CLUSTERING IN THE 1.2-JY IRAS GALAXY REDSHIFT SURVEY .2. REDSHIFT DISTORTIONS AND XI(R(P),PI)

We examine the effect of redshift space distortions on the galaxy two-point correlation function xi(r(p), pi) as a function of separations parallel (r(p)) and perpendicular (pi) to the line of sight. Modelling of xi(r(p), pi) measured from a full-sky redshift survey of IRAS galaxies allows us to characterize the moments of the velocity distribution function of pairs of galaxies. We are guided in our parametrization of models by results from numerical simulations of cold dark matter (CDM) models. It is essential that the models for xi(r(p), pi) contain the effects of both the first and second moments of the velocity distribution function, as they distort the redshift space correlations in opposing directions. We develop a method of fitting for the amplitudes of the velocity moments, and show that we can recover the correct values in Monte Carlo realizations of the data drawn from N-body simulations. We find that the relative velocity dispersion of pairs of IRAS galaxies is sigma(r) = 317(-49)+40 km s-1 at r = 1 h-1 Mpc, consistent with previous estimates derived from optically selected galaxy catalogues. Unfortunately, the use of this result to estimate OMEGA via the cosmic virial theorem is thwarted by large systematic uncertainties, making the application of this theorem to existing redshift surveys of little value. We also fit for the mean relative streaming velocity of pairs, upsilon12(r), which describes the growth of fluctuations on both linear and non-linear scales. We find that upsilon12(r) = 167(-67)+99 km s-1 at r = 4 h-1 Mpc, so that on average, approximately half the Hubble expansion velocity of pairs at this separation is cancelled by infall. At r = 10 h-1 Mpc, the amplitude of the streaming is lower and upsilon12(r) = 109(-47)+64 km s-1. Linear perturbation theory then implies that OMEGA0.6/b = 0.45(-0.18)+0.27 on scales approximately 10-15 h-1 Mpc. The amplitude of upsilon12(r) is sensitive to the assumed shape of sigma(r). Our derived result for beta is intermediate between that found on approximately 1 h-1 Mpc scales and that found on 15-40 h-1 Mpc scales, arguing for either a strong dependence of beta on scale, or an error in the determination of beta on one or more scales.