Star formation in Chamaeleon I and III: a molecular line study of the starless core population

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Table 11

Linewidths and non-thermal velocity dispersions in Cha I and III.

Line	Cha I^a					Cha III

	FWHM ^b	FWHM ^c	^d	^e	N ^f	FWHM ^b	FWHM ^c	^d	^e	N ^f
	average	median	average	median		average	median	average	median
	(km s^-1)	(km s^-1)				(km s^-1)	(km s^-1)

C¹⁸O 2–1^g	0.57±0.07	0.52	1.26±0.07	1.15	57	0.45±0.03	0.44	0.97±0.06	0.96	29
C¹⁷O 2–1^h	0.42±0.06	0.40	0.91±0.05	0.86	29	0.42±0.04	0.42	0.92±0.10	0.92	2
CH₃OH 2₁–1₁ E	0.36±0.06	0.36	0.76±0.06	0.74	28	0.39±0.04	0.40	0.85±0.09	0.86	10
CH₃OH 2₀–1₀ A⁺	0.41±0.06	0.36	0.88±0.07	0.77	38	0.39±0.02	0.40	0.85±0.06	0.87	15
N₂H⁺ 1–0^h	0.35±0.07	0.32	0.73±0.07	0.64	16	0.27±0.05	0.27	0.55±0.12	0.55	2
C³⁴S 2–1	0.40±0.07	0.37	0.89±0.07	0.81	20	0.34±0.07	0.34	0.74±0.17	0.74	2
HC₃N 10–9^h	0.30±0.06	0.27	0.65±0.09	0.55	15	0.23±0.02	0.23	0.48±0.06	0.48	3

Notes.

^(a)

Average values exclude cores Cha1-C1, C2, and C3 as we only compare cores with the same range of peak column densities in both clouds. The errors are dispersions from the mean value.

^(b)

Average FWHM linewidths over all cores in each transition.

^(c)

Median FWHM linewidth in each transition.

^(d)

Average ratio of the non-thermal-to-mean-thermal velocity dispersions for the core sample in each transition.

^(e)

Median non-thermal-to-mean-thermal velocity dispersion ratio.

^(f)

Number of cores used for the calculation.

^(g)

A fraction of the C¹⁸O 2–1 spectra in Cha I are marginally optically thick and may therefore be slightly broadened (see Sect. C.1).

^(h)

Intrinsic linewidths (FWHM) derived from a seven-component hyperfine-structure fit.

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