Show simple item record

dc.contributor.authorWilliams, D. R. A.
dc.contributor.authorMcHardy, I. M.
dc.contributor.authorBaldi, R. D.
dc.contributor.authorBeswick, R. J.
dc.contributor.authorArgo, M. K.
dc.contributor.authorDullo, B. T.
dc.contributor.authorKnapen, J. H.
dc.contributor.authorBrinks, E.
dc.contributor.authorFenech, D. M.
dc.contributor.authorMundell, C.G.
dc.contributor.authorMuxlow, T.W.B.
dc.contributor.authorPanessa, F.
dc.contributor.authorRampadarath, H.
dc.contributor.authorWestcott, J.
dc.date.accessioned2018-09-22T09:11:49Z
dc.date.available2018-09-22T09:11:49Z
dc.date.issued2017-12-21
dc.identifier.citationWilliams , 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.issn1745-3925
dc.identifier.otherPURE: 12381505
dc.identifier.otherPURE UUID: f030d6da-6343-487f-ac4b-53edb10516e4
dc.identifier.otherArXiv: http://arxiv.org/abs/1708.07011v1
dc.identifier.otherScopus: 85030685935
dc.identifier.otherORCID: /0000-0002-7758-9699/work/54143427
dc.identifier.urihttp://hdl.handle.net/2299/20632
dc.descriptionThis 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.abstractWe 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.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society: Letters
dc.rightsOpen
dc.subjectastro-ph.GA
dc.titleRadio jets in NGC 4151 where eMERLIN meets HSTen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2017-12-21
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stx2205
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record