Forthcoming galaxy redshift surveys will make high precision measurements
of the clustering of galaxies on scales in excess of 100/h Mpc. In
particular, the distortion of clustering due to the peculiar motions of
galaxies and the apparent scale of characteristic features in the galaxy
distribution have been proposed as tests of the cosmic acceleration. To obtain meaningful and robust constraints on dark energy, we need to understand any systematics in these measurements. I will present the predictions for redshift space distortions and the growth rate using the first consistent simulation of quintessence dark energy. These calculations demonstrate that despite the large scales considered, the widely used linear theory is not up to the job of modelling clustering in future surveys and, furthermore, its application can lead to catastrophic
errors. I will describe a new procedure for analysing redshift-space distortions which is a major improvement over linear theory and will allow us to make better use of the next generation of surveys.
The talk will cover the material in the papers: Jennings et al (arXiv:0908.1394, arXiv:1003.4282 & arXiv:1011.2842 )