Left panel: Comparison of the posterior distributions of second- and third-order aperture statistics with a joint analysis within a KiDS-1000-like setup. The data vector and covariance matrix are estimated by the T17 simulations, and we use filter scales of (4, 8, 16, 32) arcmin. The Hubble parameter h and the dark energy equation-of-state are fixed to the T17 values. Right panel: Comparison of the combined second- and third-order aperture statistics with the combination of second-order aperture statistics with the equal-scale third-order aperture statistics. The corresponding data vector and model vector can be found in Fig. C.3.