期刊
ASTRONOMICAL JOURNAL
卷 146, 期 6, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-6256/146/6/160
关键词
galaxies: elliptical and lenticular, cD; galaxies: kinematics and dynamics; galaxies: nuclei; galaxies: photometry
资金
- DFG Cluster of Excellence Origin and Structure of the Universe
- Deutsche Forschungsgemeinschaft through Priority Programme 1177 Galaxy Evolution
- NASA [NAS5-26555]
- Alfred P. Sloan Foundation
- National Aeronautics and Space Administration
- National Science Foundation
- U.S. Department of Energy
- Japanese Monbukagakusho
- Max Planck Society
- University of Chicago
- Fermi lab
- Institute for Advanced Study
- Japan Participation Group
- The Johns Hopkins University
- Korean Scientist Group
- Los Alamos National Laboratory
- Max-Planck-Institute for Astronomy (MPIA)
- Max-Planck-Institute for Astrophysics (MPA)
- New Mexico State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
Shallow cores in bright, massive galaxies are commonly thought to be the result of scouring of stars by mergers of binary supermassive black holes. Past investigations have suggested correlations between the central black hole mass and the stellar light or mass deficit in the core, using proxy measurements of M-BH or stellar mass-to-light ratios (Upsilon). Drawing on a wealth of dynamical models which provide both M-BH and Upsilon, we identify cores in 23 galaxies, of which 20 have direct, reliable measurements of M-BH and dynamical stellar mass-to-light ratios (Upsilon(*,dyn)). These cores are identified and measured using Core-Sersic model fits to surface brightness profiles which extend out to large radii (typically more than the effective radius of the galaxy); for approximately one-fourth of the galaxies, the best fit includes an outer (Sersic) envelope component. We find that the core radius is most strongly correlated with the black hole mass and that it correlates better with total galaxy luminosity than it does with velocity dispersion. The strong core-size-M-BH correlation enables estimation of black hole masses (in core galaxies) with an accuracy comparable to the M-BH-sigma relation (rms scatter of 0.30 dex in log M-BH), without the need for spectroscopy. The light and mass deficits correlate more strongly with galaxy velocity dispersion than they do with black hole mass. Stellar mass deficits span a range of 0.2-39 M-BH, with almost all (87%) being <10 M-BH; the median value is 2.2 M-BH.
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