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A new method to measure the virial factors in the reverberation mapping of active galactic nuclei
Liu HT(刘洪涛)1,3,4; Feng HC(封海成)1,2,3; Bai JM(白金明)1,3,4; Liu, H. T.(Chinese Acad Sci, Yunnan Observ, 396 Yangfangwang, Guandu Dist 650216, Kunming, Peoples R China)
发表期刊MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2017-04-01
卷号466期号:3页码:3323-3330
DOI10.1093/mnras/stw3261
产权排序第1完成单位
收录类别SCI
关键词Black Hole Physics Galaxies: Active Galaxies: Nuclei Quasars: Emission Lines Galaxies: Seyfert
摘要Based on the gravitational red shift, which is a prediction of Einstein's general relativity theory, of broad optical emission lines in active galactic nuclei (AGNs), a new method is proposed to estimate the virial factors f in measuring black hole massesM(RM) by the reverberation mapping of AGNs. The factors f can be measured based on two physical quantities, i.e. the gravitational red shifts z(g) and the full widths at half maxima vFWHM of broad lines. In the past, it has been difficult to determine the factors f for individual AGNs. We apply this new method to several reverberation- mapped type 1 Seyfert galaxies. There is a correlation between f and the radius of the broad-line region (BLR) r(BLR), f = 5.4r(BLR)(0.3), for the gravitationally red-shifted broad lines He II, HeI, H beta and H alpha in the narrow-line type 1 Seyfert galaxy (NLS1) Mrk 110. This correlation results from the influence of the radiation pressure of the accretion disc on the BLR clouds. This influence seems to be more important than usually thought so in AGNs. Mrk 110 has f approximate to 8-16, distinctly larger than the mean (f) approximate to 1 usually used to estimate M-RM for v(FWHM.) NGC 4593 and NLS1 Mrk 486 have f approximate to 3 and f approximate to 9, respectively. Higher f values of several tens are derived for three other NLS1s. There is a correlation between f and accretion rate U-f=1, f = 6.8M(f= 1)(0.4) for five objects, where U-f=1 = M-center dot/L-Edd(c-2) as f = 1 is assumed when estimating MRM used in the Eddington luminosity L-Edd, M-center dot is the mass accretion rate, and c is the speed of light. These larger f values will produce higher MRM values and lower Eddington ratios.
项目资助者National Natural Science Foundation of China (NSFC)(11273052, U1431228) ; NSFC(11133006) ; Training Programme for the Talents of West Light Foundation ; Chinese Academy of Sciences (CAS) ; Youth Innovation Promotion Association, CAS.
语种英语
学科领域天文学
文章类型Article
ISSN0035-8711
URL查看原文
WOS记录号WOS:000398418600056
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]BLACK-HOLE MASS ; BROAD-LINE REGION ; DIGITAL SKY SURVEY ; HIGH ACCRETION RATES ; SEYFERT 1 GALAXIES ; VELOCITY DISPERSION ; EMISSION-LINES ; GRAVITATIONAL REDSHIFT ; PROFILE VARIATIONS ; LUMINOUS QUASARS
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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/114a53/10028
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, H. T.(Chinese Acad Sci, Yunnan Observ, 396 Yangfangwang, Guandu Dist 650216, Kunming, Peoples R China)
作者单位1.Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, P. R. China
2.University of Chinese Academy of Sciences, Beijing 100049, P. R. China
3.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, P. R. China
4.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, P. R. China
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Liu HT,Feng HC,Bai JM,et al. A new method to measure the virial factors in the reverberation mapping of active galactic nuclei[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2017,466(3):3323-3330.
APA Liu HT,Feng HC,Bai JM,&Liu, H. T..(2017).A new method to measure the virial factors in the reverberation mapping of active galactic nuclei.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,466(3),3323-3330.
MLA Liu HT,et al."A new method to measure the virial factors in the reverberation mapping of active galactic nuclei".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 466.3(2017):3323-3330.
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