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

Rout, Sandeep K.; Vadawale, S.; Aarthy, E.; Ganesh, S.; Joshi, Vishal; Roy, Jayashree; Misra, Ranjeev; Yadav, J. S.

doi:10.1007/s12036-021-09696-5

Cited by 6 publications

(6 citation statements)

References 43 publications

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“…Along with being above the disk model, the mid-IR emission is also highly variable (see Table 1), and the radio to mid-IR spectrum is slightly inverted (with an index of α = 0.13 ± 0.03), which are typical signs of jet emission from BHXBs. The broadband spectral fitting performed by Rout et al (2021) also shows that an irradiated accretion disk dominates the ultraviolet and optical emission. They report an IR excess compared to what is predicted by the irradiated disk model, and interpret it as due to the presence of a jet.…”

Section: Optical/uv/ir Emission Mechanismmentioning

confidence: 83%

“…A type-C quasi-periodic oscillation (QPO) was also detected in the hard state (Bharali et al 2019), and signatures of a hot and dense accretion disk wind (with terminal velocity ∼2000 km s −1 ) were observed (Cuneo et al 2020). From the broadband spectral fitting of the source, the irradiated accretion disk was found to dominate the optical emission, while a hint of an excess near-IR emission above the prediction of the irradiated disk model was observed, likely due to synchrotron emission originated in the jet (Rout et al 2021).…”

Section: Grs 1716−249mentioning

confidence: 88%

“…In the near-IR wavelengths, the source is not detected with 2MASS during quiescence (Rout et al 2021), inferring an upper limit of 15.8 mag for the J band, 15.1 mag for the H band, and 14.3 for the K band (Skrutskie 2006). From archival J-band images of the field taken during quiescence on 1999 July 5 and 7 (MJD 51364 and 51366) with the SOFI instrument at the New Technology Telescope (NTT; La Silla, Chile), we find a 3σ upper limit of the source of J > 18.8 mag, while the nearby southern star was found to have magnitudes of J = 15.38 ± 0.05 mag (see Section 2.2.2).…”

Section: Long-term Monitoring and Quiescent Magnitudementioning

confidence: 92%

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

Saikia

Russell

Baglio

et al. 2022

ApJ

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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 ′ -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.

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Section: Optical/uv/ir Emission Mechanismmentioning

confidence: 83%

Section: Grs 1716−249mentioning

confidence: 88%

Section: Long-term Monitoring and Quiescent Magnitudementioning

confidence: 92%

See 1 more Smart Citation

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

Saikia

Russell

Baglio

et al. 2022

ApJ

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“…In the near-IR wavelengths, the source is not detected with 2MASS during quiescence (Rout et al 2021), inferring an upper limit of 15.8 mag for the J band, 15.1 mag for the H band and 14.3 for the K band (Skrutskie 2006). From archival J-band images of the field taken during quiescence on 1999 July 5 and 7 (MJD 51364 and 51366) with the SOFI instrument at the New Technology Telescope (NTT; La Silla, Chile), we find a 3σ upper limit of the source of J > 18.8 mag, while the nearby southern star was found to have magnitudes of J = 15.38 ± 0.05 mag (see Section 2.2.2).…”

Section: Long-term Monitoring and Quiescent Magnitudementioning

confidence: 99%

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

Saikia,

Russell,

Baglio

et al. 2022

Preprint

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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 -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 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 ∼ 4-8 kpc.

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“…This prompted a flurry of observations across the electromagnetic spectrum, from very high energy TeV/GeV γ-rays detected by H.E.S.S. 3 (Wagner 2021a,b;Aharonian et al 2022) and MAGIC 4 (Acciari et al 2022), and MeV γrays by Fermi-LAT 5 (Cheung et al 2021a(Cheung et al ,b, 2022; to X-rays seen by MAXI 6 (Shidatsu et al 2021), INTE-GRAL 7 (Ferrigno et al 2021), NICER 8 (Enoto et al 2021a,b;Luna et al 2021;Orio et al 2021b,c), NuS-TAR 9 (Luna et al 2021), AstroSat (Rout et al 2021), Chandra and XMM-Newton (Orio et al 2021a), as well as Swift (Page, Osborne & Aydi 2021;Page 2021a,b); to optical (Taguchi, Ueta & Isogai 2021;Munari & Valisa 2021a;Mikolajewska et al 2021;Munari & Valisa 2021b;Nikolov & Luna 2021;Shore et al 2021a;Shore, Teyssier & Thizy 2021;Shore et al 2021b;Munari, Valisa & Ochner 2021;Fajrin et al 2021;Ricra, Vannini & Baella 2021;Zamanov et al 2021); infrared (Woodward et al 2021a,b); and radio (Williams et al 2021;Sokolovsky et al 2021;Peters et al 2021). A neutrino search was performed by IceCube, though only upper limits could be placed (Pizzuto, Vandenbroucke & Santander 2021).…”

Section: Introductionmentioning

confidence: 99%

The 2021 outburst of the recurrent nova RS Ophiuchi observed in X-rays by the Neil Gehrels Swift Observatory: a comparative study

Page,

Beardmore,

Osborne

et al. 2022

Preprint

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On 2021 August 8, the recurrent nova RS Ophiuchi erupted again, after an interval of 15.5 yr. Regular monitoring by the Neil Gehrels Swift Observatory began promptly, on August 9.9 (0.37 day after the optical peak), and continued until the source passed behind the Sun at the start of November, 86 days later. Observations then restarted on day 197, once RS Oph emerged from the Sun constraint. This makes RS Oph the first Galactic recurrent nova to have been monitored by Swift throughout two eruptions. Here we investigate the extensive X-ray datasets from 2006 and 2021, as well as the more limited data collected by EXOSAT in 1985. The hard X-rays arising from shock interactions between the nova ejecta and red giant wind are similar following the last two eruptions. In contrast, the early supersoft source (SSS) in 2021 was both less variable and significantly fainter than in 2006. However, 0.3-1 keV light-curves from 2021 reveal a 35 s quasi-periodic oscillation consistent in frequency with the 2006 data. The Swift X-ray spectra from 2021 are featureless, with the soft emission typically being well parametrized by a simple blackbody, while the 2006 spectra showed much stronger evidence for superimposed ionized absorption edges. Considering the data after day 60 following each eruption, during the supersoft phase the 2021 spectra are hotter, with smaller effective radii and lower wind absorption, leading to an apparently reduced bolometric luminosity. We explore possible explanations for the gross differences in observed SSS behaviour between the 2006 and 2021 outbursts.

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

Cited by 6 publications

References 43 publications

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

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

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

The 2021 outburst of the recurrent nova RS Ophiuchi observed in X-rays by the Neil Gehrels Swift Observatory: a comparative study

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