Top-left: Binned n(z) for a tomographic 3×2pt analysis of our mock catalogues using three equipopulated bins, with no contribution from shape noise or photo-z uncertainty in the simulation. Top-right, bottom-left, bottom-right: Measured 3×2pt Pseudo-C_ℓ power spectra (cosmic shear, angular clustering, galaxy-galaxy lensing, respectively) measured over 3000 realisations for this chosen tomography, shown in crosses. We bin the power spectra 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. The solid black lines show the input model power spectra. Beneath each individual power spectrum we plot the normalised residuals of the data, defined as the fractional quantity ($C_{\ell }^{\mathrm{Measured}}/C_{\ell }^{\mathrm{Theory}})-1$, which we denote as Δ_f on the y-axis label. The vertical double-headed arrows in the off-diagonal subplots indicate that the fractional residuals, and their errors, for these spectra are extremely large due to the division by an extremely small signal.