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

本研究项目（MIRA-I.2）的目标是研制用于极高角分辨率观测恒星的光学和红外干涉仪。项目期限为4年（1998年4月- 2002年3月）。1998年对干涉仪光学、探测器、控制系统进行了研究、部分制作和测试。这些部件被内置到以前的干涉仪系统MIRA-I中。1，由两台双联望远镜（口径250毫米，基线4米）组成。这个系统探测到了几颗明亮恒星的边缘。1999年，coude望远镜被siderostat新元件望远镜（300 mm平镜，6 m基线测试系统）所取代。为mira - 1 .2常规系统建造新的观察所（30米基线）随着6米测试基线系统的建立而开始。2000年，我们在干涉仪实验室完成了新的观测室、光路真空管、观测室内光学部件、干涉仪光学、条纹探测器、倾斜镜象限传感器、延迟线真空室的建设和安装。2001年，6米测试基线干涉仪系统建成。在2001年6月底，用这个系统探测到了几颗明亮恒星的边缘。今年8月，在取得成功后，我们开始了30米基线常规系统的全尺寸建设。2001年10月开始对明亮恒星进行测试观测。然而，直到2002年3月（2001年财政年度结束）才发现了恒星边缘。通过对系统的改进和规范，我们成功地用常规的MIRA-I探测到了织女星的边缘。2系统30米基线，于2002年6月。我们将完成这个干涉仪，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.