Fig. 17

Sensitivity of the clustering ratio to the cosmological model, through
left: isocontours of the function
displaying the relative
variation in the measured galaxy clustering ratio (with respect to
the true cosmological model of the simulated data), which are induced by choosing a
wrong cosmology in the redshift-distance conversion (i.e. a wrong guess of the
cosmological parameters [Ωm,ΩX]). The
redshift-space galaxy clustering ratio (left-hand side of Eq. (8)) is measured on scales
(R,r) = (5,15) h-1 Mpc
from the stacking of the 31 Lh halo catalogues (which were
built in a cosmology with Ωm = 0.27,ΩΛ = 0.73).
The isocontours measure the strength of the Alcock-Paczynski geometric distortions,
the deformation of the cell within which galaxies are counted. Right:
the corresponding variation of the predicted mass
clustering ratio (right-hand side of Eq. (8))
with varying cosmology.
This panel evidences the sensitivity of η to Ωm through the shape of the
transfer function.
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