Development of Stellar Spectroscopic System with High-Spatial Resolution

由于大气湍流会使恒星图像退化，因此很难从地面获得高空间分辨率的光谱。我们项目的目标是在大气湍流的情况下提取高空间分辨率的客观棱镜光谱。1990年2月，我们在冈山天体物理观测站用188厘米望远镜进行了光谱散斑观测。我们使用了我们的光谱散斑相机，这是在这笔赠款的帮助下开发的。我们观测到了一颗点星，齐塔-头。通过对这颗星的数据分析，我们可以从散斑图中提取出物镜光谱。我们还观测到了双星ADS 16836。在这种情况下，我们可以分离主星和次星的光谱。从上面的结果可以证实，我们可以获得高空间分辨率的恒星物体的物镜光谱，即使是从地面。因此，我们可以完成这个项目目的的主要部分。

It was difficult to get high-spatial resolution spectra from the ground because the atmospheric turbulence degrades a stellar image. The objective of our project is to extract objective prism spectra with high-spatial resolution, in spite of the atmospheric turbulence. Here we apply stellar speckle technique to get diffraction-limited information.In February, 1990, we made spectral speckle observation with 188cm telescope at the Okayama Astrophysical Observatory. We used our spectral speckle camera, which was developed with the aid of this grant. We observed a point-star, Zeta-Tau. Through the data analysis of this star, we could extractits objective-prism spectrum from the dispersed speckle patterns.We also observed ADS 16836, a double star. In this case, we could separate the spectra of the primary star and the secondary star.From the above results, it is confirmed that we can get objective-prism spectra of stellar objects with high-spatial resolution, even if from the ground. Thus we could perform the main part of the purpose of this project.