Fe Kα line profile in AGNs: average shape and redshift dependence  

作　　者：Wei-Ming Mao Chen Hu Jian-Min Wang Gang Zhao Shu Zhang 

机构地区：[1]Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China [2]Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China [3]Graduate University of Chinese Academy of Sciences, Beijing 100049, China

出　　处：《Research in Astronomy and Astrophysics》2010年第9期905-914,共10页天文和天体物理学研究（英文版）

基　　金：the National Natural Science Foundation of China (NSFC; Grant No. 10821061);the National Basic Research Program of China (973 program; Nos. 2007CB815103 and 2009CB824800)

摘　　要：We collect a sample of 381 （271 type Ⅰ） active galactic nuclei （AGNs） with XMM-Newton observations for an analysis of the dependence of Fe Kα profiles on redshifts to test the potential cosmological evolution of spins of supermassive black holes （SMBHs）. The sample spans a redshift range of z = 0.0008 - 4.76, which allows us to rebin the sample into 7 redshift groups. Phenomenological analysis of the Fe profile suggested that the line width （δ） of the narrow or broad Fe line does not show significant changes in redshift range z 〈 0.3. Using a physical model, we significantly detect a narrow Fe Kα line at 6.4 keV with an average equivalent width （EW） = 160 eV except for the two largest redshift bins. The EW of the Fe line does not show significant changes. We also find a relativistic broad line in three redshift bins （z 〈 0.116, 0.056 〈 z 〈 0.12 and 0.12 〈 z 〈 0.3）with an average EW = 522eV.We collect a sample of 381 （271 type Ⅰ） active galactic nuclei （AGNs） with XMM-Newton observations for an analysis of the dependence of Fe Kα profiles on redshifts to test the potential cosmological evolution of spins of supermassive black holes （SMBHs）. The sample spans a redshift range of z = 0.0008 - 4.76, which allows us to rebin the sample into 7 redshift groups. Phenomenological analysis of the Fe profile suggested that the line width （δ） of the narrow or broad Fe line does not show significant changes in redshift range z 〈 0.3. Using a physical model, we significantly detect a narrow Fe Kα line at 6.4 keV with an average equivalent width （EW） = 160 eV except for the two largest redshift bins. The EW of the Fe line does not show significant changes. We also find a relativistic broad line in three redshift bins （z 〈 0.116, 0.056 〈 z 〈 0.12 and 0.12 〈 z 〈 0.3）with an average EW = 522eV.

关 键 词：GALAXIES active -- X-rays general -- methods data analysis 

分 类 号：O178[理学—数学] P157.6[理学—基础数学]