info:eu-repo/semantics/article
Depths of Maximum of Air-Shower Profiles at the Pierre Auger Observatory: II. Composition Implications.
Fecha
2014-12Registro en:
Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E.J.; Al Samarai, I.; et al.; Depths of Maximum of Air-Shower Profiles at the Pierre Auger Observatory: II. Composition Implications.; American Physical Society; Physical Review D: Particles, Fields, Gravitation and Cosmology; 90; 12; 12-2014; 1-12; 122006
2470-0010
2470-0029
CONICET Digital
CONICET
Autor
Aab, A.
Abreu, P.
Aglietta, M.
Ahn, E.J.
Al Samarai, I.
Allekotte, Ingomar
Almela, Daniel Alejandro
Asorey, Hernán Gonzalo
Bertou, Xavier Pierre Louis
Dasso, Sergio Ricardo
Dova, Maria Teresa
Etchegoyen, Alberto
Figueira, Juan Manuel
Filevich, Alberto
Garcia, Beatriz Elena
Gomez Berisso, Mariano
González, Nicolás Martín
Hampel, Matias Rolf
Hansen, Patricia Maria
Harari, Diego Dario
Jarne, Cecilia Gisele
Josebachuili Ogando, Mariela Gisele
Lucero, Luis Agustin
Mariazzi, Analisa Gabriela
Masías Meza, Jimmy Joel
Melo, Diego Gabriel
Micheletti, Maria Isabel
Mollerach, Maria Silvia
Pallotta, Juan Vicente
Piegaia, Ricardo Nestor
Platino, Manuel
Pieroni, Pablo Emanuel
Purrello, Víctor Hugo
Quel, Eduardo Jaime
Ravignani Guerrero, Diego
Ristori, Pablo Roberto
Roulet, Esteban
Rovero, Adrian Carlos
Sanchez, Federico Andrés
Sciutto, Sergio Juan
Sidelnik, Iván Pedro
Suarez, Federico
Supanitsky, Alberto Daniel
Taborda Pulgarin, Oscar Alejandro
Tapia Casanova, Alex Marcelo
Videla, M.
Wahlberg, Hernan Pablo
Wainberg, Oscar Isaac
Wundheiler, Brian
Pierre Auger Collaboration
Resumen
Using the data taken at the Pierre Auger Observatory between December 2004 and December 2012, we have examined the implications of the distributions of depths of atmospheric shower maximum (Xmax), using a hybrid technique, for composition and hadronic interaction models. We do this by fitting the distributions with predictions from a variety of hadronic interaction models for variations in the composition of the primary cosmic rays and examining the quality of the fit. Regardless of what interaction model is assumed, we find that our data are not well described by a mix of protons and iron nuclei over most of the energy range. Acceptable fits can be obtained when intermediate masses are included, and when this is done consistent results for the proton and iron-nuclei contributions can be found using the available models. We observe a strong energy dependence of the resulting proton fractions, and find no support from any of the models for a significant contribution from iron nuclei. However, we also observe a significant disagreement between the models with respect to the relative contributions of the intermediate components.