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We have used the  RXTE  and  INTEGRAL  satellites simultaneously to observe the high‐mass X‐ray binary (HMXB) 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 38°–75°. This analysis leads to a wind mass‐loss rate from the companion star of  ∼5 × 10 −8  M ⊙  yr −1  , 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 ionized gas.

Peering through the stellar wind of IGR J19140+0951 with simultaneous INTEGRAL / RXTE observations