Solar image quality assessment: a proof of concept using Variance of Laplacian method and its application to optical atmospheric condition monitoring

TL;DR

This paper demonstrates that the Variance of Laplacian method effectively quantifies solar image sharpness, revealing daily atmospheric effects and enabling optical atmospheric condition monitoring using a large dataset of solar images.

Contribution

It introduces the Image Sharpness Function (ISF) as a novel model for atmospheric degradation effects on solar images, applicable to real-time and archival data.

Findings

Image sharpness correlates with Sun altitude and atmospheric conditions.

Degradation in image quality becomes significant below a certain Sun altitude threshold.

ISF can be used for site monitoring and assessing optical atmospheric conditions.

Abstract

Here we present a proof of concept for the application of the Variance of Laplacian (VL) method in quantifying the sharpness of optical solar images. We conducted a comprehensive study using over 65,000 individual solar images acquired on more than 160 days. Each image underwent processing using a VL image processing algorithm, which assigns a 'score' based on the sharpness of the solar disk's edges. We studied the scores obtained from images acquired at different conditions. Our findings demonstrate that the sharpness of the images exhibits daily trends that are closely linked to the altitude of the Sun at the observation site. We observed a significant degradation in image quality only below a certain altitude threshold. Furthermore, we compared airmass formulae from the literature with our sharpness observations and concluded that the degradation could be modeled as an Image Sharpness Function (ISF), which exhibits similarities to airmass variations. In addition to assessing image quality, our method has the potential to evaluate the optical atmospheric conditions during daytime observations. Moreover, this technique can be easily and cost-effectively applied to archival or real-time images of other celestial bodies, such as the Moon, bright planets and defocused stars. Given that ISF is unique to each location and sensitive to sky conditions, the development of an ISF is not only beneficial for routine observation preparation but also essential for long-term site monitoring.