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ID: 59626.0, MPI für Kernphysik / Infrared Astrophysics
Modelling the spectral energy distribution of galaxies. III. Attennuation of stellar light in spiral galaxies.
Authors:Tuffs, R.J.; Popescu, C.C.; Völk, H.J.; Kylafis, N.D.; Dopita, M.A.
Language:English
Date of Publication (YYYY-MM-DD):2004-06-01
Title of Journal:Astronomy & Astrophysics
Journal Abbrev.:A & A
Volume:419
Issue / Number:3
Start Page:821
End Page:835
Copyright:© ESO 2004
Review Status:Peer-review
Audience:Experts Only
Abstract / Description: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 ultraviolet (UV) to the Far-infrared (FIR)/submillimeter (submm) and can also account for the surface brightness distribution in both the optical/Near-infrared (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 Å and 2.2 m, 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 line ratio.
Free Keywords:galaxies: spiral -- ISM dust, extinction -- radiative transfer -- galaxies: structure -- ISM: HII regions -- galaxies: bulges -- ultraviolet: galaxies
External Publication Status:published
Document Type:Article
Affiliations:MPI für Kernphysik/Group H. J. Völk/Infrared Astrophysics (R. Tuffs, H.J. Völk)
External Affiliations:Research Associate, The Astronomical Institute of the Romanian Academy, Str. Cutitul de Argint 5, Bucharest, Romania

University of Crete, Physics Department, P.O. Box 2208, 710 03 Heraklion, Crete, Greece

Foundation for Research and Technology-Hellas, 71110 Heraklion, Crete, Greece

Research School of Astronomy & Astrophysics, The Australian National University, Cotter Road, Weston Creek
ACT 2611, Australia
Identifiers:DOI:10.1051/0004-6361:20035689
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