Host Galaxy Bulge Predictors of Supermassive Black Hole Mass

Aller, M.; Richstone, D. O.

doi:10.1086/519298

Cited by 118 publications

(170 citation statements)

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“…These fits provide an error bar of ±0.4 dex, slightly worse than the ±0.3 dex error given by more sophisticated fits using a much better but also much smaller data set (Aller & Richstone 2007). These corrections affect a large fraction of the candidate black holes.…”

Section: Derivationmentioning

confidence: 72%

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The mass function of nearby black hole candidates

Caramete

Biermann

2010

A&A

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Context. The mass function of supermassive black holes in our cosmic neighborhood is required to understand the statistics of their activity and consequently the origin of ultra high energy particles. Aims. We determine a mass function of supermassive black hole candidates from the entire sky except for the Galactic plane. Methods. Using the 2MASS catalogue as a starting point, and the well-established correlation between black hole mass and the bulge of old population of stars, we derive a list of nearby black hole candidates within the redshift range z < 0.025, then perform an additional selection based on the Hubble type. We present our resulting catalogue elsewhere. The final list of black hole candidates above a mass of M BH > 3 × 10 6 M has 5829 entries. We perform a Hubble-type correction to account for selection effects, which reduces this number to 2919 black hole candidates. Here we use this catalogue to derive the black-hole mass function. We also correct for volume, so that this mass function is a volume-limited distribution to redshift 0.025. Results. The differential mass function of nearby black hole candidates is a curved function, with a straight simple power-law of index −3 above 10 8 M that becomes progressively flatter towards lower masses, turns off towards a gap below 3 × 10 6 M , and then extends into the range where nuclear star clusters replace black holes. The shape of this mass function can be explained in a simple merger picture. Integrating this mass function over the redshift range for which it has been derived, infers a total number of black holes with z < 0.025, and M BH > 10 7 M of about 2.4 × 10 4 , or, if we average uniformly, 0.6 for every square degree on the sky.

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Section: Derivationmentioning

confidence: 72%

“…) and use the black-hole mass-spheroid correlation (e.g., Faber et al 1997;Magorrian et al 1998;Silk & Rees 1998;Häring & Rix 2004;A&A 521, A55 (2010) Tremaine et al 2002;Aller & Richstone 2007) to derive the black hole mass function. We select down to 0.03 Jy at 2 microns, which is far brighter than the 2MASS catalogue completeness limit.…”

Section: Derivationmentioning

confidence: 99%

The mass function of nearby black hole candidates

Caramete

Biermann

2010

A&A

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“…The existence of tight correlations between black hole (BH) mass and properties of the host galaxy spheroid, including spheroid mass/luminosity (Kormendy & Richstone 1995;Magorrian et al 1998;Kormendy et al 2011), velocity dispersion (Ferrarese & Merritt 2000;Gebhardt et al 2000), and binding energy/potential depth (Aller & Richstone 2007;Hopkins et al 2007b;Feoli et al 2010) have fundamental implications for the growth of BHs and -given the Soltan (1982) argument which implies that most BH mass was assembled in luminous quasar phases (e.g. Salucci et al 1999;Yu & Tremaine 2002;Hopkins et al 2007d;Shankar et al 2009) -corresponding active galactic nuclei (AGN) activity.…”

Section: Introductionmentioning

confidence: 99%

Do we expect most AGN to live in discs?

Hopkins¹,

Kocevski²,

Bundy³

2014

Monthly Notices of the Royal Astronomical Society

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Recent observations have indicated that a large fraction of the low to intermediate luminosity AGN population lives in disk-dominated hosts, while the more luminous quasars live in bulge-dominated hosts (that may or may not be major merger remnants), in conflict with some previous model predictions. We therefore build and compare a semi-empirical model for AGN fueling which accounts for both merger and non-merger "triggering." In particular, we show that the "stochastic accretion" model -in which fueling in disk galaxies is essentially a random process arising whenever dense gas clouds reach the nucleusprovides a good match to the present observations at low/intermediate luminosities. However it falls short of the high-luminosity population. We combine this with models for major merger-induced AGN fueling, which lead to rarer but more luminous events, and predict the resulting abundance of disk-dominated and bulge-dominated AGN host galaxies as a function of luminosity and redshift. We compile and compare observational constraints from z ∼ 0 − 2. The models and observations generically show a transition from disk to bulge dominance in hosts near the Seyfert-quasar transition, at all redshifts. "Stochastic" fueling dominates AGN by number (dominant at low luminosity), and dominates BH growth below the "knee" in the present-day BH mass function ( 10 7 M ). However it accounts for just ∼ 10% of BH mass growth at masses 10 8 M . In total, fueling in disky hosts accounts for ∼ 30% of the total AGN luminosity density/BH mass density. The combined model also accurately predicts the AGN luminosity function and clustering/bias as a function of luminosity and redshift; however, we argue that these are not sensitive probes of BH fueling mechanisms.

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“…Subsequently, based on more and more precise experimental data, it was possible to draw up many galaxy data sets, containing measures of the SMBH masses as well as the structural parameters of the host galaxies (bulges) (Magorrian et al 1998;Tremaine et al 2002;Marconi & Hunt 2003;Gebhardt et al 2003;Häring & Rix 2004;Aller & Richstone 2007;Graham 2008a,b;Hu 2008;Kisaka et al 2008;Feoli & Mancini 2009;Gültekin et al 2009a;Beifiori et al 2009Beifiori et al , 2011.…”

Section: Introductionmentioning

confidence: 99%

“…Magorrian et al 1998;Ferrarese & Merritt 2000;Gebhardt et al 2000;Laor 2001;Merritt & Ferrarese 2001;Wandel 2002;Tremaine et al 2002;Marconi & Hunt 2003;Häring & Rix 2004;Graham & Driver 2005;Feoli & Mele 2005;Aller & Richstone 2007;Hopkins et al 2007b). Another scaling law has been recently proposed, the M • − R e σ 3 law , which is based on a pure theoretical framework, and is on the wake of the numerical results of Hopkins et al (2007a).…”

Section: Introductionmentioning

confidence: 99%

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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Host Galaxy Bulge Predictors of Supermassive Black Hole Mass

Cited by 118 publications

References 97 publications

The mass function of nearby black hole candidates

The mass function of nearby black hole candidates

Do we expect most AGN to live in discs?

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

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