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Date and Time of the Query: 2019-08-20 T12:32:37 PDT
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For refcode 2000ApJ...528..186M:
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2000ApJ...528..186M Excitation Mechanism of Near-Infrared [Fe II] Emission in Seyfert and Starburst Galaxies Hideaki Mouri Meteorological Research Institute, Nagamine 1-1, Tsukuba 305-0052, Japan; hmouri@mri-jma.go.jp Kimiaki Kawara Institute of Astronomy, University of Tokyo, Mitaka, Tokyo 181-8588, Japan and Yoshiaki Taniguchi Astronomical Institute, School of Science, Tohoku University, Aoba, Sendai 980-8578, Japan Received 1999 January 19; accepted 1999 August 10 ABSTRACT The excitation mechanism of near-infrared [Fe II] emission in Seyfert and starburst galaxies is studied. We carry out numerical calculations for photoionization and shock heating, and compare the results with the observational data. The gas-phase abundance of iron is found to be always low. This means that destruction of iron-bearing grains is insufficient to affect the [Fe II] strength. We propose that the [Fe II] strength depends primarily on the ionization structure. The [Fe II] emission is excited by electron collisions in a zone of partially ionized hydrogen, which is extensive when the gas is heated by X-rays or by a shock. These two processes are discriminated by the electron temperature of the [Fe II] region: 8000 K in heating by X-rays, and 6000 K in shock heating. The [Fe II] emission of a Seyfert galaxy originates in the narrow-line region, which is heated by X-rays from the nucleus and by shocks due to the nuclear outflow. From the [Fe II] temperature, we propose that the heating by X-rays is more important. On the other hand, the [Fe II] emission of a starburst galaxy originates in the supernova-driven shocks. We find that 0.2% of the shock energy is transferred into the [Fe II] a^6^D_9/2_- a^4^D_7/2_ line at 1.257 microns. Subject headings: galaxies: Seyfert-galaxies: starburst-line: formation ====================================================================== 2000ApJ...537.1100M Erratum In the paper "Excitation Mechanism of Near-Infrared [Fe II] Emission in Seyfert and Starburst Galaxies" by Hideaki Mouri, Kimiaki Kawara and Yoshiaki Taniguchi (ApJ 528, 186 [2000]), the two panels of Figure 6 were printed in two different sizes, as the result of an error in the printing process. The correct version of Figure 6 appears below. See Journal. ========================================================================
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