Table A.3
Overview of the physical properties of the IRDCs.
| Source | Td | M(GC) | N(H2) | N(H2,min) | n(H2) | Mvir | α | Vin | ΔVH2O | Ṁin |
| K | 103M⊙ | 1022 cm-2 | 1022 cm-2 | 103 cm-3 | 103M⊙ | km s-1 | km s-1 | 10-3M⊙ yr-1 | ||
|
|
||||||||||
| G010.4 | 20.8 ± 0.4 |
|
|
2.4 |
|
|
|
0.4 | 1.9 ± 1.0 | 2 |
| G018.7 | 22.0 ± 1.0 |
|
|
4.2 |
|
|
|
1.5 | 3.5 ± 0.9 | 18 |
| G336.9 | 15.8 ± 1.0 |
|
|
3.6 |
|
|
|
... | ... | ... |
| G337.1 | 22.4 ± 0.9 |
|
|
3.2 |
|
|
|
2.4 | 2.2 ± 0.8 | 17 |
| G337.2 | 21.9 ± 1.1 |
|
|
3.8 |
|
|
|
0.5 | 2.2 ± 2.0 | 3 |
Notes. Columns. dust temperature calculated by König et al. (2015), mass calculated with the flux from Csengeri et al. (2014), beam-averaged peak column density, minimum H2 column density needed to observe the water absorption features, derived from the fraction of continuum absorbed by water for the dark clouds (similar numbers also apply to the strongest absorption feature of the foreground clouds in each spectrum, based on their intensity), beam-averaged peak volume density, virial mass calculated from the C17O(3−2) linewidths listed in Giannetti et al. (2014), virial parameter α = Mvir/M, infall velocity from HCO+(1−0), redshift of the water lines with respect to the systemic velocity, and infall rates, calculated using 
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