409 citations · 5.2k across the 139 of their papers we have counts for
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Ultra-high-energy hadronic physics at the Pierre Auger Observatory: muon measurements
Jan Ebr
The Pierre Auger Observatory, the world's largest observatory of ultra-high-energy cosmic rays (UHECR), offers a unique insight into the properties of hadronic interactions occurri…
Modified Characteristics of Hadronic Interactions in Ultra-high-energy Cosmic-ray Showers
Jan Ebr, Jiri Blazek, Jakub Vicha +4
Data from multiple experiments suggest that the current interaction models used in Monte Carlo simulations do not correctly reproduce the hadronic interactions in air showers produ…
Large-scale cosmic ray anisotropies with 19 years of data from the Pierre Auger Observatory
The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu +355
Results are presented for the measurement of large-scale anisotropies in the arrival directions of ultra-high-energy cosmic rays detected at the Pierre Auger Observatory during 19…
The distribution of ultra-high-energy cosmic rays along the supergalactic plane measured at the Pierre Auger Observatory
The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu +364
Ultra-high-energy cosmic rays are known to be mainly of extragalactic origin, and their propagation is limited by energy losses, so their arrival directions are expected to correla…
Search for photons above 10 eV by simultaneously measuring the atmospheric depth and the muon content of air showers at the Pierre Auger Observatory
The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu +364
The Pierre Auger Observatory is the most sensitive instrument to detect photons with energies above eV. It measures extensive air showers generated by ultra high energy c…
Measurement of the Depth of Maximum of Air-Shower Profiles with energies between and eV using the Surface Detector of the Pierre Auger Observatory and Deep Learning
The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu +364
We report an investigation of the mass composition of cosmic rays with energies from 3 to 100 EeV (1 EeV= eV) using the distributions of the depth of shower maximum $X_\ma…