Fine-structure line deficit in S 140 | Astronomy & Astrophysics (A&A)

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Table 1

Parameters of the GREAT line observations.

Species	Transition	ν₀	E_up	n_crit^a	Beam FWHM	η_mb	Δv	σ_i,rms^b	σ_map,rms^c
		[MHz]	[K]	[cm^-3]	[arcsec]		[ km s^-1]	[K]	[K]


C⁺	[C ii]	1 900 536.90	91.21	3 × 10³	14.1	0.67	0.3	3.7	0.8−1.2
O	[O i]	4 744 777.49	227.71	5 × 10⁵	6.6	0.67	0.4	3.2	1.3−1.9
CO	13−12	1 496 922.91	503.10	1 × 10⁶	18.6	0.70	0.3	1.9	0.9−1.3
	16−15	1 841 345.51	751.70	2 × 10⁶	14.5	0.69	0.4	2.9	0.7−1.0

Notes.

^(a)

Collision rates from Wiesenfeld & Goldsmith (2014), Jaquet et al. (1992), Yang et al. (2010, at 50K). For optically thick lines the effective critical densities can be considerably lower due to radiative trapping.

^(b)

Noise in individual spectra.

^(c)

Noise in Nyquist-sampled map with GREAT beam full width at half maximum (FWHM).

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