Dynamical Confirmation of a Black Hole in MAXI J1820+070

Torres, M. A. P.; Casares, J.; Jiménez-Ibarra, F.; Muñoz-Darias, T.; Padilla, M. Armas; Jonker, P. G.; Heida, Marianne

doi:10.3847/2041-8213/ab39df

Cited by 108 publications

(122 citation statements)

References 46 publications

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“…Observations at various wavelengths soon suggested that the source is a BH LMXB (Baglio et al 2018;Bright et al 2018a;Del Santo & Segreto 2018;Uttley et al 2018). The black hole nature of the source was confirmed with a dynamical mass measurement by Torres et al (2019), who put the mass in the 7-8 M range. MAXI J1820+070 is a relatively nearby BH LMXB, with a distance of 2.96±0.33 kpc (Atri et al 2020), and it has low interstellar absorption (∼ 2 × 10 21 atoms cm −2 ; Kajava et al 2019).…”

Section: Introductionmentioning

confidence: 71%

A Rapid Change in X-Ray Variability and a Jet Ejection in the Black Hole Transient MAXI J1820+070

Homan

Bright

Motta

et al. 2020

ApJL

108

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We present Neutron Star Interior Composition Explorer X-ray and Arcminute Microkelvin Imager Large Array radio observations of a rapid hard-to-soft state transition in the black hole X-ray transient MAXI J1820+070. During the transition from the hard state to the soft state a switch between two particular types of quasiperiodic oscillations (QPOs) was seen in the X-ray power density spectra, from type-C to type-B, along with a drop in the strength of the broadband X-ray variability and a brief flare in the 7-12 keV band. Soon after this switch (∼1.5-2.5 hr) a strong radio flare was observed that corresponded to the launch of superluminal ejecta. Although hints of a connection between QPO transitions and radio flares have been seen in other black hole X-ray transients, our observations constitute the strongest observational evidence to date for a link between the appearance of type-B QPOs and the launch of discrete jet ejections. are usually recognized: the hard state, which shows strong rapid (subsecond) X-ray variability and a spectrum dominated by Comptonized power-law emission, and the soft state, in which rapid X-ray variability is weak and where a thermal disk blackbody component dominates the spectrum. The transitions between these two spectral states, during which sources are often classified as being in an intermediate state, are accompanied by strong evolution of the X-ray variability properties. As a source starts the transition from the hard state to the soft state, strong (type-C) low-frequency quasi-periodic oscillations (QPOs) are usually present in the power density spectra (see Wijnands et al. 1999;Remillard et al. 2002;Casella et al. 2005, for the various low-frequency QPO types). Their frequencies increase from ∼0.01 Hz to ∼10 Hz as the spectrum softens. At some point during the transition the type-C QPOs and arXiv:2003.01012v1 [astro-ph.HE]

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Section: Introductionmentioning

confidence: 71%

A Rapid Change in X-Ray Variability and a Jet Ejection in the Black Hole Transient MAXI J1820+070

Homan

Bright

Motta

et al. 2020

ApJL

108

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“…We began with the complete list of 60 likely BHXB transients presented in the BlackCAT catalogue (Corral-Santana et al 2016) as of 2019 October, and compiled their orbital periods (P orb ) and distances (d) where available. Updates to this sample included: the inclusion of a new dynamically confirmed BHXB MAXI J1820+070 at d ≈ 3 kpc (Gandhi et al 2019;Torres et al 2019;Atri et al 2019a); new likely lower limits of d 6 kpc and 5 kpc for Swift J1357.2-0933 and GX 339-4, respectively (Charles et al 2019;Heida et al 2017); and d 25 kpc for BW Cir as a likely upper limit (Gandhi et al 2019). It should be stressed that none of these updates substantially impact the sample results presented below.…”

Section: Sample Analysis and Resultsmentioning

confidence: 99%

A period-dependent spatial scatter of Galactic black hole transients

Gandhi

Rao

Charles

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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There remain significant uncertainties in the origin and evolution of black holes in binary systems, in particular regarding their birth sites and the influence of natal kicks. These are long-standing issues, but their debate has been reinvigorated in the era of gravitational wave detections and the improving precision of astrometric measurements. Using recent and archival characterization of Galactic black hole X-ray binaries (BHXBs), we report here an apparent anticorrelation between Porb (system orbital periods) and scatter in $z$ (elevation above the Galactic plane). The absence of long-period sources at high $z$ is not an obvious observational bias, and two possible explanatory scenarios are qualitatively explored: (1) a disc origin for BHXBs followed by natal kicks producing the scatter in $z$, with only the tightest binaries preferentially surviving strong kicks; and (2) a halo origin, with Porb shortening through dynamical interactions in globular clusters (GCs). For the latter case, we show a correspondence in $z$-scatter between BHXBs and the GCs with most compact core radii of <0.1 pc. However, the known absence of outbursting BHXB transients within Galactic GCs remains puzzling in this case, in contrast to the multitude of known GC neutron star XRBs. These results provide an interesting observational constraint for any black hole binary evolutionary model to satisfy.

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“…Mata Sánchez et al 2018). In this letter, we present eight epochs of high-quality near-infrared (NIR) spectroscopy supporting the presence of a cold accretion disc wind during both the hard and soft states of this dynamically confirmed (Torres et al 2019(Torres et al , 2020 BH transient.…”

Section: Introductionmentioning

confidence: 80%

Near-infrared emission lines trace the state-independent accretion disc wind of the black hole transient MAXI J1820+070

Sánchez-Sierras

Muñoz-Darias

2020

A&A

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The black hole transient MAXI J1820+070 displayed optical P Cyg profiles and other wind-related emission line features during the hard state of its discovery outburst. We present near-infrared (NIR) spectroscopy covering the different accretion states of the system during this event. Our eight-epoch data set (VLT/X-shooter) reveals strong variability in the properties of the NIR emission lines. This includes absorption troughs and extended emission line wings with kinetic properties that are remarkably similar to those inferred from the wind signatures observed in optical emission lines, indicating that they most likely trace the same accretion disc wind. Unlike the optical features, these NIR signatures are not exclusive of the hard state, as they are also witnessed across the soft state with similar observational properties. This supports the presence of a relatively steady outflow during the entire outburst of the system, and it represents the first detection of an accretion disc wind in a black hole soft state at energies other than X-rays. We discuss the visibility of the wind as a function of the spectral band and the potential of NIR spectroscopy for wind studies, in particular during luminous accretion phases.

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Dynamical Confirmation of a Black Hole in MAXI J1820+070

Cited by 108 publications

References 46 publications

A Rapid Change in X-Ray Variability and a Jet Ejection in the Black Hole Transient MAXI J1820+070

A Rapid Change in X-Ray Variability and a Jet Ejection in the Black Hole Transient MAXI J1820+070

A period-dependent spatial scatter of Galactic black hole transients

Near-infrared emission lines trace the state-independent accretion disc wind of the black hole transient MAXI J1820+070

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