The Cosmic Density of Massive Black Holes from Galaxy Velocity Dispersions

Aller, M.; Richstone, D. O.

doi:10.1086/344484

Cited by 137 publications

(180 citation statements)

References 25 publications

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“…The total energy density can be converted into the total mass density accreted by black holes during the active phase, by assuming a mass-to-energy conversion efficiency, (Aller and Richstone, 2002;Merloni et al, 2004;Elvis et al, 2002;Marconi et al, 2004):…”

Section: The Early Growth Of Massive Black Holesmentioning

confidence: 99%

Formation of supermassive black holes

Volonteri

2010

Astron Astrophys Rev

780

707

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Evidence shows that massive black holes reside in most local galaxies. Studies have also established a number of relations between the MBH mass and properties of the host galaxy such as bulge mass and velocity dispersion. These results suggest that central MBHs, while much less massive than the host (∼ 0.1%), are linked to the evolution of galactic structure. In hierarchical cosmologies, a single big galaxy today can be traced back to the stage when it was split up in hundreds of smaller components. Did MBH seeds form with the same efficiency in small proto-galaxies, or did their formation had to await the buildup of substantial galaxies with deeper potential wells? I briefly review here some of the physical processes that are conducive to the evolution of the massive black hole population. I will discuss black hole formation processes for 'seed' black holes that are likely to place at early cosmic epochs, and possible observational tests of these scenarios.

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Section: The Early Growth Of Massive Black Holesmentioning

confidence: 99%

Formation of supermassive black holes

Volonteri

2010

Astron Astrophys Rev

780

707

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show abstract

“…However, because direct dynamical measurements of black hole masses are difficult to obtain, considerable effort has been invested in identifying easily observed proxies for M bh . As an example, the standard procedure for calculating the black hole "mass function" has been to assume that all galaxies host black holes, and to use the correlation between the observable proxy and M bh to transform the observed distribution of the proxy into a distribution of M bh (e.g., Salucci et al 1999;Aller & Richstone 2002;Ferrarese 2002b;McLure & Dunlop 2004;Marconi et al 2004;Shankar et al 2004;Benson et al 2007;Tundo et al 2007;Graham et al 2007;Yu & Lu 2008;Vika et al 2009). …”

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.

246

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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“…The demography of local galaxies suggests that most-perhaps all-massive galaxies host BHs at their centers (e.g., Kormendy & Richstone 1995). The good match between the local BH mass density and the accreted BH mass density in AGNs suggests that the AGN is an indispensable phase of galaxy evolution (e.g., Soltan 1982;Yu & Tremaine 2002;Aller & Richstone 2002;Shankar et al 2004;Marconi et al 2004). The interplay between star formation and AGN activity may play a key role in the establishment of the BH-bulge correlation.…”

Section: Introductionmentioning

confidence: 99%

COSMIC EVOLUTION OF STAR FORMATION IN TYPE-1 QUASAR HOSTS SINCEz= 1

Shi

Rieke

Ogle

et al. 2009

ApJ

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We present Spitzer Infrared Spectrograph observations of a complete sample of 57 Sloan Digital Sky Survey type-1 quasars at z ∼ 1. Aromatic features at 6.2 and/or 7.7 μm are detected in about half of the sample and show profiles similar to those seen in normal galaxies at both low and high redshift, indicating a star formation origin for the features. Based on the ratio of aromatic to star formation infrared (SFIR) luminosities for normal star-forming galaxies at z ∼ 1, we have constructed the SFIR luminosity function (LF) of z ∼ 1 quasars. As we found earlier for low-redshift Palomar-Green (PG) quasars, these z ∼ 1 quasars show a flatter SFIR LF than do z ∼ 1 field galaxies, implying the quasar host galaxy population has on average a higher star formation rate (SFR) than the field galaxies do. As measured from their SFIR LF, individual quasar hosts have on average LIRG-level SFRs, which mainly arise in the circumnuclear regions. By comparing with similar measurements of low-redshift PG quasars, we find that the comoving SFIR luminosity density in quasar hosts shows a much larger increase with redshift than that in field galaxies. The behavior is consistent with pure density evolution since the average SFR and the average SFR/BH accretion rate in quasar hosts show little evolution with redshift. For individual quasars, we have found a correlation between the aromatic-based SFR and the luminosity of the nuclear radiation, consistent with predictions of some theoretical models. We propose that type-1 quasars reside in a distinct galaxy population that shows elliptical morphology but that harbors a significant fraction of intermediate-age stars and is experiencing intense circumnuclear star formation.

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The Cosmic Density of Massive Black Holes from Galaxy Velocity Dispersions

Cited by 137 publications

References 25 publications

Formation of supermassive black holes

Formation of supermassive black holes

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

COSMIC EVOLUTION OF STAR FORMATION IN TYPE-1 QUASAR HOSTS SINCEz= 1

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