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Black hole-bulge relation for narrow-line objects
Bian, WH; Zhao, YH
AbstractIt has been thought that narrow-line Seyfert I galaxies are likely to be in the early stages of the evolution of active galaxies. To test this suggestion, the ratios of the central massive black hole (MBH) mass to the bulge mass (M-bh/M-bulge) were estimated for 22 Narrow Line AGNs (NL AGNs). It is found that NL AGNs appear to have genuinely lower MBH/Bulge mass ratio (M-bh/M-bulge). The mean log(M-bh/M-bulge) for 22 NL AGNs is -3.9 +/- 0.07, which is an order of magnitude lower than that for Broad Line AGNs and quiescent galaxies. We suggest a nonlinear MBH/Bulge relation and find there exists a relation between the M-bh/M-bulge and the velocity dispersion, a, derived from the [0 fit] width. A scenario of MBH growth for NL AGNs is one of our interpretations of the nonlinear MBH/Bulge relation. The MBH growth timescales for 22 NL AGNs were calculated, with a mean value (1.29 +/- 0.24) x 10(8) yr. Another plausible interpretation is also possible: that NL AGNs occur in low-M-bulge galaxies and that in such galaxies M-bh/M-bulge is lower than that in galaxies with a higher M-bulge, if we consider that NL AGNs already have their "final" M-bh/M-bulge. More information of the bulge in NL AGNs is needed to clarify the black hole-bulge relation.
KeywordGalaxies : Active Galaxies : Bulges Galaxies : Nuclei Galaxies : Quasars Galaxies : Seyfert
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WOS IDWOS:000181441500011
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Cited Times:16[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Affiliation1.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
2.Nanjing Normal Univ, Dept Phys, Nanjing 210097, Peoples R China
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GB/T 7714
Bian, WH,Zhao, YH. Black hole-bulge relation for narrow-line objects[J]. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,2003,55(1):143-148.
APA Bian, WH,&Zhao, YH.(2003).Black hole-bulge relation for narrow-line objects.PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,55(1),143-148.
MLA Bian, WH,et al."Black hole-bulge relation for narrow-line objects".PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 55.1(2003):143-148.
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