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Scientific paper
Dec 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000immm.proc...63l&link_type=abstract
The interstellar medium in M31 and M33. Proceedings 232. WE-Heraeus Seminar, 22-25 May 2000, Bad Honnef, Germany. Edited by El
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2
Scientific paper
M31 differs from our Galaxy in several respects. Above all the present star formation rate is considerably smaller in M31, resulting in a much fainter UV radiation field. This might affect the properties of dust. However the dust/gas ratio and the extinction law in M31 are only marginally different from the Galactic ones. As expected, far-IR observations with IRAS and ISOPHOT show that the bulk of the dust in M31 is cold, with a temperature of about 16 K. Major differences with the Milky way arise in the mid-IR. ISOCAM observations have revealed a spectrum completely different from Galactic spectra, with a very strong emission band at 11.3 micron. The other mid-IR emission bands are faint. The carriers of all these bands are heated transiently by absorption of individual visible photons. Another surprising observation is the presence of abundant dust in the outskirts of M31, at no less than 25 kpc from the center. A study of the reddening of stars in M31 shows that the dust/gas ratio is at least 33% of the Galactic value.
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