Extended High-Ionization Nuclear Emission-Line Region in the Seyfert Galaxy NGC 4051

Details Extended High-Ionization Nuclear Emission-Line Region in the Seyfert Galaxy NGC 4051 Extended High-Ionization Nuclear Emission-Line Region in the Seyfert Galaxy NGC 4051

1999-10-15

arxiv.org/abs/astro-ph/9910285v1

Astronomy and Astrophysics

Astrophysics

16 pages, including figures. To Appear in the Astronomical Journal February 2000 Issue

Scientific paper

10.1086/301219

We present an optical spectroscopic analysis of the well-known Seyfert galaxy NGC 4051. The high-ionization nuclear emission-line region (HINER) traced by [Fe X]6374 is found to be spatially extended to a radius of 3a rcseconds (150 pc) west and southwest from the nucleus; NGC 4051 is the third example which has an extended HINER. The nuclear spectrum shows that the flux of [Fe X]6374 is stronger than that of [Fe VII] 6087 in our observation. This property cannot be interpreted in terms of a simple one-zone photoionization model. In order to understand what happens in the nuclear region in NGC 4051, we investigate the physical condition of the nuclear emission-line region in detail using new photoionization models in which the following three emission-line components are taken into account; (1) optically thick, ionization-bounded clouds; (2) optically thin, matter-bounded clouds; and (3) a contamination component which emits H$\alpha$ and H$\beta$ lines. Here the observed extended HINER is considered to be associated with the low-density, matter-bounded clouds. Candidates of the contamination component are either the broad-line region (BLR) or nuclear star forming regions or both. The complexity of the excitation condition found in NGC 4051 can be consistently understood if we take account of these contamination components.

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