| Project/Area Number |
01065002
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| Research Category |
Grant-in-Aid for Specially Promoted Research
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| Allocation Type | Single-year Grants |
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| Research Institution | Faculty of Science, Nagoya University |
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Principal Investigator |
FUKUI Yasuo Department of Physics, Nagoya University, Professor, 理学部, 教授 (30135298)
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| Co-Investigator(Kenkyū-buntansha) |
MIZUNO Akira Department of Physics, Nagoya University, Research Associate, 理学部, 助手 (80212231)
OGAWA Hideo Department of Physics, Nagoya University, Associate Professor, 理学部, 助教授 (20022717)
河鰭 公昭 名古屋大学, 理学部, 名誉教授 (60022513)
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| Project Period (FY) |
1989 – 1992
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| Project Status |
Completed (Fiscal Year 1992)
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| Budget Amount *help |
¥307,000,000 (Direct Cost: ¥307,000,000)
Fiscal Year 1992: ¥18,000,000 (Direct Cost: ¥18,000,000)
Fiscal Year 1991: ¥17,000,000 (Direct Cost: ¥17,000,000)
Fiscal Year 1990: ¥109,000,000 (Direct Cost: ¥109,000,000)
Fiscal Year 1989: ¥163,000,000 (Direct Cost: ¥163,000,000)
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| Keywords | radio astronomy / star formation / interstellar molecules / millimeter-wave astronomy / interstellar matter |
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| Research Abstract |
We have built the new 4m mm-wave telescope, and improved the sensitivity of the supercoducting receiver. The telescope shows a remarkably high capability in observing mm-wave radiation. The best receiver temperature achieved is as low as 20K in DSB,the best value reported so far in the literature. The main results from the research are as follows ;
1.Discovery of 62 molecular outflows. This number corresponds to one third of the total discovered so far.
2.Complete observations of the 13CO emission in the Orion A region, Taurus and Ophiuchus (150,000 spectra).
3.Complete survey for dense cores in the above three regions in the C18O emission (15,000 spectra).
4.CS survey for Orion and Ophiuchus (4,000 spectra).
5.Detection of the gas disk in GG Tau, a young T Tauri.
By analysing these data sets, we have obtained the basic properties of dense cores and their time scales, and also have located the molecular outflow as the main accretion phase in the protostellar evolution. These outcomes provide valuable observational constraints on star formation.
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