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dc.contributor.authorKraft, R.P.
dc.contributor.authorForman, W.R.
dc.contributor.authorJones, C.
dc.contributor.authorNulsen, P.E.J.
dc.contributor.authorHardcastle, M.J.
dc.contributor.authorRaychaudhury, S.
dc.contributor.authorEvans, D.A.
dc.contributor.authorSivakoff, G.R.
dc.contributor.authorSarazin, C.L.
dc.identifier.citationKraft , R P , Forman , W R , Jones , C , Nulsen , P E J , Hardcastle , M J , Raychaudhury , S , Evans , D A , Sivakoff , G R & Sarazin , C L 2011 , ' The gas dynamics of NGC 4472 revealed by XMM-Newton ' , The Astrophysical Journal , vol. 727 , no. 1 , pp. 41-54 .
dc.identifier.otherPURE: 158619
dc.identifier.otherPURE UUID: f65f9be7-d6f6-4af1-8ebd-20d1c0122420
dc.identifier.otherdspace: 2299/5479
dc.identifier.otherScopus: 84891228652
dc.description‘In these times, during the rise in the popularity of institutional repositories, the Society does not forbid authors from depositing their work in such repositories. However, the AAS regards the deposit of scholarly work in such repositories to be a decision of the individual scholar, as long as the individual's actions respect the diligence of the journals and their reviewers.’ Original article can be found at: Copyright American Astronomical Society [Full text of article not available in the UHRA]
dc.description.abstractWe present results from a 100 ks XMM-Newton observation of the hot gas in the Virgo cluster elliptical galaxy NGC 4472. We find a surface brightness discontinuity ∼21 kpc north of the nucleus, consistent with being a contact discontinuity between two moving fluids. We also detect a >60 kpc long ram-pressure stripped tail. The pressure across the discontinuity implies an infall velocity, vinfall, of 1000 km s-1 < vinfall <2200 km s-1 depending on what assumptions are made about the density and pressure of the external gas. We suggest that the NGC 4472 group is falling into a collapsing filament, which is itself falling into the Virgo cluster. The gas of a collapsing filament is rapidly decelerated as it crosses the standoff shock, but the apparent high velocity of infall for NGC 4472 could be simply due to the fact that the gravitating potential of the NGC 4472 group is unaffected by this shock. While the group falls through the shock its gas will be stripped as it passes through the stalled gas of the filament. Additionally, we find two sets of cool filamentary arms to the east and the southwest of the nucleus. One of the southwest arms is coincident with a sharp filament seen with Chandra. We interpret these arms as filaments of cool gas that have been driven out from the center of the galaxy by the buoyant evolution of a radio bubble. The age of this outburst is ∼108 yr assuming that the buoyant bubble rises with a velocity of ∼0.4cs = 200 km s -1; the energy of the outburst is a modest ∼2 × 10 56 erg.en
dc.relation.ispartofThe Astrophysical Journal
dc.subjectgalaxies: individual (NGC 4472)
dc.subjectgalaxies: jets
dc.subjectx-rays: galaxies
dc.titleThe gas dynamics of NGC 4472 revealed by XMM-Newtonen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review

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