  We have used the RXTE and INTEGRAL satellites simultaneously to observe the
High Mass X-ray binary IGR 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
37-75 degrees. This analysis leads to a wind mass-loss rate from the companion
star of ~ 10e-7 Msun/year, consistent with its expected spectral type. We have
detected a soft excess in at least three 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 prior to 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.
