Swift UVOT observations of the 2015 outburst of V404 Cygni

Oates, S. R.; Motta, S.; Beardmore, A. P.; Russell, D. M.; Gandhi, P.; Kuin, N. P. M.; Pasquale, M. de; Altamirano, D.; Breeveld, A. A.; Castro‐Tirado, Alberto J.; Knigge, Christian; Page, M. J.; Steeghs, D.

doi:10.1093/mnras/stz1998

Cited by 9 publications

(6 citation statements)

References 66 publications

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“…On the other hand, many sources like Swift J1357.2-0933 (Armas Padilla et al 2013), Swift J1910.2-0546 (Saikia et al 2022), SAX J1808.4-3658 (Patruno et al 2016, and Cen X-4 (Baglio et al 2022) show a significantly shallower correlation (∼0.1-0.3). A slightly steeper correlation (∼0.56) is seen for V404 Cyg (Bernardini et al 2016;Hynes et al 2019;Oates et al 2019), probably arising from contamination in optical fluxes from jet contribution. From our multiwavelength correlation and spectral energy distribution analysis, we can rule out a significant optical emission component arising from a jet, in GRS 1716−249.…”

Section: Optical/uv/ir Emission Mechanismmentioning

confidence: 84%

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.

show abstract

Section: Optical/uv/ir Emission Mechanismmentioning

confidence: 84%

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

Saikia

Russell

Baglio

et al. 2022

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…On the other hand, many sources like Swift J1357.2-0933 (Armas Padilla et al 2013), Swift J1910.2-0546 (Saikia et al 2022), SAX J1808.4-3658 (Patruno et al 2016 and Cen X-4 (Baglio et al 2022) show a significantly shallower correlation (∼0.1-0.3). A slightly steeper correlation (∼0.56) is seen for V404 Cyg (Bernardini et al 2016;Hynes et al 2019;Oates et al 2019), probably arising from contamination in optical fluxes from jet contribution. From our multi-wavelength correlation and spectral energy distribution analysis, we can rule out a significant optical emission component arising from a jet, in GRS 1716−249.…”

Section: Optical/uv/ir Emission Mechanismmentioning

confidence: 84%

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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“…The Swift team reported a variable X-ray flux, at times in excess of 40 times the Crab Nebula flux (Barthelmy et al 2015, Motta et al 2017, in addition to enhanced and variable UV and optical fluxes (Oates et al 2019). Enhanced fluxes from the V-band optical up to the soft 𝛾-rays (40 -100 keV) were observed with INTEGRAL (Rodriguez et al 2015& Roques et al 2015.…”

Section: Outbursts Of V404 Cygnimentioning

confidence: 99%

V404 Cygni with Fermi-LAT

Harvey,

Rulten,

Chadwick

2021

Preprint

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We revisit the well-studied outburst of the low mass X-ray binary (LMXB) system V404 Cygni, and claims of 𝛾-ray excesses observed with the Fermi-LAT instrument. Upon analysing an 11.5 year dataset with the 8-year LAT point source catalogue and 8-year background models, we find no evidence to suggest that there is high energy 𝛾-ray emission during the outburst period (or at any other time) from V404 Cygni. This is due to the proximity of V404 Cygni to the 𝛾-ray emitting blazar B2023+336, a luminous source approximately 0.3°away, which causes source confusion at the position of V404 Cygni, the luminous 𝛾-ray background, and the use of older background models and catalogues in previous studies.

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Swift UVOT observations of the 2015 outburst of V404 Cygni

Cited by 9 publications

References 66 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

V404 Cygni with Fermi-LAT

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