Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...180...27w&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 180, no. 1-2, June 1987, p. 27-49. ZWO-supported research.
Astronomy and Astrophysics
Astronomy
128
Andromeda Galaxy, Infrared Astronomy Satellite, Infrared Radiation, Interstellar Gas, Interstellar Matter, Data Reduction, Dust, Far Infrared Radiation, Hydrogen, Molecular Clouds, Radial Distribution, Star Formation, Stellar Luminosity, Temperature Distribution
Scientific paper
IRAS observations of M31 are analyzed to study the origin and properties of the IR emission, and the results are discussed in terms of recent models for the IR emission from the Galaxy. The mid-IR emission from the disk is strong and requires the presence of a hot dust component. Very small grains are the most likely candidate to explain the emission. No direct evidence is found for a contribution from stars with dust shells. A straightforward analysis of the relation between the IR emission and atomic gas implies a strong radial decrease in the dust-to-hydrogen gas ratio. The ratio of 60-100-micron intensities is remarkably constant with radius; this is hard to explain with standard models for dust heating. Most of the radiation can be attributed to dust associated with atomic hydrogen gas heated by the general interstellar radiation field. The total IR luminosity of M31 is about six times lower than that of the Galaxy.
Schwering Piet B. W.
Walterbos Reinirus Antonius Maria
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