Fast-Cadence High-Contrast Imaging with Information Field Theory

TL;DR

This paper introduces a Bayesian deconvolution algorithm for fast-cadence high-contrast imaging that improves direct exoplanet detection by resolving high brightness contrasts in short observation times using physics-inspired models.

Contribution

It presents a novel post-processing method that jointly estimates astronomical objects and atmospheric effects from sequences of telescope images, enabling high-contrast detection without field rotation.

Findings

Detected sources with brightness ratios down to 6×10^{-4} at 185 mas separation.

Achieved high-contrast imaging with very short observation times of 0.6 seconds.

Demonstrated effectiveness on real telescope data with synthetic injections.

Abstract

Although many exoplanets have been indirectly detected over the last years, direct imaging of them with ground-based telescopes remains challenging. In the presence of atmospheric fluctuations, it is ambitious to resolve the high brightness contrasts at the small angular separation between the star and its potential partners. Post-processing of telescope images has become an essential tool to improve the resolvable contrast ratios. This paper contributes a post-processing algorithm for fast-cadence imaging, which deconvolves sequences of telescope images. The algorithm infers a Bayesian estimate of the astronomical object as well as the atmospheric optical path length, including its spatial and temporal structures. For this, we utilize physics-inspired models for the object, the atmosphere, and the telescope. The algorithm is computationally expensive but allows to resolve high contrast ratios despite short observation times and no field rotation. We test the performance of the algorithm with point-like companions synthetically injected into a real data set acquired with the SHARK-VIS pathfinder instrument at the LBT telescope. Sources with brightness ratios down to $6\cdot10^{-4}$ to the star are detected at $185$ mas separation with a short observation time of $0.6\,\text{s}$.