  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.
