We have used the RXTE Â and INTEGRAL Â satellites simultaneously to observe the High Mass X-ray binary IGRÂ J19140 + 0951 .
The spectra obtained in the 3–80 keV range have allowed us to perform a precise spectral analysis of the system along its binary orbit .
The spectral evolution confirms the supergiant nature of the companion star and the neutron star nature of the compact object .
Using a simple stellar wind model to describe the evolution of the photoelectric absorption , we were able to restrict the orbital inclination angle in the range 38°–75° .
This analysis leads to a wind mass-loss rate from the companion star of \sim 5 \times 10 ^ { -8 } M _ { \sun } /year , consistent with an OB I spectral type .
We have detected a soft excess in at least four observations , for the first time for this source .
Such soft excesses have been reported in several HMXBs in the past .
We discuss the possible origin of this excess , and suggest , based on its spectral properties and occurrences around the superior conjunction , that it may be explained as the reprocessing of the X-ray emission originating from the neutron star by the surrounding ionised gas .