Reflection Spectroscopy of the Black Hole Binary XTE J1752−223 in Its Long-stable Hard State

García, Javier A.; Steiner, James F.; Grinberg, V.; Dauser, Robert C.; Connors, Riley; McClintock, Jeffrey E.; Remillard, Ron; Wilms, J.; Harrison, Fiona A.; Tomsick, John A.

doi:10.3847/1538-4357/aad231

Cited by 56 publications

(40 citation statements)

References 52 publications

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“…The overabundance of Fe has been detected in various Xray binaries (e.g. Degenaar et al 2017;García et al 2018;Tomsick et al 2018). According to Reynolds et al (2012), ra- Figure 5.…”

Section: Discussionmentioning

confidence: 98%

Broad-band spectral study of X-ray transient MAXI J1820+070 using Swift/XRT and NuSTAR

Bharali

Chauhan

Boruah

2019

Monthly Notices of the Royal Astronomical Society

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We report on a NuSTAR and Swift /XRT observation of the newly discovered X-ray transient MAXI J1820+070. Swift /XRT and NuSTAR have concurrently observed the newly detected source on 14 March 2018. We have simultaneously fitted the broadband spectra obtained from Swift /XRT and NuSTAR. The observed joint spectra in the energy range 0.6-78.0 keV are well modeled with a weak disk black-body emission, dominant thermal Comptonization and relativistic reflection fraction. We have detected a fluorescent Iron-Kα line relativistically broadened, and a Compton hump at ∼ 30 keV. We constrain the inner disk radius as well as the disk inclination angle and their values are found to be 4.1 +0.8 −0.6 R ISCO (where R ISCO ≡ radius of the innermost stable circular orbit) or 5.1 +1.0 −0.7 r g (where r g ≡ gravitational radius) and 29.8 +3.0 −2.7 • respectively. The best fit broad-band spectra suggest that the source was in the hard state and evolving. The source emission is best described by weak thermal emission along with strong thermal Comptonization from a relatively cold, optically thick, geometrically thin and ionized accretion disk. X-ray spectral modeling helps us to understand the accretion and ejection properties in the vicinity of the compact object.

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“…The overabundance of Fe has been detected in various Xray binaries (e.g. Degenaar et al 2017;García et al 2018;Tomsick et al 2018). According to Reynolds et al (2012), ra- Figure 5.…”

Section: Discussionmentioning

confidence: 98%

Broad-band spectral study of X-ray transient MAXI J1820+070 using Swift/XRT and NuSTAR

Bharali

Chauhan

Boruah

2019

Monthly Notices of the Royal Astronomical Society

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“…Extensive efforts to measure the spins of BHs in BHXBs have been made in the past decade. The best available methods (García et al 2018;McClintock et al 2014) often assume that the spin of the BH is aligned with the orbital plane of the binary. Our finding that strong natal kicks are imparted to ∼85% of BHXBs suggests that caution may be warranted in assuming the binary orbital inclination when fitting for BH spin.…”

Section: Implications For Bh-bh Systemsmentioning

confidence: 99%

Potential kick velocity distribution of black hole X-ray binaries and implications for natal kicks

Atri

Miller-Jones

Bahramian

et al. 2019

Monthly Notices of the Royal Astronomical Society

120

102

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We use Very Long Baseline Interferometry to measure the proper motions of three black hole X-ray binaries (BHXBs). Using these results together with data from the literature and Gaia-DR2 to collate the best available constraints on proper motion, parallax, distance and systemic radial velocity of 16 BHXBs, we determined their three dimensional Galactocentric orbits. We extended this analysis to estimate the probability distribution for the potential kick velocity (PKV) a BHXB system could have received on formation. Constraining the kicks imparted to BHXBs provides insight into the birth mechanism of black holes (BHs). Kicks also have a significant effect on BH-BH merger rates, merger sites, and binary evolution, and can be responsible for spin-orbit misalignment in BH binary systems. 75% of our systems have potential kicks > 70 km s −1 . This suggests that strong kicks and hence spin-orbit misalignment might be common among BHXBs, in agreement with the observed quasi-periodic X-ray variability in their power density spectra. We used a Bayesian hierarchical methodology to analyse the PKV distribution of the BHXB population, and suggest that a unimodal Gaussian model with a mean of 107±16 km s −1 is a statistically favourable fit. Such relatively high PKVs would also reduce the number of BHs likely to be retained in globular clusters. We found no significant correlation between the BH mass and PKV, suggesting a lack of correlation between BH mass and the BH birth mechanism. Our Python code allows the estimation of the PKV for any system with sufficient observational constraints.

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“…The spin is one of the two key parameters to make a full description of a black hole. So far, we have measured dozens of stellar-mass black hole spins via X-ray reflection fitting method (Wang et al 2017;Brenneman & Reynolds 2006;Walton et al 2013Walton et al , 2019Lohfink et al 2012;Brenneman et al 2011;Tripathi et al 2019;Walton et al 2016;Tomsick et al 2018;Miller et al 2013;García et al 2018b;Xu et al 2018;García et al 2015).The geometry of the corona, which is still unclear, will effect the profile of the reflection spectrum. Particularly, it has a significant impact on the emissivity profile of the reflection spectrum.…”

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confidence: 99%

A detailed study on the reflection component for the black hole candidate MAXI J1836−194

Dong

García

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a detailed spectral analysis of the black hole candidate MAXI J1836-194. The source was caught in the intermediate state during its 2011 outburst by Suzaku and RXTE. We jointly fit the X-ray data from these two missions using the relxill model to study the reflection component, and a steep inner emissivity profile indicating a compact corona as the primary source is required in order to achieve a good fit. In addition, a reflection model with a lamp-post configuration (relxilllp), which is normally invoked to explain the steep emissivity profile, gives a worse fit and is excluded at 99% confidence level compared to relxill. We also explore the effect of the ionization gradient on the emissivity profile by fitting the data with two relativistic reflection components, and it is found that the inner emissivity flattens. These results may indicate that the ionization state of the disc is not constant. All the models above require a supersolar iron abundance higher than ∼ 4.5. However, we find that the high-density version of reflionx can describe the same spectra even with solar iron abundance well. A moderate rotating black hole (a * = 0.84-0.94) is consistently obtained by our models, which is in agreement with previously reported values.2 Yanting Dong et al. INTRODUCTIONGalactic X-ray binaries are believed to be powered by accretion onto stellar-mass black holes or neutron stars. The gases in accretion disc emit thermal radiation in UV/X-ray band (Shakura & Sunyaev 1973). Some fraction of the thermal photons from the disc are then inverse Compton scattered by energetic electrons in the hypothetically hot corona, producing a hard X-ray spectrum in the form of power-law, i.e. N(E) ∝ E −Γ . A fraction of the high-energy photons will irradiate the cold accretion disc, generating the so-called X-ray reflection component (Fabian et al. 1989). The main features of the reflection spectrum are the fluorescent Fe Kα emission line at energies of 6.4-6.97 keV (depend upon the ionization state of the disc) and the Compton hump at 20-30 keV (Young et al. 1999).The profile of the reflection spectrum will be smeared due to the effects of Doppler shift, special relativity, and general relativity if it comes from the inner region of the accretion disc (Fabian et al. 2000). Observationally, the most prominent effect is that the intrinsically narrow Fe Kα line is broadened and skewed to an asymmetric shape. The profile of the broad line, especially the red wing of the line, is directly linked to the inner radius of the accretion disc which is thought to be at the innermost stable circular orbit (ISCO), i.e. R in = R ISCO . Thus, by modelling the broad iron line, we can deduce the spin of the black hole based on the relation between the spin and the ISCO (Bardeen et al. 1972). However, the line profile is readily affected by the subtraction of continuum and other components. Therefore, Reynolds (2014) pointed out that a more accurate measurement of the spin can be achieved by modelling the full reflection spectrum. The spin...

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Reflection Spectroscopy of the Black Hole Binary XTE J1752−223 in Its Long-stable Hard State

Cited by 56 publications

References 52 publications

Broad-band spectral study of X-ray transient MAXI J1820+070 using Swift/XRT and NuSTAR

Broad-band spectral study of X-ray transient MAXI J1820+070 using Swift/XRT and NuSTAR

Potential kick velocity distribution of black hole X-ray binaries and implications for natal kicks

A detailed study on the reflection component for the black hole candidate MAXI J1836−194

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