Spatial distribution of dust from cirrus to dense clouds

Details Spatial distribution of dust from cirrus to dense clouds Spatial distribution of dust from cirrus to dense clouds

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.427..615a&link_type=abstract

The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 615

Computer Science

8

Interstellar Medium, Dust, Extinction, Density Structure, Pdr, Dense Cores

Scientific paper

Large scale mapping of several star forming regions in the interstellar medium has been conducted with ISOCAM in two broad-band filters (5-8.5 and 12-18 μm). The small scale (3-6 arcsec) extended mid-IR emission of dust at different stages of evolution and in a wide range of illuminations and densities has been revealed. The structure of the infra-red emission of illuminated edges of nearby molecular clouds gives strong constraints on the penetration of UV radiations through these clouds and on their small scale density structure. For both the Horsehead nebula and the interface of the main cloud of ρ Ophiuchi, the edges of the molecular clouds strongly illuminated by B stars present extremely steep increases of column density, while the extinction of incident radiation inside the clouds appears compatible with homogeneous matter at small scale (typically below ~ 0.01 pc). Dense cores are seen as deep absorption structures against a diffuse background emission. The density profiles derived from the extinction profiles depart from a r-2 law due to a central flattening (typically for r < 0.02 pc). The steepest gradients in outer regions can be modelled with density profiles at least as steep as a r-2 law. Finally ISOCAM data also allow to extend the statistical analysis of the spatial distribution of dust in the diffuse interstellar medium down to a few arcsec scales.

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