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The origin of [Fe II] emission in NGC 4151

James E. H. Turner·Jeremy Allington-Smith·Scott Chapman·Robert Content·Christine Done·Roger Haynes·David Lee·Simon Morris
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Abstract

The centre of NGC 4151 has been observed in the J-band with the SMIRFS integral field unit (IFU) on the UK Infrared Telescope. A map of [Fe II] emission is derived, and compared with the distributions of the optical narrow line region and radio jet. We conclude that, because the [Fe II] emission is associated more closely with the visible narrow-line region than with the radio jet, it arises mainly through photoionization of gas by collimated X-rays from the Seyfert nucleus. The velocity field and strength with respect to [Pa B] are found to be consistent with this argument. The performance of the IFU is considered briefly, and techniques for observation and data analysis are discussed.

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James E. H. Turner, Jeremy Allington-Smith, Scott Chapman, Robert Content, Christine Done, Roger Haynes, David Lee, Simon Morris. 2002-03-14. The origin of [Fe II] emission in NGC 4151. https://doi.org/10.1046/j.1365-8711.2002.05214.x

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