Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/36652
Title: X-ray variability of 104 active galactic nuclei. XMM-Newton power-spectrum density profiles
Authors: González-Martín, O.
Vaughan, Simon Allan
First Published: 1-Aug-2012
Publisher: EDP Sciences for European Southern Observatory (ESO)
Citation: Astronomy & Astrophysics, 2012, 544, A80
Abstract: Context. Active galactic nuclei (AGN), powered by accretion onto supermassive black holes (SMBHs), are thought to be scaled up versions of Galactic black hole X-ray binaries (BH-XRBs). In the past few years evidence of such correspondence include similarities in the broadband shape of the X-ray variability power spectra, with characteristic bend times-scales scaling with mass. Aims. The aim of this project is to characterize the X-ray temporal properties of a sample of AGN to study the connection among different classes of AGN and their connection with BH-XRBs. Methods. We have performed a uniform analysis of the power spectrum densities (PSDs) of 104 nearby (z < 0.4) AGN using 209 XMM-Newton/pn observations. These PSDs span ≃ 3 decades in temporal frequencies, ranging from minutes to days. The PSDs have been estimated in three energy bands: 0.2−10 (total), 0.2−2 (soft), and 2−10 keV (hard). The sample comprises 61 Type-1 AGN, 21 Type-2 AGN, 15 NLSy1, and 7 BLLACS. We have fitted each PSD to two models: (1) a single power-law model and (2) a bending power-law model. Results. Among the entire sample, 72% show significant variability in at least one of the three bands tested. A high percentage of low-luminosity AGN do not show any significant variability (86% of LINERs). The PSD of the majority of the variable AGN was well described by a simple power-law with a mean index of α = 2.01   ±   0.01. In 15 sources we found that the bending power law model was preferred with a mean slope of α = 3.08   ±   0.04 and a mean bend frequency of ⟨ νb ⟩ ≃ 2 × 10[Superscript: -4] Hz. Only KUG 1031+398 (RE J1034+396) shows evidence for quasi-periodic oscillations. The “fundamental plane” relating variability timescale, black hole mass, and luminosity is demonstrated using the new X-ray timing results presented here together with a compilation of the previously detected timescales from the literature. Conclusions. Both quantitative (i.e. scaling with BH mass) and qualitative (overall PSD shapes) found in this sample of AGN are in agreement with the expectations for the SMBHs and BH-XRBs being the same phenomenon scaled-up with the size of the BH. The steep PSD slopes above the high frequency bend bear a closer resemblance to those of the “soft/thermal dominated” BH-XRB states than other states.
DOI Link: 10.1051/0004-6361/201219008
ISSN: 0004-6361
eISSN: 1432-0746
Links: http://www.aanda.org/articles/aa/abs/2012/08/aa19008-12/aa19008-12.html
http://hdl.handle.net/2381/36652
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © ESO, 2012. Reproduced with permission from Astronomy & Astrophysics, © ESO.
Description: archiveprefix: arXiv primaryclass: astro-ph.HE keywords: accretion, accretion disks, Galaxy: nucleus, galaxies: active, X-rays: galaxies eid: A80 adsurl: http://adsabs.harvard.edu/abs/2012A%26A...544A..80G adsnote: Provided by the SAO/NASA Astrophysics Data System
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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