Abstract: Fourier telescopy (FT) is an imaging method that combines the advantages of active laser lighting and synthetic aperture. Using the phase closure technique can eliminate the coarse phase of two arbitrary launch telescopes and the effects of atmospheric low-level disturbance. The resolution of reconstructed image can overcome the diffraction limit of a single telescope. For the realization of the engineering systems of the Fourier telescopy (FT), the image quality was explored when the light via the atmosphere with 36 km atmospheric height. The atmosphere was divided into 40 layers by the Rytov index method; the upper and lower boundaries of each floor and the heigth of each phase screen were calculated. To the 33 33 T-type emitter array with uniformly spaced, the number of simulated phase screens was 1 626. Fraunhofer diffraction approximation was used when beam from the emitting surface to the target. Through computer simulation, without considering the noise, for the 10 cm emission caliber, we obtain the conclusion that the higher order disturbance of atmosphere has a slight impact on the FT imaging system. Without the atmospheric high order disturbance, the Strehl of reconstruction image and diffraction limit image is 0.682 1. With that the Strehl is reduced to 0.623 6. When the signal to noise ratio of 100, the Strehl reach 0.452 5, and the target can be discriminated.