Early-type Galaxies in the Sloan Digital Sky Survey. II. Correlations between Observables

By Mariangela Bernardi, R. Sheth, James Annis, S. Burles, Daniel J. Eisenstein, Douglas P. Finkbeiner, David W. Hogg, Robert Lupton, David Schlegel, Mark SubbaRao and 21 more. 2003

236 citations recorded by the source corpus.

A magnitude-limited sample of nearly 9000 early-type galaxies, in the redshift range 0.01 ≤ z ≤ 0.3, was selected from the Sloan Digital Sky Survey using morphological and spectral criteria. The sample was used to study how early-type galaxy observables, including luminosity L, effective radius Ro, surface brightness Io, color, and velocity dispersion σ, are correlated with one another. Measurement biases are understood with mock catalogs that reproduce all of the observed scaling relations and their dependences on fitting technique. At any given redshift, the intrinsic distribution of luminosities, sizes, and velocity dispersions in our sample are all approximately Gaussian. A maximum likelihood analysis shows that σ ∝ L0.25±0.012, Ro ∝ L0.63±0.025, and Ro ∝ I-0.75±0.02 in the r* band. In addition, the mass-to-light ratio within the effective radius scales as Mo/L ∝ L0.14±0.02 or Mo/L ∝ M, and galaxies with larger effective masses have smaller effective densities: Δo ∝ M. These relations are approximately the same in the g*, i*, and z* bands. Relative to the population at the median redshift in the sample, galaxies at lower and higher redshifts have evolved only little, with more evolution in the bluer bands. The luminosity function is consistent with weak passive luminosity evolution and a formation time of about 9 Gyr ago.

Subfields: Astronomy and Astrophysics, Ecology, Instrumentation

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Citations in the corpus

The role of minor mergers in the recent star formation history of early-type galaxies (2007, background): “Note that the luminosity of a typical early-type galaxy, in the SDSS r-band, lies around M(r)∗ ∼ −21.15 (see Figure 2 in Bernardi et al. 2003).”
Ages and metallicities of early-type galaxies in the SDSS: new insight into the physical origin of the colour-magnitude and the Mg2-sigmaV relations (2006, result): “This has a slope of 0.25±0.01, i.e. very close to that found by Bernardi et al. (2003d) for a sample of co-added, high-quality spectra of SDSS early-type galaxies (see also Guzman et al. 1992; Colless et al. 1999).”
The Galaxy Luminosity Function and Luminosity Density at Redshift z = 0.1 (2002, result): “Our evolution results are similar to those found by Bernardi et al. (2003) for their sample of early-type galaxies.”
Evolutionary stellar population synthesis with MILES – I. The base models and a new line index system (2010, background): “• 200 kms−1 is roughly the mean velocity dispersion for the early-type galaxies in the Sloan Digital Sky Survey (Bernardi et al. 2003a,b,c).”
A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, background): “The observations shown are again from Marconi et al. (2004), based on the combination of the observations of Marzke et al. (1994); Kochanek et al. (2001); Nakamura et al. (2003); Bernardi et al. (2003); Sheth et al. (2003).”
Mapping Large-Scale Gaseous Outflows in Ultraluminous Galaxies with Keck II ESI Spectra: Variations in Outflow Velocity with Galactic Mass (2004, background): “…do so without disrupting the Tully-Fisher and Faber-Jackson relations between velocity, i.e. the depth of the gravitational potential, and stellar mass, V ∝ M1/4∗ (e.g. Bernardi et al. 2003), which show no obvious change at this scale (Zwaan et al. 1995; Sprayberry et al. 1995; Dale et al. 1999).”
The galaxy luminosity function at z ≃ 6 and evidence for rapid evolution in the bright end from z ≃ 7 to 5 (2014, methodology): “…catalogue using the MAG AUTO from SExtractor as an estimate for the total magnitude of the foreground galaxies, which then allowed an estimate of the velocity dispersion of the dark matter halo from the i-band absolute magnitude using the Faber-Jackson relation from Bernardi et al. (2003).”
LoCuSS: first results from strong-lensing analysis of 20 massive galaxy clusters at z= 0.2 (2009, unknown): “We therefore employ a Gaussian prior of σ⋆0 = (158±27)km s −1, making use of Bernardi et al. (2003)’s observational results on σ⋆.”
Local supermassive black holes, relics of active galactic nuclei and the X-ray background (2003, methodology): “It occurs in a region where the luminosity functions of early type galaxies are extrapolated and is due to the different functional forms adopted to fit the data (gaussian for Bernardi et al. (2003b), Schechter functions for the others).”
The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching? (2013, methodology): “The velocity dispersion, σV , of each potential lensing galaxy was estimated using the Faber-Jackson relation for earlytype galaxies from Bernardi et al. (2003), which gives a correlation between the absolute magnitude in the rest-frame i-band and σV at z = 0.”
The Dependence on Environment of the Color-Magnitude Relation of Galaxies (2003, background): “…1973; Faber & Jackson 1976; Visvanathan & Sandage 1977; Djorgovski & Davis 1987; Dressler et al. 1987; Kormendy & Djorgovski 1989; Roberts & Haynes 1994; Burstein et al. 1997; Terlevich, Caldwell, & Bower 2001; Eisenstein et al. 2003; Bernardi et al. 2003a, 2003b, 2003c; Blanton et al. 2003d).”
An Observational Determination of the Bolometric Quasar Luminosity Function (2006, background): “…estimates fromShankar et al. (2004) andMarconi et al. (2004) determined from local bulge velocity dispersion, mass, and luminosity function observations (Marzke et al. 1994; Kochanek et al. 2001; Cole et al. 2001; Nakamura et al. 2003; Blanton et al. 2003; Bernardi et al. 2003; Sheth et al. 2003).”
Black Holes in Pseudobulges and Spheroidals: A Change in the Black Hole-Bulge Scaling Relations at Low Mass (2008, methodology): “In Figure 3a we present the Faber-Jackson (Faber & Jackson 1976) relation for inactive elliptical galaxies from Bernardi et al. (2003), along with the locations of two spheroidal samples (Geha et al. 2002; Matković & Guzmán 2005).”
Feedback and the fundamental line of low-luminosity low-surface-brightness/dwarf galaxies (2002, background): “C© 2003 RAS, MNRAS 344, 1131–1144 D ow nloaded from https://academ ic.oup.com /m nras/article-abstract/344/4/1131/969782 by guest on 17 January 2020 V measuring the depth of the gravitational potential well, corresponding to roughly V ∝ M1/4∗ (e.g. Bernardi et al. 2003).”
The Masses of Nuclear Black Holes in Luminous Elliptical Galaxies and Implications for the Space Density of the Most Massive Black Holes (2006, methodology): “The seven galaxies with measuredM atMV 22:5 have average ¼ 311 25 km s 1, while equation (7) predicts only 250 km s 1 at MV 22:5 in agreement with the average at this luminosity for the SDSS sample (Bernardi et al. 2003).”
Colors, Magnitudes, and Velocity Dispersions in Early-Type Galaxies: Implications for Galaxy Ages and Metallicities (2004, methodology): “Specifically, because we k-correct following the procedure described in Bernardi et al. (2003a), all galaxies at the same redshift are assigned the same k-correction.”
SPIDER VIII - constraints on the stellar initial mass function of early-type galaxies from a variety of spectral features (2013, methodology): “Following Bernardi et al. (2003b), we have defined ETGs as bulgedominated systems (i.e. SDSS attribute fracDevr > 0.8, where fracDevr measures the fraction of galaxy light better fitted by a de Vaucouleurs, rather than an exponential, law), featuring passive spectra within the SDSS fibres (SDSS…”
Red mergers and the assembly of massive elliptical galaxies: the fundamental plane and its projections (2006, methodology): “Results for all SDSS wavebands are similar to the K-band fundamental plane (Bernardi et al. 2003a).”
Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, methodology): “…et al. 1995; Faber et al. 1995; Worthey 1997) and some studies infer no connection between metallicity and either velocity dspersion or age (e.g. Bernardi et al. 2003c, 2005) or find that the observed scaling of Mg and Hβ line profiles is consistent with more massive ellipticals having formed…”