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dc.contributor.authorCinzano, P.
dc.contributor.authorRix, H-W.
dc.contributor.authorSarzi, M.
dc.contributor.authorCorsini, E.M.
dc.contributor.authorZeilinger, W.W.
dc.contributor.authorBertola, F.
dc.date.accessioned2007-12-03T11:41:38Z
dc.date.available2007-12-03T11:41:38Z
dc.date.issued1999
dc.identifier.citationCinzano , P , Rix , H-W , Sarzi , M , Corsini , E M , Zeilinger , W W & Bertola , F 1999 , ' The kinematics and the origin of the ionized gas in NGC 4036 ' , Monthly Notices of the Royal Astronomical Society , vol. 307 , no. 2 , pp. 433448 . https://doi.org/10.1046/j.1365-8711.1999.02617.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 182070
dc.identifier.otherPURE UUID: 08308269-4a77-47f3-8a1c-86d819208401
dc.identifier.otherdspace: 2299/1140
dc.identifier.otherScopus: 0000549460
dc.identifier.urihttp://hdl.handle.net/2299/1140
dc.descriptionThe definitive version is available at www.blackwell-synergy.com. Copyright Blackwell Publishing DOI : 10.1046/j.1365-8711.1999.02617.x
dc.description.abstractWe present the kinematics and photometry of the stars and of the ionized gas near the centre of the S0 galaxy NGC4036. Dynamical models based on the Jeans Equation have been constructed from the stellar data to determine the gravitational potential in which the ionized gas is expected to orbit. Inside 10′′, the observed gas rotation curve falls well short of the predicted circular velocity. Over a comparable radial region the observed gas velocity dispersion is far higher than the one expected from thermal motions or small scale turbulence, corroborating that the gas cannot be following the streamlines of nearly closed orbits. We explore several avenues to understand the dynamical state of the gas: (1) We treat the gas as a collisionless ensemble of cloudlets and apply the Jeans Equation to it; this modeling shows that inside 4′′ the gas velocity dispersion is just high enough to explain quantitatively the absence of rotation. (2) Alternatively, we explore whether the gas may arise from the ‘just shed’ mass-loss envelopes of the bulge stars, in which case their kinematics should simply mimic that of the stars. he latter approach matches the data better than (1), but still fails to explain the low velocity dispersion and slow rotation velocity of the gas for 5′′ < r < 10′′. (3) Finally, we explore, whether drag forces on the ionized gas may aid in explaining its peculiar kinematics.While all these approaches provide a much better description of the data than cold gas on closed orbits, we do not yet have a definitive model to describe the observed gas kinematics at all radii. We outline observational tests to understand the enigmatic nature of the ionized gas.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.titleThe kinematics and the origin of the ionized gas in NGC 4036en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted1999
rioxxterms.versionofrecordhttps://doi.org/10.1046/j.1365-8711.1999.02617.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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