Show simple item record

dc.contributor.authorWalsh, J.L.
dc.contributor.authorBarth, A.
dc.contributor.authorSarzi, M.
dc.date.accessioned2010-10-19T14:55:04Z
dc.date.available2010-10-19T14:55:04Z
dc.date.issued2010
dc.identifier.citationWalsh , J L , Barth , A & Sarzi , M 2010 , ' The supermassive black hole in M84 revisited ' , The Astrophysical journal , vol. 721 , no. 1 , pp. 762-776 . https://doi.org/10.1088/0004-637X/721/1/762
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 181166
dc.identifier.otherPURE UUID: 0ece8bfa-6a5d-499d-8e39-33526c08ff8c
dc.identifier.otherdspace: 2299/4905
dc.identifier.otherScopus: 78149247505
dc.identifier.urihttp://hdl.handle.net/2299/4905
dc.descriptionOriginal article can be found at: http://iopscience.iop.org/0004-637X/ Copyright American Astronomical Society [Full text of this paper is not available in the UHRA]
dc.description.abstractThe mass of the central black hole in the giant elliptical galaxy M84 has previously been measured by two groups using the same observations of emission-line gas with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope, giving strongly discrepant results: Bower et al. found M BH = (1.5+1.1 –0.6) × 109 M , while Maciejewski & Binney estimated M BH = 4 × 108 M . In order to resolve this discrepancy, we have performed new measurements of the gas kinematics in M84 from the same archival data and carried out comprehensive gas-dynamical modeling for the emission-line disk within ~70 pc from the nucleus. In comparison with the two previous studies of M84, our analysis includes a more complete treatment of the propagation of emission-line profiles through the telescope and STIS optics, as well as inclusion of the effects of an intrinsic velocity dispersion in the emission-line disk. We find that an intrinsic velocity dispersion is needed in order to match the observed line widths, and we calculate gas-dynamical models both with and without a correction for asymmetric drift. Including the effect of asymmetric drift improves the model fit to the observed velocity field. Our best-fitting model with asymmetric drift gives M BH = (8.5+0.9 –0.8) × 108 M (68% confidence). This is a factor of ~2 smaller than the mass often adopted in studies of the M BH-σ and M BH-L relationships. Our result provides a firmer basis for the inclusion of M84 in the correlations between black hole mass and host galaxy properties. [see original online version for correct notation]en
dc.language.isoeng
dc.relation.ispartofThe Astrophysical journal
dc.titleThe supermassive black hole in M84 revisiteden
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2010
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/721/1/762
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


Files in this item

FilesSizeFormatView

There are no files associated with this item.

This item appears in the following Collection(s)

Show simple item record