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Date and Time of the Query: 2019-08-18 T01:52:52 PDT
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For refcode 1999AJ....118.2658S:
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Copyright by American Astronomical Society. Reproduced by permission
1999AJ....118.2658S A LINK BETWEEN THE H{beta} EQUIVALENT WIDTH, PROFILE WIDTH, BLR SIZE, AND OPTICAL LUMINOSITY FROM A SMALL SAMPLE OF WELL-STUDIED ACTIVE GALACTIC NUCLEI S. G. SERGEEV, V. I. PRONIK, AND E. A. SERGEEVA Crimean Astrophysical Observatory, Nauchny, 334413 Crimea, Ukraine and Isaac Newton Institute of Chile, Crimean Branch AND YU. F. MALKOV Crimean Astrophysical Observatory, Nauchny, 334413 Crimea, Ukraine Received 1999 April 15; accepted 1999 August 12 ABSTRACT We present diagrams of the relationship between the broad H{beta} emission-line parameters and the continuum luminosity obtained from a sample of 31 well-studied Seyfert 1.0-1.5 galaxies and quasars. The equivalent width of the H{beta} line is inversely correlated with the continuum luminosity at 5100 E as EW ~ L_5100_^-0.047+-/0.038, which seems to be comparable to that obtained by other authors for the Ly{alpha}. So, we have detected, although very marginally, a Baldwin effect in the H{beta} line. The remarkably small scattering of the H{beta} equivalent widths probably indicates approximately the same spectral energy distribution from optics to ionizing radiation, nearly the same covering factor, and nearly isotropic continuum emission, although some of these agents can show small systematic changes with luminosity. The intrinsic Baldwin effect for the H {beta} is clearly seen only in NGC 5548. Considering the observed lag- luminosity and lag-line-width dependences we suppose that it might be caused by full ionization of clouds. We compute the linear regression parameters (the slopes and intercepts) of the relationship between the H{beta} and optical continuum fluxes. In some cases, the regression parameters derived from the homogeneous data sets are significantly different for different observational periods. The lag of the H{beta} response to continuum variations shows a strong correlation with the luminosity. Combining the regression results on time delay and rms widths of the H{beta} line, we obtained the following mass-luminosity relationship for AGNs: L is proportional to M^1.9+/-1.1^. Key words: galaxies: active-galaxies: nuclei-galaxies:Seyfert-quasars: emission lines
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