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Fig. 2
Correlation matrix Corrgg built with the covariance of Eq. (24) for the galaxy autocorrelation, using a binning of width δl = 100 from lmin = 50 to lmax = 1950. The non-Gaussian term has a strong amplitude, contrary to the one in Corrκκ and Corrκg because of the very high noise reconstruction of the convergence 
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