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Fig. A.1.


Histograms of aperture mass statistics corresponding to the distributions in Fig. 9 with galaxy shape noise included. The filtering scale is again ϑ = 0.586′, and sources are at redshift zs  =  2.0. The profiles of the noisy distributions have all changed compared to their noiseless counterparts. Overall, the f5(R) distributions are much more difficult to distinguish from ΛCDM, as well as from each other, than in the noiseless case at this scale. In particular, this level of noise washes out the discrimination power of peak counts above 3σ.

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