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Mass composition of cosmic rays with energies from [1017.2]eV to [1020]eV using surface and fluorescence detectors of the Pierre Auger Observatory

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Figure

Figure 1. Mean (left) and standard deviation (right) of the distribution ofFor comparison, simulations for proton and iron primaries using three di Xmax as a function of energy.fferent hadronic interactionmodels are added [6].
Figure 1. Mean (left) and standard deviation (right) of the distribution ofFor comparison, simulations for proton and iron primaries using three di Xmax as a function of energy.erent hadronic interaction
Figure 4. Mean (top) and variance (bottom) of ln A for three different hadronic interaction models:EPOS-LHC (left), QGSJetII-04 (middle) and Sibyll2.3 (right) [6].
Figure 7. Mass fractions for p, He, N and Fe applied to parameterizedparts of the error bars show statistical uncertainties, while systematics are shown with thinner error bars

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