Browsing by Autor "K. Suga"

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Arrival directions of large air showers, low-mu showers and old-age low-mu air showers observed at St. Chacaltaya
(NASA Headquarters, 1985) T. Kaneko; K. Hagiwara; H. Yoshii; N. Martinić; L. Siles; P. Miranda; F. Kakimoto; Toru Obara; N. Inoue; K. Suga
Arrival directions of air showers with primary energies in the range 10 to the 16.5 power eV to 10 to the 18th power eV show the first harmonic in right ascension (RA) with amplitude of 2.7 + or - 1.0% and phase of 13-16h. However, the second harmonic in RA slightly seen for showers in the range 10 to the 18th power eV to 10 to the 19th power eV disappeared by accumulation of observed showers. The distribution of arrival directions of low-mu air showers with primary energies around 10 to the 15th power eV observed at Chacaltaya from 1962 to 1967 is referred to, relating to the above-mentioned first harmonic. Also presented in this paper are arrival directions of old-age low-mu air showers observed at Chacaltaya from 1962 to 1967, for recent interest in gamma-ray air showers.
Arrival-time distribution of muons and electrons in large air showers observed at 5200m above sea level
(American Institute of Physics, 1979) C. Aguirre; R. Anda; A. Trepp; F. Kakimoto; Y. Mizumoto; K. Suga; N. Izu; Y. Kamouchi; N. Inoue; Shinsuke Kawai
An experiment is going on at Mt. Chacaltaya in Bolivia (550 gcm−2 atmospheric depth) to observe arrival‐time distributions of muons and electrons in air showers above 1017 eV to study the early stage of longitudinal development related directly with the character of nuclear interactions and the composition of primary cosmic rays at these high energies. The preliminary results are presented at the Seminar.
Energetic delayed hadrons in large air showers observed at 5200m above sea level
(1985) T. Kaneko; K. Hagiwara; H. Yoshii; N. Martinić; L. Siles; P. Miranda; F. Kakimoto; I. Tsuchimoto; N. Inoue; K. Suga
Energetic delayed hadrons in air showers with electron sizes in the range 10 to the 6th power to 10 to the 9th power were studied by observing the delayed bursts produced in the shield of nine square meter scintillation detectors in the Chacaltaya air-shower array. The frequency of such delayed burst is presented as a function of electron size, core distance and sec theta.
Energy spectrum of surviving primary protons with energies(3÷30) TeV at5200 m a.s.l. and the cross-section for proton-air-nucleus collisions
(Springer Science+Business Media, 1975) C. Aguirre; A. Trepp; G. R. Mejía; K. Murakami; K. Kamata; Y. Toyoda; Tetsuhiko Maeda; Chiaki Yokoyama; P. K. MacKeown; K. Suga
Searches for Ultra–High‐Energy Gamma Rays from SN 1987A and Centaurus X‐3
(IOP Publishing, 1996) H. Yoshii; T. Baba; T. Kaneko; K. Suga; F. Kakimoto; S. Ogio; Y. Shirasaki; N. Gironda; M. Teshima; Y. Toyoda
Searches for gamma rays above 100 TeV from SN 1987A and above 50 TeV from Cen X-3 were carried out with an air shower array at Mount Chacaltaya over a period of 3 years. The array, which consists of 13 4 m2 and 28 1 m2 scintillation detectors, was located on a slope of about 30 facing southward to e ectively observe air showers coming from the directions of these sources. In the analysis, a selection by shower age parameter was applied to reduce the background due to showers initiated by protons or nuclei.