A broadband radio view of transient jet ejecta in the black hole candidate X-ray binary MAXI J1535–571

Chauhan, Jaiverdhan; Miller-Jones, J. C. A.; Anderson, G.; Paduano, Alessandro; Sokołowski, M.; Flynn, Chris; Hancock, P. J.; Hurley‐Walker, N.; Kaplan, David L.; Russell, Thomas; Bahramian, A.; Duchesne, S. W.; Altamirano, D.; Croft, Steve; Krimm, H. A.; Sivakoff, Gregory R.; Soria, Roberto; Trott, Cathryn M.; Wayth, R. B.; Gupta, Vivek; Johnston‐Hollitt, M.; Tingay, S. J.

doi:10.1017/pasa.2021.38

Cited by 8 publications

(6 citation statements)

References 71 publications

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“…Based on our results and the radio measurements of Russell et al (2019) and Chauhan et al (2021), in Figure 6, we present schematically a possible scenario of the evolution of the X-ray corona and the simultaneous radio jet. The parameters from the reflection suggest a rather stable inner radius of the disc that is very close to the ISCO, so the disc inner radius does not change significantly in Figure 6.…”

Section: Discussionmentioning

confidence: 74%

“…Our results of the temporal evolution of the corona may be compared to the evolution of the radio jet detected in this source. Radio measurements (Russell et al 2019(Russell et al , 2020Chauhan et al 2021) show that during the intermediate state of MAXI J1535−571 a steady, optically thick jet gradually quenches and then changes into a transient jet. More specifically, on MJD 58008, the radio observations detect a steady, optically thick jet.…”

Section: Discussionmentioning

confidence: 99%

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The evolution of the corona in MAXI J1535-571 through type-C quasi-periodic oscillations with Insight-HXMT

Zhang,

Méndez,

García

et al. 2022

Preprint

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Type-C quasi-periodic oscillations (QPOs) in black hole X-ray transients can appear when the source is in the low-hard and hard-intermediate states. The spectral-timing evolution of the type-C QPO in MAXI J1535−571 has been recently studied with Insight-HXMT. Here we fit simultaneously the time-averaged energy spectrum, using a relativistic reflection model, and the fractional rms and phase-lag spectra of the type-C QPOs, using a recently developed time-dependent Comptonization model when the source was in the intermediate state. We show, for the first time, that the time-dependent Comptonization model can successfully explain the X-ray data up to 100 keV. We find that in the hard-intermediate state the frequency of the type-C QPO decreases from 2.6 Hz to 2.1 Hz, then increases to 3.3 Hz, and finally increases to ∼ 9 Hz. Simultaneously with this, the evolution of corona size and the feedback fraction (the fraction of photons up-scattered in the corona that return to the disc) indicates the change of the morphology of the corona. Comparing with contemporaneous radio observations, this evolution suggests a possible connection between the corona and the jet when the system is in the hard-intermediate state and about to transit into the soft-intermediate state.

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Section: Discussionmentioning

confidence: 74%

Section: Discussionmentioning

confidence: 99%

The evolution of the corona in MAXI J1535-571 through type-C quasi-periodic oscillations with Insight-HXMT

Zhang,

Méndez,

García

et al. 2022

Preprint

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“…Jet opening angles have only been constrained for a number of black hole X-ray binaries (see e.g. Stirling et al 2001;Miller-Jones et al 2006;Rushton et al 2017;Tetarenko et al 2017;Tetarenko et al 2019b;Espinasse et al 2020;Chauhan et al 2021;Tetarenko et al 2021). Measurements of jet opening angles range from 0.4−1.8°in the compact jet of Cygnus X-1 (Tetarenko et al 2019b) to ∼ 58°i n XTE J1908+094 (Rushton et al 2017), although we note that Rushton et al (2017) suggested that this number is derived from the lateral expansion of the jet lobe and thus the jet opening angle is likely smaller.…”

Section: Jet Kinematicsmentioning

confidence: 90%

Time-dependent visibility modelling of a relativistic jet in the X-ray binary MAXI J1803-298

Wood¹,

Miller-Jones²,

Bahramian³

et al. 2023

Preprint

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Tracking the motions of transient jets launched by low-mass X-ray binaries (LMXBs) is critical for determining the moment of jet ejection, and identifying any corresponding signatures in the accretion flow. However, these jets are often highly variable and can travel across the resolution element of an image within a single observation, violating a fundamental assumption of aperture synthesis. We present a novel approach in which we directly fit a single time-dependent model to the full set of interferometer visibilities, where we explicitly parameterise the motion and flux density variability of the emission components, to minimise the number of free parameters in the fit, while leveraging information from the full observation. This technique allows us to detect and characterize faint, fast-moving sources, for which the standard time binning technique is inadequate. We validate our technique with synthetic observations, before applying it to three Very Long Baseline Array (VLBA) observations of the black hole candidate LMXB MAXI J1803−298 during its 2021 outburst. We measured the proper motion of a discrete jet component to be 1.37 ± 0.14 mas hr −1 , and thus we infer an ejection date of MJD 59348.08 +0.05 −0.06 , which occurs just after the peak of a radio flare observed by the Australia Telescope Compact Array (ATCA) and the Atacama Large Millimeter/Sub-Millimeter Array (ALMA), while MAXI J1803−298 was in the intermediate state. Further development of these new VLBI analysis techniques will lead to more precise measurements of jet ejection dates, which, combined with dense, simultaneous multi-wavelength monitoring, will allow for clearer identification of jet ejection signatures in the accretion flow.

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“…Results from radio have mainly explored the transient behavior of the jet and/or the relationship between the jet and accretion disk (Parikh et al 2019;Russell et al 2019Russell et al , 2020Chauhan et al 2021). Chauhan et al (2019) used radio observations to determine the distance to the source (∼4 kpc).…”

Section: Introductionmentioning

confidence: 99%

MAXI J1535–571 2017 Outburst Seen by INTEGRAL/SPI and Investigating the Origin of Its Hard Tail

Rodi

Jourdain

Roques

2022

ApJ

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On 2017 September 2 MAXI J1535–571 went into outburst and peaked at ∼5 Crab in the 2–20 keV energy range. Early in the flare, the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) performed target of opportunity pointings and monitored the source as it transitioned from the hard state to the soft state. Using quasi-simultaneous observations from MAXI/GSC and INTEGRAL/SPI, we studied the temporal and spectral evolution of MAXI J1535–571 in the 2–500 keV range. Early spectra show a Comptonized spectrum and a high-energy component dominant above ∼150 keV. CompTT fits to the SPectrometer on INTEGRAL (SPI) data found electron temperatures (kT e ) evolve from ∼31 keV to 18 keV with a tied optical depth (τ ∼ 0.85) or τ evolving from ∼1.2–0.65 with a tied kT e (∼24 keV). To investigate the nature of the high-energy component, we performed a spectral decomposition of the 100–400 keV energy band. The CompTT flux varies significantly during the hard state while the high-energy component flux is consistent with a constant flux. This result suggests that the two components originate from different locations, which favors a jet origin interpretation for the high-energy component over a hybrid corona interpretation. Lastly, two short rebrightenings during the hard-to-soft transition are compared to similar events reported in MAXI J1820+070.

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A broadband radio view of transient jet ejecta in the black hole candidate X-ray binary MAXI J1535–571

Cited by 8 publications

References 71 publications

The evolution of the corona in MAXI J1535-571 through type-C quasi-periodic oscillations with Insight-HXMT

The evolution of the corona in MAXI J1535-571 through type-C quasi-periodic oscillations with Insight-HXMT

Time-dependent visibility modelling of a relativistic jet in the X-ray binary MAXI J1803-298

MAXI J1535–571 2017 Outburst Seen by INTEGRAL/SPI and Investigating the Origin of Its Hard Tail

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