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The growth history of large-scale structure in the Universe is a powerfulprobe of the cosmological model, including the nature of dark energy. We studythe growth rate of cosmic structure to redshift $z = 0.9$ using more than$162{,}000$ galaxy redshifts from the WiggleZ Dark Energy Survey. We divide thedata into four redshift slices with effective redshifts $z =[0.2,0.4,0.6,0.76]$ and in each of the samples measure and model the 2-pointgalaxy correlation function in parallel and transverse directions to theline-of-sight. After simultaneously fitting for the galaxy bias factor werecover values for the cosmic growth rate which are consistent with our assumed$\Lambda$CDM input cosmological model, with an accuracy of around 20% in eachredshift slice. We investigate the sensitivity of our results to the details ofthe assumed model and the range of physical scales fitted, making closecomparison with a set of N-body simulations for calibration. Our measurementsare consistent with an independent power-spectrum analysis of a similardataset, demonstrating that the results are not driven by systematic errors. Wedetermine the pairwise velocity dispersion of the sample in a non-parametricmanner, showing that it systematically increases with decreasing redshift, andinvestigate the Alcock-Paczynski effects of changing the assumed fiducial modelon the results. Our techniques should prove useful for current and futuregalaxy surveys mapping the growth rate of structure using the 2-dimensionalcorrelation function.

The WiggleZ Dark Energy Survey: measuring the cosmic growth rate with the two-point galaxy correlation function