Distribution function approach to redshift space distortions. Part V:
  perturbation theory applied to dark matter halos
  Numerical simulations show that redshift space distortions (RSD) introduce
strong scale dependence in the power spectra of halos, with ten percent
deviations relative to linear theory predictions even on relatively large
scales (k<0.1h/Mpc) and even in the absence of satellites (which induce
Fingers-of-God, FoG, effects). If unmodeled these effects prevent one from
extracting cosmological information from RSD surveys. In this paper we use
perturbation theory (PT) and halo biasing model and apply it to the
distribution function approach to RSD, in which RSD is decomposed into several
correlators of density weighted velocity moments. We model each of these
correlators using PT and compare the results to simulations over a wide range
of halo masses and redshifts. We find that with an introduction of a physically
motivated halo biasing, and using dark matter power spectra from simulations,
we can reproduce the simulation results at a percent level on scales up to
k~0.15h/Mpc at z=0, without the need to have free FoG parameters in the model.
