The Masses of Nuclear Black Holes in Luminous Elliptical Galaxies and Implications for the Space Density of the Most Massive Black Holes

Abstract

Black hole masses predicted from the Mbh-sigma relationship conflict with those predicted from the Mbh-L relationship for the most luminous galaxies, such as brightest cluster galaxies (BCGs). This is because stellar velocity dispersion, sigma, increases only weakly with L for BCGs and other giant ellipticals. The Mbh-L relationship predicts that the most luminous BCGs may have Mbh approaching 10^{10}M_sol, while the M-sigma relationship always predicts Mbh<3X10^9M_sol. We argue that the Mbh-L relationship is a plausible or even preferred description for BCGs and other galaxies of similar luminosity. If cores in central stellar density are formed by binary BHs, then the inner-core cusp radius, r_gamma, may be an independent witness of Mbh. Using structural parameters derived from a large sample of early-type galaxies observed by HST, we argue that L is superior to sigma as an indicator of r_gamma in luminous galaxies. The observed r_gamma-Mbh relationship for 11 core galaxies with measured Mbh appears to be consistent with the Mbh-L relationship for BCGs. BCGs have large cores appropriate for their large luminosities that may be difficult to generate with the modest BH masses inferred from the Mbh-sigma relationship. Mbh~L may be expected to hold for BCGs, if they were formed in dissipationless mergers, which should preserve ratio of BH to stellar mass. This picture appears to be consistent with the slow increase in sigma with L and the more rapid increase in effective radii with L seen in BCGs. If BCGs have large BHs commensurate with their luminosities, then the local BH mass function for Mbh>3X10^9M_sol may be nearly an order of magnitude richer than that inferred from the Mbh-sigma relationship. The volume density of QSOs at earlier epochs may favor the predictions from the Mbh-L relationship.

62 pages, 18 figures, submitted to the Astrophysical Journal; revised after initial review

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• Episodic activities of supermassive black holes at redshift $z\le 2$: driven by mergers?
• Galaxy Core Formation by Supermassive Black Hole Binaries: the Importance of Realistic Initial Conditions and Galaxy Morphology
• Quiescent luminous red galaxies (LRGs) as cosmic chronometers: on the significance of mass and environmental dependence
• The Fundamental Plane Relation of Early-Type Galaxies: Environmental Dependence
• Chandra Observations of Abell 2261 Brightest Cluster Galaxy, a Candidate Host to a Recoiling Black Hole
• A Likely Super Massive Black Hole Revealed by its Einstein Radius in Hubble Frontier Fields Images
• Probing the Delay Time of Supermassive Black Hole Binary Mergers With Gravitational Waves
• Connecting traces of galaxy evolution: the missing core mass -- morphological fine structure relation
• Extrapolating SMBH correlations down the mass scale: the case for IMBHs in globular clusters
• Unveiling Gargantua: A new search strategy for the most massive central cluster black holes
• Early Type Galaxy Core Phase Densities
• Properties of radio-loud quasars in Sloan Digital Sky Survey
• A fundamental equation for Supermassive Black Holes
• The radio luminosity, black hole mass and Eddington ratio for quasars from the Sloan Digital Sky Survey
• A counter-image to the gravitational arc in Abell 1201: Evidence for IMF variations, or a $10^{10}$M${}_{\odot }$ black hole?
• 2D Surface Brightness Modelling of Large 2MASS Galaxies I: Photometry and Structural Parameters
• Climbing out of the shadows: building the distance ladder with black hole images
• The Fundamental Plane Is Not a Plane: Warped Nature of the Fundamental Plane of Early-type Galaxies and Its Implication for Galaxy Formation
• The core fundamental plane of B2 radio galaxies
• X-ray Observations of Optically Selected Giant Elliptical-Dominated Galaxy Groups
• Renormalized 2PN spin contributions to the accumulated orbital phase for LISA sources
• The correlations of stellar tidal disruption rates with properties of massive black holes and their host galaxies
• The Star Formation Reference Survey. IV. Stellar mass distribution of local star-forming galaxies
• Simulations of the accreted stellar halos of low-mass field galaxies
• The Compactness of Galaxy Groups in the Sloan Digital Sky Survey
• The estimation of black-hole masses in distant radio galaxies
• Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies: Black Hole Scaling Relations Are Not Biased by Selection Effects
• An updated comparison of the $M_{\bullet }$ vs $M_G{\sigma }^2$ relation with $M_{\bullet }$ vs $\sigma$ and the problem of the masses of galaxies
• The early Universe with JWST and ALMA
• Revisiting the Dichotomy of Early-type Galaxies
• A note on the interpretation of the statistical analysis of the $M_{\bullet }-M_G{\sigma }^2$ scaling relation
• LeMMINGs. V. Nuclear activity and bulge properties: a detailed multi-component decomposition of $e$-MERLIN Palomar galaxies with $HST$
• Renormalized spin coefficients in the accumulated orbital phase for unequal mass black hole binaries
• Determination of the angular momentum of the Kerr black hole from equatorial geodesic motion
• Supermassive Black Holes in Galactic Bulges
• The most massive galaxies with large depleted cores: structural parameter relations and black hole masses
• WISDOM Project -- XXVI. Cross-checking supermassive black hole mass estimates from ALMA CO gas kinematics and SINFONI stellar kinematics in the galaxy NGC 4751
• Galaxy disc central surface brightness distribution in the optical and near-infrared bands