Table 1
Derived properties of the NGC 6334 filament and comparison with other well-documented filaments.
| Filament | ⟨ Mline ⟩ a |  b |
 c |
p d | Rflat e | Width, W f | Length | Refs. |
| (M⊙/pc) | (cm-2) | (cm-2) | (pc) | (pc) | (pc) | |||
|
|
||||||||
| NGC 6334 north+south | 800–1300 | 1–2 × 1023 | 1.8 × 1022 | 2.2 ± 0.3 | 0.05 ± 0.01 | 0.15 ± 0.03 | >7 | 1 |
| (western side) | ||||||||
| NGC 6334 north+south | (900–1300) | (1–2 × 1023) | (2–4× 1022) | (1.9 ± 0.4) | (0.05 ± 0.02) | (0.19 ± 0.03) | >7 | 1 |
| (eastern side) | ||||||||
| NGC 6334 north | 1600 | 2.5 × 1023 | 2.1 × 1022 | 2.4 ± 0.3 | 0.06 ± 0.02 | 0.15 ± 0.03 | >3.5 | 1 |
| (western side) | ||||||||
| NGC 6334 northg | (800–1600) | (1.5–2.5× 1023) | (1.1 × 1023) | – | – | (0.20 ± 0.03) | >3.5 | 1 |
| (eastern side) | ||||||||
| NGC 6334 south | 500–600 | 0.7–1× 1023 | 1.2 × 1022 | (2.3 ± 0.3) | (0.07 ± 0.02) | 0.16 ± 0.04 | ~3 | 1 |
| (western side) | ||||||||
| NGC 6334 south | 700–2000 | 0.9–1× 1023 | 1.2 × 1022 | 1.8 ± 0.3 | 0.09 ± 0.02 | 0.16 ± 0.04 | ~3 | 1 |
| (eastern side) | ||||||||
|
|
||||||||
| Vela Ch | 320–400 | 8.6 × 1022 | 3.6 × 1021 | 2.7 ± 0.2 | 0.05 ± 0.02 | 0.12 ± 0.02 | 4 | 2 |
| Serpens South | 290 | 6.4 × 1022 | 3.7 × 1021 | 2.0 ± 0.3 | 0.03 ± 0.01 | 0.10 ± 0.05 | 2 | 2, 3 |
| Taurus B211/B213 | 50 | 1.5 × 1022 | 0.7 × 1021 | 2.0 ± 0.3 | 0.03 ± 0.02 | 0.09 ± 0.02 | >5 | 4 |
| Musca | 20 | 4.2 × 1021 | 0.8 × 1021 | 2.2 ± 0.3 | 0.08 | 0.14 ± 0.03 | 10 | 5, 6 |
Notes. Values given in parentheses are more uncertain due to, e.g., large error bars in the corresponding filament profiles, and should be understood as being only indicative.
Average mass per unit length of the equivalent cylindrical filament derived from one-sided integration of the observed radial column density profile after background subtraction. The actual mass per unit length of each filament segment corresponds to the mean of the eastern-side and western-side values (not explicitly given here). The outer radius of integration was 0.7 pc on the western side, 0.3 pc on the eastern side of the northern segment, and 1.4 pc on the eastern side of the southern segment, respectively, corresponding to the radius where the background starts to dominate (see Figs. A.1–A.3).
Average value of the central column density derived along the filament crest after background subtraction. Typical uncertainties are a factor ~1.5–2 for values < 1023 cm-2 and a factor ~2–3 for values > 1023 cm-2, dominated by uncertainties in the dust opacity and in the distribution of dust temperature along the line of sight (cf. Roy et al. 2014).
Background column density. This is estimated as the column density observed at the closest point to the filament’s crest for which the logarithmic slope of the radial column density profile dln NH2/ dln r becomes positive.
The eastern side of the radial column density profile of the northern filament is poorly constrained due to confusion with the two massive protostellar clumps NGC 6334 I and I(N) (cf. Fig. 2a); no meaningful Plummer fit is possible.
According to Minier et al. (2013), the Vela C filament is not a simple linear structure or “ridge”, but is part of a more complex ring-like structure at least partly shaped by ionization associated with the RCW 36 HII region.
Reference. (1) this paper; (2) Hill et al. (2012); (3) Könyves et al. (2015); (4) Palmeirim et al. (2013); (5) Cox et al. (2016); (6) Kainulainen et al. (2016).
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