RHAPSODIE: Reconstruction of High-contrAst Polarized SOurces and Deconvolution for cIrcumstellar Environments

TL;DR

This paper introduces a novel inverse approach method for reconstructing and deconvolving polarized signals from circumstellar environments in high-contrast imaging, improving accuracy especially at low signal-to-noise ratios.

Contribution

The paper presents a new inverse method that accounts for instrumental effects and noise, enhancing the extraction of polarized signals from circumstellar disks in high-contrast polarimetric imaging.

Findings

Accurately measures polarized intensity and angle of linear polarization.

Improves performance for low SNR and small polarized flux.

Enables use of incomplete polarimetry cycles for increased sensitivity.

Abstract

Polarimetric imaging is one of the most effective techniques for high-contrast imaging and characterization of circumstellar environments. These environments can be characterized through direct-imaging polarimetry at near-infrared wavelengths. The SPHERE/IRDIS instrument installed on the Very Large Telescope in its dual-beam polarimetric imaging (DPI) mode, offers the capability to acquire polarimetric images at high contrast and high angular resolution. However dedicated image processing is needed to get rid of the contamination by the stellar light, of instrumental polarization effects, and of the blurring by the instrumental point spread function. We aim to reconstruct and deconvolve the near-infrared polarization signal from circumstellar environments. We use observations of these environments obtained with the high-contrast imaging infrared polarimeter SPHERE-IRDIS at the VLT. We developed a new method to extract the polarimetric signal using an inverse approach method that benefits from the added knowledge of the detected signal formation process. The method includes weighted data fidelity term, smooth penalization, and takes into account instrumental polarization. The method enables to accurately measure the polarized intensity and angle of linear polarization of circumstellar disks by taking into account the noise statistics and the convolution of the observed objects by the instrumental point spread function. It has the capability to use incomplete polarimetry cycles which enhance the sensitivity of the observations. The method improves the overall performances in particular for low SNR/small polarized flux compared to standard methods.