Observations of the Highly Variable X-Ray Source GX 339-4

Markert, T. H.; Canizares, C. R.; Clark, G. W.; Lewin, W. H. G.; Schnopper, H. W.; Sprott, G. F.

doi:10.1086/181290

Cited by 134 publications

(67 citation statements)

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“…These discoveries included the systems LMC X-1 [43][44][45][46], LMC X-3 [43,47], GX 339−4 [48,49], and 4U 1957+11 [43,50, the "U" standing for Uhuru, an early 70's X-ray satellite that scanned much of the sky]. The first two objects reside approximately 50 kpc away in the nearby satellite galaxy, the Large Magellanic Cloud.…”

Section: The Identification Of Galactic Black Hole Candidates (Gbhcs)mentioning

confidence: 99%

Fluorescent iron lines as a probe of astrophysical black hole systems

2003

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Section: The Identification Of Galactic Black Hole Candidates (Gbhcs)mentioning

confidence: 99%

Fluorescent iron lines as a probe of astrophysical black hole systems

2003

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“…GX 339−4 is a low-mass X-ray binary (LMXB) system that has been studied extensively since its discovery (e.g., Markert et al 1973;Miyamoto et al 1991;Méndez & van der Klis 1997;Gallo et al 2004;Plant et al 2015). 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).…”

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

116

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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“…It has been studied intensively since its discovery in 1973 (Markert et al 1973) and shows a high level of activity, with an average of one outburst of varying strength every 2 years. During the hard states it reaches fluxes in excess of 150 mCrab in the Swift/BAT 15-50 keV energy band.…”

Section: Introductionmentioning

confidence: 99%

THE COMPLEX ACCRETION GEOMETRY OF GX 339–4 AS SEEN BYNuSTARANDSWIFT

Fürst

Nowak

Tomsick

et al. 2015

ApJ

113

108

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We present spectral analyses of five Nuclear Spectroscopic Telescope Array and Swift observations of GX 339-4 taken during a failed outburst during the summer of 2013. These observations cover Eddington luminosity fractions in the range ≈0.9%-6%. Throughout this outburst GX 339-4 stayed in the hard state and all five observations show similar X-ray spectra, with a hard power law with a photon index near 1.6, and significant contribution from reflection. Using simple reflection models we find unrealistically high iron abundances. Allowing for different photon indices for the continuum incident on the reflector relative to the underlying observed continuum results in a statistically better fit and reduced iron abundances. With a photon index around 1.3, the input power law on the reflector is significantly harder than that which is directly observed. We study the influence of different emissivity profiles and geometries and consistently find an improvement when using separate photon indices. The inferred inner accretion disk radius is strongly model dependent, but we do not find evidence for a truncation radius larger than r 100 g in any model. The data do not allow independent spin constraints, but the results are consistent with the literature (i.e., a 0 > ). Our best-fit models indicate an inclination angle in the range 40°-60°, consistent with limits on the orbital inclination but higher than reported in the literature using standard reflection models. The iron line around 6.4 keV is clearly broadened, and we detect a superimposed narrow core as well. This core originates from a fluorescent region outside the influence of the strong gravity of the black hole. Additionally, we discuss possible geometries.

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Observations of the Highly Variable X-Ray Source GX 339-4

Cited by 134 publications

References 0 publications

Fluorescent iron lines as a probe of astrophysical black hole systems

Fluorescent iron lines as a probe of astrophysical black hole systems

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

THE COMPLEX ACCRETION GEOMETRY OF GX 339–4 AS SEEN BYNuSTARANDSWIFT

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Observations of the Highly Variable X-Ray Source GX 339-4

Cited by 134 publications

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Fluorescent iron lines as a probe of astrophysical black hole systems

Fluorescent iron lines as a probe of astrophysical black hole systems

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

THE COMPLEX ACCRETION GEOMETRY OF GX 339–4 AS SEEN BYNuSTARANDSWIFT

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