  We report on observations of the X-ray pulsar IGR J16320-4751 (a.k.a. AX
J1631.9-4752) performed simultaneously with INTEGRAL and XMM-Newton. We refine
the source position and identify the most likely infrared counterpart. Our
simultaneous coverage allows us to confirm the presence of X-ray pulsations at
~1300 s, that we detect above 20 keV with INTEGRAL for the first time. The
pulse fraction is consistent with being constant with energy, which is
compatible with a model of polar accretion by a pulsar. We study the spectral
properties of IGR J16320-4751 during two major periods occurring during the
simultaneous coverage with both satellites, namely a flare and a non-flare
period. We detect the presence of a narrow 6.4 keV iron line in both periods.
The presence of such a feature is typical of supergiant wind accretors such as
Vela X-1 or GX 301-2. We inspect the spectral variations with respect to the
pulse phase during the non-flare period, and show that the pulse is solely due
to variations of the X-ray flux emitted by the source and not to variations of
the spectral parameters.
  Our results are therefore compatible with the source being a pulsar in a High
Mass X-ray Binary. We detect a soft excess appearing in the spectra as a
blackbody with a temperature of ~0.07 keV. We discuss the origin of the X-ray
emission in IGR J16320-4751: while the hard X-rays are likely the result of
Compton emission produced in the close vicinity of the pulsar, based on energy
argument we suggest that the soft excess is likely the emission by a
collisionally energised cloud in which the compact object is embedded.
