| Project/Area Number |
08044057
|
|---|
| Research Category |
Grant-in-Aid for international Scientific Research
|
| Allocation Type | Single-year Grants |
|---|
| Section | Joint Research |
|---|
| Research Field |
素粒子・核・宇宙線
|
|---|
| Research Institution | The Univ.of Tokyo |
|---|
Principal Investigator |
KIFUNE Tadashi Institute for Cosmic Ray Research, The Univ.of Tokyo Professor, 宇宙線研究所, 教授 (40011621)
|
|---|
| Co-Investigator(Kenkyū-buntansha) |
MURAKI Yasushi STE Laboratory, Nagoya University, Professor, 太陽地球環境研究所, 教授 (70013430)
MORI Masaki Institute for Cosmic Ray Research, The Univ.of Tokyo, Associate Professor, 宇宙線研究所, 助教授 (80210136)
TAMURA Tadahisa Kanagawa University, Assistant Professor, 工学部, 助手 (90271361)
MATSUBARA Yutaka STE Laboratory, Nagoya University, Associate Professor, 太陽地球環境研究所, 助教授 (80202323)
TANIMORI Toru Tokyo Institute of Technology, Associate Professor, 理学部, 助教授 (10179856)
西島 恭司 東海大, 理学部, 助教授 (40202238)
水本 好彦 国立天文台, 大型光学赤外線望遠鏡計画推進部, 助教授 (20219653)
荻尾 彰一 東京工業大学, 理学部, 助手 (20242258)
林田 直明 東京大学, 宇宙線研究所, 助手 (50114616)
|
|---|
| Project Period (FY) |
1996 – 1997
|
| Project Status |
Completed (Fiscal Year 1997)
|
| Budget Amount *help |
¥6,500,000 (Direct Cost: ¥6,500,000)
Fiscal Year 1997: ¥3,300,000 (Direct Cost: ¥3,300,000)
Fiscal Year 1996: ¥3,200,000 (Direct Cost: ¥3,200,000)
|
|---|
| Keywords | Gamma Ray Astronomy / Pulsar / Supernova Remnant / Active Galactic Nuclei / Origin of Cosmic Rays / Sources of High Energy Gamma Rays / Air Cerenkov Lights / Gamma Ray Telescope |
|---|
| Research Abstract |
Our preceding study before the year 1995 has enabled us (i) to commence operation of our 3.8m telescope of imaging Cerenkov lights for gamma ray detection, in 1992 the next year of the launching of Compton gamma ray satellite, (ii) to prove the powerful efficiency of high resolution camera by using the camera of the highest angular resolution until 1996, (iii) to show the ability of observations at large zenith angles for detecting very high energy gamma rays in 10-100 TeV region from the data observing the Crab from the southern hemisphere. Based on these technical development, we have discovered 1 TeV gamma rays from PSR B 1706-44.
The results obtained in 1997 are : (1) Very high energy gamma rays (-1TeV) are emitted from a region displaced from the Vela pulsar position by about 0.1ﾟ, which is consistent with the position where the pulsar was born. By comparing the observed gamma ray intensity with X-ray's, the magnetic field in the emission region is estimated as weak as 4muG.(2) The energy spectrum of gamma rays from the Crab nebula is found to continue at least up to 50 TeV,which are the gamma rays of the highest energy that have ever been detected.(3) Very high energy gamma rays has been detected from a supernova remnant SN1006. The result demonstrates that the gamma rays are produced by about 100 TeV electrons, providing a direct evidence that these electrons are shock-acceletated in the north-east rim of the supernova remnant. (4) A hint of 1 TeV gamma rays has been obtained from a gamma ray pulsar PSR B 1509-58. The data in the last year (of a higher threshold energy) shows no indication of signal, suggesting a steep energy spectrum. (6) Other objects, such as a gamma ray burst, the Galactic center Sgr A^<**>, several active galactic nuclei, unidentified EGRET sources and close X-ray binaries, are observed in the 1997 fiscal year. The data are now under analysis.
|
