Table 8: Results of PDR models for [CI] in Henize 2-10 and NGC 253. We reported also observations from Tables 2 and 3. The PDR model predictions have been multiplied by the line width ratio, $\frac{\Delta v({\rm galaxy})}{\Delta v({\rm PDR})}$ , and by the surface filling factor, PDR_FF, (see Table 6).
E NGC 253 Henize 2-10

(erg cm^-2 s^-1 sr^-1) observations observations

CI(³P₁-³P₀) $3.5\times 10^{-5}$ $3.0\times 10^{-7}$

CI(³P₂-³P₁) $3.2\times 10^{-5}$ Not observed

PDR model PDR model

CI(³P₁-³P₀) $1.1\times 10^{-4}$ $5.1\times 10^{-7}$

CI(³P₂-³P₁) $3.9\times 10^{-4}$ $1.9\times 10^{-6}$

**Table 8:** Results of PDR models for [CI] in Henize 2-10 and NGC 253. We reported also observations from Tables 2 and 3. The PDR model predictions have been multiplied by the line width ratio, $\frac{\Delta v({\rm galaxy})}{\Delta v({\rm PDR})}$ , and by the surface filling factor, PDR_FF, (see Table 6).
E	NGC 253	Henize 2-10
(erg cm^-2 s^-1 sr^-1)	observations	observations
CI(³P₁-³P₀)	$3.5\times 10^{-5}$	$3.0\times 10^{-7}$
CI(³P₂-³P₁)	$3.2\times 10^{-5}$	Not observed
	PDR model	PDR model
CI(³P₁-³P₀)	$1.1\times 10^{-4}$	$5.1\times 10^{-7}$
CI(³P₂-³P₁)	$3.9\times 10^{-4}$	$1.9\times 10^{-6}$

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