Diagnostics of dust content in spiral galaxies: Numerical simulations of radiative transfer

Details Diagnostics of dust content in spiral galaxies: Numerical simulations of radiative transfer Diagnostics of dust content in spiral galaxies: Numerical simulations of radiative transfer

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...432..114b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 432, no. 1, p. 114-127

Astronomy and Astrophysics

Astrophysics

92

Astronomical Models, Astronomical Photometry, Computerized Simulation, Cosmic Dust, Interstellar Extinction, Interstellar Matter, Mathematical Models, Radiative Transfer, Spiral Galaxies, Brightness, Light Scattering, Radiation Absorption, Stellar Color, Stellar Luminosity, Stellar Magnitude

Scientific paper

In order to find the best observable diagnostics for the amount of internal extinction within spiral galaxies, we have constructed realistic models for disk galaxies with immersed dust layers. The radiative transfer including both scattering and absorption has been computed for a range of model galaxies in various orientations. Standard galaxy surface photometry techniques were then applied to the numerical data to illustrate how different observables such as total magnitude, color and luminosity distribution behave under given conditions of dust distribution. This work reveals a set of superior diagnostics for the dust in the disk. These include not only the integrated parameters, but also the apparent disk structural parameters, the amplitude of the asymmetry between the near and far sides of the galaxy as divided by the apparent major axis and their dependence on the orientation of the galaxy with respect to the observer. Combining the above diagnostics with our impressions of real galaxies, we arrive at the qualitative conclusion that galaxy disks are generally optically thin. Quantitative conclusions will appear in subsequent work.

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