| dc.contributor.author | Turner, James E. H. | en_US |
| dc.contributor.author | Allington-Smith, Jeremy | en_US |
| dc.contributor.author | Chapman, Scott | en_US |
| dc.contributor.author | Content, Robert | en_US |
| dc.contributor.author | Done, Christine | en_US |
| dc.contributor.author | Haynes, Roger | en_US |
| dc.contributor.author | Lee, David | en_US |
| dc.contributor.author | Morris, Simon | en_US |
| dc.date.accessioned | 2014-03-12T19:21:03Z | |
| dc.date.available | 2014-03-12T19:21:03Z | |
| dc.date.issued | 2002-03 | en_US |
| dc.identifier.citation | Turner, James E. H., Jeremy Allington-Smith, Scott Chapman, Robert Content, et al. 2002. "The origin of [Fe II] emission in NGC 4151." Monthly Notices of the Royal Astronomical Society 331(2): 284-292 | en_US |
| dc.identifier.issn | 0035-8711 | en_US |
| dc.identifier.uri | http://dx.doi.org/10.1046/j.1365-8711.2002.05214.x | en_US |
| dc.identifier.uri | http://hdl.handle.net/10222/45454 | |
| dc.description.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. | en_US |
| dc.title | The origin of [Fe II] emission in NGC 4151 | en_US |
| dc.title.alternative | Monthly Notices of the Royal Astronomical Society | en_US |
| dc.type | article | en_US |
| dc.identifier.volume | 331 | en_US |
| dc.identifier.issue | 2 | en_US |
| dc.identifier.startpage | 284 | en_US |
