Low-Frequency Quasi-Periodic Oscillations in the X-ray Nova MAXI J1535-571 at the Initial Stage of Its 2017 Outburst

Mereminskiy, I. A.; Гребенев, С. А.; Prosvetov, A. V.; Семена, А. Н.

doi:10.1134/s106377371806004x

Cited by 16 publications

(14 citation statements)

References 31 publications

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“…It correlates with the NuSTAR flux and the photon index ( Fig. 7), similar to many other BH and neutron star binary systems (see, e.g., Sobczak et al 2000;Revnivtsev et al 2001;Vignarca et al 2003;Titarchuk & Fiorito 2004;Ibragimov et al 2005;Gilfanov 2010;Shidatsu et al 2014;Fürst et al 2016b;Mereminskiy et al 2018). The QPO amplitude remained stable during the first half of the observation, and started to grow in the second part.…”

Section: Power Spectrumsupporting

confidence: 81%

“…12 that observations are incompatible with the BH mass 10M and barely agree with a maximally rotating massive 100M BH. This results together with the measurements by Fürst et al (2016a) and Mereminskiy et al (2018) indicate that there are some tensions between the predictions of the Lense-Thirring precession model and the truncation radii inferred from the spectral fitting. It is also worth noting that the observed QPO changed in frequency by a factor of ≈ 2.5 while no drastic changes were observed in the spectrum.…”

Section: Black Hole Mass Estimationsupporting

confidence: 51%

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Studying temporal variability of GRS 1739–278 during the 2014 outburst

Mereminskiy

Семена

Bykov

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We report a discovery of low-frequency quasi periodic oscillation at 0.3-0.7 Hz in the power spectra of the accreting black hole GRS 1739-278 in the hard-intermediate state during its 2014 outburst based on the NuSTAR and Swift/XRT data. The QPO frequency strongly evolved with the source flux during the NuSTAR observation. The source spectrum became softer with rising QPO frequency and simultaneous increasing of the power-law index and decreasing of the cut-off energy. In the power spectrum, a prominent harmonic is clearly seen together with the main QPO peak. The fluxes in the soft and the hard X-ray bands are coherent, however, the coherence drops for the energy bands separated by larger gaps. The phase-lags are generally positive (hard) in the 0.1-3 Hz frequency range, and negative below 0.1 Hz. The accretion disc inner radius estimated with the relativistic reflection spectral model appears to be R in < 7.3R g . In the framework of the relativistic precession model, in order to satisfy the constraints from the observed QPO frequency and the accretion disc truncation radius, a massive black hole with M BH ≈ 100M is required.

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Section: Power Spectrumsupporting

confidence: 81%

Section: Black Hole Mass Estimationsupporting

confidence: 51%

Studying temporal variability of GRS 1739–278 during the 2014 outburst

Mereminskiy

Семена

Bykov

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…where the disc component dominates) and the X-ray variability decreases, reaching fractional rms amplitudes < 5 per cent. It is worth noting that quasi-periodic oscillations (QPOs) were detected during the main outburst of J1535 (Mereminskiy et al 2018;Stevens et al 2018;Huang et al 2018;Stiele & Kong 2018;Shang et al 2019;Sreehari et al 2019), however, we did not detect any significant QPO during the reflares. This result could potentially be related to differences in the physical conditions during the normal bright outburst and the fainter reflares or it could be that QPOs are too weak to be detected at the low count rates we ob-serve.…”

Section: Outburst Reflares Of Maxi J1535-571: the State Transition Identificationcontrasting

confidence: 65%

A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

Cúneo

Alabarta

Zhang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The black hole candidate and X-ray binary MAXI J1535−571 was discovered in 2017 September. During the decay of its discovery outburst, and before returning to quiescence, the source underwent at least four reflaring events, with peak luminosities of ∼1035–36 erg s−1 (d/4.1 kpc)2. To investigate the nature of these flares, we analysed a sample of NICER (Neutron star Interior Composition Explorer) observations taken with almost daily cadence. In this work, we present the detailed spectral and timing analysis of the evolution of the four reflares. The higher sensitivity of NICER at lower energies, in comparison with other X-ray detectors, allowed us to constrain the disc component of the spectrum at ∼0.5 keV. We found that during each reflare the source appears to trace out a q-shaped track in the hardness–intensity diagram similar to those observed in black hole binaries during full outbursts. MAXI J1535−571 transits between the hard state (valleys) and softer states (peaks) during these flares. Moreover, the Comptonized component is undetected at the peak of the first reflare, while the disc component is undetected during the valleys. Assuming the most likely distance of 4.1 kpc, we find that the hard-to-soft transitions take place at the lowest luminosities ever observed in a black hole transient, while the soft-to-hard transitions occur at some of the lowest luminosities ever reported for such systems.

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“…However, after AstroSat stopped observing there is a clear positive correlation between the two parameters. Mereminskiy et al (2018) and Stiele & Kong (2018) also perform a spectro-timing analysis of this source and observe a similar positive correlation between the ν QPO and power law index. The extent of the observations analysed by these authors is larger than the AstroSat observation window and thus the tight correlation we observe is a subset of the correlation observed by them.…”

Section: Timing Analysismentioning

confidence: 57%

“…in transition from the hard to the soft state. Mereminskiy et al (2018) and Stiele & Kong (2018) discuss the evolution of the QPO frequency and observe a positive correlation between the QPO centroid frequency and the power law index of the spectrum, relating the QPO centroid frequency to the inner truncation radius of the disk, Mereminskiy et al (2018) derive self-consistent results for the physical parameters of the inner Comptonising cloud. Xu et al (2018) analyse the NuSTAR spectrum and constrain the spin of the black hole to > 0.84 and inner truncation radius to < 2.01 R ISCO .…”

Section: Introductionmentioning

confidence: 99%

Spectro-timing analysis of MAXI J1535–571 using AstroSat

Bhargava

Belloni

Bhattacharya

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report the results of the analysis of an AstroSat observation of the Black Hole candidate MAXI J1535−571 during its Hard Intermediate state. We studied the evolution of the spectral and timing parameters of the source during the observation. The observation covered a period of ∼5 days and consisted of 66 continuous segments, corresponding to individual spacecraft orbits. Each segment was analysed independently. The source count rate increased roughly linearly by ∼30%. We modelled the spectra as a combination of radiation from a thermal disk component and a power-law. The timing analysis revealed the presence of strong Quasi Periodic Oscillations with centroid frequency ν QPO fluctuating in the range 1.7-3.0 Hz. We found a tight correlation between the QPO centroid frequency ν QPO and the power-law spectral index Γ, while ν QPO appeared not to be correlated with the linearly-increasing flux itself. We discuss the implications of these results on physical models of accretion.

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Low-Frequency Quasi-Periodic Oscillations in the X-ray Nova MAXI J1535-571 at the Initial Stage of Its 2017 Outburst

Cited by 16 publications

References 31 publications

Studying temporal variability of GRS 1739–278 during the 2014 outburst

Studying temporal variability of GRS 1739–278 during the 2014 outburst

A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

Spectro-timing analysis of MAXI J1535–571 using AstroSat

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