PoS - Proceedings of Science
Volume 395 - 37th International Cosmic Ray Conference (ICRC2021) - CRI - Cosmic Ray Indirect
Estimations of the muon content of cosmic ray air showers between 10 PeV and 1 EeV from KASCADE-Grande data
Presented by J.C. Arteaga Velazquez*  on behalf of  KASCADE-Grande Collaboration, W.D. Apel, J.C. Arteaga-Velázquez, K. Bekk, M. Bertaina, J. Bluemer, H. Bozdog, E. Cantoni, A. Chiavassa, F. Cossavella, K. Daumiller, V. de Souza, F. Di Pierro, P. Doll, R. Engel, D. Fuhrmann, A. Gherghel-Lascu, H.J. Gils, R. Glasstetter, C. Grupen, A. Haungs, D. Heck, J.R. Hoerandel, T. Huege, K.H. Kampert, D. Kang, H.O. Klages, K. Link, P. Luczak, H.J. Mathes, H.J. Mayer, J. Milke, C. Morello, J. Oehlschlaeger, S. . Ostapchenko, T. Pierog, H. Rebel, D. Rivera-Rangel, M. Roth, H. Schieler, S. Schoo, F.G. Schroeder, O. Sima, G. Toma, G.C. Trinchero, H. Ulrich, A. Weindl, J. Wochele and J. Zabierowskiet al. (click to show)
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Pre-published on: July 30, 2021
Published on: March 18, 2022
Measurements of KASCADE-Grande on the muon size in high energy extensive air showers (EAS) have provided evidence that the actual attenuation length of shower muons in the atmosphere is larger than the expectations from the hadronic interaction models QGSJET-II-04, EPOS-LHC and SIBYLL 2.3. This discrepancy is related with a deficient description of the shower muon content with atmospheric depth by MC models. To further explore the origin of the above anomaly, we have investigated the muon size as a function of the primary energy at different zenith angles using data from the KASCADE-Grande experiment. The procedure consisted in comparing the measured muon number flux against the predictions of a reference cosmic ray energy spectrum and from the observed difference to estimate the data/MC muon ratio that best describe the measurements. The ratio is then applied to the MC simulations and from here, we estimate the wanted muon content versus the primary energy. As a reference model, we employed the energy spectrum measured from the Pierre Auger observatory, while, for the different cosmic ray abundances, the GSF model. Results are presented using the QGSJET-II-04, EPOS-LHC, SIBYLL 2.3 and SIBYLL 2.3c models in the analysis procedure.
DOI: https://doi.org/10.22323/1.395.0376
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