An X-ray Investigation of Three Supernova Remnants in the Large Magellanic Cloud

TL;DR

This study uses multi-wavelength X-ray and optical data to analyze three supernova remnants in the Large Magellanic Cloud, revealing their physical properties and evolutionary states, including the largest remnant known in the LMC.

Contribution

It provides new X-ray observations and analysis of faint, highly evolved SNRs in the LMC, including the largest remnant, enhancing understanding of SNR populations and evolution.

Findings

Identified a previously missed population of faint SNRs.

Determined physical conditions of hot and warm gas in the remnants.

Compared observed SNR morphologies with theoretical evolution models.

Abstract

We have investigated three SNRs in the LMC using multi-wavelength data. These SNRs are generally fainter than the known sample and may represent a previously missed population. One of our SNRs is the second LMC remnant analyzed which is larger than any Galactic remnant for which a definite size has been established. The analysis of such a large remnant contributes to the understanding of the population of highly evolved SNRs. We have obtained X-ray images and spectra of three of these recently identified SNRs using the XMM-Newton observatory. These data, in conjunction with pre-existing optical emission-line images and spectra, were used to determine the physical conditions of the optical- and X-ray-emitting gas in the SNRs. We have compared the morphologies of the SNRs in the different wavebands. The physical properties of the warm ionized shell were determined from the H-alpha surface brightness and the SNR expansion velocity. The X-ray spectra were fit with a thermal plasma model and the physical conditions of the hot gas were derived from the model fits. Finally, we have compared our observations with simulations of SNR evolution.