Posterior distribution for the real KiDS-1000 data vector while the covariance is measured from the 1944 T17 galaxy shear catalogues. Here the E_n are compared to using all available combinations for the aperture filter radii θ_ap ∈ {4′,8′,14′,32′} and redshift bin combinations. We note that the prior (see Table 2) range on Ω_m is enlarged compared to the previous validation plots. The FoM values of the E_n-only or -only case should not be compared to Fig. 6, as priors of Ω_m bind their contours.