Abstract

Ours is one of several teams that independently worked on image inversion of HST wf/pc pictures to determine the spherical aberration error on the HST primary. The technique we chose to persue was based on a non-linear least squares solution for zeroike coefîcients of the aberrations of the optics. The code for modeling the optical system evolved from a relatively simple single Fourier tranform of the exit pupil to a complete multiplane diffraction propagation model with telescope jitter included.

© 1991 Optical Society of America