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Observational Study on the Evolution of Galaxy Structure

星系结构演化的观测研究

基本信息

批准号：
01044045
负责人：
KODAIRA Keiichi
金额：
$ 13.25万
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：
1989
资助国家：
日本
起止时间：
1989 至 1991
项目状态：
已结题

项目摘要

We carried out the collaborative research with University of Hawaii by sending 35 teams in total to Hawaii. Using mainly UH telescopes and other telescopes on Mauna Kea, in conjunction with Japanese instruments, we performed various observations to investigate structure of the Galactic center, structure of galaxies, and structure of star forming regions. Main results are as follows :The observation was made using a NIR camera with PtSi detector. This NIR camera with 512X512 pixels had the widest FOV and was most effective to reveal wide-area structures around the Galactic center. The result indicated that the absorption features coincided with those of, dense molecular clouds.Using UH FOS we observed compact groups of galaxies to determine their structure and kinematic properties, and to find out strong environmental effect on the evolution of galaxies by computer simulations based upon the observational results. It was suggested that wide distributed dark matter may suppress the too quick evolution. Surface photometric study of edge-on galaxies revealed that some of disks showed warping which was attributed to tidal interaction with another galaxies. NIR disk images revealed multiple scale heights in their vertical structure. Dust emission was investigated using prism- and grating spectrometers developed in Japan. Many of IRAS galaxies showed 3.3mum emission correlated to star formation activity. Thermal component of 1500K was detected from QSO's.The same spectrometers were used for investigation of circumstellar physics of young stellar objects. FU Ori objects showed watervapour absorption when they were in flare-up phase, indicating that intensitiedradiation evaporated ice grains. 4 of IRAS sources showed 3mum dust emission, similar to that seen from scattering nebulae.A mm-wave polarimetry indicated interstellar magnetic field perpendicular to the disk plane of a law-mass protostellar disk cloud.

我们与夏威夷大学进行了合作研究，共派出35个小组前往夏威夷。我们主要利用UH望远镜和莫纳克亚山上的其他望远镜，结合日本仪器，进行了各种观测，以研究银河系中心的结构、星系的结构和恒星形成区的结构。主要结果如下：利用带PtSi探测器的近红外相机进行了观测。这台512X512像素的近红外相机具有最宽的视场，最有效地揭示了银河系中心周围的广域结构。结果表明，其吸收特征与致密分子云的吸收特征一致。我们利用UH FOS观测了紧致星系群，确定了它们的结构和运动特性，并在观测结果的基础上通过计算机模拟发现了环境对星系演化的强烈影响。广泛分布的暗物质可能抑制了过快的演化。对边缘星系的表面光度研究表明，一些圆盘出现翘曲，这是由于与另一个星系的潮汐相互作用造成的。近红外圆盘图像显示其垂直结构具有多个尺度高度。利用日本研制的棱镜和光栅光谱仪对粉尘发射进行了研究。许多IRAS星系显示出与恒星形成活动相关的3.3 μ m辐射。用QSO检测了1500K的热成分。同样的光谱仪被用于研究年轻恒星天体的星周物理。傅里奥天体在爆发阶段显示出水蒸气吸收，这表明强烈的辐射蒸发了冰粒。4个IRAS源显示3mum尘埃发射，类似于从散射星云中看到的。毫米波偏振测量表明星际磁场垂直于一定质量的原恒星盘状云的盘面。