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The origin and nature of ultra high energy cosmic rays remains being amystery. However, great progress has been made in recent years due to theobservations performed by the Pierre Auger Observatory and Telescope Array. Inparticular, it is believed that the composition information of the cosmic raysas a function of the energy can play a fundamental role for the understandingof their origin. The best indicators for primary mass composition are the muoncontent of extensive air shower and the atmospheric depth of the showermaximum. In this work we consider a maximum likelihood method to perform masscomposition analyses based on the number of muons measured by underground muondetectors. The analyses are based on numerical simulations of the showers. Theeffects introduced by the detectors and the methods used to reconstruct theexperimental data are also taken into account through a dedicated simulationthat uses as input the information of the simulated showers. In order toillustrate the use of the method, we consider AMIGA (Auger Muons and Infill forthe Ground Array), the low energy extension of the Pierre Auger Observatorythat directly measures the muonic content of extensive air showers. We alsostudy in detail the impact of the use of different high energy hadronicinteraction models in the composition analyses performed. It is found thatdifferences of a few percent between the predicted number of muons have asignificant impact on composition determination.

Composition determination of cosmic rays from the muon content of the showers