| Co-Investigator(Kenkyū-buntansha) |
MCNAMARA Ber ニューメキシコ州立大学, 教授
OHTA Koji Kyoto University, 理学部, 助手 (50221825)
NAGATA Tetsuya Nagoya, University, 理学部, 助教授 (80208016)
DOI Mamoru University of Tokyo, 理学部, 助手 (00242090)
OGURA Katsuo Kokugakuin University, 文学部, 教授 (30102099)
SEKIGUCHI Masaki National Astronomical Observatory, 光学赤外線天文学研究系, 助手 (40216528)
SATO Fumio Tokyo Gakugei University, 教育学部, 教授 (70154094)
SAITO Mamoru Kyoto University, 理学部, 教授 (90012856)
KOBAYASHI Yukiyasu National Astronomical Observatory, 天文機器開発実験センター, 助教授 (50170361)
KODAIRA Kei'ichi National Astronomical Observatory, 台長 (60012845)
KAROJI Hiroshi National Astronomical Observatory, 大型光学赤外線望遠鏡計画推進部, 教授 (30221196)
WAKAMATSU Ken'ichi Gifu University, 教養部, 教授 (30021801)
TANIGUCHI Yoshiaki Tohoku University, 理学部, 助教授 (40192637)
YOSHIDA Michitoshi National Astronomical Observatory, 岡山天体物理観測所, 助手 (90270446)
SATO Shuji Nagoya University, 理学部, 教授 (50025483)
MCNAMARA Bernald j. University of New Mexico
OHTANI Hiroshi Kyoto University
|
|---|
| Research Abstract |
Drs.Yoshida and Aoki made near-infrared spectroscopy of a sample of broad line radio galaxies with moderate redshifte using KSPEC attached to the University of Hawaii 2.2m telescope at Mauna Kea, Hawaii. They detected the lines of Paalpha, Pabeta, and Halpha for seven radio galaxies andcompared the line profiles with each other. They then derived the amount of absorption in the broad line region of each galaxy from the analysis of the emission-line profiles, obtaining a hint to reveal the internal structure of broad line regions of radio galaxies.
Dr.Kobayashi made infrared observations using the infrard camera PICNIC fabricated by the national astronomical observatory. The camera was attached to the Australian national university 2.3m telescope at the Siding Spring Observatory. He carried out JHK-bands photo-polarimetry of the Galactic center region in order to determine the magnetic field structure there. He also dis a deep survey for fain galaxies toward the Galactic south pole regio
… More
n for the puropose of obtaining the cosmological parameters. The observations were carried out quite successfuly and the data is being processed now.
Using the 43m radio telescope at the National Radio Astronomy Observatory at Green Bank, West Virginia, U.S.A., Dr.Sato mapped the region (l=342*-20*, b=+2*-+30*) containing the molecular clouds in the Ophiuchus and Scorpius in the HI 21cm line. About 9500 spectra were obtained with the angular resolution of 20' , and the velocity resolution was 0.26 km/s. Preliminary analyzes clearly revealed filamentary structures in the HI channel maps at negative velocities, suggesting the correlation or anticorrelation between the distributions of the HI gas and that of the molecular gas.
Dr.Taniguchi visited Mauna Kea Observatories twice this fiscal year, one for the search for protogalaxies w the University of Hawaii 2.2m telescope and the other for the observations starburst galaxies with the JCMT 15m telescope.
For the protogalaxy search, he made a K-band deep survey of the Lockman HI hole by using of the 2.2m telescope with NICMOS3 camera. He obtained 30 hours of integration for one field at a level of K=23mag. The same field will be observed with Infrared Space Observatory at 7micron. Both the data will be utilized to study forming galaxies in the high-redshift universe.
For the JCMT observations, he made CO (J=3-2) observations of nearby starburst galaxies by using JCMT 15m submillimeter-wave telescope at Mauna Kea Observatories. He also made CO (J=1-0) observations of the same galaxies with use of the 45m radio telescope at the Nobeyama Radio Observatory. The comparison between the two transition data clearly showed that the molecular gas resided in the starburst and teh Seyfert galaxies tend to have denser and higher-temperature molecular clouds with respect to those in normal galaxy nuclei.
With their prism spectro-polarimeter PASP2 attached to the Wyoming Infrared Observatory 2.3m telescope and the 1.5-m telescope at Mt.Lemmon Observing Facility of University of Minnesota, Dr.Nagata made spectroscopy and spectro-polarimetry for several dozens of stars. He found absorption features due to the carbon-hydrogen bond in stars reddened in the diffuse interstellar medium. The distribution of interstellar ice has also been determined from the observation of stars behind the Taurus Dark cloud.
In collaboration with the Carnegie Institution, Drs.Sekiguchi and Kashikawa observed clusters of galaxies s as A2670, A194, A458, and A496 in BVR three color bands, using their mosaic CCD camera (4000x7000pixels) with a telescope at LasCampnas observatory. They found a significat difference in the luminosity function in the faint regions of these clusters. This difference is mostly due to dwarf galaxies. They are doing further data analysis and preparing articles. Less
|
