A multi-wavelength study of GRS 1716-249 in outburst : constraints on its system parameters

TL;DR

This study provides a comprehensive multi-wavelength analysis of GRS 1716-249 during its 2016-2017 outburst, revealing the origins of its emission and refining its system parameters, including a revised distance estimate.

Contribution

It offers new insights into the emission mechanisms and system parameters of GRS 1716-249, especially its distance, based on extensive multi-wavelength observations and critical reassessment of previous assumptions.

Findings

Optical/near-infrared and UV emission mainly from a multi-temperature accretion disk.

Mid-infrared and radio emission dominated by synchrotron from a compact jet.

Revised distance estimate of 4-17 kpc, most likely 4-8 kpc.

Abstract

We present a detailed study of the evolution of the Galactic black hole transient GRS 1716-249 during its 2016-2017 outburst at optical (Las Cumbres Observatory), mid-infrared (Very Large Telescope), near-infrared (Rapid Eye Mount telescope), and ultraviolet (the Neil Gehrels Swift Observatory Ultraviolet/Optical Telescope) wavelengths, along with archival radio and X-ray data. We show that the optical/near-infrared and UV emission of the source mainly originates from a multi-temperature accretion disk, while the mid-infrared and radio emission are dominated by synchrotron emission from a compact jet. The optical/UV flux density is correlated with the X-ray emission when the source is in the hard state, consistent with an X-ray irradiated accretion disk with an additional contribution from the viscous disk during the outburst fade. We also report the long-term optical light curve of the source and find that the quiescent i-band magnitude is 21.39$\pm$0.15 mag. Furthermore, we discuss how previous estimates of the system parameters of the source are based on various incorrect assumptions, and so are likely to be inaccurate. By comparing our GRS 1716-249 dataset to those of other outbursting black hole X-ray binaries, we find that while GRS 1716-249 shows similar X-ray behaviour, it is noticeably optically fainter, if the literature distance of 2.4 kpc is adopted. Using several lines of reasoning, we argue that the source distance is further than previously assumed in the literature, likely within 4-17 kpc, with a most likely range of $\sim$4-8 kpc.