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dc.contributor.authorKraft, R.P.
dc.contributor.authorHardcastle, M.J.
dc.contributor.authorSivakoff, G.R.
dc.contributor.authorJordan, A.
dc.contributor.authorNulsen, P.E.J.
dc.contributor.authorBirkinshaw, M.
dc.contributor.authorForman, W.R.
dc.contributor.authorJones, C.
dc.contributor.authorWorrall, D.M.
dc.contributor.authorCroston, J.H.
dc.contributor.authorEvans, D.A.
dc.contributor.authorRaychaudhury, S.
dc.contributor.authorMurray, S.S.
dc.contributor.authorBrassington, Nicola
dc.contributor.authorGoodger, Joanna
dc.contributor.authorHarris, W.E.
dc.contributor.authorJuett, A.M.
dc.contributor.authorSarazin, C.L.
dc.contributor.authorWoodley, K.A.
dc.identifier.citationKraft , R P , Hardcastle , M J , Sivakoff , G R , Jordan , A , Nulsen , P E J , Birkinshaw , M , Forman , W R , Jones , C , Worrall , D M , Croston , J H , Evans , D A , Raychaudhury , S , Murray , S S , Brassington , N , Goodger , J , Harris , W E , Juett , A M , Sarazin , C L & Woodley , K A 2008 , ' Evidence for Non-Hydrostatic Gas Motions in the Hot Interstellar Medium of Centaurus A ' , The Astrophysical Journal , vol. 677 , pp. L97-L100 .
dc.identifier.otherPURE: 164119
dc.identifier.otherPURE UUID: 8c6f2277-1fe9-40f9-90f3-c24954d0bdb9
dc.identifier.otherdspace: 2299/2748
dc.identifier.otherScopus: 62549100593
dc.descriptionOriginal article can be found at: Copyright American Astronomical Society DOI: 10.1086/588023 [Full text of this article is not available in the UHRA]
dc.description.abstractWe present preliminary results from a deep (600 ks) Chandra observation of the hot interstellar medium of the nearby early-type galaxy Centaurus A. We find a surface brightness discontinuity in the gas ~3.5 kpc from the nucleus spanning a 120° arc. The temperature of the gas is 0.60 ± 0.05 keV (0.68 ± 0.10 keV) interior (exterior) to the discontinuity. The elemental abundance is poorly constrained by the spectral fits, but if the abundance is constant across the discontinuity, there is a factor of 2.3 ± 0.4 pressure jump across the discontinuity. This would imply that the gas is moving at 470 ± 100 km s−1, or Mach 1.0 ± 0.2 (1.2 ± 0.2) relative to the sound speed of the gas external (internal) to the discontinuity. Alternatively, pressure balance could be maintained if there is a large (factor of ~7) discontinuity in the elemental abundance. We suggest that the observed discontinuity is the result of nonhydrostatic motion of the gas core (i.e., sloshing) due to the recent merger. In this situation, both gas motions and abundance gradients are important in the visibility of the discontinuity. Cen A is in the late stages of merging with a small late-type galaxy, and a large discontinuity in density and abundance across a short distance demonstrates that the gas of the two galaxies remains poorly mixed, even several hundred million years after the merger. The pressure discontinuity may have had a profound influence on the temporal evolution of the kiloparsec-scale jet. The jet could have decollimated, crossing the discontinuity and thereby forming the northeast radio lobe.en
dc.relation.ispartofThe Astrophysical Journal
dc.titleEvidence for Non-Hydrostatic Gas Motions in the Hot Interstellar Medium of Centaurus Aen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSPECS Deans Group
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review

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