Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size–luminosity relations

By Alister W. Graham, C. Worley. 2008

253 citations recorded by the source corpus.

While galactic bulges may contain no significant dust of their own, the dust within galaxy discs can strongly attenuate the light from their embedded bulges. Furthermore, such dust inhibits the ability of observationally determined inclination corrections to recover intrinsic (i.e. dust-free) galaxy parameters. Using the sophisticated 3D radiative transfer model of Popescu et al. and Tuffs et al., together with the recent determination of the average face-on opacity by Driver et al. in nearby disc galaxies, we provide simple equations to correct (observed) disc central surface brightness and scalelengths for the effects of both inclination and dust in the B, V, I, J and K passbands. We then collate and homogenize various literature data sets and determine the typical intrinsic scalelengths, central surface brightness and magnitudes of galaxy discs as a function of morphological type. All galaxies have been carefully modelled in their respective papers with a Sersic R l/n bulge plus an exponential disc. Using the bulge magnitude corrections from Driver et al., we additionally derive the average, dust-corrected, bulge-to-disc flux ratio as a function of galaxy type. With values typically less than 1/3, this places somewhat uncomfortable constraints on some current semi-analytic simulations. Typical bulge sizes, profile shapes, surface brightness and deprojected densities are provided. Finally, given the two-component nature of disc galaxies, we present luminosity-size and (surface brightness)-size diagrams for discs and bulges. We also show that the distribution of elliptical galaxies in the luminosity-size diagram is not linear but strongly curved.

Subfields: Astronomy and Astrophysics, Computer Vision and Pattern Recognition, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/e69b0e0f56b5c48c69b6fc0d25a3152bb2b90c80

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In Astronomy and Astrophysics

1. P. Hopkins
2. M. Cappellari
3. L. Hernquist
4. Volker Springel
5. Simon D. M. White
6. T. Naab
7. C. Conroy
8. A. Dekel

In Computer Vision and Pattern Recognition

1. F. V. D. Bosch
2. M. Cappellari
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5. J. Trevor Mendel
6. Xiaohu Yang
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In Global and Planetary Change

1. F. V. D. Bosch
2. H. Mo
3. Simon D. M. White
4. C. Conroy
5. Xiaohu Yang
6. Volker Springel
7. A. Dutton
8. Pavel Kroupa

Citations in the corpus

• Quantifying the coexistence of massive black holes and dense nuclear star clusters (2009, methodology): “We do however note that subsequent reverberation mapping estimates (Peterson et al. 2005) ), a bulge (Knapen et al. 2003) with a dust corrected magnitude of −19.13 K-mag (Graham & Worley 2008), and a BH (Seth et al. 2008, see also Shields et al. 2008).”
• Forming a large disc galaxy from a z < 1 major merger (2008, background): “…particularly attractive as the mechanism for the survival/regrowth of gas (and then stellar) discs as it provides a natural explanation to the fact that more massive galaxies tend to have large B/D ratios (Benson et al. 2007; Graham & Worley 2008), while smaller galaxies are likely disc dominated.”
• Galaxy Zoo:bars in disc galaxies (2010, background): “…profiles (Kormendy & Kennicutt 2004), while classical bulges more closely follow a de Vaucouleur profile; however (as is seen in elliptical galaxies themselves), a range of profile shapes is observed in bulges which vary with the luminosity of the bulge (Graham & Worley 2008, and refer- Figure 7.”
• The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology (2012, methodology): “Bulgeless Disk Galaxies (2010) That the bulge-todisc flux ratios are smaller than those produced by LCDM simulations is pointed out by Graham & Worley (2008).”
• Photometric scaling relations of lenticular and spiral galaxies (2010, background): “In a broader context, scaling relations for spiral galaxy samples have been extensively studied revealing several fundamental relations (see Ravikumar et al. 2006; Graham & Worley 2008 as some of the latest works).”
• The CALIFA survey across the Hubble sequence: Spatially resolved stellar population properties in galaxies (2015, background): “However, the morphology (understood as the B/D ratio (Graham & Worley 2008)) can not be the only driver of the spatial variation of the SFH along all the Hubble sequence.”
• FORMING REALISTIC LATE-TYPE SPIRALS IN A ΛCDM UNIVERSE: THE ERIS SIMULATION (2011, background): “…ratio (as determined by a twocomponent fit to the i-band surface brightness profile), B/D = 0.35, is also typical of Sb spirals, which are characterized by a median (±68/2 per cent) value logB/D = −0.53+0.27−0.30, and of many Sbc galaxies, which have logB/D = −0.86+0.34−0.40 (Graham & Worley 2008).”
• Scaling relations and the fundamental line of the local group dwarf galaxies (2008, result): “This shallower slope is consistent with the lower end of the size-luminosity c© 2006 RAS, MNRAS 000, 1–18 relation of Graham & Worley (2008) while we extend their relation to lower masses.”
• THE HERSCHEL REFERENCE SURVEY: DUST IN EARLY-TYPE GALAXIES AND ACROSS THE HUBBLE SEQUENCE (2011, background): “In larger samples, Graham & Worley (2008) and Laurikainen et al. (2010) find values for this ratio of approximately 0.1– 0.2 for Sab-Sbc galaxies and 0.3–0.5 for S0 galaxies (their Figure 4), a somewhat larger change but still too low to explain the different dust-to-stellar-mass ratios.”
• Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, background): “Flattening of the slope at low luminosities has been reported previously (e.g., Graham & Guzman 2003; Graham & Worley 2008).”
• The formation of disc galaxies in high-resolution moving-mesh cosmological simulations (2013, methodology): “The observational data were taken from the compilation of literature catalogues3 considered in Graham & Worley (2008), and have been corrected for inclination and (internal) dust extinction effects by adopting the prescription described in section 2.2 of their work.”
• DISSIPATIONLESS FORMATION AND EVOLUTION OF THE MILKY WAY NUCLEAR STAR CLUSTER (2011, background): “5000 pc , albeit with a large scatter (Faber et al. 1997; Ferrarese et al. 2006; Graham & Worley 2008).”
• A CATALOG OF BULGE+DISK DECOMPOSITIONS AND UPDATED PHOTOMETRY FOR 1.12 MILLION GALAXIES IN THE SLOAN DIGITAL SKY SURVEY (2011, background): “Some previous studies (e.g., Graham & Worley 2008) have reported a dependence of (B/T ) on nb.”
• IMPROVED ESTIMATES OF THE MILKY WAY’S STELLAR MASS AND STAR FORMATION RATE FROM HIERARCHICAL BAYESIAN META-ANALYSIS (2014, result): “Graham & Worley (2008) find the average bulge-to-disk K-band flux ratio for a sample of 79 Sbc galaxies to be B Dlog( ) 0.82= − , which converts to an average B/T of 0.13; this compares well with our Milky Way value.”
• The formation and survival of discs in a ΛcDM universe (2008, result): “The D/T ratios obtained for our simulated galaxies, even for those with well-formed discs, are low in comparison with those of real spirals (e.g. Graham & Worley 2008).”
• Environmental effects on satellite galaxies: the link between concentration, size and colour profile (2008, background): “…therefore bear in mind that the real galaxy half-light radii are slightly higher than reported in these studies, especially for massive galaxies (see also Graham & Worley (2008) who use effective radii instead of half-light radii and find a steeper size-luminosity relation for early type galaxies).”
• BULGE n AND B/T IN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS (2008, background): “Graham & Worley (2008) report low B/D ratios across the Hubble sequence based on bulge-disk decomposition of K-band images of local spiral galaxies.”
• Bayesian galaxy shape measurement for weak lensing surveys – III. Application to the Canada–France–Hawaii Telescope Lensing Survey (2012, methodology): “E-mail: l.miller1@physics.ox.ac.uk C© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society Downloaded from https://academic.oup.com/mnras/article-abstract/429/4/2858/1008446 by Said Business School user on 09 March 2018 1 IN T RO D U C T I O N Weak gravit”