| Project/Area Number |
11440067
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| Research Category |
Grant-in-Aid for Scientific Research (B)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Astronomy
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| Research Institution | National Astronomical Observatory |
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Principal Investigator |
TATEMATSU Kenichi Radio Astronomy Division, National Astronomical Observatory, Associate Professor, 電波天文学研究系, 助教授 (40202171)
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| Co-Investigator(Kenkyū-buntansha) |
YAMAMOTO Satoshi Faculty of Science,University of Tokyo Associate, 大学院・理学系研究科, 助教授 (80182624)
SEKIMOTO Yutaro Radio Astronomy Division,National Astronomical Observatory,Associate Professor, 電波天文学研究系, 助教授 (70262152)
NOGUCHI Takashi Radio Astronomy Division,National Astronomical Observatory,Associate Professor, 電波天文学研究系, 助教授 (90237826)
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| Project Period (FY) |
1999 – 2001
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| Project Status |
Completed (Fiscal Year 2001)
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| Budget Amount *help |
¥10,000,000 (Direct Cost: ¥10,000,000)
Fiscal Year 2001: ¥1,200,000 (Direct Cost: ¥1,200,000)
Fiscal Year 2000: ¥1,700,000 (Direct Cost: ¥1,700,000)
Fiscal Year 1999: ¥7,100,000 (Direct Cost: ¥7,100,000)
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| Keywords | supernova remnants / molecular clouds / interaction / submillimeter wave / receiver |
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| Research Abstract |
We have made the survey of the interaction of supernova remnants with molecular clouds throughsubmillimeter-wave observations. By observing submillimeter 345-GHz carbon monoxicide (CO) and millimeter 115-GHz CO lines of rotational transitions, we have successfully obtained the evidence of the interaction observationally. For the supernova remnant W28, we detected the narrow-line velocity component dominant in the millimeter line and the broad velocity component dominant in the submillimeter line. The former represents the unshocked gas, and the latter represents the shock-accelerated gas. Such examples of the convincing evidence have been obtained so far in only three supernova remnants, and very important for research. By comparing with excitation calculations, we derived the physical parameters of the unshockd an shocked gas. By comparing the spatial distribution of them precisely, the unshocked gas is distributed 0.4-1.0 pc outer than the shocked gas with respect to the remnant center. This is the first observational example of the detailed structure of the shock front of the interaction zone of the supernova remnant and the molecular cloud. Furthermore, by using the Mt. Fuji Submillimeter-Wave Telescope, we have made a survey of the interaction in 345-GHz CO line and 492-GHz atomic carbon (CI) line. In three remnants, we have obtained observational results showing that the CI/CO intensity ratio tends to be high in the shocked gas. In W52SNR, we observed optically thinner 13CO line, and confirmed that larger intensity ratio represents larger abundance ratio. Such abundance enhancement has been reported in one supernova remnant 1C 443 previously, and our results provide very essential information of the interaction chemistry. We have developed a sensitive submillimeter receiver system for the survey of the interaction. It employs low-power-consumption (ikW) cryocooler. Its cryogenics performance has been confirmed as good as thatin the low-altitude laboratory.
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