Radio and X-ray study of two multi-shell supernova remnants: Kes 79 and G352.7-0.1

GIACANI, E.; SMITH, M.; DUBNER, G.; LOISEAU, N.; CASTELLETTI, G.; PARON, S.

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Lugar: Paris; Año: 2009 vol. 507 p. 841 - 853

0004-6361

Aims. We investigate two multi-shell galactic supernova remnants (SNRs), Kes 79, and G352.7−0.1, to understand the causes of thismorphology.Methods. The research was carried out based on new and reprocessed archival VLA observations and XMM-Newton archival data.The surrounding gas was investigated based on data extracted from the HI Canadian Galactic Plane Survey, the 13CO Galactic RingSurvey, and the HI Southern Galactic Plane Survey.Results. The present study infers that the overall morphology of both SNRs is the result of the mass-loss history of their respectiveprogenitor stars. Kes 79 is likely to be the product of the gravitational collapse of a massive O9 star evolving near a molecular cloudand within the precursor’s wind-driven bubble, while G352.7−0.1 should be the result of interactions of the SNR with an asymmetricwind from the progenitor together with projection effects. No radio point source or pulsar wind nebula was found to be associatedwith the X-ray pulsar CXOU J185238.6+004020 in Kes 79. The X-ray study of G352.7−0.1 found that most of the thermal X-rayradiation completely fills the interior of the remnant and originates in heated ejecta. Characteristic parameters, such as radio flux,radio spectral index, age, distance, shock velocity, initial energy, and luminosity, were estimated for both SNRs.Key words. radio continuum: ISM – ISM: supernova remnants – X-rays: individuals: Kes 79 – X-rays: individuals: G352.7–0.1