Energy determination in the Akeno Giant Air Shower Array experiment

被引：324

作者：

Takeda, M

Sakaki, N

Honda, K

Chikawa, M

Fukushima, M

Hayashida, N

Inoue, N

Kadota, K

Kakimoto, F

Kamata, K

Kawaguchi, S

Kawakami, S

Kawasaki, Y

Kawasumi, N

Mahrous, AM

Mase, K

Mizobuchi, S

Morizane, Y

Nagano, M

Ohoka, H

Osone, S

Sasaki, M

Sasano, M

Shimizu, HM

Shinozaki, K

Teshima, M

Torii, R

Tsushima, I

Uchihori, Y

Yamamoto, T

Yoshida, S

Yoshii, H

机构：

[1] RIKEN, Inst Phys & Chem Res, Image Informat Div, Adv Comp Ctr, Wako, Saitama 3510198, Japan

[2] Yamanashi Univ, Fac Engn, Kofu, Yamanashi 4008511, Japan

[3] Kinki Univ, Dept Phys, Osaka 5778502, Japan

[4] Univ Tokyo, Inst Cosm Ray Res, Chiba 2778582, Japan

[5] Saitama Univ, Dept Phys, Urawa, Saitama 3388570, Japan

[6] Musashi Inst Technol, Fac Engn, Tokyo 1588557, Japan

[7] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan

[8] Nishina Mem Fdn, Tokyo 1130021, Japan

[9] Hirosaki Univ, Fac Sci & Technol, Hirosaki, Aomori 0368561, Japan

[10] Osaka City Univ, Dept Phys, Sumiyoshi Ku, Osaka 5588585, Japan

[11] Yamanashi Univ, Fac Educ, Kofu, Yamanashi 4008510, Japan

[12] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan

[13] Fukui Univ, Dept Space Commun Engn, Fukui 9108505, Japan

[14] Minist Posts & Telecommun, Commun Res Lab, Tokyo 1848795, Japan

[15] Natl Inst Radiol Sci, Chiba 2638555, Japan

[16] Chiba Univ, Dept Phys, Chiba 2638522, Japan

来源：

ASTROPARTICLE PHYSICS | 2003年 / 19卷 / 04期

基金：

日本学术振兴会;

关键词：

extensive air showers; ultra high energy cosmic rays; energy determination;

D O I：

10.1016/S0927-6505(02)00243-8

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using data from more than 10 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 [Rhys. Rev. Lett. 16 (1966) 748] and Zatsepin and Kuzmin [Zh. Eksp. Teor. Fiz. 4 (1966) 114]. 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 25% in event-reconstruction resolution and 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. (C) 2002 Published by Elsevier Science B.V.

引用

页码：447 / 462

页数：16

共 43 条

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