Are infrared dark clouds really quiescent? | Astronomy & Astrophysics (A&A)

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Table A.2

Linewidth, the intensity integrated over the dispersion of each line (subtable I), and the integrated optical depth over the velocity dispersion of the strongest line among multiplet (subtable II).

Species	Freq.¹	G28.34 S		IRDC 18530		IRDC 18306		IRDC 18308

I. Linewidth Δυ (km s^-1) and integrated intensity in four IRDCs

	(GHz)	(km s^-1)	(K km s^-1)	(km s^-1)	(K km s^-1)	(km s^-1)	(K km s^-1)	(km s^-1)	(K km s^-1)

OCS	85.1391	3.91 ± 0.66	0.26 ± 0.04	×	×	−	≤0.05	−	≤0.06
c-C₃H₂	85.3389	2.97 ± 0.10	1.51 ± 0.05	×	×	1.99 ± 0.12	0.69 ± 0.03	1.76 ± 0.23	0.34 ± 0.04
c−CH₃C₂H⁽¹⁾	85.4557	3.08 ± 0.45	0.31 ± 0.04	×	×	2.21 ± 0.42	0.18 ± 0.03	2.81 ± 0.81	0.22 ± 0.06
c−CH₃C₂H⁽²⁾	85.4573	2.44 ± 0.42	0.26 ± 0.04	×	×	1.08 ± 0.55	0.08 ± 0.03	−	≤0.08
NH₂D	85.9263	5.92 ± 1.04	0.41 ± 0.05	2.86 ± 0.44	0.17 ± 0.02	8.95 ± 1.16	0.32 ± 0.04	7.36 ± 1.53	0.21 ± 0.04
H¹³CO⁺	86.7543	3.07 ± 0.06	1.32 ± 0.02	2.01 ± 0.06	0.55 ± 0.02	2.05 ± 0.10	0.50 ± 0.02	2.09 ± 0.09	0.59 ± 0.02
SiO	86.8470	4.83 ± 0.39	0.55 ± 0.03	−	≤0.03	−	≤0.25	−	≤0.03
HN¹³C	87.0909	2.99 ± 0.07	1.12 ± 0.02	1.71 ± 0.08	0.47 ± 0.02	2.24 ± 0.10	0.41 ± 0.02	2.08 ± 0.11	0.43 ± 0.02
HNCO	87.9244	2.68 ± 0.09	0.83 ± 0.02	1.75 ± 0.14	0.25 ± 0.02	2.13 ± 0.18	0.25 ± 0.02	2.11 ± 0.35	0.17 ± 0.02
HCO⁺	89.1885	2.44 ± 0.08	5.27 ± 0.13	3.74 ± 0.05	4.74 ± 0.05	3.11 ± 0.28	1.72 ± 0.14	3.37 ± 0.06	5.52 ± 0.08
HNC	90.6636	2.59 ± 0.05	5.57 ± 0.08	3.10 ± 0.03	4.01 ± 0.03	2.94 ± 0.12	1.85 ± 0.07	2.83 ± 0.04	3.95 ± 0.05
HC₃N	90.979	3.36 ± 0.16	0.70 ± 0.03	2.22 ± 0.23	0.20 ± 0.02	2.34 ± 0.22	0.25 ± 0.02	3.03 ± 0.87	0.14 ± 0.03
¹³CS	92.4943	3.06 ± 0.39	0.22 ± 0.02	−	≤0.03	2.28 ± 0.42	0.11 ± 0.02	−	≤0.03
H₂CO	218.222	3.73 ± 0.42	0.98 ± 0.09	−	≤0.15	−	≤0.15	−	≤0.14
C¹⁸O	219.56	3.70 ± 0.07	7.83 ± 0.13	2.42 ± 0.06	3.71 ± 0.08	1.95 ± 0.06	3.75 ± 0.10	1.94 ± 0.07	3.02 ± 0.10
¹³CO	220.399	4.83 ± 0.20	21.18 ± 0.62	3.78 ± 0.13	16.24 ± 0.47	3.11 ± 0.25	9.79 ± 0.69	2.75 ± 0.13	14.15 ± 0.63
C¹⁷O	224.714	3.72 ± 0.25	2.35 ± 0.13	×	×	2.06 ± 0.12	1.26 ± 0.07	2.61 ± 0.36	0.70 ± 0.09

II. Linewidth Δυ(km s^-1) and integrated optical depth τ₀Δυ(km s^-1) of the main line in four IRDCs

	(GHz)	(km s^-1)	(km s^-1)	(km s^-1)	(km s^-1)	(km s^-1)	(km s^-1)	(km s^-1)	(km s^-1)

N₂H⁺	93.1738	2.94 ± 0.01	1.14 ± 0.01	1.84 ± 0.04	1.20 ± 0.18	1.88 ± 0.03	1.19 ± 0.15	2.02 ± 0.02	0.20 ± 0.04
C₂H	87.3169	2.90 ± 0.07	4.00 ± 0.59	1.85 ± 0.08	0.91 ± 0.48	1.73 ± 0.07	3.10 ± 0.66	1.76 ± 0.11	0.18 ± 0.17
HCN	88.6318	2.33 ± 0.06	0.23 ± 0.10	3.23 ± 0.05	0.32 ± 0.04	2.60 ± 0.19 ∗	25.80 ± 7.50^∗	3.15 ± 0.10	2.43 ± 0.83
H¹³CN	86.3402	2.96 ± 0.12	0.54 ± 0.19	2.25 ± 0.27^∗	0.23 ± 5.61^∗	1.82 ± 0.64^∗	0.62 ± 1.77^∗	1.69 ± 0.34^∗	0.17 ± 7.08^∗

Notes. 1. Transition numbers are listed in Table A.1. 2. Values are obtained from the Gaussian/hyperfine multiplets fit program based on CLASS. 3. Uncertainties on the measured intensities are typically ≤10%. 4. For species that are not detected, an upper limit equal to the 3σ rms is given. 5. “−” denotes <3σ detection in our dataset, and the intensity upper limit comes from the 3σ rms of the entire region by integrating three channels in total around the V_lsr. 6. “ ×” denotes no observations in our dataset. 7. “^∗” denotes a hyperfine multiplet that is not well fitted.

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