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|Title: ||Discovery of high-amplitude X-ray variability in the Seyfert-LINER transition galaxy NGC 7589|
|Authors: ||Yuan, W.|
Osborne, Julian P.
Watson, Michael G.
|Issue Date: ||25-Aug-2004|
|Publisher: ||Blackwell Publishing on behalf of the Royal Astronomical Society|
|Citation: ||Monthly Notices of the Royal Astronomical Society, 2004, 353 (3), pp. L29-L33 (5)|
|Abstract: ||We present the first result of a programme to search for large flux variations in the X-ray sources of the XMM Serendipitous Survey compared to previous ROSAT observations. An increase in X-ray flux by a factor >10 was discovered from the nucleus of the galaxy NGC7589 on a time-scale of less than 5 yr. The 0.4-10 keV XMM spectrum can be approximated by a power law with photon index of 1.7-1.8, though it seems to flatten above 5 keV, suggesting a possible complex model, such as partial covering or disc reflection. A classification based on an analysis of its optical spectrum places NGC 7589 in the Seyfert region, but close to the Seyfert-LINER (low-ionization nuclear emission-line region) borderline on the active galactic nucleus (AGN) diagnostic diagrams. We classify NGC 7589 as either Seyfert 1.9 or LINER I, in the light of the detection of a broad Halpha line, which makes NGC 7589 an AGN in the low-luminosity regime. We interpret the observed variability in terms of either changes in covering factor of absorbing gas in the AGN, or variability in the intrinsic X-ray luminosity. Should the latter be the case, the inferred Eddington accretion rate increased from the radiatively inefficient accretion-dominated regime to a value close to the putative critical value, at which a transition of the accretion mode is supposed to take place. This possibility presents a new prospect of studying accretion physics in the central black holes of external galaxies by direct observing changes of 'spectral state', as is common in stellar black hole binary systems.|
|DOI Link: ||10.1111/j.1365-2966.2004.08266.x|
|Version: ||Publisher Version|
|Type: ||Journal Article|
|Rights: ||Copyright © 2004 RAS. Deposited with reference to the publisher's archiving policy available from the Journal Exclusive Licence Form, which permits posting of the Blackwell Publishing PDF 6 months after publication. The definitive version is available from www.blackwell-synergy.com|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
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