| Project/Area Number |
06640363
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| Research Category |
Grant-in-Aid for General Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Research Field |
Astronomy
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| Research Institution | National Astronomical Observatory (NAO) |
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Principal Investigator |
KAMEYA Osamu National Astronomical Observatory, Mizusawa, Research Assistant, 水沢観測センター, 助手 (70202025)
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| Co-Investigator(Kenkyū-buntansha) |
TASUDA Shigeru Kagoshima Univ., Research Assistant, 工学部, 助手 (30253909)
MIYOSHI Makoto National Astronomical Observatory, Mizusawa, Research Assistant, 地球回転研究系, 助手 (50270450)
柴田 克典 国立天文台, 地球回転研究系, 助手 (60222030)
KUJI Seisuke National Astronomical Observatory, Mizusawa, Research Assistant, 地球回転研究系, 助手 (40132675)
SASAO Tetsuo National Astronomical Observatory, Mizusawa, Professor, 地球回転研究系, 教授 (20000177)
MIYAJI Takeshi National Astronomical Observatory, Nobeyama, Research Assistant (10182023)
佐藤 克久 国立天文台, 水沢観測センター, 助手 (90178715)
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| Project Period (FY) |
1994 – 1995
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| Project Status |
Completed (Fiscal Year 1995)
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| Budget Amount *help |
¥2,100,000 (Direct Cost: ¥2,100,000)
Fiscal Year 1995: ¥300,000 (Direct Cost: ¥300,000)
Fiscal Year 1994: ¥1,800,000 (Direct Cost: ¥1,800,000)
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| Keywords | Anmonia molecular lines / Gas kinetic temperature / filling factor / Acousto-Optical-Spectrometer / 分子雲 |
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| Research Abstract |
In the last year, performation of the Acousto-Optical-Spectrometer has checkedby observations of anmonia moelcuar lines using the Mizusawa 10m antenna.
We developed software for data reduction in this year. Therefore, huge amount of data was availiable to be analyzed. We also developed software for observations of using the Mizusawa 10m antenna in order to perform the galatic survey of temperature of molecular coluds more efficiently.
The observed regions are Taurus molecular cloud, Perseus molecular cloud, Orion A molecular coloud, Galactic center, W30H,and W49N.Gas kinetic temperature of these molecular coulds are measured by studying distribution of line intensities of (1,1-1,1) and (2,2-2,2) transitions of anmonia molecules. The result is that sizes of the molecular coluds, in which gas kinetic temperature is higher than 50K,are small.
We also studied distribution of filling factor which is a volume ratio of dense gas higher than 10000/cc in molecular clouds. Conparison of our results with the other anmonia data in different beam size indicates that the filling factor of Galatic center is different from that of Orion A molecular colud.
We have plan to observe more than 10,000 points for molecular coluds in order to study the detailed structure of the filling factor.
We also monitored the strength of water vaper maser emission from a famous active star forming region, W49N.
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