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首页> 外文会议>Conference on advances in optical and mechanical technologies for telescopes and instrumentation >An inverse-polished mirror for wavefront correction of space-based telescopes
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An inverse-polished mirror for wavefront correction of space-based telescopes

机译：用于天基望远镜波前校正的反抛光镜

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In this report we describe our development of a prototype inverse-polished mirror for the passive correction of the static and predictable wavefront errors (WFE) of space-based telescopes, in particular, especially for infrared coronagraphs. An artificial WFE pattern with a root mean square (rms) value of 350 nm was numerically generated to facilitate the design of the prototype mirror. The surface of the mirror is approximately flat, is 50.0 mm in diameter and 15.0 mm thick at the edge. The designed WFE pattern was constructed on the mirror surface by micro-polishing. Both the figure and roughness of the mirror surface were evaluated. The rms value of the measured surface figure was reduced to 135 nm after subtraction of the designed surface figure. The benefit of subtraction to mid-infrared coronagraph performance was simulated, which showed the contrast was improved by a factor of ～100 close to the core (closer than 10 λ/D where X and D are the wavelength and telescope aperture diameter, respectively) of the coronagraphic image of a point source. An analysis of the power spectrum density shows that the lower frequencies in the WFE are well reproduced on the mirror, while the higher frequencies remain due to the limitations imposed on the controllable spatial resolution by the fabrication process. In this study, inverse-polished mirrors combined with deformable mirrors and their application to ground-based telescopes are also discussed. To fully explore the potential of the inverse-polished mirror, a systematic allocation of the error budget is essential taking into account not only the fabrication accuracy of the mirror but also an evaluation of the telescope and other factors with non-predictable uncertainties.
机译：在本报告中，我们描述了原型反抛光镜的开发，该反抛光镜用于被动校正天基望远镜的静态和可预测波前误差（WFE），尤其是红外日冕仪。数值均方根（rms）值为350 nm的人工WFE图案被数值生成，以方便原型镜的设计。镜子的表面大约是平坦的，直径为50.0毫米，边缘厚度为15.0毫米。通过微抛光在反射镜表面上构造设计的WFE图案。评估镜面的形状和粗糙度。减去设计的表面图形后，测量的表面图形的rms值减小到135 nm。模拟了减去中红外日冕仪性能的好处，结果表明，在靠近核心处的对比度提高了约100倍（接近10λ/ D，其中X和D分别是波长和望远镜孔径）点源的日冕图像。功率谱密度的分析表明，WFE中的较低频率可以在反射镜上很好地再现，而较高的频率由于制造工艺对可控制的空间分辨率施加的限制而得以保留。在这项研究中，还讨论了反抛光镜与可变形镜的组合及其在地面望远镜中的应用。为了充分挖掘反抛光镜的潜力，必须有系统地分配误差预算，这不仅要考虑到反射镜的制造精度，还要考虑到望远镜的评估以及其他具有不可预测不确定性的因素。

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