{"paper":{"title":"The Cosmic Ray Energy Spectrum Observed with the Surface Detector of the Telescope Array Experiment","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A.L. Sampson, A. Oshima, A. Taketa, B.G. Cheon, B.K. Shin, B.T. Stokes, C.C.H. Jui, D.C. Rodriguez, D. Ikeda, D. Ivanov, D. Oku, D.R. Bergman, D. Ryu, E. Barcikowski, E.J. Cho, E. Kido, F. Kakimoto, F. Shibata, G.B. Thomson, G. Rubtsov, G. Vasiloff, H.B. Kim, H. Fujii, H. Kawai, H.K. Kim, H. Ohoka, H. Sagawa, H. Shimodaira, H. Tanaka, H. Tokuno, H. Ukai, H. Yamaoka, H. Yoshii, I.H. Park, I. Myers, I. Tkachev, J. Chiba, J.D. Smith, J.H. Kim, J.I. Shin, J. Lan, J.N. Matthews, J.W. Belz, J. Yang, K. Hayashi, K. Hibino, K. Hiyama, K. Honda, K. Ikuta, K. Kadota, K. Kasahara, K. Kitamoto, K. Kobayashi, K. Kuramoto, K. Martens, K. Miyata, K. Nagasawa, K. Oki, K. Tanaka, K. Tsutsumi, K. Yamazaki, L.M. Scott, M. Allen, M. Chikawa, M. Fukushima, M. Minamino, M. Ohnishi, M.S. Pshirkov, M. Takeda, M. Takita, M. Tanaka, M. Wood, N. Hayashida, N. Inoue, N. Sakurai, O. Kalashev, P.D. Shah, P. Sokolsky, P. Tinyakov, R. Aida, R. Anderson, R. Azuma, R. Cady, R. Ishimori, R. Yamane, R. Zollinger, S.A. Blake, S.B. Thomas, S.I. Lim, S. Iwamoto, S. Kawakami, S. Kawana, S. Kitamura, S. Machida, S. Nagataki, S. Ogio, S. Ozawa, S.R. Stratton, S. Suzuki, S. Troitsky, S. Udo, S.W. Nam, S. Yoshida, S.Y. Roh, T. Abu-Zayyad, T.A. Stroman, T. Fujii, T. Fukuda, T. Iguchi, T. Ishii, T. Kanbe, T. Matsuda, T. Matsuura, T. Matsuyama, T. Nakamura, T. Nonaka, T. Okuda, T. Shibata, T. Shirahama, T. Tomida, T. Wong, V. Kuzmin, W. Hanlon, W.R. Cho, X. Zhou, Y. Hayashi, Y.J. Kwon, Y. Kitamura, Y. Kobayashi, Y. Kondo, Y. Murano, Y. Takahashi, Y. Tameda, Y. Tsunesada, Y. Tsuyuguchi, Y. Uchihori, Y. Wada, Y. Yamakawa, Y. Yoneda, Z. Zundel","submitted_at":"2012-05-22T22:38:48Z","abstract_excerpt":"The Telescope Array (TA) collaboration has measured the energy spectrum of ultra-high energy cosmic rays with primary energies above 1.6 x 10^(18) 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 x 10^(18) eV and a steepening at 5.4 x 10^(19) eV which is consistent with the expectation from the GZK cutoff. We present the results of a technique, new to the analysis of ultra-high energy cosmic ray surface detector data, that involves generating a complete simulation of ultra-high energy cosmic rays "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1205.5067","kind":"arxiv","version":3},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}