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

TL;DR

This study uses simultaneous INTEGRAL and RXTE observations to analyze the spectral evolution of the high-mass X-ray binary IGR J19140+0951, revealing the system's stellar wind properties, orbital inclination, and detecting a soft excess likely caused by reprocessed X-ray emission.

Contribution

First simultaneous spectral analysis of IGR J19140+0951 across 3-80 keV, constraining wind properties and orbital inclination, and identifying a soft excess phenomenon.

Findings

Confirmed supergiant companion and neutron star nature.

Estimated wind mass-loss rate of ~5x10^-8 Msun/year.

Detected soft excess likely due to reprocessed X-ray emission.

Abstract

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 38--75 degrees. This analysis leads to a wind mass-loss rate from the companion star of ~5x 10e-8 Msun/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.