High Density Reflection Spectroscopy - II. The density of the inner black hole accretion disc in AGN

被引：91

作者：

Jiang, Jiachen ^{[1
,2
]}

Fabian, Andrew C. ^{[1
]}

Dauser, Thomas ^{[3
,4
]}

Gallo, Luigi ^{[5
]}

Garcia, Javier A. ^{[3
,4
,6
]}

Kara, Erin ^{[7
]}

Parker, Michael L. ^{[8
]}

Tomsick, John A. ^{[9
]}

Walton, Dominic J. ^{[1
]}

Reynolds, Christopher S. ^{[1
]}

机构：

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

[2] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China

[3] Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany

[4] Erlangen Ctr Astroparticle Phys, Sternwartstr 7, D-96049 Bamberg, Germany

[5] St Marys Univ, Dept Astron & Phys, 923 Robie St, Halifax, NS B3H 3C3, Canada

[6] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

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

[8] ESA, ESAC, E-28691 Villanueva De La Canada, Spain

[9] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 489卷 / 03期

关键词：

accretion; accretion discs; black hole physics; galaxies: Seyfert; X-rays: galaxies; X-RAY REFLECTION; XMM-NEWTON OBSERVATION; IRON K; TIME LAGS; ARK; 564; EMISSION; MASS; DISCOVERY; SPECTRA; I;

D O I：

10.1093/mnras/stz2326

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a high density disc reflection spectral analysis of a sample of 17 Seyfert 1 galaxies to study the inner disc densities at different black hole mass scales and accretion rates. All the available XMM-Newton observations in the archive are used. OM observations in the optical/UV band are used to estimate their accretion rates. We find that 65 per cent of sources in our sample show a disc density significantly higher than n(e) = 10(15) cm(-3), which was assumed in previous reflection-based spectral analyses. The best-fitting disc densities show an anticorrelation with black hole mass and mass accretion rate. High density disc reflection model can successfully explain the soft excess emission and significantly reduce inferred iron abundances. We also compare our black hole spin and disc inclination angle measurements with previous analyses.

引用

页码：3436 / 3455

页数：20

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