In the astronomical speckle interferometry, low-light CCD cameras such as the electron bombarded/multiplying CCDs (EB/EMCCDs) are being widely used for taking the faint speckle images. The detector noise affects the power spectral estimate of the astronomical object as well as the speckle noise does. The estimation errors of the object power spectrum are results of the propagation of the random fluctuations due to those noises. We have formulated a method for correcting and evaluating the estimation errors based on our detection model developed for EB/EMCCDs and the conventional model of the speckle noise. In our method, the error correction and evaluation are accomplished with the aid of the auxiliary data known as the dark and flat frames. The unbiased estimator of the object power spectrum and its SNR evaluator as derived above are verified using simulated data, where we have adopted the values of the detector parameters as obtained by measuring the actually used EMCCD camera in our observations. The results of the simulated experiments show that, within the diffraction cutoff frequency, our power spectral estimator is unbiased, and our SNR evaluator for that is useful except below the seeing cutoff.

在天文散斑干涉法中，诸如电子轰击/倍增CCD（EB / EMCCD）等低照度CCD相机被广泛用于拍摄微弱的散斑图像。探测器噪声和斑点噪声都会影响天文物体的功率谱估计。目标功率谱的估计误差是由于那些噪声引起的随机波动传播的结果。我们基于为EB / EMCCD开发的检测模型和斑点噪声的常规模型，制定了一种校正和评估估计误差的方法。在我们的方法中，误差校正和评估是借助称为暗框和平框的辅助数据完成的。使用模拟数据验证了以上得出的目标功率谱的无偏估计器及其SNR评估器，其中我们在观测中采用了通过测量实际使用的EMCCD摄像机获得的检测器参数值。模拟实验的结果表明，在衍射截止频率范围内，我们的功率谱估计器是无偏的，而我们的SNR评估器非常有用，除了在可见截止点以下。