%0 Generic %1 takeda2002energy %A Takeda, M. %A Sakaki, N. %A Honda, K. %A Chikawa, M. %A Fukushima, M. %A Hayashida, N. %A Inoue, N. %A Kadota, K. %A Kakimoto, F. %A Kamata, K. %A Kawaguchi, S. %A Kawakami, S. %A Kawasaki, Y. %A Kawasumi, N. %A Mahrous, A. M. %A Mase, K. %A Mizobuchi, S. %A Morizane, Y. %A Nagano, M. %A Ohoka, H. %A Osone, S. %A Sasaki, M. %A Sasano, M. %A Shimizu, H. M. %A Shinozaki, K. %A Teshima, M. %A Torii, R. %A Tsushima, I. %A Uchihori, Y. %A Yamamoto, T. %A Yoshida, S. %A Yoshii, H. %D 2002 %K agasa %R 10.1016/S0927-6505(02)00243-8 %T Energy determination in the Akeno Giant Air Shower Array experiment %U http://arxiv.org/abs/astro-ph/0209422 %X Using data from more than ten-years of observations with the Akeno Giant Air Shower Array (AGASA), we published a result that the energy spectrum of ultra-high energy cosmic rays extends beyond the cutoff energy predicted by Greisen, and Zatsepin and Kuzmin. In this paper, we reevaluate the energy determination method used for AGASA events with respect to the lateral distribution of shower particles, their attenuation with zenith angle, shower front structure, delayed particles observed far from the core and other factors. The currently assigned energies of AGASA events have an accuracy of $\pm$25% in event-reconstruction resolution and $\pm$18% in systematic errors around 10$^20$eV. This systematic uncertainty is independent of primary energy above 10$^19$eV. Based on the energy spectrum from 10$^14.5$eV to a few times 10$^20$eV determined at Akeno, there are surely events above 10$^20$eV and the energy spectrum extends up to a few times 10$^20$eV without a GZK-cutoff.

@misc{takeda2002energy, abstract = {Using data from more than ten-years of observations with the Akeno Giant Air Shower Array (AGASA), we published a result that the energy spectrum of ultra-high energy cosmic rays extends beyond the cutoff energy predicted by Greisen, and Zatsepin and Kuzmin. In this paper, we reevaluate the energy determination method used for AGASA events with respect to the lateral distribution of shower particles, their attenuation with zenith angle, shower front structure, delayed particles observed far from the core and other factors. The currently assigned energies of AGASA events have an accuracy of $\pm$25% in event-reconstruction resolution and $\pm$18% in systematic errors around 10$^{20}$eV. This systematic uncertainty is independent of primary energy above 10$^{19}$eV. Based on the energy spectrum from 10$^{14.5}$eV to a few times 10$^{20}$eV determined at Akeno, there are surely events above 10$^{20}$eV and the energy spectrum extends up to a few times 10$^{20}$eV without a GZK-cutoff.}, added-at = {2015-02-03T18:36:10.000+0100}, author = {Takeda, M. and Sakaki, N. and Honda, K. and Chikawa, M. and Fukushima, M. and Hayashida, N. and Inoue, N. and Kadota, K. and Kakimoto, F. and Kamata, K. and Kawaguchi, S. and Kawakami, S. and Kawasaki, Y. and Kawasumi, N. and Mahrous, A. M. and Mase, K. and Mizobuchi, S. and Morizane, Y. and Nagano, M. and Ohoka, H. and Osone, S. and Sasaki, M. and Sasano, M. and Shimizu, H. M. and Shinozaki, K. and Teshima, M. and Torii, R. and Tsushima, I. and Uchihori, Y. and Yamamoto, T. and Yoshida, S. and Yoshii, H.}, biburl = {https://www.bibsonomy.org/bibtex/271b5a78894025045d0a06eef10607d77/watz}, description = {[astro-ph/0209422v3] Energy determination in the Akeno Giant Air Shower Array experiment}, doi = {10.1016/S0927-6505(02)00243-8}, interhash = {5bab7e9992aee84132f68c46d9dac6cf}, intrahash = {71b5a78894025045d0a06eef10607d77}, keywords = {agasa}, note = {cite arxiv:astro-ph/0209422v3Comment: accepted to Astroparticle Physics, 29pages, 17+1 figures, elsart.cls The AGASA exposure is $5.1\cdot 10^{16}$ $m^2$ sr s until July 2002}, timestamp = {2015-02-03T19:44:17.000+0100}, title = {Energy determination in the Akeno Giant Air Shower Array experiment}, url = {http://arxiv.org/abs/astro-ph/0209422}, year = 2002 }