The chemistry and spatial distribution of small hydrocarbons in UV-irradiated molecular clouds: the Orion Bar PDR

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This article has an erratum: [https://doi.org/10.1051/0004-6361/201424568e]

Table 3

Line intensities of the detected C₂H N = 1 → 0 lines.

Transition	^a	^b	Relative I^c [x100]

		[K]	LTE^d	Obs.^e

(3 / 2,1) → (1 / 2,1)	0.17	0.14	4.25	4.20
(3 / 2,2) → (1 / 2,1)	1.67	1.39	41.72	41.91
(3 / 2,1) → (1 / 2,0)	0.83	0.69	20.73	20.73
(1 / 2,1) → (1 / 2,1)	0.83	0.68	20.73	20.56
(1 / 2,0) → (1 / 2,1)	0.33	0.28	8.32	8.42
(1 / 2,1) → (1 / 2,0)	0.17	0.14	4.25	4.19

Notes.

^(a)

Theoretical line strengths.

^(b)

Observed line intensities in mean beam temperature.

^(c)

Relative intensities.

^(d)

Expected relative intensities (S_ij/∑ S_ij), assuming that lines are optically thin (τ< 1).

^(e)

Observed relative intensity (T_{MB_ij}/∑ T_{MB_ij}).

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