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.
@article{arxiv.astro-ph/0203236,
title = {The origin of [Fe II] emission in NGC 4151},
author = {James E. H. Turner and Jeremy Allington-Smith and Scott Chapman and Robert Content and Christine Done and Roger Haynes and David Lee and Simon Morris},
journal= {arXiv preprint arXiv:astro-ph/0203236},
year = {2009}
}
Comments
10 pages, 8 figures, accepted for publication in MNRAS