A Misfired Outburst in the Neutron Star X-Ray Binary Centaurus X-4

Baglio, Maria Cristina; Saikia, Payaswini; Russell, D. M.; Homan, J.; Waterval, Stefan; Bramich, D. M.; Campana, S.; Lewis, Fraser; Eijnden, J. van den; Alabarta, Kevin; Covino, S.; D’Avanzo, P.; Goldoni, P.; Masetti, N.; Muñoz-Darias, T.

doi:10.3847/1538-4357/ac63ad

Cited by 7 publications

(7 citation statements)

References 76 publications

(111 reference statements)

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“…Fitting these with a blackbody using least squares, we obtain a temperature estimate of 18,000 ± 1500 K. As at this phase the outburst is substantially brighter than the quiescent state of the system we can be confident that the SED is dominated by the disk. Notably, this temperature is comfortably above the temperature of 10 4 K needed to ionize hydrogen, distinguishing this failed-transition outburst from the "misfired outburst" of Cen X-4 reported by Baglio et al (2022).…”

Section: Spectral Energy Distributionmentioning

confidence: 78%

An Optically Discovered Outburst from XTE J1859+226

Bellm,

Wang,

van Roestel

et al. 2023

ApJ

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Using the Zwicky Transient Facility, in 2021 February we identified the first known outburst of the black hole X-ray transient XTE J1859+226 since its discovery in 1999. The outburst was visible at X-ray, UV, and optical wavelengths for less than 20 days, substantially shorter than its full outburst of 320 days in 1999, and the observed peak luminosity was 2 orders of magnitude lower. Its peak bolometric luminosity was only 2 × 1035 erg s−1, implying an Eddington fraction of about 3 × 10−4. The source remained in the hard spectral state throughout the outburst. From optical spectroscopy measurements we estimate an outer disk radius of 1011 cm. The low observed X-ray luminosity is not sufficient to irradiate the entire disk, but we observe a surprising exponential decline in the X-ray light curve. These observations highlight the potential of optical and infrared synoptic surveys to discover low-luminosity activity from X-ray transients.

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Section: Spectral Energy Distributionmentioning

confidence: 78%

An Optically Discovered Outburst from XTE J1859+226

Bellm,

Wang,

van Roestel

et al. 2023

ApJ

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“…Similar values of power-law correlations have also been seen in other X-ray binaries like XTE J1817-330 (0.47± 0.03, Rykoff et al 2007), GX 339-4 (0.44± 0.01, Coriat et al 2009), GS 1354-64 (∼0.4-0.5, Koljonen et al 2016. 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.…”

Section: Optical/uv/ir Emission Mechanismmentioning

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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“…Similar values of power-law correlations have also been seen in other X-ray binaries like XTE J1817-330 (0.47 ± 0.03, Rykoff et al 2007), GX 339-4 (0.44 ± 0.01, Coriat et al 2009), and GS 1354-64 (∼0.4-0.5, Koljonen et al 2016. 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.…”

Section: Optical/uv/ir Emission Mechanismmentioning

confidence: 99%

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

Saikia

Russell

Baglio

et al. 2022

ApJ

Self Cite

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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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A Misfired Outburst in the Neutron Star X-Ray Binary Centaurus X-4

Cited by 7 publications

References 76 publications

An Optically Discovered Outburst from XTE J1859+226

An Optically Discovered Outburst from XTE J1859+226

A multi-wavelength 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

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