| Project/Area Number | 09304025 |
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| Research Category |
Grant-in-Aid for Scientific Research (A)
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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 | Nagoya University |
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Principal Investigator |
FUKUI Yasuo Nagoya University, School of Science, Professor, 大学院・理学研究科, 教授 (30135298)
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| Co-Investigator(Kenkyū-buntansha) |
DOBASHI Kazuhito Tokyo Gakugei University, Department of Astronomy and Earth Sciences, Assistant, 教育学部, 助手 (20237176)
MIZUNO Akira Nagoya University, School of Science, Assistant professor, 大学院・理学研究科, 助手 (80212231)
OGAWA Hideo Nagoya University, School of Science, Associate professor, 大学院・理学研究科, 助教授 (20022717)
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| Project Period (FY) |
1997 – 1998
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| Project Status |
Completed(Fiscal Year 1998)
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| Budget Amount *help |
¥30,000,000 (Direct Cost : ¥30,000,000)
Fiscal Year 1998 : ¥10,100,000 (Direct Cost : ¥10,100,000)
Fiscal Year 1997 : ¥19,900,000 (Direct Cost : ¥19,900,000)
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| Keywords | Radio astronomy / Star formation / Molecular cloud / Galaxies / Magellanic Clouds / Interstellar molecules |
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| Research Abstract |
In order to understand the formation process of populous stellar clusters in the Magellanic Clouds, we have carried out the most extensive observations of molecular clouds by using the 4 m mm-wave telescope. NANTEN, installed at Las Campanas. These observations have covered the Large Magellanic Cloud fully at a linear resolutions of 40 pc, in the ^<12>C0 (J=1-0) emission at 2.6 mm wavelength. The main results are summarized as follows ;
(1) There are more than 100 giant molecular clouds. Their mass ranges from l0^5 M<of sun> to 2 \ 10^6 M<of sun>.
(2) The line intensity of CO emission in the Large Magellanic Cloud is smaller by a factor of 3 than that in the Galaxy for giant molecular clouds having a similar mass.
(3) For the 55 giant molecular clouds significantly detected, we find that they are spatially well correlated with the youngest stellar clusters with < 10 Myr (26 of 55).
(4) By comparing the molecular clouds with their associated HII regions, we find giant molecular clouds are rapidly dissipated after formation of stellar clusters.
Total molecular mass is calculated as 4-7 \ 10^6 M<of sun>, corresponding to * 10 % of the neutral hydrogen mass.
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