<i>Chandra</i>
                    Detection of XTE J1650-500 in Quiescence and the Minimum Luminosity of Black Hole X-Ray Binaries

Gallo, Elena; Homan, J.; Jonker, P. G.; Tomsick, John A.

doi:10.1086/591230

Cited by 18 publications

(20 citation statements)

References 41 publications

(64 reference statements)

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“…In the case that we measured the quiescent X‐ray flux level, this indicates that the decay of the outburst phase towards quiescence had an ‘inside–out’ development, starting with the fading of the X‐ray source only later followed by the optical. Moreover, assuming we measured the quiescent X‐ray flux, the quiescent luminosity for our estimate range of distances implies an orbital period longwards of 10 h, if XTE J1752−223 follows the trend between orbital period and quiescent X‐ray luminosity reported by Garcia et al (2001) and Gallo et al (2008). Instead, if the true quiescent luminosity is lower than measured, then the inferred orbital period would be shorter and more compatible with the orbital period inferred above.…”

Section: Discussionsupporting

confidence: 53%

The black hole candidate XTE J1752−223 towards and in quiescence: optical and simultaneous X-ray-radio observations

Ratti¹,

Jonker²,

Miller-Jones³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present optical, X‐ray and radio observations of the black hole transient (BHT) XTE J1752−223 towards and in quiescence. Optical photometry shows that the quiescent magnitude of XTE J1752−223 is fainter than 24.4 mag in the i′ band. A comparison with measurements of the source during its 2009–2010 outburst shows that the outburst amplitude is more than 8 mag in the i′ band. Known X‐ray properties of the source combined with the faintness of the quiescence optical counterpart and the large outburst optical amplitude point towards a short orbital‐period system (Porb≲ 6.8 h) with an M type (or later) mass donor, at a distance of 3.5 ≲d≲ 8 kpc. Simultaneous X‐ray and radio data were collected with Chandra and the Expanded Very Large Array (EVLA), allowing constraints to be placed on the quiescent X‐ray and radio flux of XTE J1752−223. Furthermore, using data covering the final stage of the outburst decay, we investigated the low‐luminosity end of the X‐ray–radio correlation for this source and compared it with other BHTs. We found that XTE J1752−223 adds to the number of outliers with respect to the ‘standard’ X‐ray–radio luminosity relation. Furthermore, XTE J1752−223 is the second source, after the BHT H1743−322, that shows a transition from the region of the outliers towards the ‘standard’ correlation at low luminosity. Finally, we report on a faint, variable X‐ray source we discovered with Chandra at an angular distance of ∼2.9 arcsec to XTE J1752−223 and at a position angle consistent with that of the radio jets previously observed from the BHT. We discuss the possibility that we detected X‐ray emission associated with a jet from XTE J1752−223.

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Section: Discussionsupporting

confidence: 53%

The black hole candidate XTE J1752−223 towards and in quiescence: optical and simultaneous X-ray-radio observations

Ratti¹,

Jonker²,

Miller-Jones³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…In the soft state (which has luminosities similar to those of the hard state) the source appears to be NIR and optically dim relative to the distribution of other soft state LMXBs (Russell et al), but not significantly so. Furthermore, as noted by Gallo et al (2008), the late-time quiescent X-ray luminosity (L X ≈ 3 × 10 30 erg s −1 ) is at the lower end of the distribution of quiescent luminosities for black hole binaries, though, when compared with the quiescent optical luminosity (L Optical ≈ 10 30 erg s −1 ), the X-ray luminosity falls on the correlation of Russell et al, albeit at the low end. Obviously, because of NIR/optical observational bias (i.e., we only observe the brightest sources), caution has to be exercised when implying that a source is of a low luminosity compared to a distribution as we do here for the soft and quiescent states.…”

Section: The Weak Jet Of Xte J1650−500mentioning

confidence: 64%

Disentangling the NIR/optical emission of the black hole XTE J1650−500 during outburst

Curran

Chaty

Heras

2012

A&A

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Context. While the sources of X-ray and radio emission in the different states of low-mass X-ray binaries are relatively well understood, the origin of the near-infrared (NIR) and optical emission is more often debated. It is likely that the NIR/optical flux originates from an amalgam of different emission regions, because it occurs at the intersecting wavelengths of multiple processes. Aims. We aim to identify the NIR/optical emission region(s) of one such low-mass X-ray binary and black hole candidate, XTE J1650−500, via photometric, timing, and spectral analyses. Methods. We present unique NIR/optical images and spectra, obtained with the ESO-New Technology Telescope, during the peak of the 2001 outburst of XTE J1650−500. Results. The data suggest that the NIR/optical flux is due to a combination of emission mechanisms including a significant contribution from X-ray reprocessing and, at early times in the hard state, a relativistic jet that is NIR/radio dim compared to similar sources. Conclusions. The jet of XTE J1650−500 is relatively weak compared to that of other black hole low-mass X-ray binaries, possibly because we observe as it is being "turned off" or quenched at the state transition. While there are several outliers to the radio-X-ray correlation of the hard state of low-mass X-ray binaries, XTE J1650−500 is the first example of an outlier to the NIR/optical-X-ray correlation.

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“…The luminosity of MAXI J1659-152 is plotted with a crossed black circle. Based on data presented in Gallo et al (2008), Rea et al (2011), Reynolds & Miller (2011), Homan et al (2013), Yang et al (2013) and Casares & Jonker (2013). (A color version of this figure is available in the online journal.…”

Section: Discussionmentioning

confidence: 99%

Swift J1357.2−0933: the faintest black hole?

Padilla¹,

Wijnands

Degenaar³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Swift J1357.2-0933 is a confirmed very faint black hole X-ray transient and has a short estimated orbital period of 2.8 hr. We observed Swift J1357.2-0933 for ∼50 ks with XMM-Newton in 2013 July during its quiescent state. The source is clearly detected at a 0.5-10 keV unabsorbed flux of ∼ 3 × 10 −15 erg cm −2 s −1 . If the source is located at a distance of 1.5 kpc (as suggested in the literature), this would imply a luminosity of ∼ 8 × 10 29 erg s −1 , making it the faintest detected quiescent black hole LMXB. This would also imply that there is no indication of a reversal in the quiescence Xray luminosity versus orbital period diagram down to 2.8 hr, as has been predicted theoretically and recently supported by the detection of the 2.4 hr orbital period black hole MAXI J1659-152 at a 0.5-10 keV X-ray luminosity of ∼ 1.2 × 10 31 erg s −1 . However, there is considerable uncertainty in the distance of Swift J1357.2-0933 and it may be as distant as 6.3 kpc. In this case, its quiescent luminosity would be L X ∼ 1.3 × 10 31 erg s −1 , i.e., similar to MAXI J1659-152 and hence it would support the existence of such a bifurcation period. We also detected the source in optical at r ′ ∼22.3 mag with the Liverpool telescope, simultaneously to our X-ray observation. The Xray/optical luminosity ratio of Swift J1357.2-0933 agrees with the expected value for a black hole at this range of quiescent X-ray luminosities.

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Chandra Detection of XTE J1650-500 in Quiescence and the Minimum Luminosity of Black Hole X-Ray Binaries

Cited by 18 publications

References 41 publications

The black hole candidate XTE J1752−223 towards and in quiescence: optical and simultaneous X-ray-radio observations

The black hole candidate XTE J1752−223 towards and in quiescence: optical and simultaneous X-ray-radio observations

Disentangling the NIR/optical emission of the black hole XTE J1650−500 during outburst

Swift J1357.2−0933: the faintest black hole?

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