Relativistic X-Ray Jets from the Black Hole X-Ray Binary MAXI J1820+070

Espinasse, Mathilde; Corbel, S.; Kaaret, Philip; Tremou, Evangelia; Migliori, G.; Plotkin, Richard M.; Bright, J. S.; Tomsick, John A.; Tzioumis, Anastasios; Fender, R. P.; Orosz, Jerome A.; Gallo, Elena; Homan, J.; Jonker, P. G.; Miller-Jones, J. C. A.; Russell, D. M.; Motta, S.

doi:10.3847/2041-8213/ab88b6

Cited by 45 publications

(89 citation statements)

References 36 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Unfortunately, there have been no published radio measurements of the synchrotron break to independently estimate the radius and distance of the jet ejecta, but this distance is reasonable, when compared to the BHB MAXI J1535-571 where the emission height above the black hole is ∼ 10 8 R g (Russell et al 2020). We also note that recent Chandra imaging showed a transient X-ray jet ejecta at the time of the radio flare, inferring that the ejecta was a cone of 1.5 × 10 4 au by 7.7 × 10 3 au (Espinasse et al 2020). As 1 au ∼ 10 7 R g for a 10 M e black hole, this would lead to a vertical extent of the transient jet emitting in X-ray of ∼10 11 R g , and the light travel distance of several days is always below this upper limit.…”

Section: Discussionsupporting

confidence: 57%

“…MAXI J1820+070 is one of the brightest BHBs detected so far, and has exhibited a great amount of activity in radio (Bright et al 2020;Homan et al 2020), NIR (Sánchez-Sierras & Muñoz-Darias 2020), optical (Muñoz-Darias et al 2019;Paice et al 2019;Shidatsu et al 2019;Veledina et al 2019), ultraviolet (UV; Kajava et al 2019), and X-ray (Buisson et al 2019;Kara et al 2019;Espinasse et al 2020;Wang et al 2020b;Buisson et al 2021;You et al 2021;Zdziarski et al 2021). In the hard state, reverberation analysis using the Neutron Star Interior Composition Interior Explorer (NICER; Gendreau et al 2016) showed that while the broad iron line profile remained constant (and only the narrow component decreased), the frequency range where the (soft) reverberation lag dominated increased (Kara et al 2019).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Disk, Corona, Jet Connection in the Intermediate State of MAXI J1820+070 Revealed by NICER Spectral-timing Analysis

Wang

Mastroserio

Kara

et al. 2021

ApJL

Self Cite

101

View full text Add to dashboard Cite

We analyze five epochs of Neutron star Interior Composition Explorer (NICER) data of the black hole X-ray binary MAXI J1820+070 during the bright hard-to-soft state transition in its 2018 outburst with both reflection spectroscopy and Fourier-resolved timing analysis. We confirm the previous discovery of reverberation lags in the hard state, and find that the frequency range where the (soft) reverberation lag dominates decreases with the reverberation lag amplitude increasing during the transition, suggesting an increasing X-ray emitting region, possibly due to an expanding corona. By jointly fitting the lag-energy spectra in a number of broad frequency ranges with the reverberation model reltrans, we find the increase in reverberation lag is best described by an increase in the X-ray coronal height. This result, along with the finding that the corona contracts in the hard state, suggests a close relationship between spatial extent of the X-ray corona and the radio jet. We find the corona expansion (as probed by reverberation) precedes a radio flare by ∼5 days, which may suggest that the hard-to-soft transition is marked by the corona expanding vertically and launching a jet knot that propagates along the jet stream at relativistic velocities.Unified Astronomy Thesaurus concepts: Low-mass x-ray binary stars (939); Stellar mass black holes (1611); High energy astrophysics (739); Black hole physics (159); X-ray transient sources (1852)

show abstract

Section: Discussionsupporting

confidence: 57%

Section: Introductionmentioning

confidence: 99%

Disk, Corona, Jet Connection in the Intermediate State of MAXI J1820+070 Revealed by NICER Spectral-timing Analysis

Wang

Mastroserio

Kara

et al. 2021

ApJL

Self Cite

101

View full text Add to dashboard Cite

show abstract

“…The motion of RK1 was monitored for ∼300 d and, after a first phase in which it travelled at a constant speed, it appeared to rebrighten while being strongly decelerated in the second phase of its motion. Decelerating discrete ejecta have been observed in a number of other sources, namely XTE J1550-564 ), H1743-322 (Corbel et al 2005, XTE J1752-223 (Yang et al 2010;Miller-Jones et al 2011), MAXI J1535-571 (Russell et al 2019a) and MAXI J1820+070 (Bright et al 2020;Espinasse et al 2020). For some of them, the discrete knots were detected both in radio and X-rays, with the Chandra observatory.…”

Section: Late Time Behaviour Of the Discrete Ejectamentioning

confidence: 96%

“…The ejected components can travel unseen for months to years, before they are detected again at large (∼pc) scales, with the emission coming from their interaction with the surrounding interstellar medium (ISM). Notably, discrete jets have been simultaneously detected at large scales in radio and X-rays for XTE J1550-564 Kaaret et al 2003;Tomsick et al 2003;Migliori et al 2017), H1743-322 (Corbel et al 2005) and MAXI J1820+070 (Espinasse et al 2020), with a broadband power-law spectrum suggesting the synchrotron nature of the emission coming from the shock region.…”

mentioning

confidence: 99%

The black hole transient MAXI J1348–630: evolution of the compact and transient jets during its 2019/2020 outburst

Carotenuto

Corbel

Tremou

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present the radio and X-ray monitoring campaign of the 2019/2020 outburst of MAXI J1348–630, a new black hole X-ray binary (XRB) discovered in 2019 January. We observed MAXI J1348–630 for ∼14 months in the radio band with MeerKAT and the Australia Telescope Compact Array (ATCA), and in the X-rays with MAXI and Swift/XRT. Throughout the outburst we detected and tracked the evolution of the compact and transient jets. Following the main outburst, the system underwent at least 4 hard-state-only re-flares, during which compact jets were again detected. For the major outburst, we observed the rise, quenching, and re-activation of the compact jets, as well as two single-sided discrete ejecta, launched ∼2 months apart and travelling away from the black hole. These ejecta displayed the highest proper motion (≳100 mas day−1) ever measured for an accreting black hole binary. From the jet motion, we constrain the ejecta inclination and speed to be ≤46○ and ≥0.69 c, and the opening angle and transverse expansion speed of the first component to be ≤6○ and ≤0.05 c. We also infer that the first ejection happened at the hard-to-soft state transition, before a strong radio flare, while the second ejection was launched during a short excursion from the soft to the intermediate state. After traveling with constant speed, the first component underwent a strong deceleration, which was covered with unprecedented detail and suggested that MAXI J1348–630 could be located inside a low-density cavity in the interstellar medium, as already proposed for XTE J1550–564 and H1743–322.

show abstract

“…The variability in MAXI J1820+070 analysed here occurs close to but distinct in time to several other features in the state change. There may be some association with the jet: around 1 day before the flaring variability, there is a jet ejection coincident with a type B QPO (Bright et al 2020;Espinasse et al 2020;Homan et al 2020). The flaring is too late to be directly associated with the ejection but could represent settling from the post-ejection state to an equilibrium.…”

Section: Discussionmentioning

confidence: 99%

MAXI J1820+070 with NuSTAR – II. Flaring during the hard to soft state transition with a long soft lag

Buisson

Fabian

Gandhi

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We continue the analysis of NuSTAR data from the recent discovery outburst of MAXI J1820+070 (optical counterpart ASASSN-18ey), focussing on an observation including unusual flaring behaviour during the hard to soft state transition, which is a short phase of outbursts and so comparatively rarely observed. Two plateaus in flux are separated by a variable interval lasting ∼10 ks, which shows dipping then flaring stages. The variability is strongest (with fractional variability up to $F_{\rm Var}\sim 10\%$) at high energies and reduces as the contribution from disc emission becomes stronger. Flux-resolved spectra show that the variability is primarily due to the power law flux changing. We also find a long soft lag of the thermal behind the power law emission, which is $20_{-1.2}^{+1.6}$ s during the flaring phase. The lag during the dipping stage has a different lag-energy spectrum, which may be due to a wave passing outwards through the disc. Time resolved spectral fitting suggests that the lag during the flaring stage may be due to the disc re-filling after being disrupted to produce the power law flare, perhaps related to the system settling after the jet ejection which occurred around 1 day before. The timescales of these phenomena imply a low viscosity parameter, α ∼ 10−3, for the inner region of the disc.

show abstract

Relativistic X-Ray Jets from the Black Hole X-Ray Binary MAXI J1820+070

Cited by 45 publications

References 36 publications

Disk, Corona, Jet Connection in the Intermediate State of MAXI J1820+070 Revealed by NICER Spectral-timing Analysis

Disk, Corona, Jet Connection in the Intermediate State of MAXI J1820+070 Revealed by NICER Spectral-timing Analysis

The black hole transient MAXI J1348–630: evolution of the compact and transient jets during its 2019/2020 outburst

MAXI J1820+070 with NuSTAR – II. Flaring during the hard to soft state transition with a long soft lag

Contact Info

Product

Resources

About