| Project/Area Number |
12440053
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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 | Kagoshima University |
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Principal Investigator |
OMODAKA Toshihiro Kagoshima University, Faculty of Science, Professor, 理学部, 教授 (50129285)
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| Co-Investigator(Kenkyū-buntansha) |
MIYAJI Takeshi National Astronomical Observatory, Nobeyama Radio, Observatory, Associate Professor, 野辺山宇宙電波観測所, 助教授 (10182023)
KONDOU etsurou Communication Research Laboratory, Kashima Space Research Center, The head of the laboratory, 鹿島宇宙通信センター, 室長
SASAO Tetsuo National Astronomical Observatory, Earth Rotation Division, Professor, 地球回転研究系, 教授 (20000177)
HIROTA Tomoya Kagoshima University, Faculty of Science, Research Associate, 理学部, 助手 (10325764)
西尾 正則 鹿児島大学, 理学部, 助教授 (70135383)
近藤 哲朗 郵政省通信綜合研究所, 鹿島宇宙通信センター, 室長
三好 真 国立天文台, 地球回転研究系, 助手 (50270450)
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| Project Period (FY) |
2000 – 2002
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| Project Status |
Completed (Fiscal Year 2002)
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| Budget Amount *help |
¥12,700,000 (Direct Cost: ¥12,700,000)
Fiscal Year 2002: ¥1,400,000 (Direct Cost: ¥1,400,000)
Fiscal Year 2001: ¥1,200,000 (Direct Cost: ¥1,200,000)
Fiscal Year 2000: ¥10,100,000 (Direct Cost: ¥10,100,000)
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| Keywords | Phase-referencing VLBI / High-precision astrometry / Reference radio source / Project VERA / SiO maser sources / Cooled HEMT receiver / VLBI / maser / Quaser / quaser / quasar |
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| Research Abstract |
VERA (VLBI Exploration of Radio Astrometry) is a new VLBI ax mainly aimed at study of the structure and dynamics of our Galaxy through high precision phase-referencing VLBI astrometry of astronomical maser sources. VERA, with its dual-beam antenna system, will enable us to observe a galactic maser and an extra-galactic reference source simultaneously in order to remove the atmospheric fluctuation. In order for VERA to achieve a 10μ as level accuracy, allowing us to obtain parallaxes of maser sources in the whole Galaxy, it is required that the maser and reference source must be located within 2°each other. This requires a large number of reference sources spreading over Galactic plane because H2O(22GHz) and SiO(43GHz) masers which are the main targets, are mostly concentrated in the galactic plane. Hence the search for VLBI sources in the galactic plane is indispensable to the success of VERA. In order to search for 43GHz VLBI sources, we started to install the 43GHz cooled receiver to 34m antenna which belongs to Kashima Space Research Center, Communications Research Laboratory in these Funds. By this we will start a 43GHz survey of continuum radio sources in the galactic plane using this 34m telescope and Nobeyama 45m telescope. We constructed small-sized cooled dewar and has succeeded in cooling the receiver. Further, we incorporated the Local oscillator (this Grant-IN-Aid) and installed these components in 34m telescope. The system noise temperature, including atmospheric loss, was 300K. In this test observations, very serious problems arosed. As the antenna inclined, the antenna pointing accuracy become significantly poor due to both the bending and hanging down of the subreflector. This knotty problems was mainly settled by Satoru Morisaki, a graduate student of Kagoshima University. He also set up high-resolution acousto-optical spectrometers.
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