Modelling the spectral energy distribution of galaxies. III. Attenuation of stellar light in spiral galaxies

TL;DR

This paper develops detailed models for how dust and stars in spiral galaxies attenuate stellar light across a broad spectral range, accounting for various galaxy components and geometries.

Contribution

It introduces new calculations of stellar light attenuation in spiral galaxies using geometries that match the entire spectral energy distribution and surface brightness profiles, including polynomial fits for easy application.

Findings

Attenuation varies significantly between stellar components.

A general formula for composite attenuation is provided.

Optical depth can be self-consistently derived from Halpha/Hbeta ratios.

Abstract

We present new calculations of the attenuation of stellar light from spiral galaxies using geometries for stars and dust which can reproduce the entire spectral energy distribution from the UV to the FIR/submm and can also account for the surface brightness distribution in both the optical/NIR and FIR/submm. The calculations are based on the model of Popescu et al. (2000), which incorporates a dustless stellar bulge, a disk of old stars with associated diffuse dust, a thin disk of young stars with associated diffuse dust, and a clumpy dust component associated with star-forming regions in the thin disk. The attenuations, which incorporate the effects of multiple anisotropic scattering, are derived separately for each stellar component, and presented in the form of easily accessible polynomial fits as a function of inclination, for a grid in optical depth and wavelength. The wavelength range considered is between 912 AA and 2.2 micron, sampled such that attenuation can be conveniently calculated both for the standard optical bands and for the bands covered by GALEX. The attenuation characteristics of the individual stellar components show marked differences between each other. A general formula is given for the calculation of composite attenuation, valid for any combination of the bulge-to-disk ratio and amount of clumpiness. As an example, we show how the optical depth derived from the variation of attenuation with inclination depends on the bulge-to-disk ratio. Finally, a recipe is given for a self-consistent determination of the optical depth from the Halpha/Hbeta line ratio.