Dust-to-gas ratio in disk galaxies

Details Dust-to-gas ratio in disk galaxies Dust-to-gas ratio in disk galaxies

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...229..485j&link_type=abstract

Astrophysical Journal, Part 1, vol. 229, Apr. 15, 1979, p. 485-488. NSF-supported research.

Astronomy and Astrophysics

Astrophysics

5

Abundance, Cosmic Dust, Galaxies, Interstellar Gas, Interstellar Matter, Optical Polarization, Andromeda Galaxy, Centimeter Waves, Polarization Characteristics, Radio Galaxies, Spiral Galaxies

Scientific paper

Optical polarization in disk galaxies can be produced by scattering off grains. By comparing the amount of polarization with the column density of gas derived from 21 cm measurements, it is possible to estimate a dust-to-gas ratio. We argue that observations of some inner portions of M31 and M81 suggest that the dust-to-gas ratio in the observed regions is probably at least 0.005 by mass and therefore comparable to the value in the solar neighborhood.

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