Table 3
Resulting average OPRs, observed temperatures, TK, and the temperature ranges in which the OPRs are reproduced by model b, Tmod, for a density of nH = 2 × 104 cm-3 (Fig. 10) in the molecular envelopes and the dense core associated with W51, and nH = 1 × 103 cm-3 for the translucent gas (Fig. A.12).
| Source | VLSR | OPR | TK | Tmod(t ≃ 5 × 105 yrs) | Tmod(t ≳ 106 yrs) |
| (km s-1) | (K) | (K) | (K) | ||
|
|
|||||
| Molecular envelopes | |||||
| W31C | −3.5 | 2.5(± 0.1) | 30−50(a) | 28−35 | 32−35 |
| W49N | +8 | 3.5(± 0.1) | ~130(b) | 5−12 | 23−25 |
| W51 | +57 | 2.7(± 0.1) | 20−50(c) | 23−28 | 29−32 |
| G34 | +58 | 2.3(± 0.1) | 20−70(cd) | ≳35 | ≳35 |
|
|
|||||
| Dense and cold core | |||||
| W51 | +68 | 3.4(± 0.1) | 10−30(f) | 10−13 | 23−25 |
|
|
|||||
| Translucent gas | Tmod(t ≃ 104 yrs) | Tmod(t ≳ 106 yrs) | |||
| W31C | +22 | 2.2(± 0.2) | 30−100(e) | ≳27 | ≳34 |
| +28 | 2.9(± 0.2) | 20−100(e) | 5−16 | 25−29 | |
| +40 | 2.6(± 0.2) | 25−75(e) | 12−27 | 28−34 | |
| Tmod(t ≳ 5 × 104 yrs) | |||||
| W31C | +10 | ≳1.7 | ... | ... | |
| +17 | ≳4.2 | 30−85(e) | 17−21 | ||
| W49N | +39 | ≳5.0 | <15(e) | 14−19 | |
| +63 | ≳1.4 | 20−120(e) | ... | ||
Notes. Details about the models are found in Sect. 4. The tabulated errors are the formal errors (details in Sect. 3.5.)
Derived from NH3 rotational transitions (Hajigholi et al. 2016).
The excitation temperature of the CI 492 GHz line (Gerin et al. 2015).
Derived from CN and NH3 rotational transitions (Mookerjea et al. 2014).
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