The XMM-Newton X-ray emission of the SNR N120 in the LMC

TL;DR

This paper combines new XMM-Newton X-ray observations with numerical simulations to analyze the structure, emission, and evolution of the supernova remnant N120 in the Large Magellanic Cloud, revealing detailed insights into its morphology and physical conditions.

Contribution

It presents the first combined observational and simulation study of N120, demonstrating the remnant's X-ray emission characteristics and the effects of an inhomogeneous ISM on its evolution.

Findings

X-ray emission is brighter towards the east rim.

Simulations match observed X-ray luminosity and surface brightness.

Extended diffuse X-ray emission likely from the surrounding HII complex.

Abstract

We present new XMM-Newton observations of the supernova remnant N120 in the LMC, and numerical simulations on the evolution of this supernova remnant which we compare with the X-ray observations. The supernova remnant N120, together with several HII regions, forms a large nebular complex5D (also called N120) whose shape resembles a semicircular ring. From the XMM-Newton data we generate images and spectra of this remnant in the energy band between 0.2 to 2.0 keV. The images show that the X-ray emission is brighter towards the east (i.e., towards the rim of the large nebular complex). The EPIC/MOS1 and MOS2 data reveal a thermal spectrum in soft X-rays. 2D axisymmetric numerical simulations with the Yguaz\'u-a code were carried out assuming that the remnant is expanding into an inhomogeneous ISM with an exponential density gradient and showing that thermal conduction effects are negligible. Simulated X-ray emission maps were obtained from the numerical simulations in order to compare them with the observations. We find good agreement between the XMM-Newton data, previous optical kinematic data, and the numerical simulations; the simulations reproduce the observed X-ray luminosity and surface brightness distribution. We have also detected more extended diffuse X-ray emission probably due to the N120 large HII complex or superbubble.