Issue |
A&A
Volume 398, Number 1, January IV 2003
|
|
---|---|---|
Page(s) | 195 - 202 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20021650 | |
Published online | 14 January 2003 |
BeppoSAX observation of the composite remnant G327.1–1.1
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, bocchino@astropa.unipa.it
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 ( 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
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