We report on observations of the X-ray pulsar IGRÂ J16320 - 4751 ( a.k.a .
AXÂ J1631.9 - 4752 ) performed simultaneously with INTEGRAL Â 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 \sim 1300 s , that we detect above 20 keV with INTEGRAL Â 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 IGRÂ J16320 - 4751Â 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 \sim 0.07 keV .
We discuss the origin of the X-ray emission in IGRÂ 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 .