Validating the methodology for constraining the linear growth rate from
  clustering anisotropies
  Redshift-space clustering distortions provide one of the most powerful probes
to test the gravity theory on the largest cosmological scales. We perform a
systematic validation study of the state-of-the-art statistical methods
currently used to constrain the linear growth rate from redshift-space
distortions in the galaxy two-point correlation function. The numerical
pipelines are tested on mock halo catalogues extracted from large N-body
simulations of the standard cosmological framework. We consider both the
monopole and quadrupole multipole moments of the redshift-space two-point
correlation function, as well as the radial and transverse clustering wedges,
in the comoving scale range $10<r[$\Mpch$]<55$. Moreover, we investigate the
impact of redshift measurement errors on the growth rate and linear bias
measurements due to the assumptions in the redshift-space distortion model.
Considering both the dispersion model and two widely-used models based on
perturbation theory, we find that the linear growth rate is underestimated by
about $5-10\%$ at $z<1$, while limiting the analysis at larger scales, $r>30$
\Mpch, the discrepancy is reduced below $5\%$. At higher redshifts, we find
instead an overall good agreement between measurements and model predictions.
Though this accuracy is good enough for clustering analyses in current redshift
surveys, the models have to be further improved not to introduce significant
systematics in RSD constraints from next generation galaxy surveys. The effect
of redshift errors is degenerate with the one of small-scale random motions,
and can be marginalised over in the statistical analysis, not introducing any
statistically significant bias in the linear growth constraints, especially at
$z\geq1$.
