High-Resolution Imaging in the Visible with Faint Reference Stars on Large Ground-Based Telescopes

Astronomers working with faint targets will benefit greatly from improved image quality on current and planned ground-based telescopes. At present, most adaptive optic systems are targeted at the highest resolution with bright guide stars. We demonstrate a significantly new approach for measuring low-order wavefront errors by using a pupil-plane curvature wavefront sensor design. By making low order wavefront corrections, we can deliver significant improvements in image resolution in the visible on telescopes in the 2.5–8.2 m range on good astronomical sites. As a minimum, the angular resolution will be improved by a factor of 2.5–3 under any reasonable conditions and, with further correction and image selection, even sharper images may be obtained routinely. We re-examine many of the assumptions about what may be achieved with faint reference stars to achieve this performance. We show how our new design of curvature wavefront sensor combined with wavefront fitting routines based on radon transforms allow this performance to be achieved routinely. Simulations over a wide range of conditions match the performance already achieved in runs with earlier versions of the hardware described. Reference stars significantly fainter than I [Formula: see text]17[Formula: see text]m may be used routinely to produce images with a near diffraction limited core and halo much smaller than that delivered by natural seeing.