Table 3: Physical parameters at selected positions in Fig 1, obtained by fitting the observed intensity ratios to the single clump KOSMA - $\tau$ PDR models. Cols. (2)-(5) list the fitted clump densities, clump mass, clump radius and FUV field; Col. (6) is the minimum reduced $\chi ^{2}$ of the PDR fit; the FUV field derived from the FIR continuum $\chi _{\rm FIR}$ and that from the stellar radiation $\chi _{\rm star}$ are in Cols. (7) and (8); The distance to HD 281159 used for the calculation of $\chi _{\rm star}$ is listed in Col. (9).
Position n $M_{\rm cl}$ $R_{\rm cl}$ $\chi_{\rm PDR}$ $\chi^{2}_{\min}$ $\chi _{\rm FIR}$ $\chi _{\rm star}$ d

[10⁵ cm^-3] $M_{\odot}$ pc pc

Northern rim 1.91 0.2 0.01 15 1.38 39 40 0.37

Cluster 2.75 0.1 0.01 98 1.05 84 40 0.37

Ridge 4.25 0.4 0.01 38 1.23 46 40 0.37

Map center 3.98 0.1 0.01 23 1.04 23 13 0.64

$[C {\sc i}]$ peak 1.91 0.1 0.02 23 1.96 11 7 0.90

Western rim 0.63 0.2 0.02 20 2.00 6 3 1.42

Southern rim 0.44 0.4 0.02 2 2.31 1 3 1.29

**Table 3:** Physical parameters at selected positions in Fig 1, obtained by fitting the observed intensity ratios to the **single clump** KOSMA - $\tau$ PDR models. Cols. (2)-(5) list the fitted clump densities, clump mass, clump radius and FUV field; Col. (6) is the minimum reduced $\chi ^{2}$ of the PDR fit; the FUV field derived from the FIR continuum $\chi _{\rm FIR}$ and that from the stellar radiation $\chi _{\rm star}$ are in Cols. (7) and (8); The distance to HD 281159 used for the calculation of $\chi _{\rm star}$ is listed in Col. (9).
Position	n	$M_{\rm cl}$	$R_{\rm cl}$	$\chi_{\rm PDR}$	$\chi^{2}_{\min}$	$\chi _{\rm FIR}$	$\chi _{\rm star}$	d
	[10⁵ cm^-3]	$M_{\odot}$	pc					pc
Northern rim	1.91	0.2	0.01	15	1.38	39	40	0.37
Cluster	2.75	0.1	0.01	98	1.05	84	40	0.37
Ridge	4.25	0.4	0.01	38	1.23	46	40	0.37
Map center	3.98	0.1	0.01	23	1.04	23	13	0.64
$[C {\sc i}]$ peak	1.91	0.1	0.02	23	1.96	11	7	0.90
Western rim	0.63	0.2	0.02	20	2.00	6	3	1.42
Southern rim	0.44	0.4	0.02	2	2.31	1	3	1.29

Source LaTeX | All tables | In the text