A Retrograde Spin of the Black Hole in MAXI J1659–152

Rout, Sandeep K.; Vadawale, S.; Méndez, Mariano

doi:10.3847/2041-8213/ab629e

Cited by 10 publications

(9 citation statements)

References 54 publications

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“…Based on the use of different spectra, different models and updated dynamical parameters, we find a spin ranging from −1 < a * 0.35 (1σ). As reported by Rout et al (2020), we also rule out extreme prograde spin.…”

Section: Differences From Previous Measurementssupporting

confidence: 64%

“…We select 9 spectra of RXTE/PCA satisfying luminosity and state/coronal-brightness restrictions. Based on the two sets of plausible system parameters: M = 5.7 ± 1.8 M , i = 70.0 • , D = 6 ± 2 kpc and M = 4.9 ± 1.6 M , i = 80.0 • , D = 6 ± 2 kpc reported by Torres et al (2021), we constrain the spin to −1 < a * 0.44 in 90% confidence interval via the X-ray continuum-fitting method, as suggested in Rout et al (2020), there is a possibility of an extreme negative spin. Then we exclude the influence of changing N H on the spin.…”

Section: Discussionmentioning

confidence: 99%

“…In their results of the X-ray continuum-fitting show that the lower limit of the spin is pegged at -0.998, while the upper limit is 0.4. However, it should be noted that the spectra in Rout et al (2020) do not meet the f sc 25% criterion. Different from Rout et al (2020), we firstly screen the spectra with f sc 25% for the X-ray continuum-fitting and made crabcor correction.…”

Section: Differences From Previous Measurementsmentioning

confidence: 99%

“…However, it should be noted that the spectra in Rout et al (2020) do not meet the f sc 25% criterion. Different from Rout et al (2020), we firstly screen the spectra with f sc 25% for the X-ray continuum-fitting and made crabcor correction. In addition, we use the relativistic model kerrbb2 that allows the spectral hardening factor f to change, which will be closer to the actual situation.…”

Section: Differences From Previous Measurementsmentioning

confidence: 99%

“…Whereas, due to the faintness of the quiescent optical counterpart and short orbital period of MAXI J1659, it is difficult to measure its dynamic parameters (Torres et al 2021). Recently, Rout et al (2020) claims that the black hole's spin is retrograde and that it may be maximal. Through the H α emission, Torres et al (2021) find a radial velocity semi-amplitude of the donor of K 2 = 750 ± 80 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

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Estimating the spin of the black hole candidate MAXI J1659-152 with the X-ray continuum-fitting method

Feng,

Zhao,

Gou

et al. 2021

Preprint

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As a transient X-ray binary, MAXI J1659-152 contains a black hole candidate as its compact star. MAXI J1659-152 was discovered on 2010 September 25 during its only known outburst. Previously-published studies of this outburst indicate that MAXI J1659-152 may have an extreme retrograde spin, which, if confirmed, would provide an important clue as to the origin of black hole spin. In this paper, utilizing updated dynamical binarysystem parameters (i.e. the black hole mass, the orbital inclination and the source distance) provided by Torres et al. ( 2021), we analyze 65 spectra of MAXI J1659-152 from RXTE/PCA, in order to assess the spin parameter. With a final selection of 9 spectra matching our f sc 25%, soft-state criteria, we apply a relativistic thin disk spectroscopic model kerrbb2 over 3.0-45.0 keV. We find that inclination angle correlates inversely with spin, and, considering the possible values for inclination angle, we constrain spin to be −1 < a * 0.44 at 90% confidence interval via X-ray continuum-fitting. We can only rule out an extreme prograde (positive) spin. We confirm that an extreme retrograde solution is possible and is not ruled out by considering accretion torques given the young age of the system.

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Section: Differences From Previous Measurementssupporting

confidence: 64%

Section: Discussionmentioning

confidence: 99%

Section: Differences From Previous Measurementsmentioning

confidence: 99%

Section: Differences From Previous Measurementsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Estimating the spin of the black hole candidate MAXI J1659-152 with the X-ray continuum-fitting method

Feng,

Zhao,

Gou

et al. 2021

Preprint

View full text Add to dashboard Cite

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Delimiting the black hole mass in the X-ray transient MAXI J1659-152 with Hα spectroscopy

Torres

Jonker

Casares

et al. 2020

Monthly Notices of the Royal Astronomical Society

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MAXI J1659-152 is a 2.4 h orbital period X-ray dipping transient black hole candidate. We present spectroscopy of its I ≈ 23 quiescent counterpart, where we detect Hα emission with full width half maximum (FWHM) of 3200 ± 300 km s−1. Applying the correlation between the Hα FWHM and radial velocity semi-amplitude of the donor star for quiescent X-ray transients, we derive K2 = 750 ± 80 km s−1. The orbital period and K2 lead to a mass function of 4.4 ± 1.4 M⊙ (1σ). The donor to compact object mass ratio and binary inclination are likely in the range q = M2/M1 = 0.02–0.07 and i = 70○–80○. These constraints imply a 68 per cent confidence level interval for the compact object mass of 3.3 ≲ M1(M⊙) ≲ 7.5, confirming its black hole nature. These quasi-dynamical limits are compared to mass estimates from modelling of X-ray data and any discrepancies are discussed. We review the properties of optical spectroscopy and time-series photometry collected during the 2010–2011 outburst. We interpret the apparent modulations found soon after the onset of high-accretion activity and during the 2011 rebrightening event as originating in the accretion disc. These have signatures consistent with superhumps, with the 2011 modulation having a fractional period excess $\lt 0.6{\rm{per\, cent}}$ (3σ). We propose that direct irradiation of the donor by the central X-ray source was not possible due to its occultation by the disc outer regions. We argue that disc shielding significantly weakens the donor star contribution to the optical variability in systems with q ≲ 0.07, including neutron star ultra-compact X-ray binaries.

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The spin measurement of MAXI J1348-630 using the Insight-HXMT data

Song,

Jia,

Yang

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We report the results of fitting Insight-HXMT data to the black hole X-ray binary MAXI J1348-430, which was discovered on January 26th, 2019, with the Gas Slit Camera (GSC) on-board MAXI. Several observations at the beginning of the first burst were selected, with a total of 10 spectra. From the residuals of fits using disk plus power law models, X-ray reflection signatures were clearly visible in some of these observations. We use the state-of-the-art $\mathtt {relxill}$ series reflection model to fit six spectra with distinct reflection signatures and a joint fit to these spectra. In particular, we focus on the results for the black hole spin values. Assuming Rin = RISCO, the spin parameter is constrained to be $0.82^{+0.04}_{-0.03}$ with 90% confidence level (statistical only).

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A Retrograde Spin of the Black Hole in MAXI J1659–152

Cited by 10 publications

References 54 publications

Estimating the spin of the black hole candidate MAXI J1659-152 with the X-ray continuum-fitting method

Estimating the spin of the black hole candidate MAXI J1659-152 with the X-ray continuum-fitting method

Delimiting the black hole mass in the X-ray transient MAXI J1659-152 with Hα spectroscopy

The spin measurement of MAXI J1348-630 using the Insight-HXMT data

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