On the Black Hole Mass-Bulge Mass Relation

By N. Haering, Hans-Walter Rix. 2004

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We have reexamined the relation between the mass of the central black holes in nearby galaxies, Mbh, and the stellar mass of the surrounding spheroid or bulge, Mbulge. For a total of 30 galaxies bulge masses were derived through Jeans equation modeling or adopted from dynamical models in the literature. In stellar mass-to-light ratios, the spheroids and bulges span a range of a factor of 8. The bulge masses were related to well-determined black hole masses taken from the literature. With these improved values for Mbh, compared to Magorrian et al., and our redetermination of Mbulge, we find that the Mbh-Mbulge relation becomes very tight. We find Mbh ~ M with an observed scatter of ≲0.30 dex, a fraction of which can be attributed to measurement errors. The scatter in this relation is therefore comparable to the scatter in the relations of Mbh with σ and the stellar concentration. These results confirm and refine the work of Marconi & Hunt. For Mbulge ~ 5 × 1010 M☉ the median black hole mass is 0.14% ± 0.04% of the bulge mass.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c26e9c5d5350a0e477423d85bae1f8559591ed6d

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Citations in the corpus

The stochastic gravitational-wave background from massive black hole binary systems: implications for observations with Pulsar Timing Arrays (2008, methodology): “The key point is that we can infer the BHMF either relying on the MBH−σ relation, or on the MBH−Mbulge relation (e.g. Haring & Rix 2004), and the two approaches give inconsistent results especially for heavier MBHs (e.g Lauer et al. 2007).”
REVERBERATION MAPPING MEASUREMENTS OF BLACK HOLE MASSES IN SIX LOCAL SEYFERT GALAXIES (2010, background): “…and theoretical) that there is a connection between supermassive black hole (BH) growth and galaxy evolution (e.g., Silk & Rees 1998; Kormendy & Gebhardt 2001; Häring & Rix 2004; Di Matteo et al. 2005; Bennert et al. 2008; Somerville et al. 2008; Hopkins & Hernquist 2009; Shankar et al. 2009).”
Interaction of Massive Black Hole Binaries with Their Stellar Environment. I. Ejection of Hypervelocity Stars (2006, background): “The SIS potential is φ(r) = −2σ2 [ln(GMB/2σ2r) + 1] (for r RB = GMB/2σ 2), and the escape speed from rinf is then vesc ≡ √ −2φ = 2σ √ [ln(MB/M) + 1] = 5.5σ, (14) where the second equality comes from the adopted bulge– black hole mass relation M = 0.0014MB (Haring & Rix 2004).”
Universal bolometric corrections for active galactic nuclei over seven luminosity decades (2020, methodology): “In the COSMOS type 2 sample, the BH masses have been derived by L12 using the MBH−Mbulge relation by Häring & Rix (2004) after correcting for the bulge-to-total mass ratio.”
Dark matter in elliptical galaxies — II. Estimating the mass within the virial radius (2004, methodology): “A recent analysis (Häring & Rix 2004) favoursgBH = 0.15% ( Mbulge/6× 1011M⊙ )0.12 , and we will adopt below gBH = 0.15%.”
Quasar feedback: more bang for your buck (2009, background): “The cloud resides at a spherical distance r from the centre of a Hernquist (1990) profile bulge of total mass Mbul and characteristic scalelength Reff , which hosts a BH on the characteristic BH–host relations, MBH = μBH Mbul(μBH ≈ 0.0014; Häring & Rix 2004).”
REVISITING THE SCALING RELATIONS OF BLACK HOLE MASSES AND HOST GALAXY PROPERTIES (2012, methodology): “Among them, 13 bulge masses are taken from Häring & Rix (2004), who used spherical Jeans models to fit stellar kinematics.”
The relation between metallicity, stellar mass and star formation in galaxies: an analysis of observational and model data (2011, background): “Interestingly, it is these galaxies that lie closest to the observational relation found by Häring & Rix (2004).”
On the fundamental dichotomy in the local radio-AGN population (2012, background): “with a mass that correlates strongly with the stellar mass (e.g. Marconi & Hunt 2003; Häring & Rix 2004) or velocity dispersion (e.g. Gebhardt et al. 2000; Ferrarese & Merritt 2000) of the surrounding galaxy bulge.”
Jet-regulated cooling catastrophe (2010, background): “In this case, self-regulation of the BH growth possibly drives the relations observed between BH mass and their host galaxy properties (Magorrian et al. 1998; Tremaine et al. 2002; Häring & Rix 2004).”
An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, background): “The typical mass ratio is ~M M 0.002BH host (e.g., Marconi & Hunt 2003; Häring & Rix 2004; Sani et al. 2011; Kormendy & Ho 2013; a factor ∼10 lower according to Reines & Volonteri 2015).”
Observations of feedback from radio-quiet quasars - I. Extents and morphologies of ionized gas nebulae (2013, background): “…of their hosts’ stellar bulges (Magorrian et al. 1998; Gebhardt et al. 2000; Ferrarese & Merritt 2000; Tremaine et al. 2002; Marconi & Hunt 2003; Häring & Rix 2004; Gültekin et al. 2009; McConnell et al. 2011) also suggests that the energy output of the black hole in its most active – quasar…”