The Intermediate-Scale Clustering of Luminous Red Galaxies

By Idit Zehavi, Daniel J. Eisenstein, Robert Nichol, M. Blanton, David W. Hogg, J. Brinkmann, J. Loveday, A. Meiksin, D. Schneider, Max Tegmark. 2004

179 citations recorded by the source corpus.

We report the intermediate-scale (0.3-40 h-1 Mpc) clustering of 35,000 luminous early-type galaxies at redshifts 0.16-0.44 from the Sloan Digital Sky Survey. We present the redshift space two-point correlation function ξ(s), the projected correlation function wp(rp), and the deprojected real space correlation function ξ(r), for approximately volume-limited samples. As expected, the galaxies are highly clustered, with the correlation length varying from 9.8 ± 0.2 to 11.2 ± 0.2 h-1 Mpc, dependent on the specific luminosity range. For the -23.2 < Mg < -21.2 sample, the inferred bias relative to that of L* galaxies is 1.84 ± 0.11 for 1 h-1 Mpc < rp ≲ 10 h-1 Mpc, with yet stronger clustering on smaller scales. We detect luminosity-dependent bias within the sample but see no evidence for redshift evolution between z = 0.2 and z = 0.4. We find a clear indication for deviations from a power-law in the real space correlation function, with a dip at ~2 h-1 Mpc scales and an upturn on smaller scales. The precision measurements of these clustering trends offer new avenues for the study of the formation and evolution of these massive galaxies.

Subfields: Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/a4da1d5330af101fcbbddf9cc9ccab70f2883fe0

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Citations in the corpus

The 6dF Galaxy Survey: baryon acoustic oscillations and the local Hubble constant (2011, background): “In a magnitude limited sample there is a correlation between luminosity and redshift, which establishes a correlation between bias and redshift (Zehavi et al. 2005).”
What Aspects of Galaxy Environment Matter? (2006, unknown): “(3) In practice we integrate out to π = 40 h−1 Mpc, following Zehavi et al. (2005).”
HALO OCCUPATION DISTRIBUTION MODELING OF CLUSTERING OF LUMINOUS RED GALAXIES (2008, methodology): “While the two-point auto-correlation functions in Zehavi et al. (2005a) are projected along the redshift direction, similar to those in Zehavi et al. (2005b), the LRG–”
The 2dF-SDSS LRG and QSO Survey: the LRG 2-point correlation function and redshift-space distortions (2006, methodology): “However, we note that in the other recent clustering studies, noisy covariances and anticorrelations were also noted (e.g. Scranton et al. 2002; Zehavi et al. 2002, 2005).”
Large-Scale Anisotropic Correlation Function of SDSS Luminous Red Galaxies (2007, methodology): “For our analysis, we use 46,760 LRGs over 3853 deg2 in the redshift range from 0.16 to 0.47, which is the same sample as the one used in previous analyses of SDSS LRG clustering (Zehavi et al. 2005; E05).”
Testing cosmological structure formation using redshift-space distortions (2008, methodology): “Using the Sloan Digital Sky Survey (SDSS; York et al. 2000), redshift-space distortions have also been measuredin the correlation function (Zehavi et al. 2005; Okumura et al.2008; Cabré & Gaztañaga 2008), and using an Eigenmode decomposition to separate real and redshift-space effects (Tegmark et…”
Acoustic oscillations in the SDSS DR4 luminous red galaxy sample power spectrum (2005, methodology): “Since the selection criteria are very complicated, involving both cuts in magnitude and in color, and also due to the steepness of the luminosity function the usual method of using only the luminosity function to determine radial selection function does not work here (Zehavi et al. 2005).”
Measurements of H(z) and DA(z) from the two-dimensional two-point correlation function of Sloan Digital Sky Survey luminous red galaxies (2011, background): “The collision corrections applied here are different from what has been suggested in Zehavi et al. (2005).”
Forecasting cosmological constraints from redshift surveys (2008, methodology): “Using the Sloan Digital Sky Survey (SDSS; York et al. 2000), redshiftspace distortions have also been measured in the correlation function (Zehavi et al. 2005; Okumura et al. 2008; Cabré & Gazta˜naga 2008), and using an Eigenmode decomposition to separate real and redshift-space effects (Tegmark…”
Density profiles of galaxy groups and clusters from SDSS galaxy–galaxy weak lensing (2006, background): “There have also been extensive studies of LRG clustering (Eisenstein et al. 2005a,b; Masjedi et al. 2005; Zehavi et al. 2005) from 10 h−1kpc to 100 h−1Mpc scales.”
Improved Forecasts for the Baryon Acoustic Oscillations and Cosmological Distance Scale (2007, methodology): “For the biased case at z ¼ 0:3, we use the MASS case with m ¼ 10 from Seo & Eisenstein (2005), which has galaxy bias similar to the luminous red galaxy (LRG) samples in SDSS (Zehavi et al. 2005).”
On the Robustness of the Acoustic Scale in the Low-Redshift Clustering of Matter (2006, result): “These mass thresholds at z = 0.3 give large-scale bias similar to that of the SDSS Luminous Red Galaxy sample (Eisenstein et al. 2001; Zehavi et al. 2005).”
The Shape of the Sloan Digital Sky Survey Data Release 5 Galaxy Power Spectrum (2007, background): “However, the addition of an extra term, b/b ¼ 0:85þ0:15L/L þ0:04(M M0:1r ) (Tegmark et al. 2004; Zehavi et al. 2005b), allows for a sharper increase in bias with luminosity, which is a better fit to the data.”
Modelling the anisotropic two-point galaxy correlation function on small scales and single-probe measurements of H(z), DA(z) and f(z)σ8(z) from the Sloan Digital Sky Survey DR7 luminous red galaxies (2012, background): “The collision corrections applied here are different from what has been suggested in Zehavi et al. (2005).”
Very Small Scale Clustering and Merger Rate of Luminous Red Galaxies (2005, methodology): “The lower limit in the Zehavi et al. (2005a) analysis was set to eliminate the incompleteness effects that are introduced by the 5500 fiber collision radius.”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, methodology): “This study complements correlation function measurements and HODmodels of the SDSS Luminous Red Galaxy (LRG) sample (Eisenstein et al. 2001, 2005b; Zehavi et al. 2005a; Zheng et al. 2009; Kazin et al. 2010; Watson et al. 2010), which probes the most luminous galaxies out to redshift z ≈ 0.45…”