The Mass Of The Super-large Black Hole In The Active Galactic Nucleus Of The Response Map Sample

Active galactic nuclei(AGNs)are the most luminous and active objects in the uni-verse.It’s powered by accretion onto the central super massive black holes(SMBHs).Mass and spin are the primary parameters of the SMBH.The reliable measurement of black hole mass will clarify the physics of AGN and the roles of formation and evolution in galaxy.The reverberation mapping method(RM)can be used to measure the Broad-line region(BLR)size(RBLR(Hβ)),therefore can be used to calculate the black hole mass.Using a compiled sample of 120 Broad-line AGNs with mea-sured Hβtime lags from RM method.And a subsample consist with 36 low redshift broad-line AGNs(z<0.1 except PG 1617+175)with reliable measured stellar veloc-ity dispersion σ*.The calculation method of the SMBH masses(MBH)in AGN and the empirical size luminosity(RBLR-L5100)relation have been investigated.The first chapter introduces the research background,including the overview of AGN,the properties of the BLR,the RM method,RBLR-L5100 relation and the calculation method of MBH.The second chapter briefly describes our RM sample,the weighted average method and the multiple linear regression technique.In the third chapter.Considering the intrinsic scatter in the MBH-σ*relation for AGNs,for four kinds of tracers(i.e.FWHMmean,(σHβ,mean,FWHMrms,σHβ,rms)of BLR clouds velocity from the Hβline profile measured from the mean or rms spectrum,the multivariate linear regression technique is used to calibrate the mean values of the virial factors(fF,mean,fσ,mean,fF,rms,fσ,rms),as well as the FWHM-dependent factor fc.MBH from different kinds of velocity tracers and the corresponding virial factors are compared with that from σ*or σHβ,rms(the assumed best BLR clouds velocity tracer).In the fourth chapter.Dependence of the RBLR(Hβ)on the l44 and the M are investigated.Using the observational parameters RFe(the ratio of optical Fe Ⅱto Hβline flux)and DHβ(DHβ＝FWHM(Hβ)/(σHβ)to substitute M,the extended empirical RBLR-L5100 relations are presented.The origin and scatter of the RBLR-L5100 relation is discussed.The fifth chapter is the outlook.The main results can be summarized as follows:(1)Considering the intrinsic scatter in the MBH-σ*relation for AGNs,the mul-tivariate linear regression technique is used to calibrate the mean value of the virial factors,as well as the FWHM-depended factor fc.The calibrations of the factor f are fF,mean=1.12±0.17,fF,rms=1.51±0.20,fσ,mean=5.50±0.74,fσ,rms=6.61±0.81 and fc∝ FWHMmean-1.10±0.40(2)Using the a*and 4 kinds of tracers of BLR clouds velocity,the MBH are calculated.With respect to the Hβ FWHM,we prefer the line dispersion to calculate MBH·Using the FWHM-depended factor fc,we can improve MBH calculation from the Hβ FWHM and the mean factor fF,mean,with decreased offset rms respect to the other method(the MBH calculated from σ*or σHβ,rms).(3)Including the effect of M,the bivariate correlation of RBLR with L5100 and M are presented.Substituting observational parameter of RFe or DHβ for M,extend-ed empirical RBLR-L5100 relations are found,RFe is a better "fix" for the RBLR-L5100 offset than the DHβ.The best relation is log RBLR＝(0.42 ± 0.03)logl44—(0.28±0.04)RFe+(1.53 ± 0.08)ltd,with an intrinsic scatter of 0.23 dex.The extended em-pirical RBLR-L5100 relation including RFe can be used to calculate RBLR,and thus the single-epoch SMBH mass MBH.