dc.contributor.author | Walsh, J.L. | |
dc.contributor.author | Barth, A. | |
dc.contributor.author | Sarzi, M. | |
dc.date.accessioned | 2010-10-19T14:55:04Z | |
dc.date.available | 2010-10-19T14:55:04Z | |
dc.date.issued | 2010 | |
dc.identifier.citation | Walsh , 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.issn | 0004-637X | |
dc.identifier.other | PURE: 181166 | |
dc.identifier.other | PURE UUID: 0ece8bfa-6a5d-499d-8e39-33526c08ff8c | |
dc.identifier.other | dspace: 2299/4905 | |
dc.identifier.other | Scopus: 78149247505 | |
dc.identifier.uri | http://hdl.handle.net/2299/4905 | |
dc.description | Original 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.abstract | The 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.iso | eng | |
dc.relation.ispartof | The Astrophysical Journal | |
dc.title | The supermassive black hole in M84 revisited | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | https://doi.org/10.1088/0004-637X/721/1/762 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |