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Fig. A.2.


Reproduction of Fig. 10 including galaxy shape noise for the f5(R) model without neutrinos. The effect of such noise is to reduce the discrimination efficiency from ΛCDM across all aperture scales, source redshifts, and statistics shown (with the exception of certain kurtosis scales as discussed in the text). In particular, the noise dominates the measured skewness and peak count distributions at each scale so that both statistics essentially lose all previous discrimination power between f5(R) and ΛCDM, although this would likely be mitigated by a denoising procedure.

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