Radio and X-ray study of two multi-shell Supernova Remnants: Kes79 and G352.7-0.1

TL;DR

This study analyzes the morphology and physical properties of two multi-shell supernova remnants, Kes79 and G352.7-0.1, using radio and X-ray data to understand their origins and evolution.

Contribution

It provides new insights into the causes of multi-shell structures in SNRs by combining multi-wavelength observations and modeling their progenitors' mass-loss histories.

Findings

Kes79 originated from a massive O9 star near a molecular cloud.

G352.7-0.1's morphology results from asymmetric wind interactions and projection effects.

No pulsar wind nebula was detected in Kes79; G352.7-0.1's X-ray emission is from heated ejecta.

Abstract

We investigate two multi-shell galactic supernova remnants (SNRs), Kes79 and G352.7-0.1, to understand the causes of such morphology. The research was carried out based on new and reprocessed archival VLA observations and XMM-Newton archival data. The surrounding was investigated based on data extracted from the HI Canadian Galactic Plane Survey, the 13^CO Galactic Ring Survey and the HI Southern Galactic Plane Survey. The present study revealed that the overall morphology of both SNRs is the result of the mass-loss history of their respective progenitor stars. Kes79 would be the product of the gravitational collapse of a massive O9 star evolving near a molecular cloud and within the precursor's wind-driven bubble, while G352.7-0.1 would be the result of interactions of the SNR with an asymmetric wind from the progenitor together with projection effects. No radio point source or pulsar wind nebula was found associated with the X-ray pulsar CXOU J185238.6+004020 in Kes79. The X-ray study of G352.7-0.1, on its hand, revealed that most of the thermal X-ray radiation completely fills in the interior of the remnant and originates in heated ejecta. Characteristic parameters, like radio flux, radio spectral index, age, distance, shock velocity, initial energy and luminosity, were estimated for both SNRs.