Research for Diffraction Limited Imaging with Large Optical Telescope

大型光学望远镜衍射极限成像研究

基本信息

批准号：
63460009
负责人：
ISHIGURO Masato
金额：
$ 4.67万
依托单位：
National Astronomical Observatory
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (B)
财政年份：
1988
资助国家：
日本
起止时间：
1988 至 1990
项目状态：
已结题

项目摘要

In this research, we have developed an aperture synthesis method with a non-redundant aperture mask (NRM) to obtain diffraction limited images with a large optical telescope. In 1988, we constructed a data acquisition system, investigated the design method of 2-dimensional NRM, and conducted a fundamental optical simulation. In 1989, based on these results and using the data using the data acquisition system, we observed single stars and binaries with the 91 cm telescope at Dodaira Astronomical Observatory, National Astronomical Observatory (NAO). From these observations, we found that the atmospheric fluctuations are very severe in Japan and an image stabilizing system must be required. Thus, in 1990, we developed an aperture masking system with an image stabilizing function. Using the system for NRM observations with the 188 cm telescope at Okayama Astrophysical Observatory, NAO, we confirmed good response of the imaging stabilizing function and obtained a lot of fundamental data for diffraction limited imaging. From our investigations, we obtained following results :1. The radius of the coherence patch is less than 3 cm in Japan. Since the number of sub-apertures of NRM is small, total aperture area of NRM of which sub-aperture radius is equal to that of coherence patch is very small Therefore, it is required to use the mask with small redundancy for weak objects.2. At longer baselines, visibility amplitude decreases severely, because the delay difference between sub-apertures is large. Some portion of this effect can be canceled out by an image stabilizing system. In the case of bad seeing, however, it is desired to use a simple adaptive optics.

在这项研究中，我们开发了一种具有非冗余孔掩模（NRM）的孔径合成方法，以使用大型光学望远镜获得衍射有限的图像。 1988年，我们构建了一个数据采集系统，研究了二维NRM的设计方法，并进行了基本的光学模拟。在1989年，基于这些结果并使用数据采集系统使用数据，我们在Dodaira天文天文台（NAO）的Dodaira天文文章（NAO）的91 cm望远镜中观察到了单星和二进制。从这些观察结果中，我们发现日本的大气波动非常严重，必须需要图像稳定系统。因此，在1990年，我们开发了一个具有图像稳定函数的光圈掩蔽系统。使用该系统与冈山天体天文台的188 cm望远镜NAO进行NRM观测，我们证实了成像稳定功能的良好响应，并获得了许多基本数据，用于衍射有限的成像。从我们的调查中，我们获得了以下结果：1。在日本，相干斑块的半径小于3厘米。由于NRM的子孔数的数量很小，因此NRM的总孔径面积，其子孔径半径等于相干贴片的数量非常小，因此需要使用具有较小冗余的掩码来缩小物体。2。在较长的基线下，可见性幅度会严重降低，因为子孔径之间的延迟差很大。图像稳定系统可以取消此效果的某些部分。但是，在看不见的情况下，希望使用简单的自适应光学器件。