Table 4
Best fit of the CMDs for the SMC clouds.
| Luminous mass distribution | |||||
|---|---|---|---|---|---|
| Region | Model | β | M0 (104 M⊙) | N0 | N(a) |
| SMC | PLaw | −2.4 ± 0.2 | 5.3 ± 1.5 | – | 50 |
| SMC | Trunc. | −2.2 ± 0.3 | 3.8 ± 0.9 | 3.0 ± 3.0 | 50 |
| SW | Trunc. | −1.9 ± 0.3 | 3.8 ± 0.8 | 4.5 ± 4.0 | 32 |
| NE | PLaw | −3.1 ± 0.6 | 1.2 ± 0.3 | – | 15 |
| WG(b) | Trunc. | −1.5 ± 0.3 | 2.6 ± 1.3 | 2.3 ± 2.0 | 13 |
| Virial mass distribution | |||||
| Region | Model | β | M0 (104 M⊙) | N0 | N(a) |
| SMC | PLaw | −2.4 ± 0.2 | 14.5 ± 4.2 | – | 50 |
| SMC | Trunc. | −2.3 ± 0.2 | 15.5 ± 5.8 | 1.4 ± 1.0 | 50 |
| SW | Trunc. | −1.9 ± 0.3 | 13.3 ± 4.0 | 3.4 ± 3.0 | 32 |
| NE | PLaw | −3.3 ± 0.5 | 3.0 ± 2.1 | – | 15 |
| WG(b) | Trunc. | −2.0 ± 0.2 | 1.4 ± 1.0 | 3.7 ± 2.0 | 10 |
Notes. The best fit of the power law (PLaw) and truncated (Trunc.) models for the SMC clouds are given. In the case of the SW, NE, and WG regions, only the models that best fit the CMDs are indicated. The fitting was performed above the completeness limit of Mlum = 3.1 × 103 M⊙ and Mvir = 8.6 × 103 M⊙ for all regions. (a)The last column indicates the number of well-resolved clouds with S/N > 5 used for the fit. (b)For the WG region, the completeness limits are Mlum = 7.15 × 102 M⊙ and Mvir = 4 × 103 M⊙.
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