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On the relationship between black hole mass and X-ray variability amplitude in the low-mass regime of active galactic nuclei

Published online by Cambridge University Press:  07 March 2016

H. Pan ,
W. Yuan ,
X.-L. Zhou ,
X. Dong  and
B. Liu
H. Pan
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China email: [email protected]
W. Yuan
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China email: [email protected]
X.-L. Zhou
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China email: [email protected]
X. Dong
Affiliation:
Yunnan Observatories, Chinese Academy of Sciences, Kunming, Yunnan, China
B. Liu
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China email: [email protected]
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Abstract

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Recent studies of active galactic nuclei (AGN) found a statistical inverse scaling between the X-ray normalized excess variance σrms2 (variability amplitude) and the black hole mass spanning over MBH = 106 − 109M⊙. We present a study of this relation by including AGN with MBH = 105 − 106M⊙. It is found that the relation is no longer a simple extrapolation of the known inverse proportion, but starts to flatten around 106M⊙. This behavior can be understood by the shape of the power spectrum density of AGN and its dependence on the black hole mass.

Keywords

galaxies: activegalaxies: nucleiX-rays: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S312: Star Clusters and Black Holes in Galaxies across Cosmic Time , August 2014 , pp. 73 - 74
Copyright
Copyright © International Astronomical Union 2016 

References

Dong, X.-B., Ho, L. C., & Yuan, W., et al. 2012, ApJ, 755, 167Google Scholar
González-Martín, O. & Vaughan, S. 2012, A&A, 544, A80Google Scholar
Ludlam, R. M., Cackett, E. M., & Gultekin, K., et al. 2015, MNRAS, 447, 2112Google Scholar
McHardy, I. M., Koerding, E., Knigge, C., Uttley, P., & Fender, R. P. 2006, Nature, 444, 730Google Scholar
Nandra, K., George, I. M., Mushotzky, R. F., Turner, T. J., & Yaqoob, T. 1997, ApJ, 476, 70Google Scholar
Papadakis, I. E. 2004, MNRAS, 348, 207Google Scholar
Ponti, G., Papadakis, I., & Bianchi, S., et al. 2012, A&A, 542, A83Google Scholar
van der Klis, M. 1989, Timing Neutron Stars, 27Google Scholar
van der Klis, M. 1997, Statistical Challenges in Modern Astronomy II, 321Google Scholar
Zhou, X.-L., Zhang, S.-N., Wang, D.-X., & Zhu, L. 2010, ApJ, 710, 16Google Scholar