EDP Sciences
Free Access
Volume 398, Number 1, January IV 2003
Page(s) 195 - 202
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20021650
Published online 14 January 2003

A&A 398, 195-202 (2003)
DOI: 10.1051/0004-6361:20021650

BeppoSAX observation of the composite remnant G327.1-1.1

F. Bocchino1 and R. Bandiera2

1  Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
2  Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy

(Received 30 July 2002 / 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 ( $1.1\times 10^4$ 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

Offprint request: F. Bocchino, bocchino@astropa.unipa.it

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© ESO 2003

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