| Project/Area Number |
14253001
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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 | 海外学術 |
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| Research Field |
Astronomy
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| Research Institution | The University of Tokyo |
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Principal Investigator |
YOSHII Yuzuru The University of Tokyo School of science, Institute of Astronomy, Professor, 大学院・理学系研究科, 教授 (00158388)
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| Co-Investigator(Kenkyū-buntansha) |
KOBAYASHI Yukiyasu National Astronomical Observatory, Div.of Optical & Infrared Astronomy, Professor, 光学赤外線天文学・観測システム研究系, 教授 (50170361)
KAWARA Kimiaki The University of Tokyo, Institute of Astronomy, Associate professor, 大学院・理学系研究科, 助教授 (50292834)
DOI Mamorui The University of Tokyo, Institute of Astronomy, Associate professor, 大学院・理学系研究科, 助教授 (00242090)
AOKI Tsutomu The University of Tokyo, Institute of Astronomy, Research Associate, 大学院・理学系研究科, 助手 (10251414)
MINEZAKI Takeo The University of Tokyo, Institute of Astronomy, Research Associate, 大学院・理学系研究科, 助手 (60292835)
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| Project Period (FY) |
2002 – 2004
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| Project Status |
Completed (Fiscal Year 2004)
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| Budget Amount *help |
¥30,030,000 (Direct Cost: ¥23,100,000、Indirect Cost: ¥6,930,000)
Fiscal Year 2004: ¥7,540,000 (Direct Cost: ¥5,800,000、Indirect Cost: ¥1,740,000)
Fiscal Year 2003: ¥9,360,000 (Direct Cost: ¥7,200,000、Indirect Cost: ¥2,160,000)
Fiscal Year 2002: ¥13,130,000 (Direct Cost: ¥10,100,000、Indirect Cost: ¥3,030,000)
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| Keywords | Observational Cosmology / Active Galactic Nuclei / Time Variability / Cosmic Dust / Infrared Instrumentation / Automatic Observation |
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| Research Abstract |
In order to reduce vast cost of fund and manpower for the operation of long term multi-wavelength monitoring of active galactic nuclei(AGNs), we have developed the hardware and software for unmanned automatic observation and remote operation (monitoring, in fact) from Japan. We have succeeded to develop the automatic observation system (, which judges the weather is suitable for observation and select best targets during the observation), and the remote monitoring and alert system (, which helps observers to monitor the observation and makes an alert when the observation is something wrong). Now, we usually carry out the observation under the operation from Japan without on-site observer, at a consecutive period of more than a month.
Along with the development of the observation system, we increased the number of targeted AGNs for multi-wavelength monitoring. Now it reaches about 70 AGNs, and about half of them are Seyfert galaxies, which are relatively nearby and low luminous. We found
… More
that almost all targeted Seyfert galaxies are variable, and could measure precise lag times between the optical variations and the near-infrared variations for several Seyfert galaxies that have been observed for enough period (NGC4151,Minezaki et al.2004;NGC5548,Suganuma et al.2004). We also found that the lag time is roughly proportional to the square root of the luminosity of AGN. This shows that our proposed idea of luminosity distance measurement will work well. In addition, we compared the infrared lag-time and the broad emission-line lag-time, that is, compared with the inner radius of the dust torus and the size of the broad emission-line region ofAGN, which is critical work for the unified model of Seyfert types of AGNs.
Moreover, our measurement of the infrared lag-time of AGN reaches to the distance of z=0.35,which is important for the measurement of the cosmological parameters, and we succeeded to observe a type Ia supernova in a targeted AGN, which is quite useful for the calibration of the distance measurement technique. Less
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