Study on the precise observations of stellar and circum-stellar phenomena with the optical and infrared interferometer

这项研究项目(MIRA-I.2)旨在开发用于观测具有极高角分辨率的恒星的光学和红外干涉仪。该项目为期4年(1998年4月至2002年3月)，1998年对干涉仪光学系统、探测器和控制系统进行了研究、部分制造和测试。这些部件被安装在以前的干涉仪系统MIRA-I.1中，该系统由两个望远镜(口径250毫米，基线4米)组成。利用该系统对几颗亮星的条纹进行了探测。1999年，库德望远镜被铁质定位仪(300毫米平面镜，6米基线测试系统)的新元素望远镜所取代。随着6m测试基线系统的建立，MIRA-I.2(30m基线)常规系统的新观察室开始建设。2000年，我们在干涉仪实验室建造和安装了新观察室、光路真空管、观察室光学部件、干涉仪光学元件、条纹探测器、倾斜-倾斜镜象限传感器和延迟线真空室。2001年，完成了6m测试基线的干涉仪系统。2001年6月底，利用该系统探测到了几颗明亮恒星的条纹。8月，在这一成功之后，我们全面开始了30米基线的Regujar系统的建设。2001年10月开始了对明亮恒星的测试观测。然而，直到2002年3月(2001财年末)我们才能探测到织女星的条纹，通过对系统的改进和调整，我们在2002年6月成功地用常规的30m基线的MIRA-I.2系统探测到了织女星的条纹。我们将完成这台干涉仪，它是值得观测的物理参数，如恒星的半径和质量。

This research project (MIRA-I.2) is aimed to develop the optical and infrared interferometer for observing stars with the very high angular resolution. The term of this project is 4 years (Apr. 1998 - Mar. 2002).In 1998, interferometer optics, detectors, and control system were investigated, partly made and tested. These parts were built into the former interferometer system, MIRA-I.1, which consists of two coude telescopes (250 mm aperture, 4 m baseline). Fringes of several bright stars were detected with this system. In 1999, the coude telescopes were replaced with the new element telescopes of siderostat (300 mm flat mirror, the test system of 6 m baseline). The construction of the new observing houses for the regular system of MIRA-I.2 (30 m baseline) was begun along with the setup of the test baseline system of 6 m. In 2000, we made the construction and the setup of new observing houses, vacuum pipes for optical path, optical parts in the observing house, interferometer optics, fringe detectors, quadrant sensors for tip-tilt mirrors, and vacuum chamber for delay line in the interferometer laboratory. In 2001, the interferometer system of 6 m test baseline was completed. At the end of June, 2001, fringes of several bright stars were detected with this system. In August, after this success, we started the construction of the regujar system of 30 m baseline in full-scale. Test observations of bright stars were begun in October, 2001. However, we could not detect the star fringes until March, 2002 (the end of 2001 fiscal year).Making improvements and regulations of the system, we succeeded to detect the fringes of Vega with the regular MIRA-I.2 system of 30 m baseline, in June, 2002. We will complete this interferometer, which is worth observing the physical parameters, such as radius and mass of stars.