dc.contributor.author Williams, D. R. A. dc.contributor.author McHardy, I. M. dc.contributor.author Baldi, R. D. dc.contributor.author Beswick, R. J. dc.contributor.author Argo, M. K. dc.contributor.author Dullo, B. T. dc.contributor.author Knapen, J. H. dc.contributor.author Brinks, E. dc.contributor.author Fenech, D. M. dc.contributor.author Mundell, C.G. dc.contributor.author Muxlow, T.W.B. dc.contributor.author Panessa, F. dc.contributor.author Rampadarath, H. dc.contributor.author Westcott, J. dc.date.accessioned 2018-09-22T09:11:49Z dc.date.available 2018-09-22T09:11:49Z dc.date.issued 2017-12-21 dc.identifier.citation Williams , D R A , McHardy , I M , Baldi , R D , Beswick , R J , Argo , M K , Dullo , B T , Knapen , J H , Brinks , E , Fenech , D M , Mundell , C G , Muxlow , T W B , Panessa , F , Rampadarath , H & Westcott , J 2017 , ' Radio jets in NGC 4151 where eMERLIN meets HST ' , Monthly Notices of the Royal Astronomical Society: Letters , vol. 472 , no. 4 , pp. 3842–3853 . https://doi.org/10.1093/mnras/stx2205 dc.identifier.issn 1745-3925 dc.identifier.other PURE: 12381505 dc.identifier.other PURE UUID: f030d6da-6343-487f-ac4b-53edb10516e4 dc.identifier.other ArXiv: http://arxiv.org/abs/1708.07011v1 dc.identifier.other Scopus: 85030685935 dc.identifier.other ORCID: /0000-0002-7758-9699/work/54143427 dc.identifier.uri http://hdl.handle.net/2299/20632 dc.description This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society: Letters ©: 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. dc.description.abstract We present high-sensitivity eMERLIN radio images of the Seyfert galaxy NGC 4151 at 1.5 GHz. We compare the new eMERLIN images to those from archival MERLIN observations in 1993 to determine the change in jet morphology in the 22 years between observations. We report an increase by almost a factor of 2 in the peak flux density of the central core component, C4, thought to host the black hole, but a probable decrease in some other components, possibly due to adiabatic expansion. The core flux increase indicates an AGN which is currently active and feeding the jet. We detect no significant motion in 22 years between C4 and the component C3, which is unresolved in the eMERLIN image. We present a spectral index image made within the 512 MHz band of the 1.5 GHz observations. The spectrum of the core, C4, is flatter than that of other components further out in the jet. We use HST emission line images (H$\alpha$, [O III] and [O II]) to study the connection between the jet and the emission line region. Based on the changing emission line ratios away from the core and comparison with the eMERLIN radio jet, we conclude that photoionisation from the central AGN is responsible for the observed emission line properties further than 4" (360 pc) from the core, C4. Within this region, several evidences (radio-line co-spatiality, low [O III]/H$\alpha$ and estimated fast shocks) suggest additional ionisation from the jet. en dc.language.iso eng dc.relation.ispartof Monthly Notices of the Royal Astronomical Society: Letters dc.rights Open dc.subject astro-ph.GA dc.title Radio jets in NGC 4151 where eMERLIN meets HST en dc.contributor.institution School of Physics, Astronomy and Mathematics dc.contributor.institution Centre for Astrophysics Research dc.description.status Peer reviewed dc.description.versiontype Final Published version dcterms.dateAccepted 2017-12-21 rioxxterms.version VoR rioxxterms.versionofrecord https://doi.org/10.1093/mnras/stx2205 rioxxterms.type Journal Article/Review herts.preservation.rarelyaccessed true herts.rights.accesstype Open
﻿