A multi-wavelength study of the radio source G296.7-0.9: confirmation as a Galactic supernova remnant

TL;DR

This study confirms G296.7-0.9 as a Galactic supernova remnant through multi-wavelength observations, revealing its morphology, spectral index, polarization, and environmental context, with no associated neutron star or pulsar wind nebula.

Contribution

First comprehensive multi-wavelength analysis confirming G296.7-0.9 as a supernova remnant with detailed environmental and morphological insights.

Findings

G296.7-0.9 exhibits bilateral radio morphology and a spectral index of -0.5.

The remnant shows thermal X-ray emission with a bright arc near its boundary.

No evidence of a neutron star or pulsar wind nebula was found.

Abstract

We present a multi-wavelength study of the radio source G296.7-0.9. This source has a bilateral radio morphology, a radio spectral index of -0.5 +/- 0.1, sparse patches of linear polarisation, and thermal X-rays with a bright arc near the radio boundary. Considering these characteristics, we conclude that G296.7-0.9 is a supernova remnant (SNR). The age and morphology of the SNR in the context of its environment suggest that the source is co-located with an HII region, and that portions of the shock front have broken out into a lower density medium. We see no evidence for a neutron star or pulsar wind nebula associated with SNR G296.7-0.9.