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Fig. 7


Upper panels: galaxy clustering ratio ηg,R(r,ΩmX,w) (dotted line) reconstructed from SDSS DR7 data assuming R = 14  h-1 Mpc and r = 3R, plotted as a function of ΩΛ (left), Ωm (centre) and w (right), after fixing the remaining cosmological parameters, shown in each panel, to the values that minimize the logarithmic posterior (24). Grey shading is the 1-sigma deviation around the mean, and it is computed from 30 block-jackknife resampling of the data. This uncertainty depends on cosmology (because of the redshift-distance conversion model) in a stochastic way (± 20% around the mean, for the cosmologies shown in the picture). We also show the predicted scaling of the mass clustering ratio (solid line) in the corresponding cosmology. The best set of cosmological parameters pf = (0.28, 0.45, −1.2, 73.8, 0.0213, 0.96) is the very one that minimizes the difference between theoretical predictions (line) and actual data (points). For SDSS DR7 data, we find ηg,R(3R,pf) = 0.0502±0.0036 on a scale R = 14  h-1 Mpc. Lower panels: two-dimensional marginalized constraints on a curved XCDM model in which both ΩX and w are allowed to vary. Gaussian priors are taken of Ωbh2 = 0.0213±0.0010, of H0 = 73.8±2.4 km s-1 Mpc-1 and of ns = 0.96±0.014 from BBN (Pettini et al. 2008), HST (Riess et al. 2011) and WMAP7 (Larson et al. 2011) determinations, respectively. Contours are plotted for ℒ/ℒmin < 2.3,6.17.

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