Table 4
Best-fit parameters (from PLFIT) to the CMF of the ℓ = 30° and ℓ = 59° fields, for the power-law distribution.
| Population | ℓ = 30° field | ℓ = 59° field | |||
| α | M inf | α | M inf | ||
| [M⊙] | [M⊙] | ||||
|
|
|||||
| All | 1.15 ± 0.15 | 212 ± 79 | 1.20 ± 0.15 | 7.3 ± 2.2 | |
| Starless | 1.12 ± 0.18 | 206 ± 95 | 1.23 ± 0.17 | 7.5 ± 2.3 | |
| Proto-stellar | 1.06 ± 0.21 | 138 ± 105 | 0.58 ± 0.22a | 0.7 ± 2.5 | |
Notes. The Salpeter value of the power-law exponent for the IMF is α = 1.35 (Salpeter 1955).
The values of these two parameters change to α = 1.44 ± 0.39 and Minf = 9.9 ± 4.0 M⊙ when only sources for which a distance could be determined are included. See Sect. 7.2.
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