Reduced shear (top left), magnification bias (top right), and combined (bottom) corrections relative to the observed angular shear auto-correlation spectra (excluding shot noise), for four different redshift bins. For the basic reduced shear correction, the relative size of the correction increases alongside redshift, as the correction term has an additional factor of the lensing kernel compared to the power spectra. The correction plateaus at higher redshifts, because the lensed light encounters the most non-linearity and clustering at lower redshifts. It also increases with ℓ, as convergence tends to be higher on smaller physical scales. For the basic magnification bias correction, the relative size of the correction also increases with redshift. At lower redshifts, the term is subtractive, as the magnification of individual galaxies dominates, leading to an overestimation of the galaxy density. Whereas, at higher redshifts, the dilution of galaxy density dominates, leading to an underestimation of the power spectra if the correction is not made. For the combined effect of the two corrections, the magnification bias correction effectively cancels out the reduced shear correction at the lowest redshifts. Meanwhile, at intermediate redshifts, the magnification bias is small, but additive; slightly enhancing the reduced shear correction. However, at the highest redshifts, the magnification bias is particularly strong, and the combined correction is significantly greater than at lower redshifts. The corrections seen here are in the case of the wCDM cosmology of Table 1.