All Tables

Table 1: Basic properties of Henize 2-10 and NGC 253.
Table 2: Results for Henize 2-10.
Table 3: Results for the nucleus of NGC 253.
Table 4: Observed and predicted ("low $T_{\rm k}$ '' and "high $T_{\rm k}$ '' LVG models) line area ratios for Henize 2-10 and NGC 253.
Table 5: Parameters of the "best'' LVG models.
Table 6: Parameters of the "best'' PDR models.
Table 7: Observed and modeled line emissivity ratios for Henize 2-10 and NGC 253 using PDR models.
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).
Table 9: Observations of the Milky Way nucleus (from Fixsen et al. 1999), NGC 253 (from this paper), Henize 2-10 (from this paper) and the Cloverleaf QSO (from Barvainis et al. 1997; Tsuboi et al. 1999; Weiß et al. 2003).
Table 10: Flux ratios for the center of the Milky Way, NGC 253, Henize 2-10 and the Cloverleaf QSO.