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Optical Adjustment of the FITE Interferometer

机译：光学调节纤维干涉仪

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We have developed a balloon-borne far-infrared interferometer, the Far-infrared Interferometric Telescope Experiment (FITE). The final goal of spatial resolution was one arcsec at 100 mu m. As a first step, we aimed to achieve a spatial resolution of five arcsecs at 155 mu m with a 6-m baseline. FITE is a two-beam interferometer like Michelsons stellar interferometer. Positions and attitudes of all mirrors required to have their alignment checked and possibly adjusted before launch and were checked during observation. We had to satisfy three requirements: the coincidence of the phases of each beam (wavefront error), image quality of the two beams at the (common) focus, and no optical path difference between the two beams for celestial objects. In order to achieve the former two requirements, we developed an interferometer adjustment system that used a newly-developed interferometer measurement instrument. This instrument adopted a Shack-Hartmann wavefront sensor to measure wavefront errors of the two off-axis parabolic mirrors, simultaneously. With this system, the adjustment of the FITE interferometer was carried out at the Alice Springs balloon base in Australia as the JAXA's Australia balloon experiment campaign of 2018. On-site adjustment was successful; wavefront errors of the two off-axis parabolic mirrors were 1.78 mu m and 4.99 mu m (peak-to-valley), and the Hartmann constant was 13 arcsecs. As for the optical path difference, we achieved the requirement by step-wise displacement of a folding plane mirror. Results satisfied the requirements for an interferometer designed for a wavelength of 155 mu m. Improvement of spatial resolution at far-infrared wavelengths is undoubtedly important for research on protoplanetary disks, circumstellar dust shells of late-type stars, and star-forming galaxies. The method we have developed is also useful for future space interferometers.
机译：我们开发了一个气球传播的远红外干涉仪，远红外干涉望远镜实验（Fite）。空间分辨率的最终目标是100 mu m的Arcsec。作为第一步，我们旨在通过6米基线实现155亩弧度的空间分辨率。 Fite是一种双光束干涉仪，如米歇尔逊​​恒星干涉仪。在发射前检查并可能调整所有镜子的位置和态度，并在观察期间检查。我们不得不满足三个要求：每个光束（波前误差）的阶段的相吻合，两个光束的图像质量在（常见的）焦点上，并且在天体对象的两个光束之间没有光学路径差。为了实现前两种要求，我们开发了一种干涉仪调节系统，用于使用新开发的干涉仪测量仪器。该仪器采用Shack-Hartmann波前传感器，可同时测量两个轴外抛物面镜的波前误差。利用该系统，在澳大利亚的Alice Springs Balloon Base进行了Fite Tenerferometer的调整，是JAXA澳大利亚气球实验活动2018年。现场调整成功;两个轴外抛物面镜的波前误差为1.78 mu m和4.99 mu m（峰到谷），Hartmann常数是13个arcsecs。至于光路差，我们通过折叠平面镜的逐步位移实现了要求。结果满足了设计为155亩波长的干涉仪的要求。在远红外波长下的空间分辨率的改善对于改进原始圆盘，晚期型恒星和星形星系的星系尘埃壳来说无疑是重要的。我们开发的方法对于未来的空间干涉仪也是有用的。

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