Top-left: Binned n(z) for a three equipopulated bin tomographic set-up, measured from our mock catalogues that include realistic Gaussian shape noise and photo-z uncertainties in the simulation. Top-right, bottom-left, bottom-right: Cosmic shear, angular clustering, and galaxy-galaxy lensing components (respectively) of the 3×2pt data vector. We show in crosses the Pseudo-C_ℓ power spectra measured over 3000 realisations of our simulation for this chosen tomography. We bin the multipoles into ten log-spaced bandpowers and measure the signal in the range 100 ≤ ℓ ≤ 1500 for cosmic shear, and 100 ≤ ℓ ≤ 600 for galaxy clustering and galaxy-galaxy lensing. We plot the theoretical prediction in black alongside the measured data, and underneath each individual power spectrum we plot the normalised residuals, which we define as the fractional quantity ($C_{\ell }^{\mathrm{Measured}}/C_{\ell }^{\mathrm{Theory}})-1$, denoted as Δ_f on the y-axis label.