Table 7
Mass cloud derived with two dust emissivity indices β, without and with colour corrections applied, and with a different spatial sampling of the column density map.
| β = 2 | β = 1.7 | ||||
|---|---|---|---|---|---|
| No CC | CC | No CC | CC | ||
| (Masses in 103M⊙) | |||||
| (1) | (2) | (3) | (4) | (5) | (6) |
| N(H2) ≤ 3 × 1021 | 8.12 | 8.38 | 7.27 | 6.41 | 5.66 |
| N(H2) > 3 × 1021 | 3.55 | 3.28 | 2.59 | 1.73 | 1.29 |
| N(H2) > 1022 | 0.95 | 0.59 | 0.66 | 0.72 | 0.37 |
| AV > 7 mag | 1.54 | 1.14 | 1.14 | 0.74 | 0.56 |
Notes. The value β = 2 is the HGBS standard, β = 1.7 is the peak of the distribution of β in the Perseus region (Planck Collaboration XI 2014). Masses in Cols. (2), (3), and (5) were derived without applying colour corrections, while in Cols. (4) and (6) the reported masses were computed with colour corrections. In all cases but Col. (3), the column density map was created on a grid of size 14′′ and spatial resolution of36′′, default values for HGBS. In Col. (3) the column density map was projected onto the grid used for Planck data: 90′′ pixels and 5′ resolution. The 7 mag contour has been drawn assuming R = 3.1.
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