An Observed Fundamental Plane Relation for Supermassive Black Holes

By P. Hopkins, L. Hernquist, Thomas J. Cox, Brant Robertson, E. Krause. 2007

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We study observed correlations between supermassive black hole (BHs) and the properties of their host galaxies and show that the observations define a BH "fundamental plane" (BHFP), of the form MBH ∝ σ3.0±0.3R or MBH ∝ Mσ2.2±0.5, analogous to the FP of elliptical galaxies. The BHFP is preferred over a simple relation between MBH and any of σ, M*, Mdyn, or Re alone at >3 σ (99.9%) significance. The existence of this BHFP has important implications for the formation of supermassive BHs and the masses of the very largest black holes and immediately resolves several apparent conflicts between the BH masses expected and measured for outliers in both the MBH-σ and MBH-M* relations.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c78d8e9d5eac2010617eec70bcba2dd5dca9d2bf

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Citations in the corpus

ON THE COSMIC EVOLUTION OF THE SCALING RELATIONS BETWEEN BLACK HOLES AND THEIR HOST GALAXIES: BROAD-LINE ACTIVE GALACTIC NUCLEI IN THE zCOSMOS SURVEY (2009, methodology): “From the measured total λL3000 AGN luminosity we derive the bolometric one using the luminosity-dependent bolometric correction factor fbol of Hopkins et al. (2007).”
Galaxy morphology and star formation in the Illustris Simulation at z = 0 (2015, methodology): “With these, we can understand the internal correlations among galaxy properties and determine which, if any, predict galaxy morphology better than others (e.g., Hopkins et al. 2007).”
Cosmological simulations of the growth of supermassive black holes and feedback from active galactic nuclei: method and tests (2009, background): “…the mass of the SMBH essentially tracks the binding energy of the stellar bulge (Marconi & Hunt 2003; Feoli & Mele 2005; Aller & Richstone 2007; Hopkins et al. 2007, 2008), although other authors argue that the appearance of a fundamental plane is actually due to biasing caused by the presence…”
CONSTRAINTS ON BLACK HOLE GROWTH, QUASAR LIFETIMES, AND EDDINGTON RATIO DISTRIBUTIONS FROM THE SDSS BROAD-LINE QUASAR BLACK HOLE MASS FUNCTION (2010, background): “Observationally, a significant amount of recent work has utilized the argument of Soltan (1982) to indirectly map the growth of all SMBHs (e.g., Salucci et al. 1999; Yu & Tremaine 2002; Shankar et al. 2004, 2009; Marconi et al. 2004; Yu & Lu 2004; Hopkins et al. 2007c; Merloni & Heinz 2008).”
He ii REIONIZATION AND ITS EFFECT ON THE INTERGALACTIC MEDIUM (2008, methodology): “We use the Magorrian relationship to relate a galaxy’s stellar mass to its super-massive black hole mass (Hopkins et al. 2007a,b), and the halo occupation model of Tinker et al. (2005); Conroy et al. (2006); Vale & Ostriker (2006) (for details, see Hopkins et al. (2008a)) to map from halo mass to…”
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies (2007, methodology): “…the emerging picture from analysis of our merger runs (Hopkins et al. 2006a), and they are also fully reproduced in a recent semianalytic model by Hopkins et al. (2007a) in which gas-rich mergers produce quasars and the evolution of the gas fraction andmerger rates drives their evolution and…”
THE SINFONI BLACK HOLE SURVEY: THE BLACK HOLE FUNDAMENTAL PLANE REVISITED AND THE PATHS OF (CO)EVOLUTION OF SUPERMASSIVE BLACK HOLES AND BULGES (2016, background): “(32) This is similar to the dependences found by Aller & Richstone (2007), Hopkins et al. (2007b) and Mancini & Feoli (2012).”
HOW DO DISKS SURVIVE MERGERS? (2008, background): “…halo gas; Hernquist 1989; Barnes & Hernquist 1991, 1996; Hernquist et al. 1993; Mihos & Hernquist 1994b, 1996; Di Matteo et al. 2005; Naab et al. 2006; Jesseit et al. 2007; Cox et al. 2006a,b; Robertson et al. 2006b; Springel et al. 2005a; Burkert et al. 2007; Hopkins et al. 2007c, 2008a,g,b,c,d).”
How do massive black holes get their gas (2009, background): “…spheroid properties, including mass (Kormendy & Richstone 1995; Magorrian et al. 1998), velocity dispersion (Ferrarese & Merritt 2000; Gebhardt et al. 2000) and binding energy or potential well depth (Aller & Richstone 2007; Hopkins et al. 2007), implies that these phenomena are tightly coupled.”
THE NON-CAUSAL ORIGIN OF THE BLACK-HOLE–GALAXY SCALING RELATIONS (2010, background): “However this does not mean that AGN feedback does not exist.”
A synthesis model for AGN evolution: supermassive black holes growth and feedback modes (2008, methodology): “As for the accuracy of our knowledge of the bolometric correction, we refer the reader to the studies of Marconi et al. (2004); Richards et al. (2006); Hopkins et al. (2007b) and Shankar et al. (2008b).”
TOWARD THE STANDARD POPULATION SYNTHESIS MODEL OF THE X-RAY BACKGROUND: EVOLUTION OF X-RAY LUMINOSITY AND ABSORPTION FUNCTIONS OF ACTIVE GALACTIC NUCLEI INCLUDING COMPTON-THICK POPULATIONS (2014, methodology): “According to Hopkins et al. (2007), its averagek is a function ofL and is represented as k(L) = 10.83( L 1010L⊙ )0.28+ 6.08( L 1010L⊙ )−0.020.”
MOLECULAR GAS IN z ∼ 6 QUASAR HOST GALAXIES (2010, background): “…velocity dispersion and supermassive black hole (SMBH) mass in nearby galaxies (Tremaine et al. 2002; Marconi & Hunt 2003; Hopkins et al. 2007a), which suggests that the formation of the SMBH and its spheroidal host are tightly coupled (Kauffmann & Haehnelt 2000; Hopkins et al. 2007b).”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, methodology): “We employ a power-law parameterisation (Hopkins et al. 2007), which we apply to the full bolometric luminosity LAGN,obsbol = ω1 ( LAGNbol 1046 erg s−1 )ω2 , (28) where we adopt ω1 = 0.3 and ω2 = 0.07 as our default choice.”
Gravitational torque-driven black hole growth and feedback in cosmological simulations (2016, background): “…correlations between the mass of central supermassive black holes and various stellar properties of their host galaxies (e.g. Häring & Rix 2004; Hopkins et al. 2007b; Gültekin et al. 2009; Graham & Scott 2013; McConnell & Ma 2013; Woo et al. 2013; van den Bosch 2016) are often interpreted as…”
A CATALOG OF GLOBULAR CLUSTER SYSTEMS: WHAT DETERMINES THE SIZE OF A GALAXY'S GLOBULAR CLUSTER POPULATION? (2013, background): “In addition to Mdyn ∼ Reσ 2 e , another quantity used occasionally in the literature especially for pressuresupported systems such as star clusters, molecular clouds, or E galaxies, is the system’s binding energy Eb ∼ Mσ2 ∼ Reσ 4 e (e.g. McLaughlin 2000; Hopkins et al. 2007; Snyder et al. 2011).”
A semi-analytic model for the co-evolution of galaxies, black holes and active galactic nuclei (2008, methodology): “Because the depth of the spheroid’s potential well determines the amount of momentum necessary to entrain the infalling gas, Hopkins et al. (2007a) find that this leads to a ‘black hole fundamental plane’, a correlation between the final black hole mass and sets of spheroid structural/dynamical…”
Discriminating Between the Physical Processes that Drive Spheroid Size Evolution (2009, background): “Generically, in such models, the ‘most fundamental’ correlation is between BH mass and some measure of the binding energy of the material which must be ‘halted’ to arrest further accretion; Hopkins et al. (2007a) show, in high-resolution C© 2009 The Authors.”
The Spitzer/IRAC view of black hole–bulge scaling relations (2010, methodology): “Thus here we follow MH03 and Graham (2008a) and compare the residuals of MBH-σ for our bulges (expressed in equation 9) with the effective radius (column 4 in Tab.”
Stellar and Quasar Feedback in Concert: Effects on AGN Accretion, Obscuration, and Outflows (2015, background): “The masses of super-massive black holes (BHs) correlate with various host galaxy bulge properties (Magorrian et al. 1998; Ferrarese & Merritt 2000; Gebhardt et al. 2000; Hopkins et al. 2007; Aller & Richstone 2007; Feoli & Mancini 2009; Kormendy et al. 2011).”