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Date and Time of the Query: 2019-08-18 T02:48:33 PDT
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For refcode 1993ApJ...413L..15I:
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1993ApJ...413L..15I THE X-RAY BALDWIN EFFECT KAZUSHI IWASAWA Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-01, Japan AND YOSHIAKI TANIGUCHI Astronomical Institute, Tohoku University, Aoba, Sendai 980, Japan Received 1993 March 15; accepted 1993 May 25 ABSTRACT Using the X-ray data of active galactic nuclei (type 1 Seyfert galaxies and quasars) obtained by the X-ray satellite Ginga, we have found that the equivalent width of the Fe K emission line at 6.4 keV, EW(Fe K), is inversely correlated with the X-ray luminosity in the 2-10 keV band. This inverse correlation is basically similar to the well-known relation known as the "Baldwin effect," which means that the equivalent width of the C IV {lambda}1550 emission line is inversely correlated with the UV continuum luminosity (Baldwin 1977). Hence, we may call our finding "the X-ray Baldwin effect." The X-ray Baldwin effect is pronounced for type 1 Seyfert galaxies. The obtained correlation, EW(Fe K) is proportional to L_x_(2-10 keV)^-0.20+/-0.03, is quite similar to those of the original Baldwin effects for type 1 Seyfert galaxies and quasars, implying that the Fe K emission mainly comes from the broad-line regions or from the regions whose geometrical configurations are nearly the same as those of broad-line regions. Subject headings: galaxies: Seyfert - quasars: emission lines - X-rays: galaxies
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