There is observational evidence that broad-line regions （BLRs） exist in most active galactic nuclei （AGNs）, but their origin is still unclear. One scenario is that the BLRs originate from winds accelerated from th...There is observational evidence that broad-line regions （BLRs） exist in most active galactic nuclei （AGNs）, but their origin is still unclear. One scenario is that the BLRs originate from winds accelerated from the hot coronae of the disks, and the winds are suppressed when the black hole is accreting at low rates. This model predicts a relation between rh （m ~ /~f//~fEdd） and the FWHM of broad emission lines. We estimate the central black hole masses for a sample of bright AGNs by using their broad Hβ line-widths and optical luminosities. The dimensionless accretion rates rh = M/MEdd are derived from the optical continuum luminosities by using two different models： using an empirical relation between the bolometric luminosity Lbol and the optical luminosity （rh = Lbol/LEdd, a fixed radiative efficiency is adopted）; and calculating the optical spectra of accretion disks as a function of rh. We find a slgmficant correlation between the denved of and the observed line width of Hβ, FWHMα m^-0.aT, which almost overlaps the disk-corona model calculations, if the viscosity a α≈ 0.1 - 0.2 is adopted. Our results provide strong evidence for the physical link between the BLRs and accretion disks in AGNs.展开更多
We report on our research on the UV, optical line parameters and the infrared through UV to soft X-ray continuum parameters for a composite sample of narrow line and normal Seyfert 1 galaxies. The strong correlations ...We report on our research on the UV, optical line parameters and the infrared through UV to soft X-ray continuum parameters for a composite sample of narrow line and normal Seyfert 1 galaxies. The strong correlations among the line width of HB, optical line strength of Fell and the soft X-ray slope are confirmed. We found no correlations between the UV line parameters, the equivalent widths of Lya and CIV and their ratio on one hand and the optical line parameters on the other. The UV and X-ray luminosities strongly correlate with the line widths of HB and the Fe II/HB ratio. No significant correlation is found between the infrared-soft X-my continuum slope aix and the line width of HB.展开更多
In this paper,we discuss properties of SDSS J1042-0018 which is a broad line active galactic nucleus(AGN)but misclassified as an H II galaxy in the BPT diagram(SDSS J1042-0018 is called a misclassified broad line AGN)...In this paper,we discuss properties of SDSS J1042-0018 which is a broad line active galactic nucleus(AGN)but misclassified as an H II galaxy in the BPT diagram(SDSS J1042-0018 is called a misclassified broad line AGN).The emission lines around Hαand around Hβare well described by different model functions,considering broad Balmer lines to be described by Gaussian or Lorentz functions.Different model functions lead to different determined narrow emission line fiuxes,but the different narrow emission line fiux ratios lead SDSS J1042-0018 as an H II galaxy in the BPT diagram.In order to explain the unique properties of the misclassified broad line AGN SDSS J1042-0018,two methods are proposed,the star-forming contributions and the compressed narrow emission line regions with high electron densities near to critical densities of forbidden emission lines.Fortunately,the strong star-forming contributions can be preferred in SDSS J1042-0018.The misclassified broad line AGN SDSS J1042-0018,well explained by star-forming contributions,could provide further clues on the applications of BPT diagrams to the normal broad line AGNs.展开更多
With the support by the National Natural Science Foundation of China,a collaboration led by Prof.Wang Jianmin(王建民)from the Institute of High Energy Physics,Chinese Academy of Sciences proposes a new mechanism for t...With the support by the National Natural Science Foundation of China,a collaboration led by Prof.Wang Jianmin(王建民)from the Institute of High Energy Physics,Chinese Academy of Sciences proposes a new mechanism for the origin of the broad-line region in Active Galactic Nuclei,which was published展开更多
Since the unknown emission features in the spectrum of quasar 3C 273 have beenfirst identified as the blended Fell multiplets, many papers have contributed to thetheoretical and observation research of Fell emission i...Since the unknown emission features in the spectrum of quasar 3C 273 have beenfirst identified as the blended Fell multiplets, many papers have contributed to thetheoretical and observation research of Fell emission in the spectra of Seyferts andquasars. Usually, optical FeII emission lines are produced by transitions from展开更多
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 ...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 the BLR. It is suggested that this cutoff effect is physical background to explain the observations that high ionization lines in the spectra of AGNs have some systematic blue shifts relative to those low ionization lines which usually characterize their source system velocities.展开更多
The physics behind the spectral energy distribution （SED） of blazars remains open. We assembled 36 blazars to tackle the factors that control their SED. Now, many blazar spectra have the ＂double hump＂ feature in t...The physics behind the spectral energy distribution （SED） of blazars remains open. We assembled 36 blazars to tackle the factors that control their SED. Now, many blazar spectra have the ＂double hump＂ feature in the radio and far-IR frequencies. For these a parameter, △, is created to characterize the behavior of the SED. We found a significant correlation between the broad-line luminosity （LBLR） and △. Because L BLR is an indicator of the accreting power of the source in blazars, we derived a linear correlation, △ oc M1/3.18, which suggests that the SED of blazars may depend on the accretion rate, like that of BL Lac objects. We also found a significant correlation between m and △ for a sample of 11 blazars （out of one of 36） with available black hole masses. This implies the Eddington accretion ratio may influence the shape of the SED of blazars.展开更多
X-ray changing-look active galactic nuclei(CL AGNs) are a subpopulation of AGNs,whose lineof-sight column densities increase/decrease within several years.The physical mechanism for the variation of column density is ...X-ray changing-look active galactic nuclei(CL AGNs) are a subpopulation of AGNs,whose lineof-sight column densities increase/decrease within several years.The physical mechanism for the variation of column density is unclear.We reduce the X-ray data from XMM-Newton and Nu STAR observations for a CL AGN NGC 1365 with strong variation of column densities.The X-ray spectrum quickly softens as the X-ray luminosity increases and optical-to-X-ray spectral index also increases as increasing of optical luminosity.These results support that NGC 1365 also undergoes strong spectral evolution as that recently suggested for the optically selected CL AGNs with reappearance/disappearance of broad emission lines.Therefore,the variation of column density may be driven by the variable disk winds during the strong evolution of disk/corona.展开更多
基金Supported by the National Natural Science Foundation of China.
文摘There is observational evidence that broad-line regions （BLRs） exist in most active galactic nuclei （AGNs）, but their origin is still unclear. One scenario is that the BLRs originate from winds accelerated from the hot coronae of the disks, and the winds are suppressed when the black hole is accreting at low rates. This model predicts a relation between rh （m ~ /~f//~fEdd） and the FWHM of broad emission lines. We estimate the central black hole masses for a sample of bright AGNs by using their broad Hβ line-widths and optical luminosities. The dimensionless accretion rates rh = M/MEdd are derived from the optical continuum luminosities by using two different models： using an empirical relation between the bolometric luminosity Lbol and the optical luminosity （rh = Lbol/LEdd, a fixed radiative efficiency is adopted）; and calculating the optical spectra of accretion disks as a function of rh. We find a slgmficant correlation between the denved of and the observed line width of Hβ, FWHMα m^-0.aT, which almost overlaps the disk-corona model calculations, if the viscosity a α≈ 0.1 - 0.2 is adopted. Our results provide strong evidence for the physical link between the BLRs and accretion disks in AGNs.
基金the National Natural Science Foundationof China and Chinese Panden Project.
文摘We report on our research on the UV, optical line parameters and the infrared through UV to soft X-ray continuum parameters for a composite sample of narrow line and normal Seyfert 1 galaxies. The strong correlations among the line width of HB, optical line strength of Fell and the soft X-ray slope are confirmed. We found no correlations between the UV line parameters, the equivalent widths of Lya and CIV and their ratio on one hand and the optical line parameters on the other. The UV and X-ray luminosities strongly correlate with the line widths of HB and the Fe II/HB ratio. No significant correlation is found between the infrared-soft X-my continuum slope aix and the line width of HB.
基金the kind support of Starting Research Fund of Nanjing Normal Universitythe kind support of NSFC-12173020the kind support of Da Chuang project of Nanjing Normal University for undergraduate students。
文摘In this paper,we discuss properties of SDSS J1042-0018 which is a broad line active galactic nucleus(AGN)but misclassified as an H II galaxy in the BPT diagram(SDSS J1042-0018 is called a misclassified broad line AGN).The emission lines around Hαand around Hβare well described by different model functions,considering broad Balmer lines to be described by Gaussian or Lorentz functions.Different model functions lead to different determined narrow emission line fiuxes,but the different narrow emission line fiux ratios lead SDSS J1042-0018 as an H II galaxy in the BPT diagram.In order to explain the unique properties of the misclassified broad line AGN SDSS J1042-0018,two methods are proposed,the star-forming contributions and the compressed narrow emission line regions with high electron densities near to critical densities of forbidden emission lines.Fortunately,the strong star-forming contributions can be preferred in SDSS J1042-0018.The misclassified broad line AGN SDSS J1042-0018,well explained by star-forming contributions,could provide further clues on the applications of BPT diagrams to the normal broad line AGNs.
文摘With the support by the National Natural Science Foundation of China,a collaboration led by Prof.Wang Jianmin(王建民)from the Institute of High Energy Physics,Chinese Academy of Sciences proposes a new mechanism for the origin of the broad-line region in Active Galactic Nuclei,which was published
文摘Since the unknown emission features in the spectrum of quasar 3C 273 have beenfirst identified as the blended Fell multiplets, many papers have contributed to thetheoretical and observation research of Fell emission in the spectra of Seyferts andquasars. Usually, optical FeII emission lines are produced by transitions from
基金Project supported by Pangden Project FoundationNational Natural Science Foundation of China.
文摘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 the BLR. It is suggested that this cutoff effect is physical background to explain the observations that high ionization lines in the spectra of AGNs have some systematic blue shifts relative to those low ionization lines which usually characterize their source system velocities.
基金This work was supported by the Natural Science Foundation of Yunnan Province of China.
文摘The physics behind the spectral energy distribution （SED） of blazars remains open. We assembled 36 blazars to tackle the factors that control their SED. Now, many blazar spectra have the ＂double hump＂ feature in the radio and far-IR frequencies. For these a parameter, △, is created to characterize the behavior of the SED. We found a significant correlation between the broad-line luminosity （LBLR） and △. Because L BLR is an indicator of the accreting power of the source in blazars, we derived a linear correlation, △ oc M1/3.18, which suggests that the SED of blazars may depend on the accretion rate, like that of BL Lac objects. We also found a significant correlation between m and △ for a sample of 11 blazars （out of one of 36） with available black hole masses. This implies the Eddington accretion ratio may influence the shape of the SED of blazars.
基金support from the National Natural Science Foundation of China (NSFC,Grant No.U1931203)support from NSFC (Grant Nos.12025303,11890693 and 11421303)+3 种基金the CAS Frontier Science Key Research Program (QYZDJ-SSWSLH006)the K.C.Wong Education Foundation.Z.C.He is supported by NSFC (Grant No.11903031)USTC Research Funds of the Double First-Class Initiative YD 3440002001supported by NSF grant AST1907290。
文摘X-ray changing-look active galactic nuclei(CL AGNs) are a subpopulation of AGNs,whose lineof-sight column densities increase/decrease within several years.The physical mechanism for the variation of column density is unclear.We reduce the X-ray data from XMM-Newton and Nu STAR observations for a CL AGN NGC 1365 with strong variation of column densities.The X-ray spectrum quickly softens as the X-ray luminosity increases and optical-to-X-ray spectral index also increases as increasing of optical luminosity.These results support that NGC 1365 also undergoes strong spectral evolution as that recently suggested for the optically selected CL AGNs with reappearance/disappearance of broad emission lines.Therefore,the variation of column density may be driven by the variable disk winds during the strong evolution of disk/corona.
