Measurement of the Depth of Maximum of Extensive Air Showers above 10^18 eV

  title={Measurement of the Depth of Maximum of Extensive Air Showers above 10^18 eV},
  author={The Pierre Auger Collaboration},
We describe the measurement of the depth of maximum, Xmax, of the longitudinal development of air showers induced by cosmic rays. Almost four thousand events above 10^18 eV observed by the fluorescence detector of the Pierre Auger Observatory in coincidence with at least one surface detector station are selected for the analysis. The average shower maximum was found to evolve with energy at a rate of (106 +35/-21) g/cm^2/decade below 10^(18.24 +/- 0.05) eV and (24 +/- 3) g/cm^2/decade above… 

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  • Atom. Nucl. 56 (1993), 346; S.S. Ostapchenko, Nucl. Phys. Proc. Suppl. 151 (2006), 143; T. Pierog and K. Werner, Phys. Rev. Lett. 101 (2008), 171101; E.J. Ahn et al., Phys. Rev. D80
  • 2009
Pierre Auger Coll.
  • Nucl. Phys. Proc. Suppl
  • 2009
  • Phys. 3 (1995), 349; B.R. Dawson et al., Astropart. Phys. 5
  • 1996
Fly’s Eye Coll.
  • Phys. Rev. Lett
  • 1993
  • J. Phys. 56 (2006) A161; J. Bluemer, R. Engel and J. R. Hoerandel, Prog. Part. Nucl. Phys. 63, 293
  • 2009
  • 15th ICRC 12 (1977), 89; T.K. Gaisser et al., Proc. 16th ICRC 9 (1979), 258; J. Linsley and A.A. Watson, Phys. Rev. Lett. 46
  • 1981
Pierre Auger Coll.
  • Proc. 31st ICRC (2009),
  • 2009
  • 15th ICRC, 8, 353
  • 1977
  • Rev. D 79 (2009), 094008; R. Ulrich et al., Proc. 31st ICRC
  • 2009