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.

我们通过将35支球队派往夏威夷，与夏威夷大学进行了合作研究。我们主要使用Mauna Kea上的UH望远镜和其他望远镜，并与日本仪器一起进行了各种观察，以研究银河系中心的结构，星系结构以及恒星形成区域的结构。主要结果如下：观察是使用带有PTSI检测器的NIR摄像头进行的。这款具有512x512像素的NIR摄像头具有最宽的FOV，并且最有效地揭示了银河系中心周围的宽面积结构。结果表明，吸收特征与密集的分子云相吻合。使用UH FOS，我们观察到了紧凑的星系组以确定其结构和运动学特性，并通过基于观察结果的计算机模拟来发现对星系进化的强烈环境影响。有人提出，宽分布的暗物质可能会抑制太快的演变。边缘星系的表面光度研究表明，一些磁盘显示翘曲，这归因于潮汐与另一个星系的相互作用。 NIR磁盘图像显示了其垂直结构中的多个尺度高度。使用日本开发的棱镜和光栅光谱仪研究了尘埃排放。许多IRAS星系显示出3.3mum发射与恒星形成活性相关。从QSO中检测到1500K的热成分。相同的光谱仪用于研究年轻恒星物体的偶尔物理学。 Fu Ori物体处于爆炸阶段时显示出水的吸收，表明加强放射蒸发的冰粒。 IRAS的4个源显示出3MUM尘埃发射，类似于散射星云。一个mm-wave极化法指示与垂直于立法质原质磁盘云的磁盘平面的星际磁场。