The G11.11-0.12 Infrared-Dark Cloud has a filamentary appearance , both in absorption against the diffuse 8 \mu m Galactic background , and in emission from cold dust at 850 \mu m. 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 \kappa _ { 8 } / \kappa _ { 850 } \leq 1010 , which is well below that expected for the diffuse ISM where \kappa _ { 8 } / \kappa _ { 850 } \sim 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 \mu m 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 \Sigma ( r ) \propto r ^ { - \alpha } , where \alpha \geq 3 , indicating that G11.11-0.12 is the first observed filament with a profile similar to that of a non-magnetic isothermal cylinder .