Comparison between [CII] (filled light gray), [CI](1–0) (gray), and C¹⁸O(1–0) (black) line profiles for all positions in Table 1. Relative intensities among the spectra have been scaled for display purposes. The observations trace different phases of the ISM from ionized, neutral, and molecular gas. Narrow and strong emission and absorption features in the C¹⁸ O(1–0) optically thin line common to all positions are marked with vertical dotted lines as they are most likely foreground components located in the Galactic disk somewhere along the LOS and outside the GC.