Linear feature detection algorithm for astronomical surveys - II. Defocusing effects on meteor tracks

TL;DR

This paper models how large aperture telescopes detect meteors as defocused linear tracks, deriving formulas to estimate meteor size and distance from brightness profiles, aiding automated detection in astronomical surveys.

Contribution

It provides an analytic model for defocused meteor tracks in astronomical images and validates it with simulations, improving automatic meteor detection methods.

Findings

Brightness profiles can reveal meteor size and distance.

Satellite tracks are distinguishable by narrower FWHM.

Atmospheric seeing complicates meteor profile analysis.

Abstract

Given the current limited knowledge of meteor plasma micro-physics and its interaction with the surrounding atmosphere and ionosphere, meteors are a highly interesting observational target for high-resolution wide-field astronomical surveys. Such surveys are capable of resolving the physical size of meteor plasma heads, but they produce large volumes of images that need to be automatically inspected for possible existence of long linear features produced by meteors. Here we show how big aperture sky survey telescopes detect meteors as defocused tracks with a central brightness depression. We derive an analytic expression for a defocused point source meteor track and use it to calculate brightness profiles of meteors modeled as uniform brightness disks. We apply our modeling to meteor images as seen by the SDSS and LSST telescopes. The expression is validated by Monte Carlo ray-tracing simulations of photons traveling through the atmosphere and the LSST telescope optics. We show that estimates of the meteor distance and size can be extracted from the measured FWHM and the strength of the central dip in the observed brightness profile. However, this extraction becomes difficult when the defocused meteor track is distorted by the atmospheric seeing or contaminated by a long lasting glowing meteor trail. The FWHM of satellites tracks is distinctly narrower than meteor values, which enables removal of a possible confusion between satellites and meteors.