A Multiwavelength Study of GRS 1716-249 in Outburst: Constraints on Its System Parameters

Saikia, Payaswini; Russell, David M.; Baglio, M. C.; Bramich, D. M.; Casella, Piergiorgio; Trigo, Maria Diaz; Gandhi, Poshak; Jiang, Jiachen; Maccarone, Thomas; Soria, Roberto; Al Noori, Hind; Al Yazeedi, Aisha; Alabarta, Kevin; Belloni, Tomaso; Bel, Marion Cadolle; Ceccobello, Chiara; Corbel, Stéphane; Fender, Rob; Gallo, Elena; Homan, Jeroen; Koljonen, Karri; Lewis, Fraser; Markoff, Sera B.; Miller-Jones, James C. A.; Rodriguez, Jerome; Russell, Thomas D.; Shahbaz, Tariq; Sivakoff, Gregory R.; Testa, Vincenzo; Tetarenko, Alexandra J.
Bibliographical reference

The Astrophysical Journal

Advertised on:
6
2022
Number of authors
30
IAC number of authors
1
Citations
9
Refereed citations
8
Description
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 find evidence for a weak, but highly variable jet component at mid-infrared wavelengths. We also report the long-term optical light curve of the source and find that the quiescent ${i}^{{\prime} }$ -band magnitude is 21.39 ± 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 data set to those of other outbursting black hole X-ray binaries, we find that while GRS 1716-249 shows similar X-ray behavior, 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 ~4-8 kpc.
Related projects
Black hole in outburst
Black holes, neutron stars, white dwarfs and their local environment

Accreting black-holes and neutron stars in X-ray binaries provide an ideal laboratory for exploring the physics of compact objects, yielding not only confirmation of the existence of stellar mass black holes via dynamical mass measurements, but also the best opportunity for probing high-gravity environments and the physics of accretion; the most

Montserrat
Armas Padilla