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

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 statistically significant at the ∼5 confidence level, with a quality factor of Q = f Δ f > 13.6 ....

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Bibliographic Details
Published in:The Astrophysical journal 2017-11, Vol.849 (1), p.9
Main Authors: Zhang, Peng, Zhang, Peng-fei, Yan, Jing-zhi, Fan, Yi-zhong, Liu, Qing-zhong
Format: Article
Language:English
Subjects:
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BLACK HOLES
Cameras
Confidence intervals
Galaxies
galaxies: active
galaxies: individual (Mrk 766)
galaxies: nuclei
GALAXY NUCLEI
MASS
OSCILLATIONS
Periodic variations
PERIODICITY
Q factors
QUALITY FACTOR
Quasi-Periodic Oscillations
Seyfert galaxies
Spectral analysis
Spectrum analysis
Stars & galaxies
Supermassive black holes
X-RAY GALAXIES
X-rays: galaxies
XMM (spacecraft)
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Summary: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 statistically significant at the ∼5 confidence level, with a quality factor of Q = f Δ f > 13.6 . The X-ray intensity changed by a factor of 3, with a root mean square fractional variability of 14.3%. Furthermore, this QPO signal is present 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 just be 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 shed some light on the physical origins of our event.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa8d6e