| Co-Investigator(Kenkyū-buntansha) |
HAYASHI Saeko National Astronomical Observatory, 光学赤外線天文学研究系, 助手 (90183912)
NAKAGIRI Masao National Astronomical Observatory, 光学赤外線天文学研究系, 助手 (00124678)
NISHIMURA Tetsuo National Astronomical Observatory, 光学赤外線天文学研究系, 助教授 (90260017)
TAKATO Naruhisa National Astronomical Observatory, 大型光学赤外線望遠鏡計画推進部, 助手
KAROJI Hiroshi National Astronomical Observatory, 光学赤外線天文学研究系, 助教授 (30221196)
TAMURA Motohide National Astronomical Observatory, 光学赤外線天文学研究系, 助手 (00260018)
IYE Masanori National Astronomical Observatory, 大型光学赤外線望遠鏡計画推進部, 教授 (30111446)
YAMASHITA Takuya National Astronomical Observatory, 光学赤外線天文学研究系, 助手 (00211631)
GATLEY Ian National Optical Astronomical Observatory, 主任研究員
TANAKA Masuo Tokyo University. Faculty of Science, 理学部, 助手 (70188340)
WAKAMATSU Kenichi Gifu University. Liberal Arts Faculty, 教養部, 教授 (30021801)
DEGUCHI Shuji National Astronomical Observatory, 電波天文学研究系, 助手 (20197825)
YOSHII Yuzuru National Astronomical Observatory, 位置天文・天体力学研究系, 助教授 (00158388)
OKAMURA Sadanori Tokyo University. Faculty of Science, 理学部, 教授 (20114423)
TANIGUCHI Yoshiaki Tohoku University. Faculty of Science, 理学部, 助教授 (40192637)
MAIHARA Toshinori Kyoto University. Faculty of Science, 理学部, 助教授 (90025445)
NAGATA Tetsuya Kyoto University. Faculty of Science, 理学部, 助手 (80208016)
KAIFU Norio National Astronomical Observatory, 光学赤外線天文学研究系, 教授 (50011630)
SATO Shuji National Astronomical Observatory, 理学部, 教授 (50025483)
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| Budget Amount *help |
¥3,000,000 (Direct Cost: ¥3,000,000)
Fiscal Year 1993: ¥3,000,000 (Direct Cost: ¥3,000,000)
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| Research Abstract |
T.Nagata and N.Kobayashi have carried out spectropolarimetric observations for five infrared sources within 0.5 degree of the Galactic center in the wavelength from 1.4 to 4.2 microns using the 1.5m CTIO infrared telescope, Chile. They detected the polarization ; it is represented very well by a power law p(lambda), but all the five objects have polarization well in excess of this power law in the whole 2.8 - 4.2micron. This excess polarization might be caused by grains located in the general diffuse interstellar medium or grains specific to the inner Galaxy. The shape of the polarization increase seems different from that of the molecular cloud sources. The carrier of the 3.0 micron features is not distributed ubiquitously in the line of sight.
S.Deguchi measured the linear polarization of the extreme high-velocity water masers in NGC4258 at 22 GHz with the 37-m radio telescope at Haystack Observatory near Boston, Massachusetts, U.S.A., during July 6 - 8. Because of atmospheric and ins
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trumental troubles due to heat waves in the east coast, we could integrate the H2O spectra for about 2 hours each for the I, Q, and U components of the polarization. We found the degree of linear polarization less than 30 % and this will restrict the possible model of the high velocity masers in the NGC4258 galaxy.
K.Wakamatsu carried out an extensive redshift survey of Ophiuchus cD cluster with CTIO 1.5-m and 3.0-m Lick telescopes. The cluster was discovered by Wakamatsu and Malkan as the 3rd brightest X-ray cluster in the sky. The cluster is found to be accomplished with several irregular clusters and so to from "Ophiuchus supercluster". This supercluster may be connected with Hercules supercluster by a prominent wall structure.
Y.Taniguchi observed several nearby starburst nuclei both in CO(J=3-2) and CO(J=1-0) at JCMT15-m and Nobeyama 45-m radio telescopes, respectively. The beam-matched observations give a mean intensity ratio of CO(J=3-2)/CO(J=1-0) = 0.9+-0.2. This value is significantly larger than that of giant molecular clouds in our Galaxy (0.4+-0.05). Hence, we conclude that the molecular gas in the starburst nuclei is significantly warm (T kin>25K). Our observations first give the very reliable beam-matched measurements in the research field of starburst phenomena.
Y.Taniguchi and his collaborators made the K-band deep survey with a high-sensitivity infrared camera NICMOS3 on the UH88 telescope. They obtained 20 hours integration data of one filed which will be observed by ISO. They will observe this filed in April, 1994, and will detect very faint objects with K= 23 mag. Since this survey is the deepest one in this research fields, they will contribute to the understanding the formation of galaxies and the observational cosmology.
S.Sato visited three University facilities (Univ. of Wyoming, Univ. of Minnesota, and New Mexico State University) to discuss the future possibility of collaboration using medium-size telescopes in some long-term runs. It is expected to use the WIRO2.3-m and Mt.Lemmon 1.5-m telescopes in the intervals of three one-week runs and two ten-days runs from June through October, respectively. Although Apache Point 3.5-m and 1.0-m telescopes are designed for optical purposes, there might be a possibility to modify them into infrared works by minor changes. Nine persons ( Y.Taniguchi, H.Suto, T.Hasegawa, K.Wakamatsu, M.Tanaka, K.Iwasawa, F.Sato, Y.Sofue, and K.Ogura ) were delegated for astronomical observations with various wavelengths in the optical, infrared and radio regions. Less
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