Dust emission from an isolated interstellar cloud

Details Dust emission from an isolated interstellar cloud Dust emission from an isolated interstellar cloud

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...220..226l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 220, no. 1-2, Aug. 1989, p. 226-234. Research supported by ASTRON and NWO.

Astronomy and Astrophysics

Astronomy

32

Cosmic Dust, Infrared Sources (Astronomy), Interstellar Matter, Molecular Clouds, Astronomical Maps, Hydrocarbons, Infrared Astronomy Satellite, Radiation Distribution, Radiative Transfer

Scientific paper

The emission and absorption properties of dust are studied by examining the extended infrared emission obtained from IRAS survey data and extinction derived from star counts for an isolated and highly regular cloud (l = 300 deg, b = -17 deg). From the variation of the infrared colors as functions of opacity, the dependence of infrared emission on the exciting radiation field is analyzed. The color variations suggest that the emission in the IRAS wavelength range can be separated into at least three components. The 100-micron surface brightness remains proportional to blue extinction up to almost 2 mag, implying that the emission originates from a population of grains which absorbs strongly at visual and near-infrared wavelengths. Using a model for the radiative transfer in the cloud, it is shown that the spectral distribution and color variations can be reproduced by assuming two additional populations of particles: warm grains in thermal equilibrium of T not lower than 50 K to explain the 60-micron emission, and polyaromatic hydrocarbon molecules for the 12 and 25-micron emission.

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