Nature of the Galactic Interstellar Dust Derived from IR Observations

Details Nature of the Galactic Interstellar Dust Derived from IR Observations Nature of the Galactic Interstellar Dust Derived from IR Observations

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc...67s&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Recent observational studies of the diffuse infrared emission from interstellar dust grains are reviewed, and a new interpretation of the mid- and far-infrared diffuse emission from the Galaxy is presented. The observational data available for this purpose are intensities by the IRAS (Infrared Astronomical Satellite) 12, 25, 60, and 100 μ m bands, the COBE (Cosmic Background Explorer) 12, 25, 60, 100, 140, 240 μ m bands, and the IRTS (Infrared Telescope in Space) 155 μ m band. Since the diffuse emission at longer than 100 μ m is well fitted with the thermal emission from the dust grain at a single temperature with the spectral index of 2, it can be attributed to interstellar grains in a steady-state of thermal equilibrium with the general radiation field in the Galactic plane. The intensity of the IRAS 12 μ m band is proportional to the integrated intensity of the emission from the thermal equilibrium grain as that of the 3.3 μ m UIR band is. The 60 μ m intensity is well predictable from the spectrum at longer than 100 μ m. The intensities at 25 and 60 μ m are not proportional to the integrated intensities of the thermal equilibrium grain, but have steeper dependencies. This fact may be attributed to the effect of multiple excitation by the UV photons to very small grains.

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