Reconstruction of a Wavefront Distorted by Atmospheric Turbulence with Account for Optical Scheme of the Telescope

Reconstruction of a wavefront containing turbulent distortions of optical radiation is considered. The Hartmann method based reconstruction is carried out using the wave function approximation by Zernike polynomials according to estimates of local slopes and analyzed on the basis of filling Hartmannograms with focal spots, depending on the telescope design. The volume and quality of information about phase distortions of radiation are estimated using the Hartmannograms formed in the receiver plane, thereby developing methods for reducing the telescope induced residual reconstruction error.