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2000ApJ...528..186M - Astrophys. J., 528, 186-200 (2000/January-1)
Excitation mechanism of near-infrared [Fe II] emission in Seyfert and starburst galaxies.
MOURI H., KAWARA K. and TANIGUCHI Y.
Abstract (from CDS):
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] a6D9/2-a4D7/2 line at 1.257 µm.
Abstract Copyright: ∼
Journal keyword(s): Galaxies: Seyfert - Galaxies: Starburst - Line: Formation
Errata: erratum vol. 537, p. 1100 (2000)
Simbad objects: 60
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