Very small grains in the Milky Way and external galaxies

Details Very small grains in the Milky Way and external galaxies Very small grains in the Milky Way and external galaxies

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990nascp3084..108l&link_type=abstract

In its The Interstellar Medium in External Galaxies: Summaries of Contributed Papers p 108-110 (SEE N91-14100 05-90)

Other

Cosmic Dust, H I Regions, H Ii Regions, Infrared Radiation, Infrared Reflection, Interstellar Matter, Milky Way Galaxy, Molecular Clouds, Radiation Distribution, Radiative Transfer, Reflection Nebulae, Color, Destruction, Far Fields, Illuminating, Mass Ratios, Populations, Spiral Galaxies

Scientific paper

These studies of the infrared colors of reflection nebulae, HL HI clouds, HII regions and external galaxies have shown the following results. Different classes of objects locate in different regions on the R vs Fv (60)/Fv (100) diagram. This is determined both by differences in dust properties and by differences in the illuminating radiation field. For example, HL clouds and reflection nebulae almost have the same behavior since both are in the diffuse Interstellar Medium (ISM) and can be expected to have similar grain populations; the small difference in their infrared colors can be explained by the difference of the illuminating radiation field. On the other hand, the dramatic difference of R=vFv (12)/Fv (far IR) between HII region and diffuse ISM may be due to the destruction of the Very Small Grain (VSG) component in the HII regions, although radiation transfer effects may play a part as well. The ratio R=vFv (12)/Fv (far IR) is approximately constant in normal spiral galaxies. This implies that the mass ratio b=Mass (VSG)/Mass (dust) does not vary greatly from one galaxy to another.

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