BeppoSAX observation of the composite remnant G327.1-1.1

Abstract

We report an X-ray study of the composite supernova remnant G327.1-1.1, with particular emphasis on its thermal emission. By virtue of a combined spatial and spectral analysis, we have been able to model the X-ray emission of the remnant as a sum of two components: a non-thermal component, due to the pulsar nebula and the pulsar itself, and a thermal component, of which we have analysed spectrum and morphology, after proper subtraction of the plerion. We discuss three possible interpretations of the thermal emission of \src: pure Sedov expansion, expansion through a inhomogeneous medium with evaporation from ISM clouds, and radiative expansion. On the light of our new data and interpretation, we have re-derived all the physical parameters of this SNR. In the framework of Sedov or radiative expansion we derive a longer age than previously estimated ($1.1\times 10^4$), thus not requiring a high velocity for the pulsar.

8 pages, 5 figures, full res version at http://www.astropa.unipa.it/Library/OAPA_preprints/h3891.ps.gz

References in corpus (1)

• Thermal X-ray composites as an effect of projection

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• Radio Polarization Observations of the Snail: A Crushed Pulsar Wind Nebula in G327.1-1.1 with a Highly Ordered Magnetic Field
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• MeV-GeV Gamma-ray Emission from SNR G327.1-1.1 Discovered by the Fermi-LAT
• likely Detection of GeV gamma-Ray Emission from the composite supernova remnant COMP G327.1+1.1 with Fermi-LAT