Multi-wavelength view of the galactic black-hole binary GRS 1716-249

TL;DR

This study analyzes the multi-wavelength spectral energy distribution of the galactic black-hole binary GRS 1716-249, revealing the dominant emission mechanisms across different energy ranges and the role of jets and disk irradiation.

Contribution

It provides a comprehensive multi-wavelength analysis of GRS 1716-249, identifying the contributions of irradiated disks, jets, and corona to the emission spectrum.

Findings

Irradiated accretion disk dominates UV and optical emission.

Infrared excess likely due to jet synchrotron emission.

Hard X-ray irradiation influences soft X-ray emission.

Abstract

The origins of X-ray and radio emissions during an X-ray binary outburst are comparatively better understood than those of ultraviolet, optical and infrared radiation. This is because multiple competing mechanisms peak in these mid-energy ranges. Ascertaining the true emission mechanism and segregating the contribution of different mechanisms, if present, is important for correct understanding of the energetics of the system and hence its geometry. We have studied the multi-wavelength spectral energy distribution of the galactic X-ray binary GRS 1716-249 ranging from near infrared (0.0005 keV) to hard X-rays (120 keV) using observations from AstroSat, Swift, and Mount Abu Infrared Observatory. Broadband spectral fitting suggests that the irradiated accretion disk dominates emission in ultraviolet and optical regimes. The near infrared emission exhibits some excess than the prediction of the irradiated disk model, which is most likely due to Synchrotron emission from jets as suggested by radio emission. Irradiation of the inner disk by the hard X-ray emission from the Corona also plays a significant role in accounting for the soft X-ray emission.