Table 2
Properties of the clumps in the field of G319.88+00.79.
| Name | l | b | N(H2)1 | T dust 2 | M 3 | R eq 4 | n(H2)5 |
| (°) | (°) | (cm-2) | (K) | (M⊙) | (″) | (cm-3) | |
|
|
|||||||
| C 1 | 319.9012 | +00.7935 | 5.3 × 1022 | 22.3 ± 1.9 | 303 (246 ) |
25.2 (0.32 pc) | 5.4 × 104 |
| C 2 | 319.8668 | +00.7868 | 8.3 × 1022 | 19.7 ± 1.4 | 497 (458 ) |
24.9 (0.31 pc) | 8.6 × 104 |
| C 3 | 319.8324 | +00.7925 | 7.5 × 1022 | 14.4 ± 1.2 | 766 (623 ) |
119.7×24.3 (1.5 pc × 0.3 pc) | 1.6–8.0 × 104 |
Notes.
Peak column density corrected for a background value ~4.6 × 1021 cm-2 (the lowest value of column density in a field of radius 10′ centred on the exciting star; this low column density value is located at 
, outside any feature associated with the bipolar nebula and its parental cloud).
Dust temperature derived from the SED, based on the integrated fluxes of the clumps in the range 160–500 μm.
Mass obtained by integrating the column density in an aperture following the level at the N(H2) peak’s half intensity. In brackets is the mass obtained by integrating the 250 μm emission in an aperture following the level at the 250 μm peak’s half intensity and using the temperature in Col. 5.
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