Adaptive pupil masking for quasi-static speckle suppression

TL;DR

This paper introduces an adaptive pupil masking technique that dynamically alters the telescope's diffraction pattern to suppress quasi-static speckles, thereby enhancing the detection of faint companions around bright stars.

Contribution

The study demonstrates that adaptive pupil masks can effectively convert static speckles into dynamic ones, significantly improving contrast and detection capabilities in high-contrast imaging.

Findings

Speckles become dynamic, smoothing the PSF in long exposures.

Contrast ratio improves by approximately 100 times in short exposures.

Faint companions up to 18 magnitudes fainter can be detected.

Abstract

Quasi-static speckles are a current limitation to faint companion imaging of bright stars. Here we show through simulation and theory that an adaptive pupil mask can be used to reduce these speckles and increase the visibility of faint companions. This is achieved by placing an adaptive mask in the conjugate pupil plane of the telescope. The mask consists of a number of independently controllable elements which can either allow the light in the subaperture to pass or block it. This actively changes the shape of the telescope pupil and hence the diffraction pattern in the focal plane. By randomly blocking subapertures we force the quasi-static speckles to become dynamic. The long exposure PSF is then smooth, absent of quasi-static speckles. However, as the PSF will now contain a larger halo due to the blocking, the signal to noise ratio (SNR) is reduced requiring longer exposure times to detect the companion. For example, in the specific case of a faint companion at 5xlambda/D the exposure time to achieve the same SNR will be increased by a factor of 1.35. In addition, we show that the visibility of companions can be greatly enhanced in comparison to long-exposures, when the dark speckle method is applied to short exposure images taken with the adaptive pupil mask. We show that the contrast ratio between PSF peak and the halo is then increased by a factor of approximately 100 (5 magnitudes), and we detect companions 11 magnitudes fainter than the star at 5xlambda/D and up to 18 magnitudes fainter at 22.5xlambda/D.