  We investigate the spatial distribution of the physical and chemical
properties of the hot X-ray emitting plasma of the supernova remnant IC 443, in
order to get important constraints on its ionization stage, on the progenitor
supernova explosion, on the age of the remnant, and its physical association
with a close pulsar wind nebula.
  The hard X-ray thermal emission (1.4-5.0 keV) of IC 443 displays a
centrally-peaked morphology, its brightness peaks being associated with hot
(kT>1 keV) X-ray emitting plasma. A ring-shaped structure, characterized by
high values of equivalent widths and median photon energy, encloses the PWN.
Its hard X-ray emission is spectrally characterized by a collisional ionization
equilibrium model, and strong emission lines of Mg, Si, and S, requiring
oversolar metal abundances. Dynamically, the location of the ejecta ring
suggests an SNR age of ~4,000 yr.
  The presence of overionized plasma in the inner regions of IC 443, addressed
in previous works, is much less evident in our observations.
