The Millennium Galaxy Catalogue: the B-band attenuation of bulge and disc light and the implied cosmic dust and stellar mass densities

By S. Driver, C. Popescu, R. Tuffs, J. Liske, Alister W. Graham, P. Allen, R. Propris. 2007

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Based on our sample of 10 095 galaxies with bulge‐disc decompositions we derive the empirical BMGC-band internal attenuation‐inclination relation for galaxy discs and their associated central bulges. Our results agree well with the independently derived dust models of Tuffs et al., leading to a direct constraint on the mean opacity of spiral discs of τ f = 3.8 ± 0.7 (central face-on BMGC-band opacity). Depending on inclination, the BMGC-band attenuation correction varies from 0.2 to 1.1 mag for discs and from 0.8 to 2.6 mag for bulges. We find that, overall, 37 per cent of all BMGC-band photons produced in discs in the nearby Universe are absorbed by dust, a figure that rises to 71 per cent for bulge photons. The severity of internal dust extinction is such that one must incorporate internal dust corrections in all optical studies of large galaxy samples. This is particularly pertinent for optical Hubble Space Telescope comparative evolutionary studies as the dust properties will also be evolving. We use the new results to revise our recent estimates of the spheroid and disc luminosity functions. The implied stellar mass densities at redshift zero are somewhat higher than our earlier estimates: ρdiscs =

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

On the galaxy stellar mass function, the mass-metallicity relation, and the implied baryonic mass function (2008, methodology): “12 of Driver et al. 2007 for the effect modelled from face-on to edge-on).”
A CATALOG OF BULGE+DISK DECOMPOSITIONS AND UPDATED PHOTOMETRY FOR 1.12 MILLION GALAXIES IN THE SLOAN DIGITAL SKY SURVEY (2011, background): “Disks are known to be dusty (e.g., Driver et al. 2007, and references therein), and this dust can broaden the intrinsic disk/bulge luminosity-size or luminosity-color distributions.”
A COMPREHENSIVE ANALYSIS OF UNCERTAINTIES AFFECTING THE STELLAR MASS–HALO MASS RELATION FOR 0 < z < 4 (2010, background): “The effects of dust are also known to change depending on galaxy inclination (e.g., Driver et al. 2007).”
Quantifying the coexistence of massive black holes and dense nuclear star clusters (2009, methodology): “Starting with the total apparent B-band galaxy magnitude of 10.64 mag (RC3), we have applied a Galactic dust correction AB = 0.07 mag (Schlegel et al. 1998) and, assuming an inclination of 34 degrees, a (disc) inclination-attenuation correction of 0.25 mag (Driver et al. 2007).”
Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly (2009, background): “The dust density of SMGs at z < 0.5 (Column 9 of Table 1) is approximately 3% of the total local (0.013 < z < 0.18) dust budget of log ρdust = 5.57 +0.12 −0.17M⊙ Mpc −3 given by Driver et al. (2007) based on an assumed dustto-light ratio.”
A census of metals and baryons in stars in the local universe (2007, methodology): “…et al. (2001), (3) Fukugita et al. (1998) from the compilation of Pagel (2002), (4) Glazebrook et al. (2003), (5) Bell et al. (2003), (6) Rudnick et al. (2003), (7) Rudnick et al. (2006), (8) Panter et al. (2007), (9) Driver et al. (2007a), (10) Driver et al. (2007b), (11) Shankar et al. (2006).”
First X-ray-based statistical tests for clumpy-torus models: eclipse events from 230 years of monitoring of Seyfert AGN (2014, background): “With the exception of Cen A (see §5.6.1), we rely on Shao et al. (2007) and Driver et al. (2007), who derive the inclination dependence of dust extinction for disk-dominated galaxies.”
Measuring the galaxy–mass and galaxy–dust correlations through magnification and reddening (2009, methodology): “For example, using the attenuation-inclination relation for galaxy discs and their associated central bulges, Driver et al. (2007) quantified the mean attenuation of a large sample of galaxies and estimated Ωdiskdust ≃ 2 × 10 −6.”
Galaxy luminosities, stellar masses, sizes, velocity dispersions as a function of morphological type (2009, background): “It is about 20 per cent smaller than the value reported by Driver et al. (2007) (once shifted to the same IMF, for which we have chosen Chabrier 2003; see Table 2).”
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.”
Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size–luminosity relations (2008, methodology): “Combining their tables with the statistically determined average opacity τ fB = 3.8 ± 0.7 reported by Driver et al. (2007), Section 2 of this paper derives two new equations which can be used to easily correct the observed B, V, I, J and K-band disc scalelengths and central surface brightnesses for…”
Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: a Sloan Digital Sky Survey perspective (2008, background): “In order to try a more meaningful comparison with the results in Driver et al. (2007a), we can assume that all galaxies with stellar masses below 1010 M are pure discs.”
Galaxy and Mass Assembly (GAMA): ugriz galaxy luminosity functions (2011, methodology): “We make no attempt here to correct for intrinsic dust extinction within each galaxy, as was done by Driver et al. (2007), nor to extrapolate the Petrosian magnitudes to total, as done, for example, by Graham et al. (2005) and Hill et al. (2011).”
MegaMorph - multiwavelength measurement of galaxy structure: complete Sersic profile information from modern surveys (2012, background): “…2009; Suh et al. 2010) and discs (e.g., Bell & de Jong 2000; MacArthur et al. 2004; Tortora et al. 2010; Gonzalez-Perez et al. 2011) and centrally concentrated dust atten- uation (Driver et al. 2007; Masters et al. 2010) can produce similar effects (Möllenhoff et al. 2006; Pastrav et al. 2012).”
Galaxy And Mass Assembly (GAMA): mass–size relations of z < 0.1 galaxies subdivided by Sérsic index, colour and morphology (2014, background): “…centrally concentrated bulge superimposed on a young more diffuse disc, i.e. the bulge is more evident in the K band while the disc is more evident in the r band; see Driver et al. 2007a,b); (iv) and, to a much lesser degree, any metallicity gradients which may also exist (La Barbera et al. 2010).”
Empirical determination of the shape of dust attenuation curves in star-forming galaxies (2011, background): “…of sight, in combination with models for the dust distribution in galaxies, NIR photometry, or rotationcurves, the amount of attenuation suffered by starlight before it reaches the observer can be constrained (e.g. Giovanelli & Haynes 2002; Driver et al. 2007; Maller et al. 2009; Yip et al. 2010).”
The evolution of stellar mass and the implied star formation history (2008, methodology): “Driver et al. (2007) adopt the diet Salpeter IMF and using a survey of galaxies in the B band obtain a result of ∗ = 0.0054 ± 0.0008.”
Modelling the spectral energy distribution of galaxies - V. The dust and PAH emission SEDs of disk galaxies (2010, methodology): “We note here that the attenuation-inclination relation predicted for this fixed ratio of opacities in the two dust disks was found to successfully reproduce the observed attenuationinclination relation of a large and statistically completesample of galaxies from the Millennium Galaxy Catalogue Surve”