Diagnostics for the structure of AGNs'broad line regions with reverberation mapping data:confirmation of the two-component broad line region model

We re-examine the ten Reverberation Mapping(RM) sources with public data based on the two-component model of the Broad Line Region(BLR).In fitting their broad Hβ Mlines,six of them only need one Gaussian component,one of them has a double-peak profile,one has an irregular profile,and only two of them need two components,i.e.,a Very Broad Gaussian Component(VBGC) and an Inter-Mediate Gaussian Component(IMGC).The Gaussian components are assumed to come from two distinct regions in the two-component model;they are the Very Broad Line Region(VBLR) and the Inter-Mediate Line region(IMLR).The two sources with a two-component profile are Mrk 509 and NGC 4051.The time lags of the two components of both sources satisfy tIMLR/tVBLR=V 2VBLR/V 2IMLR,where tIMLR and tVBLR are the lags of the two components while VIMLR and VVBLR represent the mean gas velocities of the two regions,supporting the two-component model of the BLR of Active Galactic Nuclei(AGNs).The fact that most of these ten sources only have the VBGC confirms the assumption that RM mainly measures the radius of the VBLR;consequently,the radius obtained from the R-L relationship mainly represents the radius of VBLR.Moreover,NGC 4051,with a lag of about 5 days in the one component model,is an outlier on the R-L relationship as shown in Kaspi et al.(2005);however this problem disappears in our two-component model with lags of about 2 and 6 days for the VBGC and IMGC,respectively.

The correlation between the Doppler factor and broad line region luminosity in blazars

The disk-jet symbiosis is a fundamental problem in our understanding of the Active Galactic Nuclei(AGN).We explore the relation between the Doppler factors of the jet of blazars and their broad line region luminosity LBLR.Since different methods measuring might differ substantially,we use data obtained from 3 independent methods and compile 3 samples of sources for each of them,respectively.Two samples consist of blazars,that is,Flat Spectrum Radio Quasars(FSRQs) and BL Lacertae objects(BL Lacs),and the other consists of BL Lacs.is one of the most important jet properties and LBLR is thought to be the proxy of the accretion power.Correlation analysis to these samples shows that there exists a significant correlation between and LBLR,which supports the idea that the jet powering process is closely linked with the accretion process and provides new evidence for disk-jet connection.Furthermore,the results are consistent with the idea that the Blandford-Znajek mechanism is sufficient for BL Lacs and a hybrid model is needed for FSRQs.

Line profiles of the two-phase medium broad-line region in active galactic nuclei

In the framework of BLR in AGNs, i.e. large number of small, cold and dense emission-line clouds immerging in an intercloud hot medium, a delicate radiation model for a typical emission cloud is established, in which the backside photoionization of the cloud against the central continuum source by the scattered diffuse continuum in the hot medium is considered. Under the assumption of the radial kinematics of the BLR clouds, the line profiles for the two important UV emission-lines, Lya and CIV/11549 are computed; and based on these calculations, various physical factors that affect the properties of the emission-line profiles are discussed. It is concluded that: (i) when the BLR clouds is inflow, there exists a confining hot medium with density around 2 x 105 cm-3. In this case, theoretical line profiles agree well with the observational; (ii) both symmetric Lya and nearly symmetric CIV line profiles show blue velocity shifts, the quantities of which are sensitive to the cutoff of the outer radius of

浅析近红外光度与宽线区光度的关系

研究了69个平谱射电类星体(Flat Spectrum Radio Quasars)的近红外射线光度与宽线区光度之间的关系,发现它们之间存在较强的相关性。在排除了红移的影响后,两者的相关性变的非常微弱。这表明平谱射电类星体的近红外辐射与宽线区辐射可能具有不同的物理辐射机制。还讨论了近红外光度与中心超大质量黑洞质量之间的相关性。

Kinematic Models of BLR Gas and Line Profiles of HeIλ5876 and Hβ in AGNs

The present paper derives the modified expression of broad emission line profiles for the kinematic model of radiation pressure driving BLR gas outflow in the BLR, and discusses the intrinsic emission difference between the two lines HeIλ5876 and Hβ. It is shown that the fact that the observed line width of HeIλ5876 is broader than that of Hβ cannot be explained by W. G. Mathews’ modified model. For comparison, line profiles of gravitational infall model and orbital disk model are also calculated; the latter is in good agreement with the observations. Thereupon, conclusion is reached that gravitational infall is an important process in the BLR gas motion.