The initial gas-phase sulfur abundance in the Orion Molecular Cloud from sulfur radio recombination lines

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Volume 647 (March 2021)

A&A, 647 (2021) L7

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Table B.1.

Cnα line spectroscopic parameters obtained from a two-Gaussian line fit to C and He RRLs.

Line	Frequency	I = ∫T_MBdv^(a)	v_LSR	Δv	T_{MB, Peak}^(a)	S/N^(b)	Line	Frequency
	[GHz]	[K km s⁻¹]	[km s⁻¹]	[km s⁻¹]	[K]			[GHz]
C59α	31.23889	0.410 (0.011)	10.7 (0.1)	2.8 (0.1)	0.139	25	S59α	31.23978
C58α	32.86859	0.404 (0.009)	10.7 (0.1)	2.6 (0.1)	0.146	32	S58α	32.86953
C57α	34.61364	0.378 (0.009)	10.7 (0.1)	2.5 (0.1)	0.141	29	S57α	34.61463
C56α	36.48445	0.399 (0.011)	10.7 (0.1)	2.6 (0.1)	0.147	30	S56α	36.48550
C55α	38.49255	0.402 (0.010)	10.7 (0.1)	2.6 (0.1)	0.146	26	S55α	38.49365
C54α	40.65077	0.407 (0.013)	10.7 (0.1)	2.6 (0.1)	0.146	22	S54α	40.65193
C53α	42.97340	0.377 (0.022)	10.7 (0.1)	2.5 (0.1)	0.145	18	S53α	42.97463
C52α	45.47640	0.260 (0.012)	10.7 (0.1)	2.2 (0.1)	0.112	12	S52α	45.47770
C51α	48.17762	0.319 (0.023)	10.6 (0.1)	2.2 (0.2)	0.138	8	S51α	48.17900

Notes. The last column provides the frequencies of the Snα RRLs.

^(a)

Intensities in main beam temperature.

^(b)

S/N determined from the line emission peak at a spectral resolution of 38 kHz. Parentheses indicate the uncertainty obtained by the Gaussian fitting routine.

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