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

By R. Tuffs, C. Popescu, H. Voelk, N. Kylafis, M. A. D. Mpik, Heidelberg, U. Crete, Heraklion, F. F. Research, Technology-Hellas and 3 more. 2004

181 citations recorded by the source corpus.

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. ([CITE]), 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 A and 2.2 ${\mu}$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 ${\rm H\alpha}/{\rm H\beta}$ line ratio.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/7b786438cab973903b3c5568afd6e0d9e0219abb

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Citations in the corpus

Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, methodology): “They used the optical B-band disc luminosity density from the Millennium Galaxy Catalogue scaled by a fixed dust mass-to-light ratio from Tuffs et al. (2004).”
Discovery of an Extended Ultraviolet Disk in the Nearby Galaxy NGC 4625 (2005, background): “If the effects of scattering are considered E(B − V ) could be as low as 0.04mag (Tuffs et al. 2004).”
Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample (2007, background): “…correct model would specify the locations of the stellar sources and the absorbing dust and would solve the radiative transfer problem (e.g., Tuffs et al. 2004), but this would require many uncertain assumptions about the relative distributions of stars and dust, as well as massive…”
Galaxy and Mass Assembly (GAMA): the star formation rate dependence of the stellar initial mass function (2011, methodology): “We explore several popular empirical dust models (Cardelli et al. 1989; Calzetti 2001; Fischera & Dopita 2005) along with radiative transfer model predictions of the effects of dust extinction (Popescu et al. 2000; Tuffs et al. 2004; Popescu et al. 2011).”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, background): “A large body of theoretical studies of dust radiative transfer in galaxies (e.g., Witt & Gordon 2000; Charlot & Fall 2000; Charlot & Longhetti 2001; Tuffs et al. 2004; Jonsson et al. 2009) shows that the actual relation between the reddening of an integrated spectrum and its dust attenuation can…”
Galaxy And Mass Assembly (GAMA): the galaxy stellar mass function at z < 0.06 (2011, methodology): “Driver et al. (2007), using the dust models of Popescu et al. (2000) and Tuffs et al. (2004), confirmed this with the largest deviation for edge-on systems.”
Dust in starburst nuclei and ULIRGs - SED models for observers (2006, methodology): “Three–dimensional codes have been applied to spirals (Kylafis & Bahcall (1987), Popescu et al. (2000), Tuffs et al. (2004)) using ray tracing or Monte Carlo techniques (Bianchi et al. 2000).”
A Concise Reference to (Projected) Sérsic R 1/n Quantities, Including Concentration, Profile Slopes, Petrosian Indices, and Kron Magnitudes (2005, background): “Modelling opacity is non–trivial as there are strong inclination dependencies (Cho loniewski 1991; Jones, Davies & Trewhella 1996; Graham 2001b) however models are being developed to provide detailed corrections (e.g., Pierini et al. 2004; Tuffs et al. 2004).”
An Ultraviolet-to-Radio Broadband Spectral Atlas of Nearby Galaxies (2006, methodology): “…line (normalized to an infrared-to-ultraviolet ratio of unity at zero inclination) shows the expected effect of extinction on the ultraviolet data with changing inclination using the thin disk model and a central face-on optical depth in the B band of τ fB = 2 described in Tuffs et al. (2004).”
A simple model to interpret the ultraviolet, optical and infrared emission from galaxies (2008, background): “Their model also accounts for the fact that stars are born in dense molecular clouds, which dissipate after some time, and hence, that newly born stars are more attenuated than older stars (see also, e.g., Charlot & Fall 2000; Tuffs et al. 2004).”
GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies (2012, background): “These models calculate the effective obscuration and produce attenuation curves as outputs, which are generally very different from the extinction curves affecting the flux of each star (e.g., Witt & Gordon, 2000; Pierini et al., 2004; Tuffs et al., 2004; Panuzzo et al., 2007).”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, methodology): “This is achieved by associating stars in different age ranges with the thin-disc, thick-disc and bulge components of the versatile model of radiative transfer of Tuffs et al. (2004).”
Empirical determination of the shape of dust attenuation curves in star-forming galaxies (2011, background): “This two component dust distribution has been included in several models for dust in galaxies (Silva et al. 1998; Charlot & Fall 2000; Popescu et al. 2000; Tuffs et al. 2004).”
CIGALE: a python Code Investigating GALaxy Emission (2018, background): “So far this constraint has largely confined radiative transfer models to theoretical studies (e.g. Gordon et al. 2001; Tuffs et al. 2004; Trayford et al. 2017) and to only a handful of in-depth observational case studies, generally on edge-on galaxies (e.g. Xilouris et al. 1999; Popescu et al.…”
Fitting the integrated spectral energy distributions of galaxies (2010, methodology): “…component being used for the subsequent (i.e. directly emitted photons by stars, then photons scattered once by dust, photons scattered twice etc.) and these equations iterated to convergence (see e.g. Kylafis and Bahcall 1987; Xilouris et al. 1998; Xilouris et al. 1999; Tuffs et al. 2004).”
Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size–luminosity relations (2008, methodology): “The sophisticated dust/star galaxy model of Popescu et al. (2000) and Tuffs et al. (2004) incorporates clumpiness and an explicit treatment of various grain compositions and sizes within a 3D distribution.”
Modelling the spectral energy distribution of galaxies - V. The dust and PAH emission SEDs of disk galaxies (2010, methodology): “…diffuse structures can affect the amplitude and wavelength dependence both of the UV/optical attenuation and of the dust emission (Kuchinski et al. 1998, Bianchi et al. 2000a, Witt & Gordon 2000, Misselt et al. 2001, Misiriotis & Bianchi 2002, Pierini et al. 2004, Tuffs et al. 2004, Bianchi 2008).”
On the galaxy stellar mass function, the mass-metallicity relation, and the implied baryonic mass function (2008, methodology): “Notably, Driver et al. (2007) obtain the largest value of f s and the method uses comparisons of discs and bulges viewed at various orientations to constrain their dust model (Tuffs et al. 2004).”