Jet-dominated quiescent states in black hole X-ray binaries: the case of V404 Cyg

Xie, Fu-Guo; Yang, Qi-Xiang; Ma, Renyi

doi:10.1093/mnrasl/slu068

Cited by 21 publications

(22 citation statements)

References 51 publications

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“…Several studies of V404 Cygni in quiescence have favored a synchrotron origin for the X-ray emission (e.g., Bernardini & Cackett 2014;Xie et al 2014;Markoff et al 2015). In this case, the observed G » 2 implies that the synchrotron emitting particles are radiatively cooled (see, e.g., Plotkin et al 2013), and/or that the particle acceleration mechanisms along the jet become less efficient as luminosity decreases (i.e., the maximum Lorentz factor of accelerated particles becomes smaller, see, e.g., Connors et al 2016 for recent discussions on both scenarios).…”

Section: Comments On Jet Synchrotron X-ray Emissionmentioning

confidence: 99%

“…Thus, V404 Cygni is arguably the best-studied quiescent BHXB (e.g., Casares et al 1992;Shahbaz et al 1994;Narayan et al 1997;Hynes et al 2004Hynes et al , 2009Miller-Jones et al 2008;Bernardini & Cackett 2014;Xie et al 2014;Markoff et al 2015;Bernardini et al 2016a;Rana et al 2016), thereby allowing rich comparisons between our observations and its pre-outburst properties.…”

Section: Introductionmentioning

confidence: 99%

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The 2015 Decay of the Black Hole X-Ray Binary V404 Cygni: Robust Disk-Jet Coupling and a Sharp Transition Into Quiescence

Plotkin

Miller-Jones

Gallo

et al. 2017

ApJ

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We present simultaneous X-ray and radio observations of the black hole X-ray binary V404 Cygni at the end of its 2015 outburst. From 2015 July 11-August 5, we monitored V404 Cygni with Chandra, Swift, and NuSTAR in the X-ray, and with the Karl G. Jansky Very Large Array and the Very Long Baseline Array in the radio, spanning a range of luminosities that were poorly covered during its previous outburst in 1989 (our 2015 campaign covers10 erg s 33 X 34 1 ). During our 2015 campaign, the X-ray spectrum evolved rapidly from a hard photon index of). We argue that V404 Cygni reaching G » 2 marks the beginning of the quiescent spectral state, which occurs at a factor of ≈3-4 higher X-ray luminosity than the average pre-outburst luminosity of »´-8 10 erg s 32 1. V404 Cygni falls along the same radio/X-ray luminosity correlation that it followed during its previous outburst in 1989, implying a robust disk-jet coupling. We exclude the possibility that a synchrotron-cooled jet dominates the X-ray emission in quiescence, leaving synchrotron self-Compton from either a hot accretion flow or from a radiatively cooled jet as the most likely sources of X-ray radiation, and/or particle acceleration along the jet becoming less efficient in quiescence. Finally, we present the first indications of correlated radio and X-ray variability on minute timescales in quiescence, tentatively measuring the radio emission to lag the X-ray by  15 4 minute, suggestive of X-ray variations propagating down a jet with alength of<3.0 au.

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Section: Comments On Jet Synchrotron X-ray Emissionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The 2015 Decay of the Black Hole X-Ray Binary V404 Cygni: Robust Disk-Jet Coupling and a Sharp Transition Into Quiescence

Plotkin

Miller-Jones

Gallo

et al. 2017

ApJ

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“…Variable remnant activity, attributed to a compact jet, was detected from radio to hard X-rays (e.g. Hynes et al 2004;Xie et al 2014). V404 is one of the few sources that defines the radio/X-ray correlation over a wide range of luminosities, down into quiescence (Corbel et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Correlated optical, X-ray, andγ-ray flaring activity seen with INTEGRAL during the 2015 outburst of V404 Cygni

Rodríguez

Bel

Alfonso-Garzón

et al. 2015

A&A

103

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After 25 years of quiescence, the microquasar V404 Cyg entered a new period of activity in June 2015. This X-ray source is known to undergo extremely bright and variable outbursts seen at all wavelengths. It is therefore an object of prime interest to understand the accretion-ejection connections. These can, however, only be probed through simultaneous observations at several wavelengths. We made use of the INTEGRAL instruments to obtain long, almost uninterrupted observations from 2015 June 20, 15:50 UTC to June 25, 4:05 UTC, from the optical V band up to the soft γ-rays. V404 Cyg was extremely variable in all bands, with the detection of 18 flares with fluxes exceeding 6 Crab (20-40 keV) within three days. The flare recurrence can be as short as ∼20 min from peak to peak. A model-independent analysis shows that the >6 Crab flares have a hard spectrum. A simple 10-400 keV spectral analysis of the off-flare and flare periods shows that the variation in intensity is likely to be only due to variations of a cut-off power-law component. The optical flares seem to be at least of two different types: one occurring in simultaneity with the X-ray flares, the other showing a delay greater than 10 min. The former could be associated with X-ray reprocessing by either an accretion disk or the companion star. We suggest that the latter are associated with plasma ejections that have also been seen in radio.

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“…Xie, Yang & Ma 2014;Markoff et al 2015;Plotkin et al 2015Plotkin et al , 2016. Several X-ray binaries have confirmed radio detections in quiescence (Gallo, Fender & Hynes 2005;Gallo et al 2006Gallo et al , 2014Miller-Jones et al 2011Strader et al 2012;Chomiuk et al 2013;Dzib, Massi, & Jaron 2015;Tetarenko et al 2016) and they are all black hole candidate systems.…”

Section: Introductionmentioning

confidence: 99%

Polarized synchrotron emission in quiescent black hole X-ray transients

Russell¹,

Shahbaz²,

Lewis³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present near-infrared polarimetric observations of the black hole X-ray binaries Swift J1357.2-0933 and A0620-00. In both sources, recent studies have demonstrated the presence of variable infrared synchrotron emission in quiescence, most likely from weak compact jets. For Swift J1357.2-0933 we find that the synchrotron emission is polarized at a level of 8.0 ± 2.5 per cent (a 3.2 σ detection of intrinsic polarization). The mean magnitude and rms variability of the flux (fractional rms of 19-24 per cent in K S -band) agree with previous observations. These properties imply a continuously launched (stable on long timescales), highly variable (on short timescales) jet in the Swift J1357.2-0933 system in quiescence, which has a moderately tangled magnetic field close to the base of the jet. We find that for A0620-00, there are likely to be three components to the optical-infrared polarization; interstellar dust along the line of sight, scattering within the system, and an additional source that changes the polarization position angle in the reddest (H and K S ) wave-bands. We interpret this as a stronger contribution of synchrotron emission, and by subtracting the line-of-sight polarization, we measure an excess of ∼ 1.25±0.28 per cent polarization and a position angle of the magnetic field vector that is consistent with being parallel with the axis of the resolved radio jet. These results imply that weak jets in low luminosity accreting systems have magnetic fields which possess similarly tangled fields compared to the more luminous, hard state jets in X-ray binaries.

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Jet-dominated quiescent states in black hole X-ray binaries: the case of V404 Cyg

Cited by 21 publications

References 51 publications

The 2015 Decay of the Black Hole X-Ray Binary V404 Cygni: Robust Disk-Jet Coupling and a Sharp Transition Into Quiescence

The 2015 Decay of the Black Hole X-Ray Binary V404 Cygni: Robust Disk-Jet Coupling and a Sharp Transition Into Quiescence

Correlated optical, X-ray, andγ-ray flaring activity seen with INTEGRAL during the 2015 outburst of V404 Cygni

Polarized synchrotron emission in quiescent black hole X-ray transients

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