Detection of a Possible X-Ray Quasi-Periodic Oscillation in the Active Galactic Nucleus 1h 0707–495

Pan, Hai-Wu; Yuan, Weimin; Yao, Shujie; Zhou, Xin-Lin; Liu, Bifang; Zhou, Hongyan; Zhang, Shuang‐Nan

doi:10.3847/2041-8205/819/2/l19

Cited by 56 publications

(77 citation statements)

References 51 publications

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“…It is widely believed that the QPO signals can be produced by instabilities in the inner accretion disk, or pulsating accretion when it is close to the Eddington limit, or X-ray hot spots orbiting the BH or disk precession according to Bardeen-Petterson effect Li & Narayan 2004;Sunyaev 1973;Guilbert et al 1983;Bardeen & Petterson 1975;Mukhopadhyay et al 2003;Gangopadhyay et al 2012 (Gierliński et al 2008) and 1H 0707−495 (Pan et al 2016;Zhang et al 2017) have been argued to be the High Frequency QPOs (HFQPOs; Zhou at al. 2010;Zhou et al 2015).…”

Section: The Time-averaged Spectra Analysismentioning

confidence: 99%

“…In this work the power spectra of LSP method is checked with the independent results of WWZ approach. Particularly for the light-curves on 2005 May 31 (Obs ID: 0304030601), following the previous works (Gierliński et al 2008;Pan et al 2016;Zhang et al 2017), we divide the EPIC light-curve into two segments (Segment I and Segment II), as shown in the upper panel of Fig. 1.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Please also see Zhou at al. (2010); Zhou et al (2015) and Pan et al (2016) for more information. Note: The spectral parameters obtained from the fitting of the time-averaged spectrum and the three time-resolved spectra.…”

Section: The Time-averaged Spectra Analysismentioning

confidence: 99%

“…The QPO signal frequency and the mass of the SMBH of Mrk 766 is found to be consistent with the relation suggested in the former literature Kluzniak & Abramowicz 2002;Zhou at al. 2010;Zhou et al 2015;Pan et al 2016). This work is organized as following: in Section 2 we describe the data analysis and show the main results, and in Section 3 we have a summary with some discussions.…”

Section: Introductionmentioning

confidence: 99%

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An X-Ray Periodicity of ∼1.8 hr in Narrow-line Seyfert 1 Galaxy Mrk 766

Zhang

Yan³

et al. 2017

ApJ

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In the narrow-line Seyfert 1 galaxy Mrk 766, a Quasi-Periodic Oscillation (QPO) signal with a period of ∼ 6450 s is detected in the XMM-Newton data collected on 2005 May 31. This QPO signal is highly statistical significant at the confidence level at ∼ 5σ with the quality factor of Q = f /∆f > 13.6. The X-ray intensity changed by a factor of 3 with root mean square fractional variability of 14.3%. Furthermore, this QPO signal presents in the data of all three EPIC detectors and two RGS cameras and its frequency follows the f QPO -M BH relation spanning from stellar-mass to supermassive black holes. Interestingly, a possible QPO signal with a period of ∼ 4200 s had been reported in the literature. The frequency ratio of these two QPO signals is ∼ 3:2. Our result is also in support of the hypothesis that the QPO signals can be just transient. The spectral analysis reveals that the contribution of the soft excess component below ∼ 1 keV is different between epochs with and without QPO, this property as well as the former frequency-ratio are well detected in X-ray BH binaries, which may have shed some lights on the physical origin of our event.

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Section: The Time-averaged Spectra Analysismentioning

confidence: 99%

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: The Time-averaged Spectra Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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An X-Ray Periodicity of ∼1.8 hr in Narrow-line Seyfert 1 Galaxy Mrk 766

Zhang

Yan³

et al. 2017

ApJ

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“…In X-rays, a significant transient QPO has been detected in NLS1 galaxy RE J1034+396 (Gierliński et al 2008). Recently, the other significant transient QPO signal has been reported in NLS1s galaxy 1H 0707-495 (Pan et al 2016) and Mrk 766 (Zhang et al 2017b). In this work, we reanalyze the data set adopted by Pan et al (2016) with the Weighted-Wavelet Z-transform method.…”

Section: Introductionmentioning

confidence: 99%

Two Transient X-Ray Quasi-periodic Oscillations Separated by an Intermediate State in 1H 0707-495

Zhang

Liao

et al. 2018

ApJ

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In the narrow-line Seyfert 1 galaxy 1H 0707-495, recently a transient quasi-periodic oscillation (QPO) signal with a frequency of ∼ 2.6 × 10 −4 Hz has been detected at a high statistical significance. Here, we reanalyze the same set of XMM-Newton data observed on 2008 February 4 with the WeightedWavelet Z-transform (WWZ) method. In addition to confirming the previous findings, we also find another QPO signal with a frequency of ∼ 1.2 × 10 −4 Hz in a separated X-ray emission phase at the significance level of ∼ 3.7σ. The signal is also found fitting an auto-regressive model though at a lower significance. The frequency ratio between these two signals is ∼ 2 : 1. The analysis of other XMMNewton measurements of 1H 0707-495 also reveals the presence of the ∼ 2.6 × 10 −4 Hz (∼ 1.2 × 10 −4Hz) QPO signal on 2007 May 14 (2010 September 17) at the significance level of ∼ 4.2σ (∼ 3.5σ). The QPO frequency found in this work follows the f QP O − M BH relation reported in previous works spanning from stellar-mass to supermassive black holes. This is the first time to observe two separated transient X-ray QPO signals in active galactic nuclei (AGNs), which sheds new light on the physics of accreting supermassive black holes.

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Stellar tidal disruption events in general relativity

et al. 2019

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A tidal disruption event (TDE) ensues when a star passes too close to the supermassive black hole (SMBH) in a galactic center and is ripped apart by the tidal field of the SMBH. The gaseous debris produced in a TDE can power a bright electromagnetic flare as it is accreted by the SMBH; so far, several dozen TDE candidates have been observed. For SMBHs with masses above ∼ 10 7 M , the tidal disruption of solar-type stars occurs within ten gravitational radii of the SMBH, implying that general relativity (GR) is needed to describe gravity. Three promising signatures of GR in TDEs are: (1) a super-exponential cutoff in the volumetric TDE rate for SMBH masses above ∼ 10 8 M due to direct capture of tidal debris by the event horizon, (2) delays in accretion disk formation (and a consequent alteration of the early-time light curve) caused by the effects of relativistic precession on stream circularization, and (3) quasi-periodic modulation of X-ray emission due to global precession of misaligned accretion disks and the jets they launch. We review theoretical models and simulations of TDEs in Newtonian gravity, then describe how relativistic modifications give rise to these proposed observational signatures, as well as more speculative effects of GR. We conclude with a brief summary of TDE observations and the extent to which they show indications of these predicted relativistic signatures.

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Detection of a Possible X-Ray Quasi-Periodic Oscillation in the Active Galactic Nucleus 1h 0707–495

Cited by 56 publications

References 51 publications

An X-Ray Periodicity of ∼1.8 hr in Narrow-line Seyfert 1 Galaxy Mrk 766

An X-Ray Periodicity of ∼1.8 hr in Narrow-line Seyfert 1 Galaxy Mrk 766

Two Transient X-Ray Quasi-periodic Oscillations Separated by an Intermediate State in 1H 0707-495

Stellar tidal disruption events in general relativity

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