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Fig. 5


Projected two-point correlation function wp(rp) associated with the best-fitting power-law function (left side) and best-fit power-law parameters r0 and γ along with 68.3% and 95.4% joint confidence levels (right side) in four UV absolute magnitude subsamples (upper panel) and four stellar mass subsamples (lower panel). The symbols and error bars (see Sect. 3 for the error estimation method) denote measurements of the composite correlation function for different luminosity (circles) and stellar mass (squares) subsamples selected from VUDS survey in the redshift range 2 < z < 3.5. For clarity, offsets are applied both to the data points and best-fitting curves of the wp (rp), i.e. the values of wp(rp) and associated best fits for galaxy subsamples with increasing luminosity and stellar masses were staggered by 0.5 dex each. Error contours on the fit parameters are obtained taking into account the full covariance matrix. The 68.3% and 95.4% joint confidence levels are defined in terms of the corresponding likelihood intervals that we obtain from our fitting procedure.

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