AI 中文总结
本文针对CMOS成像仪像素位置存在1%-3%偏差的问题，提出将像素位置测量精度提升至10⁻³像素水平以下的校准方法，可用于艾里斑最小二乘拟合以提高PSF质心定位精度。
AI 中文摘要
要将恒星的质心位置确定到恒星图像半高全宽（FWHM）的10⁻⁴水平以下，许多系统误差源都很重要。质心误差的一个更重要来源是焦平面阵列中像素的位置不完美。在本文中，我们讨论了多个商用CMOS探测器的像素位置校准。焦平面阵列是制造精度达数十纳米的半导体器件，但如果像素上存在量子效率（QE）梯度，像素的有效位置会产生偏差。在大多数CMOS成像仪中，我们通常看到像素位置变化为像素的1%至3%。本文介绍了如何将每个像素的位置测量到10⁻³像素水平以下，还介绍了如何将此信息用于艾里斑的最小二乘拟合，以获得更高精度的点扩散函数（PSF）质心位置。
英文摘要
Many sources of systematic error are important to centroid the position of a star below the level of $10^{-4}$ of the FWHM of the stellar image. One of the more important sources of centroiding error is the imperfect position of the pixels in a focal plane array. In this paper, we discuss the calibration of pixel position of multiple commercial CMOS detectors. Focal plane arrays are semiconductor devices fabricated with 10's nanometer precision. However, the effective location of a pixel can be biased if there's a QE gradient across the pixel. We typically see pixel position variations of 1--3\% of a pixel in most CMOS imagers. This paper describes how we measure the position of each pixel below the $10^{-3}$ pixel level. We also describe how this information might be used in a least square fitting of an airy spot to obtain a higher accuracy position of the centroid of the PSF.
