Table 2
Global characteristics of the W43 molecular and star-forming complex in comparison with other star-forming complexes.
| Region | Assumed | Equivalent diameter | Velocity range | Total H2 Mass | Clouds mass | Dense clumps mass | 8 μm luminosity | |
| distance | from 13CO | from 13CO | from 12CO | from 13CO | from submma | from 8 μmb | ||
| [kpc] | [pc] | [ ] |
[M⊙] | [M⊙] | [M⊙,%] | [L⊙] | ||
|
|
||||||||
| W43 | 6.0 | ~140 | 80 to 110 | 7.1 × 106 | 4.2 × 106 | 8.4 × 105, 12% | 1.60 × 107 | |
| Cygnus X | 1.7c | ~160c | –10 to 20c | 5.0 × 106c | 8.0 × 105c | 6.0 × 104 , 1%d | 6.57 × 106e | |
| W51 | 7.0 | ~100f | 56 to 65f | ~1.2 × 106f | ... | 5.5 × 105 | ... | |
| CMZ | 8.5 | ~350g | –225 to 225g | ~3.0 × 108g | ~2.0 × 107g | 4.0 × 106 | ... | |
| W49 | 11.4h | ~45h | –5 to 25h | ... | ~5.0 × 105h | 2.0 × 105 | ... | |
Notes.
The dense clumps mass is calculated from the ATLASGAL 870 μm images and MAMBO2 1.3 mm for Cygnus X, from which 
5 pc cloud structures have been filtered (more precisely, 5.6 pc for W43, 5 pc for Cygnus X, 6.5 pc for W51, 4.0 pc for CMZ, and 5.3 pc for W49), and using Eq. (4). The percentage of dense clumps formed out of the total H2 gas (taken from column 5) is estimated for the regions where the total H2 mass is more reliable;
The 8 μm luminosity is measured from band 4 of Spitzer, which has a bandwidth of 2.93 μm centered at 7.91 μm;
From Schneider et al. (2006);
From Motte et al. (2007) at 1.2mm;
From Hora et al. (2009);
From Dahmen et al. (1998) using C18O;
From Simon et al. (2001).
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