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Fabian, A. C; Kara, E; Walton, D. J; Wilkins, D. R; Ross, R. R; Lozanov, K; Uttley, P; Gallo, L. C; Zoghbi, A; Miniutti, G; Boller, T; Brandt, W. N; Cackett, E. M; Chiang, C.-Y; Dwelly, T; Malzac, J; Miller, J. M; Nardini, E; Ponti, G; Reis, R. C; Reynolds, C. S; Steiner, J. F; Tanaka, Y; Young, A. J
Monthly notices of the Royal Astronomical Society, 03/2013, Letnik: 429, Številka: 4Journal Article
The narrow-line Seyfert 1 galaxy IRAS 13224−3809 has been observed with XMM-Newton for 500 ks. The source is rapidly variable on time-scales down to a few 100 s. The spectrum shows strong broad Fe − K and L emission features which are interpreted as arising from reflection from the inner parts of an accretion disc around a rapidly spinning black hole. Assuming a power law emissivity for the reflected flux and that the innermost radius corresponds to the innermost stable circular orbit, the black hole spin is measured to be 0.989 with a statistical precision better than 1 per cent. Systematic uncertainties are discussed. A soft X-ray lag of 100 s confirms this scenario. The bulk of the power-law continuum source is located at a radius of 2-3 gravitational radii.
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JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
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in: SICRIS
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