The ‘universal’ radio/X-ray flux correlation: the case study of the black hole GX 339−4

Corbel, S.; Coriat, M.; Brocksopp, C.; Tzioumis, A. K.; Fender, R. P.; Tomsick, John A.; Buxton, M.; Bailyn, Charles D.

doi:10.1093/mnras/sts215

Cited by 261 publications

(427 citation statements)

References 96 publications

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“…Adopting a Bayesian regression model (Kelly 2007), and assuming errors of 0.3 dex in both r and X, the best-fitting slopes are: β = 0.62 ± 0.04 for GX339-4 (consistent with the value 0.62 ± 0.01 reported by Corbel et al 2013); β = 0.52 ± 0.07 for V404 Cyg (consistent with the value 0.51 ± 0.06 reported by Corbel, Körding & Kaaret 2008), and β = 0.72 ± 0.09 for XTE J1118+480 (this work; largely based on 2005 data from Brocksopp et al 2010 andDunn et al 2010). Employing a variety of clustering analysis algorithms in order to establish whether a single or multiple cluster model better describes the full data set (24 systems) yields inconclusive results; while two clusters are readily identified by various algorithms, different algorithms identify somewhat different memberships.…”

Section: Summary and Discussionsupporting

confidence: 73%

“…All considered, 0.3 dex, or a factor ∼2 in luminosity seems to be a fair representation of the observed short-term radio and X-ray luminosity variability for hard and quiescent state black hole X-ray binaries (Garcia et al 2001;Gallo et al 2006;Gallo et al 2007;Hynes et al 2003aHynes et al , 2004Hynes et al , 2006Hynes et al , 2009Bradley et al 2007;Miller-Jones et al 2008;Bernardini & Cackett 2014; notice that σ 0.15 dex was adopted in previous works, e.g. Corbel et al 2013), and it also accounts for the uncertainties in the slope of the partially self-absorbed radio jet (often assumed as flat; please see § 5 for a quantitative discussion).…”

Section: Xte J1118+480 In the Radio/x-ray Domainmentioning

confidence: 86%

“…The net energy flux can be estimated using the exposure map to set the average photon energies in the source and background apertures; this gives a 0.5-7 keV absorbed flux of 1.44×10 −14 erg s −1 cm −2 , with 90 per cent confidence bounds between 1.22 and 1.66×10 −14 erg s −1 cm −2 . Assuming the standard value of 1.3×10 20 cm −2 for the Galactic hydrogen equivalent column towards XTE J1118+480 (McClintock et al 2001a;Reis, Miller & Fabian 2009), and a power law spectrum with photon index Γ = 2.1 (typical of quiescent black hole X-ray binaries; Plotkin, Gallo & Jonker 2013), this corresponds to an unabsorbed 1-10 keV (to allow for a proper comparison with Corbel et al 2013) flux of 1.2×10 −14 erg s −1 cm −2 , that is, a luminosity of 4.3×10 30 erg s −1 for a distance of 1.7 kpc.…”

Section: Chandra X-ray Telescopementioning

confidence: 99%

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The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

Gallo¹,

Miller-Jones²,

Russell³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We report on deep, coordinated radio and X-ray observations of the black hole X-ray binary XTE J1118+480 in quiescence. The source was observed with the Karl G. Jansky Very Large Array for a total of 17.5 hrs at 5.3 GHz, yielding a 4.8±1.4 µJy radio source at a position consistent with the binary system. At a distance of 1.7 kpc, this corresponds to an integrated radio luminosity between 4-8 ×10 25 erg s −1 , depending on the spectral index. This is the lowest radio luminosity measured for any accreting black hole to date. Simultaneous observations with the Chandra X-ray Telescope detected XTE J1118+480 at 1.2 × 10 −14 erg s −1 cm −2 (1-10 keV), corresponding to an Eddington ratio of ∼4 × 10 −9 for a 7.5 M black hole. Combining these new measurements with data from the 2005 and 2000 outbursts available in the literature, we find evidence for a relationship of the form r =α+β X (where denotes logarithmic luminosities), with β = 0.72 ± 0.09. XTE J1118+480 is thus the third system -together with GX339-4 and V404 Cyg -for which a tight, non-linear radio/X-ray correlation has been reported over more than 5 dex in X . Confirming previous results, we find no evidence for a dependence of the correlation normalisation of an individual system on orbital parameters, relativistic boosting, reported black hole spin and/or black hole mass. We then perform a clustering and linear regression analysis on what is arguably the most up-to-date collection of coordinated radio and X-ray luminosity measurements from quiescent and hard state black hole X-ray binaries, including 24 systems. At variance with previous results, a two-cluster description is statistically preferred only for random errors < ∼ 0.3 dex in both r and X , a level which we argue can be easily reached when the known spectral shape/distance uncertainties and intrinsic variability are accounted for. A linear regression analysis performed on the whole data set returns a best-fitting slope β = 0.61 ± 0.03 and intrinsic scatter σ 0 = 0.31 ± 0.03 dex.

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Section: Summary and Discussionsupporting

confidence: 73%

Section: Xte J1118+480 In the Radio/x-ray Domainmentioning

confidence: 86%

Section: Chandra X-ray Telescopementioning

confidence: 99%

See 1 more Smart Citation

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

Gallo¹,

Miller-Jones²,

Russell³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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154

200

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“…It shows relatively frequent outbursts (four in the last decade); all four X-ray states typically seen in X-ray binaries (XRBs) have been detected in this system, and X-ray observations of this system have been very important in shaping the theory of LMXBs (e.g., Miyamoto et al 1995;Homan & Belloni 2005;Plant et al 2014). The relation between X-ray and radio emission from XRBs also relies heavily on observations of GX 339−4 (e.g., Corbel et al 2013;Gallo et al 2014).…”

Section: Introductionmentioning

confidence: 99%

The Mass Function of GX 339–4 from Spectroscopic Observations of Its Donor Star^*

Heida

Jonker

Torres

et al. 2017

ApJ

113

108

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We obtained 16 VLT/X-shooter observations of GX 339−4 in quiescence during the period 2016 May-September and detected absorption lines from the donor star in its NIR spectrum. This allows us to measure the radial velocity curve and projected rotational velocity of the donor for the first time. We confirm the 1.76 day orbital period and we find that K 2 = 219±3 km s −1 , γ = 26±2 km s −1 , and v i sin = 64±8 km s −1 . From these values we compute a mass function f (M) = 1.91±0.08  M , a factor ∼3 lower than previously reported, and a mass ratio q = 0.18±0.05. We confirm the donor is a K-type star and estimate that it contributes~-4% 50% of the light in the J-and H-bands. We constrain the binary inclination to 37°< < i 78°and the black hole (BH) mass to. GX 339−4 may therefore be the first BH to fall in the "mass-gap" of 2-5 M e .

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“…The quasi-simultaneous radio and Xray fluxes in LH state of XRBs roughly follow a universal nonlinear correlation (FR ∝ F b X , b ∼ 0.5 − 0.7, Hannikainen et al 1998;Corbel et al 2003;Gallo et al 2003;Corbel et al 2013). Recently, more and more XRBs deviate from the universal correlations (e.g., Xue & Cui 2007;Cadolle Bel et al 2007;Soleri et al 2010;Jonker et al 2010;Coriat et al 2011;Ratti et al 2012) and form a different 'outliers' track with a much steeper radio-X-ray correlation (b ∼ 1.4 as initially found in H1743−322, Coriat et al 2011).…”

Section: Introductionmentioning

confidence: 90%

Revisit the Fundamental Plane of black hole activity from sub-Eddington to quiescent state

Dong¹,

Wu²

2015

Mon. Not. R. Astron. Soc.

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It is very controversial whether radio-X-ray correlation as defined in low-hard state of X-ray binaries (XRBs) can extend to quiescent state (e.g., X-ray luminosity less than a critical value of L X,c ∼ 10 −5.5 L Edd ) or not. In this work, we collect a sample of XRBs and low luminosity active galactic nuclei (LLAGNs) with wide distribution of Eddington ratios (L X /L Edd ∼ 10 −9 − 10 −3 ) to reexplore the fundamental plane between 5 GHz radio luminosity, L R , 2-10 keV X-ray luminosity, L X , and black hole (For the whole sample, we confirm the former fundamental plane of Merloni et al. and Falcke et al. that ξ X ∼ 0.6 and ξ M ∼ 0.8 even after including more quiescent BHs. The quiescent BHs follow the fundamental plane very well, and, however, FR I radio galaxies follow a steeper track comparing other BH sources. After excluding FR Is, we investigate the fundamental plane for BHs in quiescent state with L X < L X,c and sub-Eddington BHs with L X > L X,c respectively, and both subsamples have a similar slope, ξ X ∼ 0.6, which support that quiescent BHs may behave similar to those in low-hard state. We further select two subsamples of AGNs with BH mass in a narrow range (FR Is with M BH = 10 8.8±0.4 and other LLAGNs with M BH = 10 8.0±0.4 ) to simulate the behavior of a single supermassive BH evolving from sub-Eddington to quiescent state. We find that the highly sub-Eddington sources with L X /L Edd ∼ 10 −6 − 10 −9 still roughly stay on the extension of radio-X-ray correlation as defined by other sub-Eddington BHs. Our results are consistent with several recent observations in XRBs that the radio-X-ray correlation as defined in lowhard state can extend to highly sub-Eddington quiescent state.

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The ‘universal’ radio/X-ray flux correlation: the case study of the black hole GX 339−4

Cited by 261 publications

References 96 publications

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

The Mass Function of GX 339–4 from Spectroscopic Observations of Its Donor Star^*

Revisit the Fundamental Plane of black hole activity from sub-Eddington to quiescent state

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The ‘universal’ radio/X-ray flux correlation: the case study of the black hole GX 339−4

Cited by 261 publications

References 96 publications

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

The Mass Function of GX 339–4 from Spectroscopic Observations of Its Donor Star*

Revisit the Fundamental Plane of black hole activity from sub-Eddington to quiescent state

Contact Info

Product

Resources

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The Mass Function of GX 339–4 from Spectroscopic Observations of Its Donor Star^*