Fundamental Planes and the Barless<i>M</i><sub>BH</sub>‐σ Relation for Supermassive Black Holes

Graham, Alister W.

doi:10.1086/587473

Cited by 157 publications

(216 citation statements)

References 109 publications

(108 reference statements)

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“…The evidence of a correlation between the residuals and the effective radius is obtained by considering only spiral and lenticular bulges. Graham (2008b) reached the same result studying a sample of 40 galaxies. In particular he found that the barred galaxies are responsible for much of the trend between the M • − σ residuals and R e , whereas the elliptical galaxies alone do not provide substantial support for the existence of a FP plane for SMBHs.…”

Section: A Possible Fundamental Plane For Supermasssive Black Holessupporting

confidence: 62%

“…Plotting the dependence of the residual of the M • −σ relation on R e and M , the results of Hopkins et al (2007b) are clearly in conflict with that of the other authors (Aller & Richstone 2007;Graham 2008b;Sani et al 2011). Of course, the explanation of this difference has to be found in the different analysis approach.…”

Section: A Possible Fundamental Plane For Supermasssive Black Holesmentioning

confidence: 77%

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The scaling relation between the mass of supermassive black holes and the kinetic energy of random motions of the host galaxies

Mancini¹,

Feoli²

2012

A&A

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Context. Thanks to the improved angular resolution of modern telescopes and kinematic models, the existence of supermassive black holes (SMBHs) in the inner part of galaxies, regardless their morphology and nuclear activity, has been established on quite solid grounds. A possible correlation between the mass of SMBHs (M • ) and the evolutionary state of their host galaxies is expected and is currently under a heated debate. Aims. Based on the recent 2D decomposition of 3.6 μm Spitzer/IRAC images of local late-and early-type galaxies with M • measurements, we investigated various scaling laws, studying what is the best predictor of the mass of the central black holes, that is the one with the lowest value of intrinsic scatter. In particular, we focused on the M • − M G σ 2 law, that is the relation between the mass of SMBHs and the kinetic energy of random motions of the corresponding host galaxies, M G is the mass and σ the velocity dispersion of the host galaxy (bulge). Methods. In order to find the best fit for each of the scaling laws examined, we performed a least-squares regression of M • on x for the considered sample of galaxies, x being a whatever known parameter of the galaxy bulge. For this purpose, we made use of both the linear regression LINMIX_ERR and FITEXY methods. Results. Our analysis shows that M • − M G σ 2 law fits the examined experimental data successfully as much as the other known scaling laws (all correlations have similar intrinsic scatters within the errors) and shows a value of χ 2 (estimated by FITEXY) better than the others, a result which is consistent with previous determinations at shorter wavelengths. This means that a combination of σ and M G (or R e ) could be necessary to drive the correlations between M • and other bulge properties. This issue has been investigated by a careful, although not fully conclusive, analysis of the residuals of the various relations. Conclusions. In order to avoid rushed conclusions on galaxy activity and evolution, the indirect inferring of the masses of the supermassive black holes from the kinetic energy of random motions via the M • − M G σ 2 relation should be considered, especially when applied to higher redshift galaxies (z > 0.01). This statement is suggested by a reanalysis of Sloan Digital Sky Survey (SDSS) data used to study the black hole growth in the nearby Universe. By adopting the M • − M G σ 2 relation instead of the M • − σ relation, a radio-quiet/radio-loud dichotomy appears in the SMBH mass distribution of the corresponding SDSS early-type AGN galaxies.

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Section: A Possible Fundamental Plane For Supermasssive Black Holessupporting

confidence: 62%

Section: A Possible Fundamental Plane For Supermasssive Black Holesmentioning

confidence: 77%

The scaling relation between the mass of supermassive black holes and the kinetic energy of random motions of the host galaxies

Mancini¹,

Feoli²

2012

A&A

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“…Different observations now question that BH-host correlations indeed appear as tight as previously claimed for all types of galaxies (e.g., Hu 2008;Graham 2008;Gültekin et al 2009;Graham & Li 2009). Significant outliers exist (e.g., Mathur et al 2001;Grupe & Mathur 2004;Watson et al 2007), BHs are currently observed also in the centres of bulgeless galaxies (e.g., Ghosh et al 2008;Satyapal et al 2009;Araya salvo et al 2012), and the AGN-starformation correlations disappear for all but highest luminosity AGNs (Shao et al 2010;Grier et al 2011).…”

Section: Introductionmentioning

confidence: 74%

Black holes in pseudobulges: demography and models

Shankar

Marulli

Mathur

et al. 2012

A&A

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Context. There is mounting evidence that a significant fraction of black holes (BHs) today live in late-type galaxies, including bulgeless galaxies and those hosting pseudobulges, and are significantly undermassive with respect to the scaling relations followed by their counterpart BHs in classical bulges of similar stellar (or even bulge) mass. Aims. Here we discuss the predictions of two state-of-the-art hierarchical galaxy formation models in which BHs grow via mergers and, in one, also via disc instability. Our aim is to understand if the wealth of new data on local BH demography is consistent with standard models. Methods. We follow the merger trees of representative subsamples of BHs and compute the fractional contributions of different processes to the final BH mass. Results. We show that the model in which BHs always closely follow the growth of their host bulges, also during late disk instabilities (i.e., bars), produces too narrow a distribution of BHs at fixed stellar mass to account for the numerous low-mass BHs now detected in later-type galaxies. Models with a looser connection between BH growth and bar instability instead predict the existence of a larger number of undermassive BHs, in better agreement with the observations. Conclusions. The scatter in the updated local BH-bulge mass relation (with no restriction on galaxy type) appears to be quite large when including later-type systems, but it can still be managed to be reproduced within current hierarchical models. However, the fuelling of BHs during the late bar-instability mode needs to be better quantified/improved to properly fit the data. We conclude discussing how the possibly large number of BHs in later type galaxies demands for an in-depth revision of the local BH mass function and its modelling.

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“…For example, the two most commonly used proxies, stellar velocity dispersion and bulge luminosity, lead to rather different estimates of φ(M bh ) (e.g., Lauer et al 2007a;Tundo et al 2007, but see also Graham 2008): the luminosity-based estimate predicts many more massive black holes. To date, there is no consensus on which is correct, at least for the more massive galaxies.…”

Section: Introductionmentioning

confidence: 99%

Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation

Shankar¹,

Bernardi²,

Sheth³

et al. 2016

Mon. Not. R. Astron. Soc.

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251

369

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We compare the set of local galaxies having dynamically measured black holes with a large, unbiased sample of galaxies extracted from the Sloan Digital Sky Survey. We confirm earlier work showing that the majority of black hole hosts have significantly higher velocity dispersions σ than local galaxies of similar stellar mass. We use Monte-Carlo simulations to illustrate the effect on black hole scaling relations if this bias arises from the requirement that the black hole sphere of influence must be resolved to measure black hole masses with spatially resolved kinematics. We find that this selection effect artificially increases the normalization of the M bh -σ relation by a factor of at least ∼ 3; the bias for the M bh -M star relation is even larger. Our Monte Carlo simulations and analysis of the residuals from scaling relations both indicate that σ is more fundamental than M star or effective radius. In particular, the M bh -M star relation is mostly a consequence of the M bh -σ and σ-M star relations, and is heavily biased by up to a factor of 50 at small masses. This helps resolve the discrepancy between dynamically-based black hole-galaxy scaling relations versus those of active galaxies. Our simulations also disfavour broad distributions of black hole masses at fixed σ. Correcting for this bias suggests that the calibration factor used to estimate black hole masses in active galaxies should be reduced to values of f vir ∼ 1. Black hole mass densities should also be proportionally smaller, perhaps implying significantly higher radiative efficiencies/black hole spins. Reducing black hole masses also reduces the gravitational wave signal expected from black hole mergers.

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Fundamental Planes and the BarlessM_BH‐σ Relation for Supermassive Black Holes

Cited by 157 publications

References 109 publications

The scaling relation between the mass of supermassive black holes and the kinetic energy of random motions of the host galaxies

The scaling relation between the mass of supermassive black holes and the kinetic energy of random motions of the host galaxies

Black holes in pseudobulges: demography and models

Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation

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Fundamental Planes and the BarlessMBH‐σ Relation for Supermassive Black Holes

Cited by 157 publications

References 109 publications

The scaling relation between the mass of supermassive black holes and the kinetic energy of random motions of the host galaxies

The scaling relation between the mass of supermassive black holes and the kinetic energy of random motions of the host galaxies

Black holes in pseudobulges: demography and models

Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation

Contact Info

Product

Resources

About

Fundamental Planes and the BarlessM_BH‐σ Relation for Supermassive Black Holes