Publication details for Silvia PascoliJennings, Elise, Baugh, Carlton M. & Pascoli, Silvia (2011). Modelling redshift space distortions in hierarchical cosmologies. Monthly Notices of the Royal Astronomical Society 410(3): 2081-2094.
- Publication type: Journal Article
- ISSN/ISBN: 0035-8711, 1365-2966
- DOI: 10.1111/j.1365-2966.2010.17581.x
- Keywords: Methods: numerical, Cosmology: theory, Large-scale structure of Universe.
- Further publication details on publisher web site
- Durham Research Online (DRO) - may include full text
Author(s) from Durham
The anisotropy of clustering in redshift space provides a direct measure of the growth rate of large-scale structure in the Universe. Future galaxy redshift surveys will make high-precision measurements of these distortions, and will potentially allow us to distinguish between different scenarios for the accelerating expansion of the Universe. Accurate predictions are needed in order to distinguish between competing cosmological models. We study the distortions in the redshift space power spectrum in Lambda cold dark matter (ΛCDM) and quintessence dark energy models, using large-volume N-body simulations, and test predictions for the form of the redshift space distortions. We find that the linear perturbation theory prediction is a poor fit to the measured distortions, even on surprisingly large scales k≥ 0.05 h Mpc−1. An improved model for the redshift space power spectrum, including the non-linear velocity divergence power spectrum, is presented and agrees with the power spectra measured from the simulations up to k∼ 0.2 h Mpc−1. We have found a density–velocity relation which is cosmology independent and which relates the non-linear velocity divergence spectrum to the non-linear matter power spectrum. We provide a formula which generates the non-linear velocity divergence P(k) at any redshift, using only the non-linear matter power spectrum and the linear growth factor at the desired redshift. This formula is accurate to better than 5 per cent on scales k < 0.2 h Mpc−1 for all the cosmological models discussed in this paper. Our results will extend the statistical power of future galaxy surveys.