Fig. 1. Metapupil and foot print

Fig. 2. Extracting the local area of phase screen by Zernike model method

Fig. 3. Refocusing principle of light field camera

Fig. 4. Conceptual graph of two-layer atmosphere turbulence screens and three natural guide stars based light field tomography simulation system

Fig. 5. Numerical simulation results of light field tomography at situation of natural guide stars. (a) Fisrt layer of atmosphere turbulence screen; (b) Second layer of atmosphere turbulence screen. From top to bottom is the original atmosphere aberration, the restoration atmospheric phase, the residual error and the Zernike coefficient before and after reconstruction respectively

Fig. 6. Conceptual graph of two-layer atmosphere turbulence screens and three laser guide stars based light field tomography simulation system

Fig. 7. Numerical simulation results of light field tomography at situation of laser guide stars. (a) Fisrt layer of atmosphere turbulence screen; (b) Second layer of atmosphere turbulence screen. From top to bottom is the original atmosphere aberration, the restoration atmospheric phase, the residual error and the Zernike coefficient before and after reconstruction respectively

Fig. 7. [in Chinese]

Fig. 8. Adaptive optics simulation system based on light field camera

Fig. 9. Wavefront distortion at telescope pupil

Fig. 10. Layout of deformable mirror actuators

Table 1. [in Chinese]