Notes. Forthe integrated flux density and other information on the H42α line, see Bendo et al. (2016). ^(a)Approximate flux densities for the blue- and redshifted line peaks, obtained from the 15 m SEST (Wang et al. 2004) and ALMA. Uncertainties in the ALMA data are ≈5–10 mJy from the noise level and 10% of the flux density from the calibration, while differences in the chosen area (≫10 arcsec) do not lead to significant changes. For the SEST, rms uncertainties are of order 40 mJy (c-C₃ H₂), 12 mJy (H¹³ CN/HC¹⁵N), 150 mJy (HCN), and 100 mJy (CS). As indicated by a question mark, the SEST detected HC¹⁵ N only tentatively. HCO provides a quartet of hyperfine components among which the strongest feature is seen by ALMA. ^(b) From Gaussian fits (see Wang et al. 2004 for the SEST data). ^(c)For the weak lines, it is not clear whether absorption is not observed because of a signal-to-noise ratio (S/N) that is too low or whether it is truly absent. In the case of HC¹⁵N, which has two more abundant isotopologues showing weak absorption in a specific velocity interval and because HC¹⁵ N is not seen within exactly this velocity range, absorption is likely present.