THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: NO EVIDENCE FOR EVOLUTION IN THE ${{M}_{\bullet }}-{{\sigma }_{*}}$ RELATION TO $z\sim 1$

Shen, Yue; Greene, Jenny E.; Ho, Luis C.; Brandt, W. N.; Denney, K. D.; Horne, K.; Jiang, Linhua; Kochanek, C. S.; McGreer, Ian D.; Merloni, A.; Peterson, B. M.; Petitjean, P.; Schneider, Donald P.; Schulze, Andreas; Strauss, Michael A.; Tao, C.; Trump, Jonathan R.; Pan, Kaike; Bizyaev, Dmitry

doi:10.1088/0004-637x/805/2/96

Cited by 110 publications

(170 citation statements)

References 82 publications

(158 reference statements)

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“…The least secure assumption is that a universal M • /σ relation holds near its present-day value as the black hole grows. However, this is broadly consistent with observations of active galactic nuclei 14,23 up to z ∼ 1, and with simulations of large scale structure evolution 24,25 up to z ∼ 4. Mergers between two cental black holes increase the black hole mass, but also affect the dynamics around it.…”

supporting

confidence: 90%

A universal minimal mass scale for present-day central black holes

Alexander

Bar-Or

2017

Nat Astron

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Intermediate-mass black holes (IMBHs) of mass M • ≈ 10 2 -10 5 solar masses, M , are the long-sought missing link 1 between stellar black holes, born of supernovae 2 , and massive black holes 3 , tied to galaxy evolution by the empirical M • /σ correlation 4,5 . We show that low-mass black hole seeds that accrete stars from locally dense environments in galaxies following a universal M • /σ relation 6, 7 grow over the age of the Universe to be above M 0 ≈ 3 × 10 5 M (5% lower limit), independent of the unknown seed masses and formation processes. The mass M 0 depends weakly on the uncertain formation redshift, and sets a universal minimal mass scale for present-day black holes. This can explain why no IMBHs have yet been found 3 , and it implies that present-day galaxies with σ < S 0 ≈ 40 km s −1 lack a central black hole, or formed it only recently. A dearth of IMBHs at low redshifts has observable implications for tidal disruptions 8 and gravitational wave mergers 9 . The early stages of massive black hole growth are poorly understood 10 . High-luminosity active galactic nuclei at very high redshift 11 z further imply rapid growth soon after the Big Bang. Suggested formation mechanisms typically rely on the extreme conditions found in the early Universe (very low metallicity, very high gas or star density). It is therefore plausible that these black hole seeds were formed in dense environments, at least a Hubble time ago (z > 1.8 for a look-back time of t H = 10 Gyr) 12 .β between black hole mass, M • , and stellar velocity dispersion, σ , that is observed in the local Universe over more than about three decades in massive black hole mass, correlates M • and σ on scales that are well outside the massive black hole's radius of dynamical influence 3 ,2 . Recent analyses of large heterogeneous galaxy samples find that a universal M • /σ relation holds for all galaxy types 6, 7 , although the scope of this relation and its evolution with redshift remain controversial 13 . Here we adopt the empirical fit ), where δ = 0.49 ± 0.03 is the root mean square of the intrinsic scatter. We assume that this universal M • /σ holds at all redshifts 14 , and that the black hole seeds grow in a locally (within a few r h ) dense stellar environment. By fixing r h , the M • /σ relation then imposes tight connections between the black hole and the dynamical properties of its stellar surroundings 15 , and specifically the rate at which it consumes stars (see Methods section).A central black hole grows by (1) the accretion of stars, compact remnants and dark matter particles that are deflected toward it on nearly radial orbits, and either fall whole through the event horizon or are tidally disrupted outside it, and then accreted; (2) viscosity-driven accretion of interstellar gas; and (3) mergers with other black holes. Of these growth channels, only the accretion of stars must follow from the existence of a central black hole in a stellar system. Moreover, the tidal disruption event * Department of Particle Physics & Astrophysics, W...

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supporting

confidence: 90%

A universal minimal mass scale for present-day central black holes

Alexander

Bar-Or

2017

Nat Astron

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“…Observations remain inconclusive regarding such evolution (e.g. Bongiorno et al 2014;Schulze & Wisotzki 2014;Shen et al 2015;Sun et al 2015;Willott et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Gravitational torque-driven black hole growth and feedback in cosmological simulations

Anglés-Alcázar¹,

Davé

Faucher-Giguère

et al. 2016

Mon. Not. R. Astron. Soc.

247

184

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We investigate black hole-host galaxy scaling relations in cosmological simulations with a self-consistent black hole growth and feedback model. The sub-grid accretion model captures the key scalings governing angular momentum transport from galactic scales down to parsec scales, while our kinetic feedback implementation enables the injection of outflows with properties chosen to match observed nuclear outflows. We show that "quasar mode" feedback can have a large impact on the thermal properties of the intergalactic medium and the growth of galaxies and massive black holes for kinetic feedback efficiencies as low as 0.1 % relative to the bolometric luminosity. Nonetheless, our simulations suggest that the black hole-host scaling relations are only weakly dependent on the effects of black hole feedback on galactic scales, owing to feedback suppressing the growth of galaxies and massive black holes by a similar amount. In contrast, the rate at which gravitational torques feed the central black hole relative to the host galaxy star formation rate governs the slope and normalization of the black hole-host correlations. Our results suggest that a common gas supply regulated by gravitational torques is the primary driver of the observed co-evolution of black holes and galaxies.

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“…However, our results suggest that searches for evolution in terms of Mstar are less well-motivated (because the observed M bh -M bulge relation is more biased and less fundamental). On the other hand, most analyses based on Soltantype arguments or direct detections suggest that the M bh -σ relation evolves weakly if at all (e.g., Gaskell & Kormendy 2009;Shankar et al 2009a;Zhang et al 2012;Shen et al 2015, but see also Woo et al 2008). This further paves the way towards using black holes and quasars as cosmological distance estimators (e.g., Hönig et al 2014).…”

Section: Implications For the Co-evolution Of Black Holes And Galaxiesmentioning

confidence: 99%

“…One way to test this co-evolution is by exploring the cosmic evolution of the above scaling relations. Thus, the characterization of the scaling relations of black holes with their hosts is the subject of intense observational efforts, both locally and at high redshift (e.g., Shields et al 2006;Lauer et al 2007b;Treu et al 2007;Woo et al 2008;Gaskell & Kormendy 2009;Shankar et al 2009a;Merloni et al 2010;Schulze & Wisotzki 2011;Falomo et al 2014;Shen et al 2015).…”

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.

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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THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: NO EVIDENCE FOR EVOLUTION IN THE ${{M}_{\bullet }}-{{\sigma }_{*}}$ RELATION TO $z\sim 1$

Cited by 110 publications

References 82 publications

A universal minimal mass scale for present-day central black holes

A universal minimal mass scale for present-day central black holes

Gravitational torque-driven black hole growth and feedback in cosmological simulations

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

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