Deconvolution of infrared telescope images can partially recover the distribution of light in the sky. The light from point sources and extended sources is modeled as a grid of closely-spaced points. A matrix of influence coefficients contains the response of the telescope-instrument combination to light at the grid points. A non-negative least-squares routine finds the sky flux densities that reproduce the instrument data. A personal computer program and examples of infrared telescope data deconvolution are presented.