Earliest phases of star formation (EPoS) - Dust temperature distributions in isolated starless cores

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Volume 592 (August 2016)

A&A, 592 (2016) A61

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Table 4

Comparison of N_H peak column densities with previous dust emission studies.

Reference	CB 4	CB 17	CB 26	CB 27	B 68	CB 244	Remarks
		SMM	SMM2			SMM2

lau97a	...	4.3e22	...	...	...	...	1.3 mm on-off, T ≡ 20 K^a, κ₀^e = 0.008 cm² g^-1
lau97b	...	2.9e22	...	...	...	...	0.45–1.3 mm on-off, T ≡ 20 K^a, κ₀ = 0.008 cm² g^-1
lau10	...	2.0e23	...	...	...	3.0e23	0.45–1.2 mm maps, T ≡ 10 K^a, κ₀ = 0.005 cm² g^-1
stutz10	...	...	...	...	...	8.0e22	0.1–1.2 mm maps, mBB fit^b, κ₀ = 0.005 cm² g^-1
lau13	7.5e21	2.5e22	1.4e22	1.9e22	2.5e22	4.6e22	0.1–1.2 mm maps, mBB fit^b, κ₀ = 0.009 cm² g^-1
nielb12	...	...	...	...	4.3e22	...	0.1–1.2 mm maps, RTI^c, κ₀ = 0.007 cm² g^-1
lipp13	9.2e21^f	3.0e22^f	2.0e22	2.7e22	5.5e22	9.1e22	0.1–1.2 mm maps, RTI^c, κ₀ = 0.007 cm² g^-1
roy14	...	...	...	...	2.6e22	...	0.16–0.5 mm maps, AI^d, κ₀ = 0.009 cm² g^-1
schma14	...	4.3e22	...	...	...	...	0.1–1.2 mm maps, RTI^c, κ₀ = 0.007 cm² g^-1
This work	1.0e22^f	3.0e22^f	1.7e22	2.6e22	2.8e22	9.2e22	0.1–1.2 mm maps, RTI^c, κ₀ = 0.007 cm² g^-1

Notes.

^(a)

T_d fixed due to lack of observational constraints.

^(b)

Modified blackbody fit to LoS-averaged T_d.

^(c)

Ray-tracing inversion, accounting for LoS T_d variation.

^(d)

Abel inversion, accounting for LoS T_d variation.

^(e)

For direct comparability, we list here the total (gas + dust) opacity at λ = 1.0 mm, κ₀, of the ISM model used in the respective paper.

^(f)

Peak column density probably underestimated by up to 30% due to beam-smoothing; see discussion in Sect. 5.1.1.

Reference. lau97a: Launhardt & Henning (1997); lau97b: Launhardt et al. (1997); lau10: Launhardt et al. (2010); stutz10: Stutz et al. (2010); lau13: Launhardt et al. (2013); nielb12: Nielbock et al. (2012); lipp13: Lippok et al. (2013); roy14: Roy et al. (2014); schma14: Schmalzl et al. (2014).

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