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Fig. 9.


Correlation matrix P defined in Eq. (50), obtained from the covariance matrix in a (w0, wa) flat cosmology, for an optimistic setting. Left panel: photometric survey combination, without cross-correlation. Right panel: cross-correlation term. The inclusion of cross-correlation between GCph and WL significantly reduces the correlation among the dark-energy parameters w0, wa and the standard parameters ns, h, and Ωb, 0. The FoC reduces from 1907 in the case with no cross-correlations to 824 in the GCph+WL+ case. This, in turn, leads to reduced uncertainties on all parameters.

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