THE MBH–LSPHEROID RELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES

By Alister W. Graham, Nicholas Scott. 2012

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From a sample of 72 galaxies with reliable supermassive black hole masses Mbh, we derive the Mbh–(host spheroid luminosity, L) relation for (1) the subsample of 24 core-Sérsic galaxies with partially depleted cores, and (2) the remaining subsample of 48 Sérsic galaxies. Using Ks-band Two Micron All Sky Survey data, we find the near-linear relation Mbh∝L1.10 ± 0.20Ks for the core-Sérsic spheroids thought to be built in additive dry merger events, while we find the relation Mbh∝L2.73 ± 0.55Ks for the Sérsic spheroids built from gas-rich processes. After converting literature B-band disk galaxy magnitudes into inclination- and dust-corrected bulge magnitudes, via a useful new equation presented herein, we obtain a similar result. Unlike with the Mbh–(velocity dispersion) diagram, which is also updated here using the same galaxy sample, it remains unknown whether barred and non-barred Sérsic galaxies are offset from each other in the Mbh–L diagram. While black hole feedback has typically been invoked to explain what was previously thought to be a nearly constant Mbh/MSpheroid mass ratio of ∼0.2%, we advocate that the near-linear Mbh–L and Mbh–MSpheroid relations observed at high masses may have instead arisen largely from the additive dry merging of galaxies. We argue that feedback results in a dramatically different scaling relation, such that black hole mass scales roughly quadratically with the spheroid mass in Sérsic galaxies. We therefore introduce a revised cold-gas “quasar” mode feeding equation for semi-analytical models to reflect what we dub the quadratic growth of black holes in Sérsic galaxies built amidst gas-rich processes. Finally, we use our new Sérsic Mbh–L equations to predict the masses of candidate intermediate mass black holes in almost 50 low-luminosity spheroids containing active galactic nuclei, finding many masses between that of stellar mass black holes and supermassive black holes.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/745b6fc767ef7e0f717698fb9a40855d0f170fd0

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Citations in the corpus

Observational evidence for intermediate-mass black holes (2017, background): “However, this is not the case for the MBH−Mbulge relation: the BH mass of IMBHs/low-mass AGN tends to be lower at a given bulge mass than expected from an extrapolation of the relation found for classical bulges (e.g., Greene et al. 2008; Jiang et al. 2011; Graham & Scott 2013, 2015; Baldassare et a”
Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies (2013, background): “In contrast, Graham & Scott (2013) adopt σe = 55 km s−1, in part because they do not include V (r).”
CO-EVOLUTION OF GALACTIC NUCLEI AND GLOBULAR CLUSTER SYSTEMS (2013, background): “Horizontal dotted lines on the right show the range of the central black hole mass fraction, from Sani et al. (2011); Kormendy & Ho (2013); Graham & Scott (2013). a later epoch ofzi = 3.”
THE M87 BLACK HOLE MASS FROM GAS-DYNAMICAL MODELS OF SPACE TELESCOPE IMAGING SPECTROGRAPH OBSERVATIONS (2013, background): “At the high-mass end, the slope, intrinsic scatter, and possibly the functional form of theMBH − host galaxy relations are not well constrained (Gültekin et al. 2009; Graham & Scott 2013; McConnell & Ma 2013).”
PS1-10jh: THE DISRUPTION OF A MAIN-SEQUENCE STAR OF NEAR-SOLAR COMPOSITION (2013, background): “Additionally, we might expect that that grazing encounters (e.g. small β) should outnumber deep encounters (Frank & Rees 1976), and the black hole mass should follow established Mh-L relations (Graham & Scott 2013).”
Rates of stellar tidal disruption as probes of the supermassive black hole mass function (2014, methodology): “…TDE rates in every galaxy in our extended sample of Nuker galaxies, calculated under the assumption of a Kroupa PDMF and the latest calibration of the McConnell & Ma (2013, hereafter MM13) M•−σ relationship (this relation is broadly consistent with other recent analyses, e.g. Graham & Scott 2013).”
Gravitational torque-driven black hole growth and feedback in cosmological simulations (2016, background): “…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 indirect evidence for the effects of…”
Black holes on FIRE: stellar feedback limits early feeding of galactic nuclei (2017, result): “Our fiducial simulations predict undermassive BHs in lowmass galaxies, in agreement with observations of the local MBH–Mbulge relation (e.g. Graham & Scott 2013; Savorgnan et al. 2016), and substantial scatter in MBH at Mbulge ∼ 1010 M owing to rapid convergence on to the scaling relation once BHs…”
Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes (2018, background): “While the M-L relation is also biased towards higher mass/luminosity, recent works have attempted to better constrain the low mass regime, discovering strong indications of a steeper slope in the M-L relation, at MBH 106 M (Graham & Scott 2013).”
Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation (2016, methodology): “…selection effect: black hole dynamical mass estimates are only possible if (some multiple of) the black hole’s sphere of influence2, rinfl ≡ GMbh/σ 2, (2) has been resolved (e.g., Peebles 1972; Merritt & Ferrarese 2001a; Barth 2004; Batcheldor 2010; Gültekin et al. 2011; Graham & Scott 2013).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, methodology): “Moreover, the new data compiled by Kormendy & Ho (2013) and the analysis in Graham & Scott (2013) both imply that the correlation of MBH is significantly poorer with stellar bulge mass than with σ.”
Expected properties of the first gravitational wave signal detected with pulsar timing arrays (2015, background): “…different SBH-galaxy relations found in the literature (Häring & Rix 2004; Gültekin et al. 2009; Sani et al. 2011; Graham et al. 2011; Graham 2012; Graham & Scott 2013; Beifiori et al. 2012; McConnell & Ma 2013; Kormendy & Ho 2013), spanning a broad range of uncertainty and including recent…”
THE SINFONI BLACK HOLE SURVEY: THE BLACK HOLE FUNDAMENTAL PLANE REVISITED AND THE PATHS OF (CO)EVOLUTION OF SUPERMASSIVE BLACK HOLES AND BULGES (2016, methodology): “Finally, Graham & Scott (2013) claim that “Sersic galaxies” follow a quadratic more than a linearMBH -MBu relation.”
Supermassive black holes and their feedback effects in the IllustrisTNG simulation (2017, methodology): “This leads to a buildup of the black hole mass – stellar mass relation according to the scenario outlined in Graham & Scott (2013).”