Open AccessThe origin of [Fe ii ] emission in NGC 4151
Author(s) -
Turner James E. H.,
AllingtonSmith Jeremy,
Chapman Scott,
Content Robert,
Done Christine,
Haynes Roger,
Lee David,
Morris Simon
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05214.x
Subject(s) - physics , astrophysics , photoionization , jet (fluid) , collimated light , line (geometry) , telescope , emission spectrum , infrared , astronomy , h alpha , optics , spectral line , ionization , laser , ion , geometry , mathematics , quantum mechanics , thermodynamics
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 β 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.