Cosmic ray observables obtained with the best-fit parameters in the Mixed Composition Dip Model, corresponding to point A for (log₁₀(R∕km), log₁₀(L_γ∕(erg s⁻¹))) = (8.1,50.5) in Fig. 11. Top: simulated energy spectrum of UHECR (multiplied by E³ ) compared to data from Valiño et al. (2015). Spectra at Earth are grouped according to the mass number as follows: A = 1 (red), 2≤ A ≤ 4 (gray), 5 ≤ A ≤ 22 (green), 23 ≤ A ≤ 28 (cyan), total (brown). Bottom: average and standard deviation of the X_max distribution as predicted (assuming EPOS-LHC, Pierog et al. 2015, for UHECR-air interactions) for the model versus pure (¹ H (red), ⁴ He (grey), ¹⁴N (green), and ⁵⁶Fe (blue)) compositions, compared to data from Porcelli et al. (2015).