A late jet rebrightening revealed from multiwavelength monitoring of the black hole candidate XTE J1752−223★

Russell, D. M.; Curran, P. A.; Muñoz-Darias, T.; Lewis, Fraser; Motta, S.; Stiele, H.; Belloni, T.; Miller-Jones, J. C. A.; Jonker, P. G.; O’Brien, Kieran; Homan, J.; Casella, P.; Gandhi, P.; Soleri, P.; Markoff, Sera; Maitra, D.; Gallo, Elena; Bel, M. Cadolle

doi:10.1111/j.1365-2966.2011.19839.x

Cited by 27 publications

(32 citation statements)

References 89 publications

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“…XTE J1752−223 is such a case in which a late flare occurred ∼55 days after the transition to the hard state. Russell et al (2012) measured the SED optical to Xray spectral index during the flare to be −1.0 ± 0.3 which is consistent with synchrotron emission from a compact jet. A detailed investigation of SMARTS light curves in the H and I bands show that apart from the large flare with simultaneous enhancement in the OIR and X-rays, there is an earlier, smaller flare observed close to the first detection of the compact core with the VLBA ).…”

Section: The Origin Of the Flare In X-rays And Opticalsupporting

confidence: 62%

Multiwavelength observations of the black hole transient Swift J1745−26 during the outburst decay

Kalemci

Arabacı

Güver

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We characterized the broad-band X-ray spectra of Swift J1745−26 during the decay of the 2013 outburst using INTEGRAL ISGRI, JEM-X and Swift XRT. The X-ray evolution is compared to the evolution in optical and radio. We fit the Xray spectra with phenomenological and Comptonization models. We discuss possible scenarios for the physical origin of a ∼50 day flare observed both in optical and Xrays ∼170 days after the peak of the outburst. We conclude that it is a result of enhanced mass accretion in response to an earlier heating event. We characterized the evolution in the hard X-ray band and showed that for the joint ISGRI-XRT fits, the e-folding energy decreased from 350 keV to 130 keV, while the energy where the exponential cut-off starts increased from 75 keV to 112 keV as the decay progressed. We investigated the claim that high energy cut-offs disappear with the compact jet turning on during outburst decays, and showed that spectra taken with HEXTE on RXTE provide insufficient quality to characterize cut-offs during the decay for typical hard X-ray fluxes. Long INTEGRAL monitoring observations are required to understand the relation between the compact jet formation and hard X-ray behavior. We found that for the entire decay (including the flare), the X-ray spectra are consistent with thermal Comptonization, but a jet synchrotron origin cannot be ruled out.

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Section: The Origin Of the Flare In X-rays And Opticalsupporting

confidence: 62%

Multiwavelength observations of the black hole transient Swift J1745−26 during the outburst decay

Kalemci

Arabacı

Güver

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…However, the 2007 event was markedly different to the others in that GX 339-4 did not return to quiescence after the peak was reached, and remained in the hard state during 2008 and 2009 during which it fluctuated significantly in O/IR fluxes. Rebrightening events have been observed in the O/IR during the outbursts of 4U1543-47 (Buxton & Bailyn 2004) and XTE J1550-564 , and in optical/X-ray fluxes in XTE J1752-223 (Russell et al 2012). The shape of the rebrightening events in all three systems are remarkably similar in that they exhibit a fastrise-exponential-decay profile.…”

Section: Discussionmentioning

confidence: 61%

“…These differences may provide clues as to how much material has been either accreted by the black hole or ejected via the jets. Research is now starting to focus on how much jets contribute to the overall flux of the system at high and low luminosities (e.g., Russell et al 2010;Soleri & Fender 2011) and decomposition of the disk/jet fluxes (e.g., Maitra et al 2009;Russell et al 2010Russell et al , 2011Russell et al , 2012T. Dinçer et al, submitted).…”

Section: Discussionmentioning

confidence: 99%

Optical and Near-Infrared Monitoring of the Black Hole X-Ray Binary Gx 339-4 During 2002-2010

Buxton¹,

Bailyn²,

Capelo³

et al. 2012

The Astronomical Journal

102

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We present the optical/infrared (O/IR) light curve of the black hole X-ray binary GX 339-4 collected at the SMARTS 1.3 m telescope from 2002 to 2010. During this time the source has undergone numerous state transitions including hard-to-soft state transitions when we see large changes in the near-IR flux accompanied by modest changes in optical flux, and three rebrightening events in 2003, 2005, and 2007 after GX 339-4 transitioned from the soft state to the hard. All but one outburst show similar behavior in the X-ray hardness-intensity diagram. We show that the O/IR colors follow two distinct tracks that reflect either the hard or soft X-ray state of the source. Thus, either of these two X-ray states can be inferred from O/IR observations alone. From these correlations we have constructed spectral energy distributions of the soft and hard states. During the hard state, the near-IR data have the same spectral slope as simultaneous radio data when GX 339-4 was in a bright optical state, implying that the near-IR is dominated by a non-thermal source, most likely originating from jets. Non-thermal emission dominates the near-IR bands during the hard state at all but the faintest optical states, and the fraction of non-thermal emission increases with increasing optical brightness. The spectral slope of the optical bands indicate that a heated thermal source is present during both the soft and hard X-ray states, even when GX 339-4 is at its faintest optical state. We have conducted a timing analysis of the light curve for the hard and soft states and find no evidence of a characteristic timescale within the range of 4-230 days.

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“…Such indices were also observed in the flare spectrum of XTE J1752−223 (Russell et al 2012) and GX 339−4 (Dinçer et al 2012;). This would mean that all these OIR flares are produced by the hot flow but not the jet.…”

Section: Broad-band Spectra and Infrared Flaresmentioning

confidence: 53%

Modelling Spectral and Timing Properties of Accreting Black Holes: The Hybrid Hot Flow Paradigm

Poutanen

Veledina

2014

Space Sci Rev

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The general picture that emerged by the end of 1990s from a large set of optical and X-ray, spectral and timing data was that the X-rays are produced in the innermost hot part of the accretion flow, while the optical/infrared (OIR) emission is mainly produced by the irradiated outer thin accretion disc. Recent multiwavelength observations of Galactic black hole transients show that the situation is not so simple. Fast variability in the OIR band, OIR excesses above the thermal emission and a complicated interplay between the X-ray and the OIR light curves imply that the OIR emitting region is much more compact. One of the popular hypotheses is that the jet contributes to the OIR emission and even is responsible for the bulk of the X-rays. However, this scenario is largely ad hoc and is in contradiction with many previously established facts. Alternatively, the hot accretion flow, known to be consistent with the X-ray spectral and timing data, is also a viable candidate to produce the OIR radiation. The hot-flow scenario naturally explains the power-law like OIR spectra, fast OIR variability and its complex relation to the X-rays if the hot flow contains non-thermal electrons (even in energetically negligible quantities), which are required by the presence of the MeV tail in Cyg X-1. The presence of non-thermal electrons also lowers the equilibrium electron temperature in the hot flow model to 100 keV, making it more consistent with observations. Here we argue that any viable model should simultaneously explain a large set of spectral and timing data and show that the hybrid (thermal/non-thermal) hot flow model satisfies most of the constraints.

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A late jet rebrightening revealed from multiwavelength monitoring of the black hole candidate XTE J1752−223★

Cited by 27 publications

References 89 publications

Multiwavelength observations of the black hole transient Swift J1745−26 during the outburst decay

Multiwavelength observations of the black hole transient Swift J1745−26 during the outburst decay

Optical and Near-Infrared Monitoring of the Black Hole X-Ray Binary Gx 339-4 During 2002-2010

Modelling Spectral and Timing Properties of Accreting Black Holes: The Hybrid Hot Flow Paradigm

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