  We present an X-ray analysis of the central region of supernova remnant (SNR)
G332.5-5.6 through an exhaustive analysis of XMM-Netwon observations with
complementary infrared observations. We characterize and discuss the origin of
the observed X-ray morphology, which presents a peculiar plane edge over the
west side of the central region. The morphology and spectral properties of the
X-ray supernova remnant were studied using a single full frame XMM-Newton
observation in the 0.3 to 10.0 keV energy band. Archival infrared WISE
observations at 8, 12 and 24 \mu m were also used to investigate the properties
of the source and its surroundings at different wavelengths. The results show
that the extended X-ray emission is predominantly soft (0.3-1.2 keV) and peaks
around 0.5 keV, which shows that it is an extremely soft SNR. X-ray emission
correlates very well with central regions of bright radio emission. On the west
side the radio/X-ray emission displays a plane-like feature with a terminal
wall where strong infrared emission is detected. Our spatially resolved X-ray
spectral analysis confirms that the emission is dominated by weak atomic
emission lines of N, O, Ne, and Fe, all of them undetected in previous X-ray
studies. These characteristics suggest that the X-ray emission is originated in
an optically thin thermal plasma, whose radiation is well fitted by a
non-equilibrium ionization collisional plasma (VNEI) X-ray emission model. Our
study favors a scenario where G332.5-5.6 is expanding in a medium with an
abrupt density change (the wall), likely a dense infrared emitting region of
dust on the western side of the source.
