Swift J1753.5−0127: The Black Hole Candidate with the Shortest Orbital Period

Zurita, C.; Durant, Martin; Torres, M. A. P.; Shahbaz, T.; Casares, J.; Steeghs, D.

doi:10.1086/588721

Cited by 97 publications

(183 citation statements)

References 31 publications

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“…In addition, we include V-band optical and J, H, and K-band NIR data points obtained in April and July 2009 at the Magellan and MDM observatories. The V-band magnitude was found to be consistent with the previous measurements of Zurita et al (2008), as such the NIR data should be representative of the infrared portion of the SED at the time of our Suzaku observations. The radio data points represent the radio detection shortly after the 2005 outburst and likely represent upper limits to the radio flux at the time of our observations (Cadolle Bel et al 2007); these are also consistent with the non-detection at 5 GHz and 8 GHz by Soleri et al (2008).…”

Section: Jet And/or Coronasupporting

confidence: 89%

“…In Figure 7, we plot the absorption corrected spectral energy distribution (SED) for Swift J1753.5−0127. The optical data are from Zurita et al (2008) and were taken during at approximately the same time as our Suzaku spectra. In addition, we include V-band optical and J, H, and K-band NIR data points obtained in April and July 2009 at the Magellan and MDM observatories.…”

Section: Jet And/or Coronamentioning

confidence: 99%

“…Radio observations with the MERLIN array also detected a variable counterpart . Observations at optical wavelengths by Zurita et al (2008) have also detected a significant modulation with a period of 3.2 hr, which they identify as a superhump period slightly larger than the actual orbital period. This would make Swift J1753.5−0127 the black hole binary with the shortest known orbital period.…”

Section: Introductionmentioning

confidence: 96%

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SUZAKUBROADBAND SPECTROSCOPY OFSWIFTJ1753.5–0127 IN THE LOW-HARD STATE

Reynolds

Miller

Homan

et al. 2009

ApJ

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We present Suzaku observations of the Galactic black hole candidate Swift J1753.5−0127 in the low-hard state (LHS). The broadband coverage of Suzaku enables us to detect the source over the energy range 0.6-250 keV. The broadband spectrum (2-250 keV) is found to be consistent with a simple power-law (Γ ∼ 1.63). In agreement with previous observations of this system, a significant excess of soft X-ray flux is detected consistent with the presence of a cool accretion disk. Estimates of the disk inner radius infer a value consistent with the innermost stable circular orbit (ISCO; R in 6R g , for certain values of, e.g., N H , i), although we cannot conclusively rule out the presence of an accretion disk truncated at larger radii (R in ∼ 10-50R g ). A weak, relativistically broadened iron line is also detected, in addition to disk reflection at higher energy. However, the iron-K line profile favors an inner radius larger than the ISCO (R in ∼ 10-20R g ). The implications of these observations for models of the accretion flow in the LHS are discussed.

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Section: Jet And/or Coronasupporting

confidence: 89%

Section: Jet And/or Coronamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

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SUZAKUBROADBAND SPECTROSCOPY OFSWIFTJ1753.5–0127 IN THE LOW-HARD STATE

Reynolds

Miller

Homan

et al. 2009

ApJ

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“…The dearth of cross-correlations is in part due to the logistics of arranging simultaneous observations with the few instruments capable, within the short window following an outburst. In this respect, SWIFT J1753.5Ϫ0127 has been unique, by persisting in its low/hard state (relatively bright) for years after outburst (Zurita et al 2008). We may find that similar relationships exist in other systems, which have gone undetected for technical reasons.…”

Section: Cross-correlationmentioning

confidence: 99%

“…Further details of our observational campaign, including spectroscopy, longer term multiband optical photometry, and detailed periodogram analysis, are to be published separately in Durant et al (2008), and an analysis is presented in Zurita et al (2008) of the long-term R-band variability and orbit-like modulation. Here we intend to make the minimum number of processing steps and assumptions to obtain the X-ray/optical cross-correlation functions (CCFs), which are a unique phenomenological hint of black hole accretion physics.…”

Section: Introductionmentioning

confidence: 99%

SWIFT J1753.5-0127: A Surprising Optical/X-Ray Cross-Correlation Function

Durant

Gandhi

Shahbaz

et al. 2008

ApJ

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We have conducted simultaneous optical and X-ray observations of SWIFT J1753.5Ϫ0127 with RXTE and ULTRACAM, while the system persisted in its relatively bright low/hard state. In the cross-correlation function, we find that the optical emission, with a broad negative peak, leads the X-ray emission by a few seconds and has a smaller positive peak at positive lags. This is markedly different from what was seen for the similarly interesting system XTE J1118ϩ480, and it is the first time that such a correlation function has been so clearly measured. We suggest a physical scenario for its origin.

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The radio/X‐ray correlation in Swift J1753.5–0127

et al. 2016

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Great effort has gone into trying to explain the two observed radio/X-ray correlation tracks seen in the low/hard state of black hole X-ray binaries in recent years. The original, "standard" correlation of the form L R ∝ L b X , where b = 0.7 ± 0.1, is paired with a separate, lower correlation track with a steeper slope of ∼ 1-1.4, at least at high luminosities. These outlier sources seem to show fainter radio emission than expected for a given X-ray luminosity, thus acquiring the term "radio-quiet". While most sources seem to maintain their intrinsic correlation slopes over decades in luminosity, a growing sample of sources have recently been reported to move from one correlation to the other. We present preliminary results from a coordinated radio/X-ray monitoring campaign of the radio-quiet black hole binary Swift J1753.5−0127, spanning nearly two years in time. Our observations add lower-luminosity coverage to an existing sample of observations, and we observe the radio-quiet track to proceed horizontally towards the standard correlation as the X-ray luminosity slowly starts to decrease. The source stays on the transition track for ∼ 60 days, during which its X-ray luminosity is observed to drop by more than an order of magnitude while its radio luminosity stays constant. Time-averaged X-ray energy spectra show very little change during this phase, leaving no obvious parameters to explain the observed transition behaviour.

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Swift J1753.5−0127: The Black Hole Candidate with the Shortest Orbital Period

Cited by 97 publications

References 31 publications

SUZAKUBROADBAND SPECTROSCOPY OFSWIFTJ1753.5–0127 IN THE LOW-HARD STATE

SUZAKUBROADBAND SPECTROSCOPY OFSWIFTJ1753.5–0127 IN THE LOW-HARD STATE

SWIFT J1753.5-0127: A Surprising Optical/X-Ray Cross-Correlation Function

The radio/X‐ray correlation in Swift J1753.5–0127

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