Long XMM observation of the narrow-line Seyfert 1 galaxy IRAS 13224-3809: rapid variability, high spin and a soft lag

被引：98

作者：

Fabian, A. C. ^{[1
]}

Kara, E. ^{[1
]}

Walton, D. J. ^{[1
]}

Wilkins, D. R. ^{[1
]}

Ross, R. R. ^{[2
]}

Lozanov, K. ^{[1
]}

Uttley, P. ^{[3
]}

Gallo, L. C. ^{[4
]}

Zoghbi, A. ^{[5
]}

Miniutti, G. ^{[6
]}

Boller, T. ^{[7
]}

Brandt, W. N. ^{[8
]}

Cackett, E. M. ^{[9
]}

Chiang, C. -Y. ^{[1
]}

Dwelly, T. ^{[10
]}

Malzac, J. ^{[1
]}

Miller, J. M. ^{[11
]}

Nardini, E. ^{[12
]}

Ponti, G. ^{[7
]}

Reis, R. C. ^{[11
]}

Reynolds, C. S. ^{[5
]}

Steiner, J. F. ^{[1
]}

Tanaka, Y. ^{[7
]}

Young, A. J. ^{[13
]}

机构：

[1] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[2] Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA

[3] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands

[4] St Marys Univ, Dept Astron & Phys, Halifax, NS B3H 3C3, Canada

[5] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[6] Ctr Astrobiol CSIC INTA, Dep Astrofis, LAEFF, E-28691 Madrid, Spain

[7] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany

[8] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[9] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA

[10] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[11] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[12] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[13] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2013年 / 429卷 / 04期

关键词：

accretion; accretion discs; black hole physics; line: profiles; X-rays: general; X-RAY REFLECTION; BLACK-HOLE SPIN; IRON-K; SPECTRAL PROPERTIES; EMISSION-LINES; IRAS-13224-3809; REVERBERATION; NEWTON;

D O I：

10.1093/mnras/sts504

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页码：2917 / 2923

页数：7

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