The jackknife mean (${\overline{\mathit{C}}}_{\ell }^{\mathrm{JK}}$) before (in blue) and after (in red) correcting for the jackknife footprint is shown in comparison to the original angular power spectra computed for the entire footprint C_ℓ. The lines and error bars represent the mean and spread across ten realisations. The difference is scaled as a function of the sample covariance standard deviation (σ_S i.e. the square root of the diagonals C_S) with grey bands representing 2% standard deviations from the C_ℓ for the entire footprint. The figure is divided into subplots for each angular auto and cross spectra pair, where P denotes overdensity, and E- and B-modes from weak lensing and the numbers 0 and 1 denote the tomographic bin. The sky correction is important for correcting the auto spectra for angular clustering but otherwise the correction has a minimal effect with the exception of a few cross-spectra (in particular P0 × E1).