signs of splitting, making the classification of this object uncertain (USco-type or Eagle-type). Possible splitting can also be noted in Orion, specifically towards HD 37903 (K I line).