C I observations in the CQ Tauri proto-planetary disk: evidence of a very low gas-to-dust ratio ?

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Table 4:

Observed and predicted line flux.
	C I $^3P_1\rightarrow ^3P_0$		C I $^3P_2 \rightarrow ^3P_1$		$\Sigma_{100}$	p
	(Jy km s^-1)		(Jy km s^-1)		(10¹⁷ cm^-2)
Obs.	< 6.6		<25
T_k	50 K	100 K	50 K	100 K
Model A	30	48	68	135	12.0	2.3
Model B	13	15	33	52	2.3	1.5
Model C	26	37	60	111	8.7	1.4
Thick	60	128	125	300	1000	1.5
Model J/B4	8-11		24-29

Notes. Model A: $\chi=10^4$ , g/d = 100; B: $\chi=10^2$ , g/d = 10; C: Kurucz A3, g/d = 10; Thick: flux for optically thick lines. Predictions are for an assumed local line width of 0.2 km s^-1. Model J is from Jonkheid et al. (2007), their model B4. All the line fluxes are scaled for a source distance of 140 pc. $\Sigma_{100}$ and p are the results of the power-law fitting of the modeled C I surface densities (Fig. 3).

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