The<i>XMM–Newton</i>spectra of the 2012 outburst of the black hole candidate 4U 1630−47 revisited

Wang, Yanan; Méndez, Mariano

doi:10.1093/mnras/stv2814

Cited by 8 publications

(9 citation statements)

References 33 publications

(88 reference statements)

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“…Since this could be an underestimation, the lower limit to total N H is then estimated to be 6.1 × 10 22 cm −2 towards the line of sight of 4U 1630−47. The X-ray derived N H values are often much larger than 6 × 10 22 cm −2 (this work, T14, Wang & Méndez 2016). Therefore, the extinction determined from the radio maps when the source is behind MC −79 is consistent with extinction derived using X-ray spectral fitting.…”

Section: Extinction Towards 4u 1630−47supporting

confidence: 71%

“…tures observed simultaneously with radio originated from a local jet (Díaz Trigo et al 2013). We must note that models without presence of baryonic jets can explain the data as well (Wang & Méndez 2016), and an even a simpler explanation could be that the radio emission is unrelated to iron line features, because it is caused by the interaction of a previously launched jet with a thick ISM (Neilsen et al 2014).…”

Section: Introductionmentioning

confidence: 96%

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A Dust-scattering Halo of 4U 1630–47 Observed with Chandra and Swift: New Constraints on the Source Distance

Kalemci

Maccarone

Tomsick

2018

ApJ

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We have observed the Galactic black hole transient 4U 1630−47 during the decay of its 2016 outburst with Chandra and Swift to investigate the properties of the dust scattering halo created by the source. The scattering halo shows a structure that includes a bright ring between 80 ′′ and 240 ′′ surrounding the source, and a continuous distribution beyond 250 ′′ . An analysis of the 12 CO J = 1 − 0 map and spectrum in the line of sight to the source indicate that a molecular cloud with a radial velocity of -79 km s −1 (denoted MC −79) is the main scattering body that creates the bright ring. We found additional clouds in the line of sight, calculated their kinematic distances and resolved the well known "near" and "far" distance ambiguity for most of the clouds. At the favored far distance estimate of MC −79, the modeling of the surface brightness profile results in a distance to 4U 1630−47 of 11.5 ± 0.3 kpc. If MC −79 is at the near distance, then 4U 1630−47 is at 4.7 ± 0.3 kpc. Future Chandra, Swift, and sub-mm radio observations not only can resolve this ambiguity, but also would provide information regarding properties of dust and distribution of all molecular clouds along the line of sight. Using the results of this study we also discuss the nature of this source and the reasons for the anomalously low soft state observation observed during the 2010 decay.

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Section: Extinction Towards 4u 1630−47supporting

confidence: 71%

Section: Introductionmentioning

confidence: 96%

A Dust-scattering Halo of 4U 1630–47 Observed with Chandra and Swift: New Constraints on the Source Distance

Kalemci

Maccarone

Tomsick

2018

ApJ

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“…Alternatively, an absorption feature could be produced by the ISM. For instance, emission lines have been claimed in the past that could in fact be an artefact due to non-solar elemental abundance in the ISM (e.g., Wang & Méndez 2016), which triggered us to employ vphabs instead of phabs to explore the origin of the absorption line. Our analysis (see Section 3.2), however, shows that the width of this absorption feature is hardly influenced by variations of the iron abundance in the photoelectric absorption component.…”

Section: Absorption Features In Igr J17091mentioning

confidence: 99%

The reflection component in the average and heartbeat spectra of the black hole candidate IGR J17091-3642 during the 2016 outburst

Wang

Méndez

Altamirano

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present simultaneous NuSTAR and Swift observations of the black hole transient IGR J17091-3642 during its 2016 outburst. By jointly fitting six NuSTAR and four Swift spectra, we found that during this outburst the source evolves from the hard to the hard/soft intermediate and back to the hard state, similar to the 2011 outburst. Unlike in the previous outburst, in this case we observed both a broad emission and an moderately broad absorption line in our observations. Our fits favour an accretion disc with an inclination angle of ∼45 • with respect to the line of sight and a high iron abundance of 3.5 ± 0.3 in units of the solar abundance. We also observed heartbeat variability in one NuSTAR observation. We fitted the phase-resolved spectra of this observation and found that the reflected emission varies independently from the direct emission, whereas in the fits to the average spectra these two quantities are strongly correlated. Assuming that in IGR J17091-3642 the inner radius of the disc both in the average and the phase-resolved spectra is located at the radius of the innermost stable circular orbit, with 90% confidence the spin parameter of the black hole in this system is −0.13 ≤ a * ≤ 0.27.

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“…They found that the absorption features disappeared and an emission line appeared at very high luminosity, which implies a significant change in the degree of ionization of wind with increasing luminosity. Later, using a simpler model for the same XMM-Newton spectra, Wang & Méndez (2016) showed the presence of a variable element abundance and a strongly-ionized absorber near the black hole. Using Chandra/HETGS grating spectra of 4U 1630-47, Neilsen et al (2013Neilsen et al ( , 2014 found robust and strong absorption line caused by the outflowing wind launched during the outburst phase of 4U 1630-47.…”

Section: Introductionmentioning

confidence: 99%

AstroSat and Chandra View of the High Soft State of 4U 1630–47 (4U 1630–472): Evidence of the Disk Wind and a Rapidly Spinning Black Hole

Pahari

Bhattacharyya

Rao

et al. 2018

ApJ

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We present the X-ray spectral and timing analysis of the transient black hole X-ray binary 4U 1630-47, observed with the AstroSat, Chandra and MAXI space missions during its soft X-ray outburst in 2016. The outburst, from the rising phase until the peak, is neither detected in hard X-rays (15-50 keV) by the Swift/BAT nor in radio. Such non-detection along with the source behavior in the hardnessintensity and color-color diagrams obtained using MAXI data confirm that both Chandra and AstroSat observations were performed during the high soft spectral state. The High Energy Grating (HEG) spectrum from the Chandra high-energy transmission grating spectrometer (HETGS) shows two strong, moderately blueshifted absorption lines at 6.705 +0.002 −0.002 keV and 6.974 +0.004 −0.003 keV, which are produced by Fe XXV and Fe XXVI in a low-velocity ionized disk wind. The corresponding outflow velocity is determined to be 366±56 km/s. Separate spectral fits of Chandra/HEG, AstroSat/SXT+LAXPC and Chandra/HEG+AstroSat/SXT+LAXPC data show that the broadband continuum can be well described with a relativistic disk-blackbody model, with the disk flux fraction of ∼ 0.97. Based on the best-fit continuum spectral modeling of Chandra, AstroSat and Chandra+AstroSat joint spectra and using the Markov Chain Monte Carlo simulations, we constrain the spectral hardening factor at 1.56 +0.14 −0.06 and the dimensionless black hole spin parameter at 0.92 ± 0.04 within the 99.7% confidence interval. Our conclusion of a rapidly-spinning black hole in 4U 1630-47 using the continuum spectrum method is in agreement with a previous finding applying the reflection spectral fitting method.

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TheXMM–Newtonspectra of the 2012 outburst of the black hole candidate 4U 1630−47 revisited

Cited by 8 publications

References 33 publications

A Dust-scattering Halo of 4U 1630–47 Observed with Chandra and Swift: New Constraints on the Source Distance

A Dust-scattering Halo of 4U 1630–47 Observed with Chandra and Swift: New Constraints on the Source Distance

The reflection component in the average and heartbeat spectra of the black hole candidate IGR J17091-3642 during the 2016 outburst

AstroSat and Chandra View of the High Soft State of 4U 1630–47 (4U 1630–472): Evidence of the Disk Wind and a Rapidly Spinning Black Hole

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