| Project/Area Number |
05452017
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| Research Category |
Grant-in-Aid for General Scientific Research (B)
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| Allocation Type | Single-year Grants |
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| Research Field |
Astronomy
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| Research Institution | The University of Tokyo |
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Principal Investigator |
NAKADA Yoshikazu The University of Tokyo, Faculty of Science, Associate Professor, 理学部, 助教授 (80011740)
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| Co-Investigator(Kenkyū-buntansha) |
ICHIKAWA Takashi The University of Tokyo, Faculty of Science, Research Associate, 理学部, 助手 (80212992)
HAMABE Masaru The Universty of Tokyo, Faculty of Science, Research Associate, 理学部, 助手 (00156415)
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| Project Period (FY) |
1993 – 1994
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| Project Status |
Completed (Fiscal Year 1994)
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| Budget Amount *help |
¥7,000,000 (Direct Cost: ¥7,000,000)
Fiscal Year 1994: ¥2,100,000 (Direct Cost: ¥2,100,000)
Fiscal Year 1993: ¥4,900,000 (Direct Cost: ¥4,900,000)
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| Keywords | red giant / Galaxy |
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| Research Abstract |
Red giants exhibit a range of properties which make them particularly useful to study a distant region of our galaxy. They are intrinsically bright, making it possible to detect and work on them at a distance of several kpc. They are abundant enough to search for the global structure of the galaxy.
A CCD camera installed onto the Kiso Schmidt Telescope was used to take images towards the anti-Galactic center. The medium band filters [79] and [81] were added to wide band filters V and I in order to discriminate carbon stars from M-type red giants.
Color magnitude diagrams obtained from these images showed two sequences which probably correspond to the Perseus arm and the outer edge of our Galaxy. Rather steep decline of the stellar density distribution was indicated from the apparently clear delineation of the lower sequence. Several stars were found on the carbon star branch of each color-color diagram. On the other hand, few stars were located on the M-type giant branch. The confirmation of this marked contrast is a subject of the future study.
Nearly one hundred IRAS sources were observed for the SiO maser emission with the Nobeyama 45m radio telescope. The detection rate was surprisingly low, partly due to the contamination by the carbon rich sources. They were also observed with the Kiso Schmidt telescope repeatedly to determine the period of their light variation. Development of the large format CCD camera was just started at Kiso Observatory. Survey observations using this new CCD camera will flourish in the futere study of the Galactic structure.
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