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Fig. 10


Clustering ratio ηg,R estimated from Lh haloes in real space (diamonds) is shown as a function of the filtering radius R and of the correlation length r = 3R. We also plot the clustering ratio estimated after perturbing the cosmological redshift of haloes with random errors (triangles). These random velocities are drawn from a Gaussian distribution with standard deviation σcz = (1 + z)σu km s-1 with σu as indicated. Also shown is the theoretically predicted value of obtained by inserting into Eq. (8) the corresponding value of σu. The points and error bars correspond to the average and standard deviation of the mean of the measurements over 31Lh catalogues. Such error bars, in practice, would correspond to the typical uncertainty in a survey with 31 times larger volume and 10 times higher galaxy number density than the VIPERS W4 sample.

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