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dc.contributor.authorBarth, A. J.
dc.contributor.authorSarzi, M.
dc.contributor.authorRix, H-W.
dc.contributor.authorHo, L. C.
dc.contributor.authorFilippenko, A.V.
dc.contributor.authorSargent, W.L.W.
dc.date.accessioned2013-07-03T15:02:10Z
dc.date.available2013-07-03T15:02:10Z
dc.date.issued2001-07-01
dc.identifier.citationBarth , A J , Sarzi , M , Rix , H-W , Ho , L C , Filippenko , A V & Sargent , W L W 2001 , ' Evidence for a Supermassive Black Hole in the S0 Galaxy NGC 3245 ' , The Astrophysical Journal , vol. 555 , no. 2 , pp. 685-708 . https://doi.org/10.1086/321523
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 646362
dc.identifier.otherPURE UUID: 35d4302f-c99a-49d5-8fb3-47b98ce96870
dc.identifier.otherBibtex: urn:af07b653645a8c84aaef88d0a678a4d1
dc.identifier.otherScopus: 0035838638
dc.identifier.urihttp://hdl.handle.net/2299/11077
dc.description.abstractThe S0 galaxy NGC 3245 contains a circumnuclear disk of ionized gas and dust with a radius of 1.1" (110 pc), making it an ideal target for dynamical studies with the Hubble Space Telescope (HST). We have obtained spectra of the nuclear disk with the Space Telescope Imaging Spectrograph, using a 0.2" wide slit at five parallel positions. Measurements of the Hα and [N II] emission lines are used to map out the kinematic structure of the disk in unprecedented detail. The data reveal a rotational velocity field with a steep velocity gradient across the innermost 0.4". We construct dynamical models for a thin gas disk in circular rotation, using HST optical images to map out the gravitational potential due to stars. Our modeling code includes the blurring due to the telescope point-spread function and the nonzero slit width, as well as the instrumental shift in measured wavelength for light entering the slit off-center, so as to simulate the data as closely as possible. The Hα+[N II] surface brightness measured from an HST narrowband image is folded into the models, and we demonstrate that many of the apparent small-scale irregularities in the observed velocity curves are the result of the patchy distribution of emission-line surface brightness. Over most of the disk, the models are able to fit the observed radial velocity curves closely, although there are localized regions within the disk that appear to be kinematically disturbed relative to the overall rotational pattern. The velocity dispersion of [N II] λ6584 rises from σ~50 km/s in the outer disk to ~160 km/s at the nucleus, and most of this line width cannot be attributed to rotational or instrumental broadening. To account for the possible dynamical effect of the intrinsic velocity dispersion in the gas, we also calculate models that include a correction for asymmetric drift. This correction increases the derived black hole mass by 12% but leads to slightly poorer fits to the data. A central dark mass of (2.1+/-0.5)×10^8 Msolar is required for the models to reproduce the steep central velocity gradient. This value for the central mass is consistent with recently discovered correlations between black hole mass and bulge velocity dispersion.en
dc.format.extent24
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subjectBlack Hole Physics, Galaxies: Elliptical and Lenticular, cD, galaxies: individual (NGC 3245), Galaxies: Kinematics and Dynamics, Galaxies: Nuclei
dc.titleEvidence for a Supermassive Black Hole in the S0 Galaxy NGC 3245en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1086/321523
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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