  We have analyzed an observation of the supernova remnant N132D in the Large
Magellanic Cloud, performed with the Low Energy Concentrator Spectrometer
(LECS) and the Medium Energy Concentrator Spectrometer (MECS) instruments on
board the X-ray satellite BeppoSAX. Thanks to the good sensitivity of the
LECS/MECS combination over the range 0.3--8.5~keV we were able to detect the
presence of an additional hotter plasma with respect to what had been
previously assumed for this remnant. This hotter component is the source of the
Fe-K line emission visible in the spectrum. Using a two component NEI plasma
model we find that the best fitting abundance values indicate that N132D is
also O-rich from the X-ray point of view. We briefly discuss the origin of the
hot component and tentatively associate it with a radio bright region.
