Table A.1:

CH⁺ (0-1) absorption line analysis results.

Source	Remarka				N(CH+)
		(km s-1)	(km s-1)		(1012 cm-2)
W33A		2.47 0.13	5.18 0.23	0.28 0.01	4.68 0.40
		10.08 1.17	8.38 4.55	0.03 0.01	0.95 0.66
		16.82 0.05	2.56 0.15	0.28 0.01	2.37 0.24
W49N	E	-3.62 0.06	3.63 0.13	0.18 0.01	>2.1
W51		0.91 0.05	2.21 0.12	0.18 0.01	1.26 0.13
		7.37 0.03	5.13 0.07	0.83 0.01	13.90 0.35
		13.14 0.07	2.73 0.18	0.21 0.01	1.88 0.20
		17.34 0.16	3.41 0.48	0.10 0.01	1.11 0.23
		23.44 0.06	5.83 0.15	0.35 0.01	6.56 0.28
		39.97 0.11	3.76 0.22	0.18 0.01	2.24 0.21
	E	47.16 0.47	5.25 0.55	0.84 0.09	>14.3
	E	49.32 0.06	2.40 0.27	0.94 0.16	>7.3
	E	53.97 0.11	7.26 0.15	1.94 0.03	>45.9
	E	71.56 0.03	3.73 0.07	0.48 0.01	>5.8
	remark				N(CH+)
Source		(km s-1)	(km s-1)	(km s-1)	(1012 cm-2)
W33A	E, S	20.0	45.0	>53.6	>166.5
W49N	E, S	0.0	22.0	>39.3	>122.2
	E	22.0	30.0	>13.5	>41.9
	S	30.0	49.0	>41.1	>127.6
	S	49.0	77.5	>48.1	>149.5
W51	E, S	60.0	70.0	>17.7	>54.9

Notes. The column densities are derived assuming an excitation temperature of 3 K, a lower limit for the absorption components detected at velocity intervals corresponding to the source itself. The first part of the table are the results of the multi-Gaussian decomposition procedure. The second part results from the analysis of the spectra over given velocity ranges: for the saturated features, lower limits on the column densities are inferred assuming a conservative lower limit on the optical depth of 2.3 (Neufeld et al. 2010).
^(a) E = absorption line profile observed in the star-forming region. may be underestimated, hence the lower limit on . S = saturated line profile.