The energy-dependent X-ray timing characteristics of the narrow-line Seyfert 1 Mrk 766

被引:38
|
作者
Markowitz, A. [1 ]
Papadakis, I.
Arevalo, P.
Turner, T. J.
Miller, L.
Reeves, J. N.
机构
[1] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA
[2] Univ Crete, Dept Phys, Iraklion, Greece
[3] Univ Southampton, Sch Phys & Astron, Southampton, Hants, England
[4] Univ Maryland, Dept Phys, Baltimore, MD USA
[5] Univ Oxford, Dept Phys, Oxford, England
[6] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
来源
ASTROPHYSICAL JOURNAL | 2007年 / 656卷 / 01期
基金
英国科学技术设施理事会;
关键词
galaxies : active; galaxies : individual (Mrk 766); galaxies : Seyfert; X-rays : galaxies;
D O I
10.1086/510616
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the energy-dependent power spectral density (PSD) and cross spectral properties of Mrk 766, obtained from combining data obtained during an XMM-Newton observation spanning six revolutions in 2005 with data obtained from an XMM-Newton long look in 2001. The PSD shapes and rms-flux relations are found to be consistent between the 2001 and 2005 observations, suggesting that the 2005 observation is simply a low-flux extension of the 2001 observation and permitting us to combine the two data sets. The resulting PSD has the highest temporal frequency resolution for any AGN PSD measured to date. Applying a broken power-law model yields break frequencies that increase in temporal frequency with photon energy. Obtaining a good fit when assuming energy-independent break frequencies requires the presence of a Lorentzian at (4.6 +/- 0.4) x 10(-4) Hz whose strength increases with photon energy, a behavior seen in black hole X-ray binaries. The cross spectral properties are measured; temporal frequency-dependent soft-to-hard time lags are detected in this object for the first time. Cross spectral results are consistent with those for other accreting black hole systems. The results are discussed in the context of several variability models, including those based on inwardly propagating viscosity variations in the accretion disk.
引用
收藏
页码:116 / 128
页数:13
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