光学干涉仪像面组束中的串扰
Crosstalk in image plane beam combination for optical interferometers
摘要：
光学干涉仪中的像面光束组合将来自多个基线的干涉条纹复用到单个检测器上。星光光束以非冗余模式排列在组合器的入口处，使得来自每个基线的信号可以在频域中彼此分离。如果来自不同基线的信号在频域中重叠，则这会在条纹测量中产生称为基线串扰的系统误差。在本文中，我们量化的串扰所产生的组合的大气看到和光束传播的距离为数百米。我们发现，在理想的条件下，大气波前误差和光束传输没有贡献的串扰。然而，当孔径光阑包括在光束训练中时，我们观察到波前误差可导致在实际观察条件下由高达$ΔV^{2} = 6.6\times10^{-3}$的串扰引起的平方可见度误差。
英文摘要：
Image plane beam combination in optical interferometers multiplexes the interference fringes from multiple baselines onto a single detector. The beams of starlight are arranged in a non-redundant pattern at the entrance of the combiner so that the signal from each baseline can be separated from one another in the frequency domain. If the signals from different baselines overlap in the frequency domain, this can give rise to a systematic error in the fringe measurements known as baseline crosstalk. In this paper we quantify crosstalk arising from the combination of atmospheric seeing and beam propagation over distances of order hundreds of metres. We find that in idealised conditions atmospheric wavefront errors and beam propagation do not contribute to crosstalk. However, when aperture stops are included in the optical beam train we observe that wavefront errors can result in squared visibility errors arising from crosstalk as high as $ΔV^{2} = 6.6\times10^{-3}$ under realistic observing conditions.
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