Fig. 10

Top panel: projected correlation functions of VIPERS galaxies in the
redshift interval
0.5 < z < 1 for the
individual W1 and W4 fields as well as for the combined sample. As a comparison, the
± 1σ dispersion among the mean
wp(rp) in the mocks is
shown with the shaded region and the non-linear mass prediction in the assumed
cosmology with the dotted curve. Bottom panel: relative difference
between the measured wp(rp)
in the W1 and W4 fields and the combined projected correlation function
.
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