Abstract
The G11.11-0.12 infrared-dark cloud has a filamentary appearance, both in absorption against the diffuse 8 μm Galactic background and in emission from cold dust at 850 μm. A detailed comparison of the dust properties at these two wavelengths reveals that standard models for the diffuse interstellar dust in the Galaxy are not consistent with the observations. The ratio of absorption coefficients within the cloud is κ8/κ850 ≤ 1010, which is well below that expected for the diffuse interstellar medium where κ8/κ850 ~ 1700. This may be due to the formation of ice mantles on the dust and grain coagulation, both of which are expected within dense regions of molecular clouds. The 850 μm emission probes the underlying radial structure of the filament. The profile is well represented by a marginally resolved central region and a steeply falling envelope, with Σ(r) ∝ r-α, where α ≥ 3, indicating that G11.11-0.12 is the first observed filament with a profile similar to that of a nonmagnetic isothermal cylinder.
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