Showa25 |
1950 |
The Asahi hut (50m2 wooden) was built on
Mt.Norikura with the Asahi Bounty for Science. |
Showa28 |
1953 |
The Asahi hut developed into the Cosmic Ray Observatory,
University of Tokyo (1 Aug). |
Showa30 |
1955 |
The main building and research facilities of the Norikura
Observatory were built (with the opening ceremony on 29
Aug). |
Showa31 |
1956 |
-- The Cosmic Ray Division (composed of Air Shower
group and Emulsion group) of Institute for Nuclear Study,
University of Tokyo, began. |
Showa32 |
1957 |
The Norikura Observatory participated in IGY (international
Geophysical Year) activities, and began the air shower
observation. |
Showa33 |
1958 |
The emulsion chamber on Norikura started operation. |
Showa34 |
1959 |
-- Institute for Nuclear Study started observation
of air showers. |
Showa35 |
1960 |
-- The Emulsion group of Institute for Nuclear Study
developed large-size baloon.
-- The overseas special project (: international collaborations
in India, Brazil and Bolivia) of the Japan Society for
the Promotion of Science began. |
Showa41 |
1966 |
-- The baloon project of Emulsion group of Institute
for Nuclear Study, University of Tokyo, was transferred
to the Institute of Space and Aeronautical Science, University
of Tokyo. |
Showa43 |
1968 |
-- The emulsion group of Institute for Nuclear Study
started cosmic ray observation on Mt.Fuji with the emulsion
chamber. |
Showa47 |
1972
|
The full-time director was posted.
Construction of MUTRON started.
-- The cosmic dust group in the Cosmic Ray Division of
Institute for Nuclear Study was established. |
Showa48 |
1973 |
The ultra-high energy weak interation division was established.
The overseas special project (: International collaborations
in India, Brazil and Bolivia) was transferred from the
Japan Society for the Promotion of Science. |
Showa49 |
1974 |
The full-time chief clerk was posted. |
Showa50 |
1975 |
MUTRON was completed.
Construction of the Akeno Observatory started.
The ultra-high energy strong interaction division was
established. |
Showa51 |
1976 |
Institute for Cosmic Ray Research was established (25
Aug); The ultra-high energy strong interation division
was divided into the first and the second divisions, and
the three divisions (muon measurement, experimental meson
physics and cosmic ray study) were transferred from Institute
for Nuclear Study, University of Tokyo. Resultantly the
Institute was composed of six divisions and one observatory. |
Showa52 |
1977 |
The Akeno observatory became an attached institution
(18 Apr). |
Showa53 |
1978 |
The Akeno Observatory performed the opening ceremony
(6 Oct). |
Showa54 |
1979 |
The Akeno 1km2 air shower detector was completed.
The special facility for emulsion chamber at Mt.Fuji was
constructed.
The 16th International Cosmic Ray Conference was held
in Kyoto (Aug). |
Showa56 |
1981 |
Japan-China collaboration on the experiments using emulsion
chambers began. |
Showa57 |
1982 |
The division of cosmic ray detections (for guest staff)
was estabblished. |
Showa58 |
1983 |
The collaboration on the nucleon decay experiment at
the Kamioka mine began.
The facilities (i.e. mass spectrometer etc.) for the research
of the primary cosmic rays were installed. |
Showa61 |
1986 |
The small committee for the future plan examination
(I) was organized. |
Showa62 |
1987 |
The underground detector at Kamioka observed neutrino
burst from the supernova for the first time in the world.
Construction of the 100km2 wide area air shower
detector, named AGASA, at the Akeno Observatory was started.
The report from the small committee for the future plan
examination (I) was submitted. |
Showa63 |
1988 |
The underground detector at Kamioka observed the deficit
of neutrino flux from the sun. |
Heisei01 |
1989 |
The large increases of neutrons due to a solar flare
were observed at the Norikura Observatory (26 Sep). |
Heisei02 |
1990 |
The 100km2 wide area air shower detector,
AGASA, was completed at Akeno. |
Heisei03 |
1991 |
Construction of Super-Kamiokande began.
The small committee for the future plan examination (II)
was organized. |
Heisei04 |
1992 |
The division of the neutrino astrophysics was established
and the division of the cosmic ray detections (for guest
staff) was closed.
The gravitational wave group joined (belonging to the
muon measurement division)
The cangaroo project in Australia started, and observed
TeV gamma rays from a pulsar (PSR1706-44). |
Heisei05 |
1993 |
Construction of air shower gamma ray detector in Tibet
began. |
Heisei06 |
1994 |
The computer house was built at Kamioka (Jan).
The digging of a cave for SuperKamiokande was finished
(Jun).
A giant air shower with energy of 2×1020 eV
was observed at Akeno
The evaluation of the Institute achievements by outsiders
was carried out.
The anormalous zenith angle dependence of the atmospheric
neutrinos was observed at Kamioka. |
Heisei07 |
1995 |
The division of the neutrino astrophysics was abolished
and the Kamioka Observatory for the cosmic elementary
particle research was established (1 Apr)
The completion ceremony of Super-Kamiokande was held before
filling water (Nov). |
Heisei08 |
1996 |
The full-scale operation of Super-Kamiokande began (1
Apr) |
Heisei09 |
1997 |
The air shower gamma ray detector in Tibet was completed. |
Heisei10 |
1998 |
The discovery of finite neutrino masses by Super-Kamiokande
was officially announced (5 Jun).
Construction of the Kashiwa campus started (Nov). |
Heisei11 |
1999 |
The Research Center for Cosmic Neutrinos was established
(1 Apr).
The Cangaroo project 2 began in Australia.
Preparation of the Cangaroo project 3 began in Australia. |