Milli-meter and Optical-Infrared Astronomical Observations by Using High-Level Overseas Telescopes.

利用海外高水平望远镜进行毫米波和光学红外天文观测。

• 批准号: 05041070
• 负责人: KOZAI Yoshihide
• 金额: $ 1.92万
• 依托单位: National Astronomical Observatory
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for international Scientific Research
• 财政年份: 1993
• 资助国家: 日本
• 起止时间: 1993 至 无数据
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-05041070/
• 关键词: Starburst Galaxies; Active Galactic Nuclei; Interstellar Medium; Cluster of Galaxies; Molecular Hydrogen Absorption; Search for primeval galaxies; Development of astronomical instruments; Redshift survey

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 … More 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

T.Nagata和N.小林利用智利的1.5米CTIO红外望远镜，对银河系中心0.5度范围内波长为1.4 - 4.2微米的5个红外源进行了分光偏振观测。他们探测到了偏振;它可以用幂律p（lambda）很好地表示，但所有五个物体的偏振都远远超过了整个2.8 - 4.2微米的幂律。这种过度极化可能是由位于一般弥漫星际介质中的颗粒或银河系内部特有的颗粒引起的。偏振增加的形状似乎不同于分子云源。S.Deguchi在美国马萨诸塞州波士顿附近的Haystack天文台用37米射电望远镜测量了22 GHz的NGC 4258极高速水脉泽的线偏振，7月6 - 8日由于大气和INS ...更多信息 由于东海岸的热浪，我们可以为偏振的I、Q和U分量分别积分H2O光谱约2小时。K.Wakamatsu用CTIO 1.5-m和3.0-m Lick望远镜对蛇夫座cD星系团进行了广泛的红移测量。这个星团是由若松和马尔坎发现的，是天空中第三亮的X射线星团。发现这个星团是由几个不规则星团组成的，从而形成了“蛇夫座超星团”。Y.Taniguchi分别用JCMT 15-m和Nobeyama 45-m射电望远镜观测到了CO（J=3-2）和CO（J=1-0）中的几个邻近星暴核。束匹配观测给出CO（J=3-2）/CO（J=1-0）= 0.9 ± 0.2的平均强度比。这个值明显大于我们银河系中巨大分子云的值（0.4+-0.05）。因此，我们得出结论，星暴核中的分子气体是明显温暖的（Tkin> 25 K）。我们的观测首次在星暴现象的研究领域中给出了非常可靠的光束匹配测量，谷口勇和他的合作者在UH 88望远镜上用高灵敏度红外相机NICMOS 3进行了K波段的深度观测。他们获得了一个字段的20小时集成数据，将由ISO观察。他们将于1994年4月对这一领域进行观测，并将探测K= 23等的非常微弱的天体。由于这是这一研究领域中最深入的一次，他们将为理解星系的形成和观测宇宙学做出贡献。（怀俄明州大学、明尼苏达州大学和新墨西哥州州立大学）讨论在某些长期运行中使用中型望远镜进行合作的未来可能性。预计它将使用WIRO 2.3米望远镜和莱蒙山1.5米望远镜，从6月到10月分别进行三次为期一周的运行和两次为期十天的运行。虽然阿帕奇点3.5米和1.0米望远镜是为光学目的设计的，但也有可能通过微小的改动将它们改装成红外望远镜。委派了9人（谷口Y.、苏托H.、长谷川T.、若松K.、田中M.、岩泽K.、佐藤F.、索菲Y.和小仓K.）进行光学、红外和无线电区域各种波长的天文观测。少

项目成果

Y.Taniguchi: "^<12>CO(3-2) & (1-0) Emission Line Observations of Nearby Starburst Nuclei" The Astrophysical Journal. (印刷中). (1994)

Y.Taniguchi：“^<12>CO(3-2) & (1-0) 附近星爆核的发射线观测”天体物理学杂志（1994 年）。

T.Nagata: "Blight Near-Infrared Sources within 1ﾟ of the Galactic center. I. Survey and 1-20micron Photometry" The Astrophysical Journal. 406. 501-511 (1993)

T.Nagata：“银河中心 1ﾟ 范围内的 Blight 近红外源。I. 调查和 1-20 微米光度测量”《天体物理学杂志》406. 501-511 (1993)。

K.Wakamatsu: "Structure of Polar Ring Galaxies : Shock waves in the Gas of Polar rings" Astronomical Journal.105. 1457-1464 (1993)

K.Wakamatsu：“极环星系的结构：极环气体中的冲击波”天文学杂志.105。

Y.Taniguchi: "^<12>CO(3-2) & (1-0) Emission Line Observations of Nearby Starburst Nuclei" The Astrophycal Journal. 107. No.6 in press (1994)

Y.谷口：“^<12>CO(3-2)

H.Shiba: "Detection of Water Vapor in T Tauri Stars" Astrophysical Journal Supplement.89. 299-319 (1993)

H.Shiba：“金牛座T星中水蒸气的检测”天体物理学杂志增刊.89。