<i>SUZAKU</i>BROADBAND SPECTROSCOPY OF<i>SWIFT</i>J1753.5–0127 IN THE LOW-HARD STATE

Reynolds, M. T.; Miller, J. M.; Homan, J.; Miniutti, G.

doi:10.1088/0004-637x/709/1/358

Cited by 32 publications

(43 citation statements)

References 62 publications

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“…In Interactive Spectral Interpretation System (ISIS), the model corresponds to tbnew(1)*(diskbb(1)+nthcomp(1)). In addition, we fix the neutral hydrogen column density N H value to 0.194 × 10 22 cm −2 (Wilkinson & Uttley ) and the thermal‐Comptonization electron temperature kT e to 53 keV (Reynolds et al ). The seed photon temperature for Comptonization is tied to the disc blackbody inner disc temperature.…”

Section: Spectral‐timing Analysis and Resultsmentioning

confidence: 99%

Accretion flow diagnostics with X-ray spectral timing: the hard state of SWIFT J1753.5-0127

Cassatella

Uttley

Maccarone

2012

Monthly Notices of the Royal Astronomical Society

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Recent XMM-Newton studies of X-ray variability in the hard states of black hole X-ray binaries (BHXRBs) indicate that the variability is generated in the 'standard' optically thick accretion disc that is responsible for the multi-colour blackbody emission. The variability originates in the disc as mass-accretion fluctuations and propagates through the disc to 'light up' inner disc regions, eventually modulating the power-law emission that is produced relatively centrally. Both the covariance spectra and time-lags that cover the soft bands strongly support this scenario.Here, we present a comparative spectral-timing study of XMM-Newton data from the BHXRB SWIFT J1753.5−0127 in a bright 2009 hard state with that from the significantly fainter 2006 hard state to show for the first time the change in disc spectral-timing properties associated with a global increase in both the accretion rate and the relative contribution of the disc emission to the bolometric luminosity.We show that, although there is strong evidence for intrinsic disc variability in the more luminous hard state, the disc variability amplitude is suppressed relative to that of the power-law emission, which contrasts with the behaviour at lower luminosities where the disc variability is slightly enhanced when compared with the power-law variations. Furthermore, in the higher luminosity data the disc variability below 0.6 keV becomes incoherent with the power-law and higher energy disc emission at frequencies below 0.5 Hz, in contrast with the coherent variations seen in the 2006 data. We explain these differences and the associated complex lags in the 2009 data in terms of the fluctuating disc model, where the increase in accretion rate seen in 2009 leads to more pronounced and extended disc emission. If the variable signals are generated at small radii in the disc, the variability of disc emission can be naturally suppressed by the fraction of unmodulated disc emission arising from larger radii. Furthermore, the drop in coherence can be produced by disc accretion fluctuations arising at larger radii which are viscously damped and hence unable to propagate to the inner, power-law emitting region.

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Section: Spectral‐timing Analysis and Resultsmentioning

confidence: 99%

Accretion flow diagnostics with X-ray spectral timing: the hard state of SWIFT J1753.5-0127

Cassatella

Uttley

Maccarone

2012

Monthly Notices of the Royal Astronomical Society

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“…Although the presence of strongly truncated accretion disks in the hard state of microquasars is still a matter of debate, our results and those presented in T15 are consistent with previous multiwavelength studies of Swift J1753.5-0127 that all hint at large inner radii (see, e.g., Zhang et al 2010;Froning et al 2014). On the other hand, several authors claimed the detection of a cold accretion disk extending to the ISCO (Reis et al 2009;Reynolds et al 2010;Mostafa et al 2013), based solely on X-ray data, in particular the detection of iron emission lines. These seemingly contradictory results can be reconciled if we consider the presence of both a strongly truncated disk and a residual one created by condensation of the Comptonization component.…”

Section: Discussionmentioning

confidence: 99%

Optical and Near-Infrared Spectroscopy of the Black Hole Swift J1753.5–0127

Rahoui

Tomsick

Coriat

et al. 2015

ApJ

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We report on a multiwavelength observational campaign of the black hole (BH) X-ray binary Swift J1753.5-0127 that consists of an ESO/X-shooter spectrum supported by contemporaneous Swift/X-ray Telescope+Ultra-Violet/Optical Telescope (UVOT) and Australia Telescope Compact Array data. Interstellar mediumabsorption lines in the X-shooter spectrum allowus to determine-=  E B V 0.45 0.02 () along the line of sight to the source. We also report detection of emission signatures of He II l4686, Hα, and, for the first time, H I l10906 and Paβ. The double-peaked morphology of these four lines is typical of the chromosphere of a rotating accretion disk. Nonetheless, the paucity of disk features points toward a low level of irradiation in the system. This is confirmed through spectral energy distribution modeling, and we find that the UVOT+X-shooter continuum mostly stems from the thermal emission of a viscous disk. We speculate that the absence of reprocessing is due to the compactness of an illumination-induced envelope that fails to reflect enough incoming hard X-ray photons back to the outer regions. The disk also marginally contributes to the Compton-dominated X-ray emission and is strongly truncated, with an inner radius about 1000 times larger than the BHʼs gravitational radius. A near-infrared excess is present, and we associate it with synchrotron radiation from a compact jet. However, the measured X-ray flux is significantly higher than what can be explained by the optically thin synchrotron jet component. We discuss these findings in the framework of the radio-quiet versus X-ray-bright hypothesis, favoring the presence of a residual disk, predicted by evaporation models, that contributes to the X-ray emission without enhancing the radio flux.

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“…broad lines and smeared edges) are detected in X‐ray binaries indicating complicated ionization stages in, or motion of, the reflecting media (e.g. Miller 2007; Cackett et al 2008, 2009a,b; di Salvo et al 2009; Reis, Fabian & Young 2009; Reynolds et al 2010). The complicated modelling of these modified lines show a line centred mainly on 6.4 keV (errors in a range from 6.0 to 6.9 keV) with large broadening of the widths (equivalent widths in a range of 50–400 eV) including extended red‐wings due to general relativistic effects (i.e.…”

Section: Discussionmentioning

confidence: 99%

Frequency-resolved spectroscopy of XB 1323−619 using XMM-Newton data: detection of a reflection region in the disc

Balman¹

2010

Monthly Notices of the Royal Astronomical Society

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We present the frequency-resolved energy spectra (FRS) of the low-mass X-ray binary dipper XB 1323−619 during persistent emission in four different frequency bands using an archival XMM-Newton observation. FRS method helps to probe the inner zones of an accretion disc. XB 1323−619 is an Atoll source and a type-I burster. We find that the FRS is well described by a single blackbody component with kT in a range 1.0-1.4 keV responsible for the source variability in the frequency ranges of 0.002-0.04 and 0.07-0.3 Hz. We attribute this component to the accretion disc and possibly emission from an existing boundary layer supported by radiation pressure. The appearance of the blackbody component in the lower frequency ranges and disappearance towards the higher frequencies suggests that it may also be a disc-blackbody emission. We detect a different form of FRS for the higher frequency ranges of 0.9-6 and 8-30 Hz which is modelled best with a power law and a Gaussian emission line at 6.4 +0.2 −0.3 keV with an equivalent width of 1.6 +0.4 −1.2 and 1.3 +0.7 −0.9 keV for the two frequency ranges, respectively. This iron fluorescence line detected in the higher frequency ranges of spectra shows the existence of reflection in this system within the inner disc regions. The conventional spectrum of the source also shows a weak broad emission line around 6.6 keV. In addition, we find that the 0.9-6 Hz frequency band shows two quasi-periodic oscillation (QPO) peaks at 1.4 +1.0 −0.2 and 2.8 +0.2 −0.2 Hz at about 2.8σ -3.1σ confidence level. These are consistent with the previously detected ∼1 Hz QPO from this source. We believe they relate to the reflection phenomenon. The emission from the reflection region, being a variable spectral component in this system, originates from the inner regions of the disc with a maximum size of 4.7 × 10 9 cm and a minimum size of 1.6 × 10 8 cm calculated using light travel time considerations and our frequency-resolved spectra.

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

Cited by 32 publications

References 62 publications

Accretion flow diagnostics with X-ray spectral timing: the hard state of SWIFT J1753.5-0127

Accretion flow diagnostics with X-ray spectral timing: the hard state of SWIFT J1753.5-0127

Optical and Near-Infrared Spectroscopy of the Black Hole Swift J1753.5–0127

Frequency-resolved spectroscopy of XB 1323−619 using XMM-Newton data: detection of a reflection region in the disc

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