Research on fiber-feed stellar interferometer with wavefront control

波前控制光纤馈源恒星干涉仪研究

• 批准号: 03640242
• 负责人: BABA Naoshi
• 金额: $ 1.28万
• 依托单位: Hokkaido University,(Faculty of Engineering)
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (C)
• 财政年份: 1991
• 资助国家: 日本
• 起止时间: 1991 至 1992
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-03640242/
• 关键词: Stellar interferometer; Adaptive optics; Channeled spectra; Optical path-length; Wavefront correction; チャネルドスペクトル; チャンネルドスペクトル

It is desirable to correct atmospherically distorted wavefront before feeding the light into optical fiber or waveguide optics. In order to correct the distorted wavefront,it is necessary to sense the wavefront with some means. We proposed a new approach to estimate the distorted wavefront from the point-spread function at the focal plane of a telescope. We conducted several computer simulations to test our method. We showed that a distorted wavefront could be estimated from a noisy point-spread function. It is also shown that the distorted wavefront can be corrected by a segmented mirror or by a continuous face-sheet mirror with use of the information of the estimated wavefront.One of very important factors to develop stellar interferometer is the way how to detect the optical-path difference and to correct it. We developed an optical system to correct the optical-path difference with use of channeled spectrum. We also tested a method to detect the optical-path difference by forming spatial fringe pattern. This method is exemplified to be useful for the precise detection of the optical-path difference.We have shown that the dispersion of air causes crucial effects for the compensation of the optical-path difference. We demonstrated by optical simulation that the effect of the air dispersion could be detectable from the spatial fringe pattern formed with two beams from telescopes.

希望在将光馈送到光纤或波导光学器件之前校正大气畸变的波前。为了校正畸变的波前，必须采用一定的方法对波前进行检测。提出了一种由望远镜焦平面上的点扩散函数估计畸变波前的新方法。我们进行了几次计算机模拟来测试我们的方法。我们表明，一个扭曲的波前可以从一个嘈杂的点扩散函数估计。研究表明，利用波前估计信息，可以通过分段反射镜或连续面片反射镜对畸变波前进行校正。如何检测光程差并进行校正是恒星干涉仪发展的一个重要因素，我们研制了一种利用通道光谱进行光程差校正的光学系统。同时，我们还试验了一种通过形成空间条纹图来检测光程差的方法。该方法可用于光程差的精确测量，并指出空气的色散对光程差的补偿起着至关重要的作用。我们通过光学模拟证明了空气色散的影响可以从望远镜的两束光形成的空间条纹图中检测出来。

项目成果

N.Baba: "High resolution imaging with large telescope" Proc.Sino-Japan Symp.'Engineering Optics'. 353-358 (1992)

N.Baba：“大型望远镜高分辨率成像”Proc.Sino-Japan Symp.工程光学。

N.BABA et al.: "Wavefront correction from point spread function" Appl.Opt.

N.BABA 等人：“点扩散函数的波前校正”Appl.Opt。