Adaptive optics 2026-10-05
Adaptive optics measures changing wavefront errors and corrects them using a deformable mirror. A wavefront sensor supplies measurements to a fast feedback controller; a guide star provides the reference. It improves astronomical seeing toward diffraction-limited resolution.
The angular diffraction-limited resolution of a telescope scales as , with wavelength and illuminated diameter . Larger diameter resolves smaller angular structure, while longer wavelength makes atmospheric phase correction easier.
For a large aperture in the standard turbulence model, astronomical seeing is approximately radians, with Fried parameter . Maintaining comparable correction requires a deformable mirror actuator pitch of order , so the number of actuators across a diameter is proportional to and the total illuminated actuator count is proportional to . Therefore
Longer wavelengths require fewer actuators and have slightly smaller uncorrected atmospheric angular blur, even though the telescope's diffraction-limited resolution scale increases with wavelength.
A wavefront error ripple of period generates a pair of speckles at angular displacement . Combining this with gives the deformable-mirror control radius along an actuator row or column:
A square actuator lattice has a square ideal frequency region: . Its full width is , approximately diffraction-limited resolution elements per side, or in area. The circular subset within the row-direction radius contains approximately such elements. The primary aperture shapes each speckle's point spread function; it does not turn the square sampling limit into a circular one.
This full square describes phase-error control. Simultaneous amplitude and phase correction with a single pupil-plane deformable mirror generally requires restricting the dark region to a half-plane; it is a different constraint from the sampling bandwidth.