THE FUNDAMENTAL PLANE OF ACCRETION ONTO BLACK HOLES WITH DYNAMICAL MASSES

By K. Gültekin, E. Cackett, Jonathan M. Miller, T. Di Matteo, S. Markoff, D. Richstone. 2009

156 citations recorded by the source corpus.

Black hole accretion and jet production are areas of intensive study in astrophysics. Recent work has found a relation between radio luminosity, X-ray luminosity, and black hole mass. With the assumption that radio and X-ray luminosities are suitable proxies for jet power and accretion power, respectively, a broad fundamental connection between accretion and jet production is implied. In an effort to refine these links and enhance their power, we have explored the above relations exclusively among black holes with direct, dynamical mass-measurements. This approach not only eliminates systematic errors incurred through the use of secondary mass measurements, but also effectively restricts the range of distances considered to a volume-limited sample. Further, we have exclusively used archival data from the Chandra X-ray Observatory to best isolate nuclear sources. We find log LR = (4.80 ± 0.24) + (0.78 ± 0.27)log MBH + (0.67 ± 0.12)log LX, in broad agreement with prior efforts. Owing to the nature of our sample, the plane can be turned into an effective mass predictor. When the full sample is considered, masses are predicted less accurately than with the well-known M–σ relation. If obscured active galactic nuclei are excluded, the plane is potentially a better predictor than other scaling measures.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/97460d7027726782de4ac8b634eb5bcd25fd3275

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Citations in the corpus

MOCCA code for star cluster simulations – IV. A new scenario for intermediate mass black hole formation in globular clusters (2015, background): “A strong motivation for searching for IMBHs is the observed relation between the black hole (BH) mass and the velocity dispersion of its host galaxy (e.g. Ferrarese & Merritt 2000; Gültekin et al. 2009, and refer nces therein).”
The 'universal' radio/X-ray flux correlation : the case study of the black hole GX 339-4 (2012, background): “…of the fundamental plane of BH activity and the possibility of universal scaling laws for accreting BHs across all mass scales (Merloni, Heinz & di Matteo 2003; Falcke, Körding & Markoff 2004; Körding, Falcke & Corbel 2006; Wang, Wu & Kong 2006; Gültekin et al. 2009; Plotkin et al. 2011).”
Using the Fundamental Plane of black hole activity to distinguish X-ray processes from weakly accreting black holes (2011, methodology): “…studies over the past few years (including the original discovery papers) have indeed used the FP to investigate the origin of X-rays, but with varied success (Körding, Falcke & Corbel 2006a, hereafter K06; Wang, Wu & Kong 2006; Li, Wu & Wang 2008; Gültekin et al. 2009a; Yuan, Yu & Ho 2009).”
Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, background): “…the BH mass and other physical properties of its host: galaxy bulge stellar mass, luminosity, velocity dispersion (Magorrian et al. 1998; Ferrarese & Merritt 2000; Gebhardt et al. 2000; Tremaine et al. 2002; Marconi & Hunt 2003; Gültekin et al. 2009) and dark matter halo mass (Ferrarese 2002).”
PHOTON RINGS AROUND KERR AND KERR-LIKE BLACK HOLES (2013, background): “The uncertainty of the mass of the supermassive black hole at the center of M87 is currently reported to be ≈ 29% assuming no uncertainty in the distance (see Gültekin et al. 2009 and references therein; see, however, Walsh et al. 2013).”
Hot Accretion Flows Around Black Holes (2014, background): “Their generalized correlation takes the form (Gültekin et al. 2009), log ( LR erg s−1 ) = (0.7± 0.1) log ( LX erg s−1 ) + (0.8± 0.3) log ( M M⊙ ) + (4.8± 0.2), (36) and is referred to as the “fundamental plane of black hole activity”.”
X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects (2014, background): “During such active phases, a strong physical coupling (generally termed ‘feedback’) could have established a long-lasting link between hosts and SMBHs, leading to the well-known local scaling relations (e.g., Ferrarese & Merritt 2000; Gebhardt et al. 2000; Gültekin et al. 2009).”
THREE-YEAR SWIFT–BAT SURVEY OF ACTIVE GALACTIC NUCLEI: RECONCILING THEORY AND OBSERVATIONS? (2010, background): “However, two of the most famous Compton-thick AGNs (Circinus and NGC 4945) display an Eddington ratio far from unity (i.e., 10−2, see Gültekin et al. 2009), proving that this argument still escapes a conclusive explanation.”
Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies (2013, methodology): “The BH detection in Greenhill, Moran & Herrnstein (1997b) was rejected by Gültekin et al. (2009c) because the maser rotation curve is asymmetric and because the maser disk inclination is only approximately constrained to be edge-on by its linear distribution at PA ≈ 45◦.”