Clustering of luminous red galaxies I: large scale redshift space distortions

TL;DR

This paper analyzes large-scale redshift space distortions in luminous red galaxies from SDSS DR6, providing measurements of cosmological parameters and testing gravity models using clustering data and mock simulations.

Contribution

It introduces a detailed modeling of redshift space distortions in LRG clustering, deriving cosmological constraints and testing gravity theories with SDSS data and simulations.

Findings

Estimated b=0.34 b1 0.03 from quadrupole analysis

Measured a_{0m}=0.245 b1 0.020 and b b1 0.09 from axips plane

Standard gravity consistent with data for a_8 between 0.80 and 0.92

Abstract

This is the first paper of a series where we study the clustering of LRG galaxies in the latest spectroscopic SDSS data release, DR6, which has 75000 LRG galaxies covering over 1 $Gpc^3/h^3$ at $0.15<z<0.47$. Here we focus on modeling redshift space distortions in $\xips$, the 2-point correlation in separate line-of-sight and perpendicular directions, on large scales. % and away from the line-of-sight. We use large mock simulations to study the validity of models and errors. We show that errors in the data are dominated by a shot-noise term that is 40% larger than the Poisson error commonly used. We first use the normalized quadrupole for the whole sample (mean z=0.34) to estimate $\beta=f(\Omega_m)/b=0.34 \pm 0.03$, where $f(\Omega_m)$ is the linear velocity growth factor and $b$ is the linear bias parameter that relates galaxy to matter fluctuations on large scales. We next use the full $\xips$ plane to find $\Omega_{0m}= 0.245 \pm 0.020$ (h=0.72) and the biased amplitude $b \sigma_8 = 1.56 \pm 0.09$. For standard gravity, we can combine these measurements to break degeneracies and find $\sigma_8=0.85 \pm 0.06$, $b=1.85 \pm 0.25$ and $f(\Omega_m)=0.64 \pm 0.09$. We present constraints for modified theories of gravity and find that standard gravity is consistent with data as long as $0.80<\sigma_8<0.92$. We also calculate the cross-correlation with WMAP5 and show how both methods to measure the growth history are complementary to constrain non-standard models of gravity. Finally, we show results for different redshift slices, including a prominent BAO peak in the monopole at different redshifts. (Abridged)