Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud - I. N159W

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Volume 596 (December 2016)

A&A, 596 (2016) A85

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Table 3

Comparison with previous CO excitation analyses.

Parameter	Location^a	This work		Nikolić+07^d	Pineda+08^e	Mizuno+10^f
		All^b	Sub^c

T_k (K)	[0, 2]	324	72	15–95
T_k (K)	[0, 1]	471	126		~80	~70

n(H₂) (10³ cm^-3)	[0, 2]	2.9	16.0	10
n(H₂) (10³ cm^-3)	[0, 1]	2.2	7.9		~10	~4

N(CO) (10¹⁷ cm^-2)	[0, 2]	3.4	8.5	6–12
N(CO) (10¹⁷ cm^-2)	[0, 1]	2.7	8.5		~10^g	~35

Ω (10^-1)	[0, 2]	1.6	1.0	0.9–7.0
Ω (10^-1)	[0, 1]	2.1	1.0		~2

Notes.

^(a)

Pixel location (Fig. 8). [0, 2] and [0, 1] correspond to (05^h39^m36.8^s, − 69°45′12.6′′) and (05^h39^m36.8^s, − 69°45′42.6′′).

^(b)

“All”: RADEX solutions determined using all available CO transitions (Sect. 4.2).

^(c)

“Sub”: RADEX solutions for CO transitions only up to J = 7–6 (Sect. 4.5).

^(d)

CO(1–0), CO(2–1), CO(3–2), ¹³CO(1–0), and ¹³CO(2–1) lines were modeled with the non-LTE radiative transfer model by Jansen et al. (1994).

^(e)

CO (J_u = 1, 4, and 7), ¹³CO (J_u = 1 and 4), and [CI] (609 μm and 370 μm) transitions were analyzed using the escape probability radiative transfer model by Stutzki & Winnewisser (1985).

^(f)

CO (J_u = 1, 2, 3, 4, and 7) and ¹³CO (J_u = 1, 2, 3, and 4) data were combined with the large velocity gradient (LVG) model by Goldreich & Kwan (1974).

^(d,e,f)

All analyses were done on 45′′ scales.

^(g)

CO linewidth of 10 km s^-1 is used for this estimate.

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