SWIFT J1753.5-0127: A Surprising Optical/X-Ray Cross-Correlation Function

Durant, Martin; Gandhi, P.; Shahbaz, T.; Fabian, A.; Miller, J. M.; Dhillon, V. S.; Marsh, T. R.

doi:10.1086/590906

Cited by 68 publications

(91 citation statements)

References 14 publications

(21 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Extrapolating this power law to optical/NIR wavelengths shows that a spectral break is required at optical/UV frequencies. Analysis of optical data of Swift J1753.5−0127 in its current state by Hynes et al (2009) favors a case where any jet emission is insignificant at optical wavelengths consistent with our extrapolated power-law; this is in agreement with an independent observation/analysis by Durant et al (2008Durant et al ( , 2009). Gandhi (2009) has shown, based on analysis of optical data from XTE J1118+480, GX 339−4, and Swift J1753.5−0127 that the variability at optical wavelengths is inconsistent with being produced by reprocessing of X-rays in the accretion disk and instead favor a model where the emission in the LHS is dominated by the jet, e.g., Malzac et al (2004).…”

Section: Jet And/or Coronasupporting

confidence: 89%

SUZAKUBROADBAND SPECTROSCOPY OFSWIFTJ1753.5–0127 IN THE LOW-HARD STATE

Reynolds

Miller

Homan

et al. 2009

ApJ

View full text Add to dashboard Cite

We present Suzaku observations of the Galactic black hole candidate Swift J1753.5−0127 in the low-hard state (LHS). The broadband coverage of Suzaku enables us to detect the source over the energy range 0.6-250 keV. The broadband spectrum (2-250 keV) is found to be consistent with a simple power-law (Γ ∼ 1.63). In agreement with previous observations of this system, a significant excess of soft X-ray flux is detected consistent with the presence of a cool accretion disk. Estimates of the disk inner radius infer a value consistent with the innermost stable circular orbit (ISCO; R in 6R g , for certain values of, e.g., N H , i), although we cannot conclusively rule out the presence of an accretion disk truncated at larger radii (R in ∼ 10-50R g ). A weak, relativistically broadened iron line is also detected, in addition to disk reflection at higher energy. However, the iron-K line profile favors an inner radius larger than the ISCO (R in ∼ 10-20R g ). The implications of these observations for models of the accretion flow in the LHS are discussed.

show abstract

Section: Jet And/or Coronasupporting

confidence: 89%

SUZAKUBROADBAND SPECTROSCOPY OFSWIFTJ1753.5–0127 IN THE LOW-HARD STATE

Reynolds

Miller

Homan

et al. 2009

ApJ

View full text Add to dashboard Cite

show abstract

“…Hence, the spectral model also predicts the connection between the OIR and the X-ray aperiodic variability. However, simultaneous analysis of light curves in these wavelengths (Motch et al 1983;Kanbach et al 2001;Hynes et al 2003;Durant et al 2008;Gandhi et al 2010) has revealed a complicated connection between them, which can be understood if one considers several components contributing to the optical (Veledina et al 2011), namely the hot accretion flow and the reprocessed radiation. Additionally, the jet optically thin synchrotron emission can also be significant (e.g., Casella et al 2010).…”

Section: Introductionmentioning

confidence: 99%

A Unified Lense-Thirring Precession Model for Optical and X-Ray Quasi-Periodic Oscillations in Black Hole Binaries

Veledina

Poutanen

Ingram

2013

ApJ

View full text Add to dashboard Cite

Recent observations of accreting black holes reveal the presence of quasi-periodic oscillations (QPO) in the optical power density spectra. The corresponding oscillation periods match those found in X-rays, implying a common origin. Among the numerous suggested X-ray QPO mechanisms, some may also work in the optical. However, their relevance to the broadband-optical through X-ray-spectral properties have not been investigated. For the first time, we discuss the QPO mechanism in the context of the self-consistent spectral model. We propose that the QPOs are produced by Lense-Thirring precession of the hot accretion flow, whose outer parts radiate in optical wavelengths. At the same time, its innermost parts are emitting X-rays, which explains the observed connection of QPO periods. We predict that the X-ray and optical QPOs should be either in phase or shifted by half a period, depending on the observer position. We investigate the QPO harmonic content and find that the variability amplitudes at the fundamental frequency are larger in the optical, while the X-rays are expected to have strong harmonics. We then discuss the QPO spectral dependence and compare the expectations to the existing data.

show abstract

“…There are three possible candidates that may account for this emission: the irradiated disc (Cunningham 1976;Gierliński et al 2009), hot accretion flow (Veledina et al 2013a) and the jet (Hynes et al 2002;Gallo et al 2007). Sometimes the OIR fluxes are higher than expected from any candidate alone (Chaty et al 2003;Gandhi et al 2010), and the complex optical/X-ray cross-correlation functions ⋆ E-mail: juri.poutanen@utu.fi (Kanbach et al 2001;Durant et al 2008) support this anticipation, suggesting contribution of two components simultaneously (Veledina, Poutanen, & Vurm 2011b). The source of OIR emission cannot be determined by only using photometric data and some additional information about the OIR-X-ray connection, short time-scale variability properties and the long-term spectral variations is required (see review in Poutanen & Veledina 2014).…”

Section: Introductionmentioning

confidence: 99%

Colours of black holes: infrared flares from the hot accretion disc in XTE J1550–564

Poutanen

Veledina

Revnivtsev

2014

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Outbursts of the black hole (BH) X-ray binaries are dramatic events occurring in our Galaxy approximately once a year. They are detected by the X-ray telescopes and often monitored at longer wavelengths. We analyse the X-ray and optical/infrared (OIR) light-curves of the BH binary XTE J1550-564 during the 2000 outburst. By using the observed extreme colours as well as the characteristic decay time-scales of the OIR and X-ray light curves, we put strong constraints on the extinction towards the source. We accurately separate the contributions to the OIR flux of the irradiated accretion disc and a non-thermal component. We show that the OIR non-thermal component appears during the X-ray state transitions both during the rising and the decaying part of the outburst at nearly the same X-ray hardness but at luminosities differing by a factor of 3. The line marking the quenching/recovery of the non-thermal component at the X-ray hardness-flux diagram seems to coincide with the 'jet line' that marks the presence of the compact radio jet. The inferred spectral shape and the evolution of the non-thermal component during the outburst, however, are not consistent with the jet origin, but are naturally explained in terms of the hybrid hot flow scenario, where non-thermal electrons emit synchrotron radiation in the OIR band. This implies a close, possibly causal connection between the presence of the hot flow and the compact jet. We find that the non-thermal component is hardening during the hard state at the decaying stage of the outburst, which indicates that the acceleration efficiency is a steep function of radius at low accretion rate.

show abstract

SWIFT J1753.5-0127: A Surprising Optical/X-Ray Cross-Correlation Function

Cited by 68 publications

References 14 publications

SUZAKUBROADBAND SPECTROSCOPY OFSWIFTJ1753.5–0127 IN THE LOW-HARD STATE

SUZAKUBROADBAND SPECTROSCOPY OFSWIFTJ1753.5–0127 IN THE LOW-HARD STATE

A Unified Lense-Thirring Precession Model for Optical and X-Ray Quasi-Periodic Oscillations in Black Hole Binaries

Colours of black holes: infrared flares from the hot accretion disc in XTE J1550–564

Contact Info

Product

Resources

About