Table 3
Median values of mass, temperature, distance and completeness limits toward the ℓ = 30° and ℓ = 30° fields.
| Population | ℓ = 30° field | ℓ = 59° field | |||||||
| Temperature | Mass | Distance | Completenessa | Temperature | Mass | Distance | Completenessb | ||
| [K] | [M⊙] | [kpc] | [M⊙] | [K] | [M⊙] | [kpc] | [M⊙] | ||
|
|
|||||||||
| All | 21.8 | 99.6 | 7.6 | 73.0 | 17.6 | 2.1 | 3.6 | 0.7 | |
| Starless | 19.7 | 112.6 | − | − | 17.4 | 2.2 | − | − | |
| Proto-stellar | 24.3 | 89.9 | − | − | 19.8 | 1.9 | − | − | |
Notes.
At distances of 5.2 kpc (where the bulk of the sources is located) and 10 kpc (where much less sources are found, see Russeil et al. 2011) the completeness limits are ~34 and ~126 M⊙, respectively.
At distances of 2.3 kpc (where the bulk of the sources is located) and 9.5 kpc (Perseus arm, see Russeil et al. 2011) the completeness limits are ≃0.4 and ≃7.6 M⊙, respectively.
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