The cosmic-ray energy spectrum observed with the surface detector of the telescope array experiment

T. Abu-Zayyad*, R. Aida, M. Allen, R. Anderson, R. Azuma, E. Barcikowski, J. W. Belz, D. R. Bergman, S. A. Blake, R. Cady, B. G. Cheon, J. Chiba, M. Chikawa, E. J. Cho, W. R. Cho, H. Fujii, T. Fujii, T. Fukuda, M. Fukushima, W. HanlonK. Hayashi, Y. Hayashi, N. Hayashida, K. Hibino, K. Hiyama, K. Honda, T. Iguchi, D. Ikeda, K. Ikuta, N. Inoue, T. Ishii, R. Ishimori, D. Ivanov, S. Iwamoto, C. C H Jui, K. Kadota, F. Kakimoto, O. Kalashev, T. Kanbe, K. Kasahara, H. Kawai, S. Kawakami, S. Kawana, E. Kido, H. B. Kim, H. K. Kim, J. H. Kim, J. H. Kim, K. Kitamoto, S. Kitamura, Y. Kitamura, K. Kobayashi, Y. Kobayashi, Y. Kondo, K. Kuramoto, V. Kuzmin, Y. J. Kwon, J. Lan, S. I. Lim, S. Machida, K. Martens, T. Matsuda, T. Matsuura, T. Matsuyama, J. N. Matthews, M. Minamino, K. Miyata, Y. Murano, I. Myers, K. Nagasawa, S. Nagataki, T. Nakamura, S. W. Nam, T. Nonaka, S. Ogio, M. Ohnishi, H. Ohoka, K. Oki, D. Oku, T. Okuda, A. Oshima, Shunsuke Ozawa, I. H. Park, M. S. Pshirkov, D. C. Rodriguez, S. Y. Roh, G. Rubtsov, D. Ryu, H. Sagawa, N. Sakurai, A. L. Sampson, L. M. Scott, P. D. Shah, F. Shibata, T. Shibata, H. Shimodaira, B. K. Shin, J. I. Shin, T. Shirahama, J. D. Smith, P. Sokolsky, B. T. Stokes, S. R. Stratton, T. Stroman, S. Suzuki, Y. Takahashi, M. Takeda, A. Taketa, M. Takita, Y. Tameda, H. Tanaka, K. Tanaka, M. Tanaka, S. B. Thomas, G. B. Thomson, P. Tinyakov, I. Tkachev, H. Tokuno, T. Tomida, S. Troitsky, Y. Tsunesada, K. Tsutsumi, Y. Tsuyuguchi, Y. Uchihori, S. Udo, H. Ukai, G. Vasiloff, Y. Wada, T. Wong, M. Wood, Y. Yamakawa, R. Yamane, H. Yamaoka, K. Yamazaki, J. Yang, Y. Yoneda, S. Yoshida, H. Yoshii, X. Zhou, R. Zollinger, Z. Zundel

*この研究の対応する著者

研究成果: Article査読

202 被引用数 (Scopus)

抄録

The Telescope Array (TA) collaboration has measured the energy spectrum of ultra-high energy cosmic rays (UHECRs) with primary energies above 1.6 × 1018 eV. This measurement is based upon four years of observation by the surface detector component of TA. The spectrum shows a dip at an energy of 4.6 × 1018 eV and a steepening at 5.4 × 1019 eV which is consistent with the expectation from the GZK cutoff. We present the results of a technique, new to the analysis of UHECR surface detector data, that involves generating a complete simulation of UHECRs striking the TA surface detector. The procedure starts with shower simulations using the CORSIKA Monte Carlo program where we have solved the problems caused by use of the "thinning" approximation. This simulation method allows us to make an accurate calculation of the acceptance of the detector for the energies concerned.

本文言語English
論文番号L1
ジャーナルAstrophysical Journal Letters
768
1
DOI
出版ステータスPublished - 2013 5 1

ASJC Scopus subject areas

  • 宇宙惑星科学
  • 天文学と天体物理学

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