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Galaxy redshift surveys provide a distorted picture of the universe due to the non-Hubble component of galaxy motions. By measuring such distortions in the linear regime one can constrain the quantity β = OMEGA⁰. 6^/b where OMEGA is the cosmological density parameter and b is the (linear) bias factor for optically selected galaxies. In this paper we apply two techniques for estimating β from the Stromlo-APM redshift survey: (1) measuring the anisotropy of the redshift space correlation function in spherical harmonics, and (2) comparing the amplitude of the direction-averaged redshift space correlation function to the real space correlation function. We test the validity of these techniques, particularly whether the assumption of linear theory is justified, using two sets of large N-body simulations. We find that the first technique is affected by nonlinearities on scales up to ~30 h^-1^ Mpc. The second technique is less sensitive to nonlinear effects and so is more useful for existing redshift surveys. The Stromlo-APM survey data favours a low value for β, with β <~ 0. 6. A bias parameter b ~ 2 is thus required if OMEGA = 1. However, higher-order correlations measured from the APM galaxy survey indicate a low value for the bias parameter b ~ 1, requiring that OMEGA <~ 0. 5. We also measure the relative bias for samples of galaxies of various luminosity and morphological type and find that low-luminosity galaxies are roughly three times less biased than L^*^ galaxies. For the galaxy population as a whole, we measure a real space variance of galaxy counts in 8 h^-1^ Mpc spheres of (σ₈_²^) g_ = 0. 89 +/- 0. 05.
Loveday et al. (Sun,) studied this question.