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Dependence of the broad Fe K alpha line on the physical parameters of AGN
Liu, Zhu1,2; Yuan, Weimin1,2; Lu, Youjun2,3; Carrera, Francisco J.4; Falocco, Serena6; Dong XB(董小波)6,7; Liu, Z; Yuan, WM
发表期刊MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2016-11-21
卷号463期号:1页码:684-695
DOI10.1093/mnras/stw2042
产权排序第6完成单位
收录类别SCI
关键词Galaxies: Active X-rays: Galaxies
摘要In this paper, the dependence of the broad Fe K alpha line on the physical parameters of AGN, such as the black hole mass M-BH, accretion rate (equivalently represented by Eddington ratio lambda(Edd)) and optical classification is investigated by applying the X-ray spectra stacking method to a large sample of AGN which have well measured optical parameters. A broad-line feature is detected (> 3 sigma) in the stacked spectra of the high lambda(Edd) sub-sample (log lambda(Edd) > -0.9). The profile of the broad line can be well fitted with relativistic broad-line model, with the line energy consistent with highly ionized Fe K alpha line (i.e. Fe xxvi). A model consisting of multiple narrow lines cannot be ruled out, however. We found hints that the Fe K line becomes broader as the lambda(Edd) increases. No broad-line feature is shown in the sub-sample of broad-line Seyfert 1 (BLS1) galaxies and in the full sample, while a broad line might be present, though at low significance, in the sub-sample of narrow-line Seyfert 1 (NLS1) galaxies. We find no strong dependence of the broad line on black hole masses. Our results indicate that the detection/properties of the broad Fe K alpha line may strongly depend on lambda(Edd), which can be explained if the ionization state and/or truncation radius of the accretion disc changes with lambda(Edd). The non-detection of the broad line in the BLS1 sub-sample can be explained if the average equivalent width of the relativistic Fe K alpha line is weak or/and the fraction of sources with relativistic Fe K alpha line is small in BLS1 galaxies.
项目资助者National Natural Science Foundation of China(11473035, 11273027, 11303046) ; Strategic Priority Research Program The Emergence of Cosmological Structures of the Chinese Academy of Sciences(XDB09000000) ; NSF(11473062) ; MINECO/FEDER(AYA2015-64346-C2-1-P) ; ESA Member States ; NASA
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0035-8711
URL查看原文
WOS记录号WOS:000386464900055
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]ACTIVE GALACTIC NUCLEI ; ADVECTION-DOMINATED ACCRETION ; DIGITAL SKY SURVEY ; SEYFERT 1 GALAXIES ; PHOTON IMAGING CAMERA ; 2XMM CATALOG SOURCES ; MASSIVE BLACK-HOLE ; RAY SPECTRAL SLOPE ; XMM-NEWTON ; EDDINGTON RATIO
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被引频次:2[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/9754
专题丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
通讯作者Liu, Z; Yuan, WM
作者单位1.Key Laboratory of Space Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
2.University of Chinese Academy of Sciences, School of Astronomy and Space Science, Beijing 100049, China
3.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
4.Instituto de Física de Cantabria (CSIC-UC), Avenida de los Castros, E-39005 Santander, Spain
5.KTH Royal Institute of Technology, Department of Physics and the Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden
6.Yunnan Observatories, Chinese Academy of Sciences, Kunming, Yunnan 650011, China
7.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, Yunnan 650011, China
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Liu, Zhu,Yuan, Weimin,Lu, Youjun,et al. Dependence of the broad Fe K alpha line on the physical parameters of AGN[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2016,463(1):684-695.
APA Liu, Zhu.,Yuan, Weimin.,Lu, Youjun.,Carrera, Francisco J..,Falocco, Serena.,...&Yuan, WM.(2016).Dependence of the broad Fe K alpha line on the physical parameters of AGN.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,463(1),684-695.
MLA Liu, Zhu,et al."Dependence of the broad Fe K alpha line on the physical parameters of AGN".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 463.1(2016):684-695.
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