Early-Type Galaxies in the Sloan Digital Sky Survey. III. The Fundamental Plane

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

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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 (SDSS) using morphological and spectral criteria. The fundamental plane relation in this sample is Ro ∝ σ1.49±0.05I in the r* band. It is 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 a little. If the fundamental plane is used to quantify this evolution, then the apparent magnitude limit can masquerade as evolution; once this selection effect has been accounted for, the evolution is consistent with that of a passively evolving population that formed the bulk of its stars about 9 Gyr ago. One of the principal advantages of the SDSS sample over previous samples is that the galaxies in it lie in environments ranging from isolation in the field to the dense cores of clusters. The fundamental plane shows that galaxies in dense regions are slightly different from galaxies in less dense regions.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: a Sloan Digital Sky Survey perspective (2008, methodology): “Bernardi et al. (2003b) used estimates of the velocity dispersion that includes Fourier-fitting results, which, as mentioned above, overestimate the velocity dispersion for low-mass galaxies.”
Internal and Collective Properties of Galaxies in the Sloan Digital Sky Survey (2006, methodology): “The fundamental plane and the color-magnitudevelocity dispersion relation for early type galaxies with SDSS have been investigated by Bernardi et al. (2003a, 2005) Very recently Desroches et al. (2006) showed that the fundamental plane projections of elliptical galaxies depend on luminosity using…”
A Wide-Field Hubble Space Telescope Study of the Cluster Cl 0024+16 at z = 0.4. I. Morphological Distributions to 5 Mpc Radius (2003, background): “For the E+S0 population, fundamental plane (Djorgovski & Davis 1987; Dressler et al. 1987) studies indicate rest-frame Vband brightening of 0:4 0:6 mag by z ¼ 0:4 (van Dokkum & Franx 1996; Treu et al. 1999, 2001a; van Dokkum et al. 2001a; Bernardi et al. 2003).”
Families of dynamically hot stellar systems over 10 orders of magnitude in mass (2011, background): “However, some of these studies only focus on stellar systems of rather high luminosities/masses, excluding dwarf elliptical galaxies and globular clusters (e.g. Bender et al. 1992, 1993; Bernardi et al. 2003).”
The Evolution of the MBH-σ Relation (2005, background): “Later studies improved the accuracy of the local correlation (e.g., Tremaine et al. 2002, hereafter T02) and explored the relation between SMBH mass and other galaxy properties more fully (Wandel 2002; Ferrarese 2002; Marconi & Hunt 2003; Bernardi et al. 2003; Baes et al. 2003).”
A Theoretical Interpretation of the Black Hole Fundamental Plane (2007, methodology): “This yields similar results to the direct fitting method of Bernardi et al. (2003b) from the spheroid FP, which minimizes ∆ 2 = [ log(MBH) −α log(σ) −β log(Re) − δ ]2 , (5) and corresponds exactly to the method used in fitting the observations in Paper I, to which we compare.”
Density profiles of galaxy groups and clusters from SDSS galaxy–galaxy weak lensing (2006, background): “…dispersion (Faber 1973; Visvanathan & Sandage 1977; Djorgovski & Davis 1987; Kormendy & Djorgovski 1989; Bower et al. 1992; Roberts & Haynes 1994; Bernardi et al. 2003) of which the Faber-Jackson relation (Faber & Jackson 1976) is a projection; and simple light profiles, the de Vaucouleurs…”
Observational evidence for AGN feedback in early-type galaxies (2007, methodology): “The Bernardi et al. (2003a) catalogue is based primarily in the likelihood of the surface-brightness profile resembling a de Vaucouleurs law and a high concentration index.”
Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, methodology): “This was tested by Bernardi et al. (2003b, 2006) with a sample of ∼ 40, 000 SDSS morphology- and color-selected ETGs spanning a wide range of environmental conditions, from dense cluster cores to very low densities.”
THE SLOAN LENS ACS SURVEY. X. STELLAR, DYNAMICAL, AND TOTAL MASS CORRELATIONS OF MASSIVE EARLY-TYPE GALAXIES (2010, methodology): “We combine effective radii and stellar velocity dispersions to construct a dimensional mass, defined as Mdim ≡ 5reσ 2 e/2 G , (1) where the number 5 is the canonical choice for the virial coefficient of dynamical masses of massive ETGs (e.g., Bernardi et al. 2003; Cappellari et al. 2006).”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, result): “However the exponents of the FP were found to deviate significantly from the virial predictions, as confirmed by all numerous subsequent studies (e.g. Hudson et al. 1997; Scodeggio et al. 1998; Pahre et al. 1998; Colless et al. 2001; Bernardi et al. 2003).”
Evolution and Environment of Early-Type Galaxies (2005, methodology): “The luminosity function of this sample changes slightly with redshift (Bernardi et al. 2003b).”
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…”
The Fundamental Scaling Relations of Elliptical Galaxies (2005, methodology): “These simulated remnants exhibit a scatter about their mean FP of h 2i1/2 ¼ 0:062, comparable to both the observed scatter in the FP at optical wavelengths (e.g., Bernardi et al. 2003a) and that produced by the dissipational simulations.”
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).”
DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, background): “…are statistically indistinguishable from the best-fit correlations (over the rangeobserved) determined from volume-limited samples of (primarily field) early-type galaxies in the SDSS, in e.g. Shen et al. (2003); Bernardi et al. (2003, 2007); Gallazzi et al. (2006); von der Linden et al. (2007).”
Early and Rapid Merging as a Formation Mechanism of Massive Galaxies: Empirical Constraints (2005, methodology): “Using Sloan Digital Sky Survey (SDSS) data, the merger fraction for close pairs, with an average galaxy luminosity of Mg∗ = −20.13, was computed as 0.5% (Allam et al. 2004).”
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure (2012, background): “The argument rests on the observation that there are not significant differences in the fundamental plane of field ellipticals and cluster ellipticals (e.g., Kochanek et al. 2000; Bernardi et al. 2003; La Barbera et al. 2010).”
Feedback in simulations of disc-galaxy major mergers (2005, background): “…2003; Boylan-Kolchin et al. 2005, 2006; Robertson et al. 2006), a tight correlation between the velocity dispersion, effective radius, and luminosity, on which all ellipticals reside (Djorgovski & Davis 1987; Dressler et al. 1987; Bender et al. 1992; Bernardi et al. 2003; Padmanabhan et al. 2004).”