BeppoSAX observation of the composite remnant G327.1–1.1
Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
2 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
Corresponding author: F. Bocchino, firstname.lastname@example.org
Accepted: 11 November 2002
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 G327.1–1.1: 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 ( yr), thus not requiring a high velocity for the pulsar.
Key words: acceleration of particles / radiation mechanisms: non-thermal / ISM: clouds / ISM: individual objects: G327.1–1.1 / ISM: supernova remnants
© ESO, 2003