X-Ray Coronal Properties of Swift/BAT-selected Seyfert 1 Active Galactic Nuclei

被引：39

作者：

Kamraj, Nikita ^{[1
]}

Brightman, Murray ^{[1
]}

Harrison, Fiona A. ^{[1
]}

Stern, Daniel ^{[2
]}

Garcia, Javier A. ^{[1
,3
,4
]}

Balokovic, Mislav ^{[5
,6
]}

Ricci, Claudio ^{[7
,8
,9
]}

Koss, Michael J. ^{[10
,11
]}

Mejia-Restrepo, Julian E. ^{[12
]}

Oh, Kyuseok ^{[13
,14
]}

Powell, Meredith C. ^{[15
]}

Urry, C. Megan ^{[5
,6
]}

机构：

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

[2] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

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

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

[5] Yale Ctr Astron & Astrophys, 52 Hillhouse Ave, New Haven, CT 06511 USA

[6] Yale Univ, Dept Phys, POB 208120, New Haven, CT 06520 USA

[7] Univ Diego Portales, Nucleo Astron, Fac Ingn, Av Ejercito Libertador 441, Santiago 22, Chile

[8] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[9] George Mason Univ, Dept Phys & Astron, MS 3F3,4400 Univ Dr, Fairfax, VA 22030 USA

[10] Eureka Sci, 2452 Delmer St Suite 100, Oakland, CA 94602 USA

[11] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA

[12] European Southern Observ, Casilla 19001, Santiago 19, Chile

[13] Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea

[14] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan

[15] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA

来源：

ASTROPHYSICAL JOURNAL | 2022年 / 927卷 / 01期

基金：

美国国家航空航天局; 新加坡国家研究基金会;

关键词：

AGN SPECTROSCOPIC SURVEY; HIGH-ENERGY CUTOFF; BLACK-HOLE MASS; XMM-NEWTON; BEPPOSAX OBSERVATIONS; GAMMA-RAY; SPECTRUM; NUSTAR; BROAD; GALAXIES;

D O I：

10.3847/1538-4357/ac45f6

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The corona is an integral component of active galactic nuclei (AGNs) which produces the bulk of the X-ray emission above 1-2 keV. However, many of its physical properties and the mechanisms powering this emission remain a mystery. In particular, the temperature of the coronal plasma has been difficult to constrain for large samples of AGNs, as constraints require high-quality broadband X-ray spectral coverage extending above 10 keV in order to measure the high-energy cutoff, which provides constraints on the combination of coronal optical depth and temperature. We present constraints on the coronal temperature for a large sample of Seyfert 1 AGNs selected from the Swift/BAT survey using high-quality hard X-ray data from the NuSTAR observatory combined with simultaneous soft X-ray data from Swift/XRT or XMM-Newton. When applying a physically motivated, nonrelativistic disk-reflection model to the X-ray spectra, we find a mean coronal temperature kT ( e ) = 84 +/- 9 keV. We find no significant correlation between the coronal cutoff energy and accretion parameters such as the Eddington ratio and black hole mass. We also do not find a statistically significant correlation between the X-ray photon index, Gamma, and Eddington ratio. This calls into question the use of such relations to infer properties of supermassive black hole systems.

引用

页数：12

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