Galaxy luminosities, stellar masses, sizes, velocity dispersions as a function of morphological type

By Mariangela Bernardi, Francesco Shankar, Joseph B. Hyde, S. Mei, F. Marulli, R. Sheth. 2009

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We provide fits to the distribution of galaxy luminosity, size, velocity dispersion and stellar mass as a function of concentration index Cr and morphological type in the Sloan Digital Sky Survey (SDSS). (Our size estimate, a simple analogue of the SDSS cmodel magnitude, is new: it is computed using a combination of seeing-corrected quantities in the SDSS data base, and is in substantially better agreement with results from more detailed bulge/disc decompositions.) We also quantify how estimates of the fraction of ‘early’- or ‘late’-type galaxies depend on whether the samples were cut in colour, concentration or light profile shape, and compare with similar estimates based on morphology. Our fits show that ellipticals account for about 20 per cent of the r-band luminosity density, , and 25 per cent of the stellar mass density, ρ*; including S0s and Sas increases these numbers to 33 per cent and 40 per cent, and 50 per cent and 60 per cent, respectively. The values of and ρ*, and the mean sizes, of E, E+S0 and E+S0+Sa samples are within 10 per cent of those in the Hyde & Bernardi, Cr≥ 2.86 and Cr≥ 2.6 samples, respectively. Summed over all galaxy types, we find ρ*∼ 3 × 108 M⊙ Mpc−3 at z∼ 0. This is in good agreement with expectations based on integrating the star formation history. However, compared to most previous work, we find an excess of objects at large masses, up to a factor of ∼10 at M*∼ 5 × 1011 M⊙. The stellar mass density further increases at large masses if we assume different initial mass functions for elliptical and spiral galaxies, as suggested by some recent chemical evolution models, and results in a better agreement with the dynamical mass function. We also show that the trend for ellipticity to decrease with luminosity is primarily because the E/S0 ratio increases at large L. However, the most massive galaxies, M*≥ 5 × 1011 M⊙, are less concentrated and not as round as expected if one extrapolates from lower L, and they are not well fit by pure deVaucouleur laws. This suggests formation histories with recent radial mergers. Finally, we show that the age–size relation is flat for ellipticals of fixed dynamical mass, but, at fixed Mdyn, S0s and Sas with large sizes tend to be younger. Hence, samples selected on the basis of colour or Cr will yield different scalings. Explaining this difference between E and S0 formation is a new challenge for models of early-type galaxy formation.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/819ddf68a9da002203bdf04e2e46d46bdaa054f6

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Citations in the corpus

THE SIZE–VIRIAL RADIUS RELATION OF GALAXIES (2012, methodology): “C O ] 1 4 D ec 2 01 2 tions (SMFs) known to underestimate abundance of massive galaxies (Bernardi et al. 2010) and the double power law fit to the M∗ − M relation of Moster et al. (2012) does not capture the upturn in the relation at M∗ .”
The massive end of the luminosity and stellar mass functions: Dependence on the fit to the light profile (2013, methodology): “Finally, we computed k- and evolution corrections for each object following Bernardi et al. (2010), and hence, luminosities.”
Stellar masses of SDSS-III/BOSS galaxies at z ∼ 0.5 and constraints to galaxy formation models (2012, result): “On the other hand, the most recent redeterminations of the massive end of the local galaxy mass function (Bernardi et al. (2010)) give a higher mass density at the massive end, in better agreement with BOSS and the other high-z works.”
X-ray coronae in simulations of disc galaxy formation (2010, methodology): “…(Efstathiou et al. 1982; Mo et al. 1998; Syer et al. 1999), enabling the model to reproduce the abundance of morphological types observed in the local Universe (e.g. Driver et al. 2006, 2007; Fukugita et al. 2007; Bernardi et al. 2010; Parry et al. 2009). c© 2009 RAS ar X iv :1 00 5.”
The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, methodology): “…the models; (iii) fitting flattened two-dimensional models directly to the galaxy images, where the profile of the models is again parametrized by an R1/4 (e.g. Bernardi et al. 2003), or by an R1/4 bulge plus exponential disc (e.g. Gebhardt et al. 2003; Bernardi et al. 2010; Saglia et al. 2010).”
Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation (2016, methodology): “15 dex higher stellar masses than a Chabrier IMF (e.g., Bernardi et al. 2010).”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, methodology): “For the mass range we consider here, this is quite close to just assuming that all galaxies have recycled ∼ 55% of their stellar mass (i.e., ∫ Ṁsfr dt ∼ 1.8×M⋆,0), 11 which for a Chabrier (2003a) IMF is very similar to the commonly used “instantaneous recycling approximation” for all stars m > 1M⊙.”
Search for Gravitational Lensing Signatures in LIGO-Virgo Binary Black Hole Events (2019, background): “2018, arXiv e-prints, arXiv:1811.12907 Thorne, K. S. 1983, in Gravitational radiation, 1–57 Turner, E. L., Ostriker, J. P., & Gott, III, J. R. 1984, ApJ, 284, 1 Vallisneri, M., Kanner, J., Williams, R., Weinstein, A., & Stephens, B. 2015, in Journal of Physics Conference Series, Vol. 610, 012021 Vei”
GALEX–SDSS–WISE LEGACY CATALOG (GSWLC): STAR FORMATION RATES, STELLAR MASSES, AND DUST ATTENUATIONS OF 700,000 LOW-REDSHIFT GALAXIES (2016, background): “While ModelMag produces stable colors, the degree to which it will estimate the total light will depend on galaxy size, morphology (Bernardi et al. 2010; Taylor et al. 2011) and color gradient.”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “The characteristic Schechter function mass Mchar is larger for quiescent or spheroid-dominated galaxies, and the slope is much shallower (e.g. Bernardi et al. 2010).”
Revisiting the Hubble sequence in the SDSS DR7 spectroscopic sample: a publicly available Bayesian automated classification (2010, methodology): “As shown in the top panel of figure 2 this selection results in a significant fraction of galaxies with low probabilities of being elliptical galaxies (as also shown in Bernardi et al. 2010b).”
Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos (2014, methodology): “05 ≈ 2.7 for the Chabrier IMF (see, e.g., Table 2 in Bernardi et al. 2010).”
THE AVERAGE STAR FORMATION HISTORIES OF GALAXIES IN DARK MATTER HALOS FROM z = 0–8 (2012, methodology): “Using these combined data sets, we find that observations of the evolution of galaxy star formation rates and stellar masses can now be reconciled (see also Bernardi et al. 2010 and Moster et al. 2013).”
THE NATURE OF LINER-LIKE EMISSION IN RED GALAXIES (2011, background): “It could also be due to the higher fraction of flat systems (lenticular galaxies) in the faint sample (Bernardi et al. 2010).”
RECONSTRUCTING THE STELLAR MASS DISTRIBUTIONS OF GALAXIES USING S4G IRAC 3.6 AND 4.5 μm IMAGES. II. THE CONVERSION FROM LIGHT TO MASS (2014, unknown): “6 by 0.05 dex to 0.3 dex (see Bell & de Jong 2001; Z09; Bernardi et al. 2010).”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, background): “For old enough stellar populations (Age ∼ 5− 10 Gyr) with mc ∼ 1 the stellar M/L can equal or even exceed that of a Salpeter IMF.”
The ATLAS3D project – I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria (2010, background): “(5) As found by previous authors there is little scatter in the relation at the high-mass end, while at the lower mass-end some galaxies appear to be still in transition between the blue and red sequence (Strateva et al. 2001; Conselice 2006; van den Bergh 2007; Bernardi et al. 2010).”
A catalogue of 2D photometric decompositions in the SDSS-DR7 spectroscopic main galaxy sample: preferred models and systematics (2014, methodology): “The cModel magnitudes (defined in Bernardi et al. 2010) are calculated from the linear combination of the independently fit SDSS deV and Exp models that best fits the galaxy.”