Spatial deconvolution of spectropolarimetric data: an application to quiet Sun magnetic elements

TL;DR

This paper presents a deconvolution method to correct for the telescope's PSF effects in space-based spectropolarimetric data, improving the analysis of quiet Sun magnetic elements.

Contribution

The study introduces a novel deconvolution technique applied to Hinode/SP data to enhance spatial resolution and accurately infer magnetic properties.

Findings

Improved spatial resolution of quiet Sun magnetic features.

More accurate magnetic field measurements after deconvolution.

Validated deconvolution method with noisy data.

Abstract

Observations of the Sun from the Earth are always limited by the presence of the atmosphere, which strongly disturbs the images. A solution to this problem is to place the telescopes in space satellites, which produce observations without any (or limited) atmospheric aberrations. However, even though the images from space are not affected by atmospheric seeing, the optical properties of the instruments still limit the observations. In the case of diffraction limited observations, the PSF establishes the maximum allowed spatial resolution, defined as the distance between two nearby structures that can be properly distinguished. In addition, the shape of the PSF induce a dispersion of the light from different parts of the image, leading to what is commonly termed as stray light or dispersed light. This effect produces that light observed in a spatial location at the focal plane is a combination of the light emitted in the object at relatively distant spatial locations. We aim to correct the effect produced by the telescope's PSF using a deconvolution method, and we decided to apply the code on Hinode/SP quiet Sun observations. We analyze the validity of the deconvolution process with noisy data and we infer the physical properties of quiet Sun magnetic elements after the deconvolution process.