Table 5
Far-IR CO emission: observations and envelope models.
| Object | LCO(obs) | LCO(env) | ||
| (L⊙) | (L⊙) | (%) | ||
|
|
||||
| High-mass YSOsa | ||||
|
|
||||
| G327-0.6 | 1.9 | 1.6 | 84 | |
| W51N-e1 | 25.8 | 14.6 | 56 | |
| DR21(OH) | 1.2 | 0.7 | 58 | |
| NGC 6334-I | 3.4 | 2.4 | 71 | |
| G5.89-0.39 | 3.9 | 1.8 | 46 | |
| NGC 7538-I1 | 2.1 | 1.6 | 77 | |
|
|
||||
| Low-mass YSOsb | ||||
|
|
||||
| NGC 1333 I2A | 4.1 × 10-3 | 0.3 × 10-3 | 7 | |
| HH46 | 6.9 × 10-3 | 0.5 × 10-3 | 7 | |
| DK Cha | 5.1 × 10-3 | 0.1 × 10-3 | 2 | |
Notes.
Observed CO luminosities are calculated using detected transitions only, from J = 14–13 to 30–29, depending on the source (see Table C.1). The corresponding envelope CO luminosities are calculated using the same transitions.
Results from Visser et al. (2012). The observed CO emission is taken to be the total CO emission from all modeled physical components.
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