The Shack–Hartmann wavefront sensor (SHWFS) has been widely used for measuring aberrations in adaptive optics systems. However, its traditional wavefront reconstruction method usually has limited precision under field conditions because the weight-of-center calculation is affected by many factors, such as low signal-to-noise-ratio objects, strong turbulence, and so on. In this paper, we present a ResNet50+ network that reconstructs the wavefront with high precision from the spot pattern of the SHWFS. In this method, a nonlinear relationship is built between the spot pattern and the corresponding Zernike coefficients without using a traditional weight-of-center calculation. The results indicate that the root-mean-square (RMS) value of the residual wavefront is 0.0128 μm, which is 0.79% of the original wavefront RMS. Additionally, we can reconstruct the wavefront under atmospheric conditions, if the ratio between the telescope aperture’s diameter D and the coherent length r ₀ is 20 or if a natural guide star of the ninth magnitude is available, with an RMS reconstruction error of less than 0.1 μm. The method presented is effective in the measurement of wavefronts disturbed by atmospheric turbulence for the observation of weak astronomical objects.

Shack-Hartmann 波前传感器 (SHWFS) 已广泛用于测量自适应光学系统中的像差。然而，其传统的波前重建方法通常在现场条件下精度有限，因为中心权重计算受到许多因素的影响，例如低信噪比对象、强湍流等。在本文中，我们提出了一个 ResNet50+ 网络，它可以从 SHWFS 的光斑图案中高精度地重建波前。在该方法中，在不使用传统的中心权重计算的情况下，在光斑图案和相应的泽尼克系数之间建立了非线性关系。结果表明，残余波前的均方根 (RMS) 值为 0.0128 μm，为原始波前 RMS 的 0.79%。此外，D和相干长度r ₀为 20 或者如果九等的自然导星可用，RMS 重建误差小于 0.1 μm。所提出的方法可有效地测量受大气湍流干扰的波前，用于观测弱天文物体。