The Velocity Dispersion Function of Early-Type Galaxies

By R. Sheth, Mariangela Bernardi, P. Schechter, S. Burles, Daniel J. Eisenstein, Douglas P. Finkbeiner, Joshua A. Frieman, Robert Lupton, David Schlegel, Mark SubbaRao and 4 more. 2003

185 citations recorded by the source corpus.

The distribution of early-type galaxy velocity dispersions, ϕ(σ), is measured using a sample drawn from the Sloan Digital Sky Survey database. Its shape differs significantly from that obtained by simply using the mean correlation between luminosity L and velocity dispersion σ to transform the luminosity function into a velocity function: ignoring the scatter around the mean σ-L relation is a bad approximation. An estimate of the contribution from late-type galaxies is also made, which suggests that ϕ(σ) is dominated by early-type galaxies at velocities larger than ~200 km s-1.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/cc79915f8f6de2a1dd396f9cbb9c76d99add94a5

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Citations in the corpus

Selection Bias in Observing the Cosmological Evolution of the M•-σ and M•-L Relationships (2007, methodology): “For the velocity-dispersion function we use the Sheth et al. (2003) SDSS results, augmented at the highend as prescribed by Bernardi et al. (2006) to account for an artificial high- cutoff in Sheth et al. Both functions are shown in Figure 1.”
The Masses of Nuclear Black Holes in Luminous Elliptical Galaxies and Implications for the Space Density of the Most Massive Black Holes (2006, methodology): “Bernardi et al. (2006) reprocessed the SDSS data and recovered a number of galaxies with larger dispersions than those used in Sheth et al. (2003).”
Galaxy luminosities, stellar masses, sizes, velocity dispersions as a function of morphological type (2009, methodology): “When fitting to equation (9), a reasonable understanding of the covariance between the fitted parameters can be got by asking that all parameter combinations give the same mean density (Sheth et al. 2003): ρX = φ∗ X∗ [(1 + α)/β] (α/β) .”
Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research (2004, methodology): “Wyithe & Loeb (2003) and the Shankar et al. (2004) used yet another, more direct approach, and employed the velocity dispersion function directly measured by Sheth et al. (2003) from SDSS data.”
Internal and Collective Properties of Galaxies in the Sloan Digital Sky Survey (2006, methodology): “The axis ratio of 0.2 due to the intrinsic thickness is consistent with previous works (Sheth et al. 2003).”
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies (2007, background): “The z ¼ 0 constraint is indicated by the dark gray area taken from the compilation of Marconi et al. (2004), which is based on a combination of different observational data (Kochanek et al. 2001; Nakamura et al. 2003; Bernardi et al. 2003; Sheth et al. 2003).”
A Theoretical Interpretation of the Black Hole Fundamental Plane (2007, methodology): “We adopt the distribution of velocity dispersionsσ from Sheth et al. (2003), and the early-type galaxy stellar mass function from Bell et al. (2003), with the addition of BCGs at high masses from Lin & Mohr (2004) (yielding a shallower power law-like falloff at high masses, as opposed to an…”
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).”
Gravitational Lens Time Delays: A Statistical Assessment of Lens Model Dependences and Implications for the Global Hubble Constant (2006, methodology): “…For the ellipticity, we use the Gaussian distribution with median e ¼ 0:3 and dispersion 0.16 that is consistent with observed distributions of isodensity contour shapes of elliptical galaxies (Bender et al. 1989; Saglia et al. 1993; Jorgensen et al. 1995; Rest et al. 2001; Sheth et al. 2003).”
The Cosmic Energy Inventory (2004, unknown): “The Sheth et al. (2003) estimate of the velocity dispersion function for early-type galaxies is dN = φ∗ ( σ σ∗ )α β Γ(α/β) dσ σ e−(σ/σ∗) β , (76) with α = 6.5, β = 1.93, σ∗ = 89 km s −1, φ∗ = 0.0020 Mpc −1.”
Local supermassive black holes, relics of active galactic nuclei and the X-ray background (2003, methodology): “For the velocity function we have considered only the error on φ⋆, the number density at σ⋆, since the other errors are strongly correlated among themselves (Sheth et al. 2003).”
Fundamental Planes and the Barless MBH-σ Relation for Supermassive Black Holes (2008, unknown): “A value of 400 km s −1 is used here due to the rapid decline in the number density of systems with higher velocity dispersions (Sheth et al. 2003; Bernardi et al. 2006).”
Self-regulated Growth of Supermassive Black Holes in Galaxies as the Origin of the Optical and X-Ray Luminosity Functions of Quasars (2003, methodology): “The reason is that the observed velocity function does not agree with that derived from the galaxy luminosity function and the Faber-Jackson relation (for a discussion, see Sheth et al. 2003).”
The stochastic gravitational-wave background from massive black hole binary systems: implications for observations with Pulsar Timing Arrays (2008, methodology): “The MBH population predicted at z = 0 is then found to be consistent with the BHMF derived observationally by inferring MBH masses from measurements of the bulge stellar velocity dispersion (Sheth et al. 2003).”
Gravitational lensing of gravitational waves: A statistical perspective (2018, unknown): “This is consistent with the observations (Jorgensen et al. 1995; Sheth et al. 2003).”
A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, methodology): “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).”