The cosmic growth of the active black hole population at 1 &lt;z &lt;2 in zCOSMOS, VVDS and SDSS

Schulze, Andreas; Bongiorno, A.; Gavignaud, I.; Schramm, Malte; Silverman, John D.; Merloni, A.; Zamorani, G.; Hirschmann, Michaela; Mainieri, V.; Wisotzki, L.; Shankar, Francesco; Fiore, F.; Koekemoer, Anton M.; Temporin, S.

doi:10.1093/mnras/stu2549

Cited by 100 publications

(186 citation statements)

References 184 publications

(374 reference statements)

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“…We assigned broad, Schechter-type Eddington ratio distributions to our mock black holes in line with empirical estimates (e.g., Shankar et al 2013b;Schulze et al 2015, and references therein). Long-dashed and dot-dashed lines in Figure 11 show the limiting active black hole mass that is still detectable above a bolometric luminosity of L bol = 10 42 erg s −1 and L bol = 10 43 erg s −1 .…”

Section: On Why We Support the Intrinsic Black Hole-galaxy Scaling Rementioning

confidence: 68%

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.

245

371

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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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Section: On Why We Support the Intrinsic Black Hole-galaxy Scaling Rementioning

confidence: 68%

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.

245

371

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“…Then, the overall radiative efficiency,L Mc 2 , is 10 −3 . Such low radiative efficiencies cannot be common in active galactic nuclei (AGNs), given their average accretion efficiency of 0.1 (Sołtan 1982;Marconi et al 2004;Silverman et al 2008;Schulze et al 2015). Also, if such high accretion rates are common in AGNs, the implied BH mass growth rates will be much faster than currently thought.…”

Section: The Luminosity and Mass Accretion Ratementioning

confidence: 99%

On the Lamppost Model of Accreting Black Holes

Niedźwiecki

Zdziarski

Szanecki

2016

ApJL

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We study the lamppost model, in which the X-ray source in accreting black hole (BH) systems is located on the rotation axis close to the horizon. We point out a number of inconsistencies in the widely used lamppost model relxilllp, e.g., neglecting the redshift of the photons emitted by the lamppost that are directly observed. They appear to invalidate those model fitting results for which the source distances from the horizon are within several gravitational radii. Furthermore, if those results were correct, most of the photons produced in the lamppost would be trapped by the BH, and the luminosity generated in the source as measured at infinity would be much larger than that observed. This appears to be in conflict with the observed smooth state transitions between the hard and soft states of X-ray binaries. The required increase of the accretion rate and the associated efficiency reduction also present a problem for active galactic nuclei. Then, those models imply the luminosity measured in the local frame is much higher than that produced in the source and measured at infinity, due to the additional effects of time dilation and redshift, and the electron temperature is significantly higher than that observed. We show that these conditions imply that the fitted sources would be out of the e ± pair equilibrium. On the other hand, the above issues pose relatively minor problems for sources at large distances from the BH, where relxilllp can still be used.

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“…A broken power law shaped ERDF While alternative ERDF shapes have been discussed previously (Kollmeier et al 2006;Kauffmann & Heckman 2009;Hopkins & Hernquist 2009;Cao 2010;Aird et al 2012;Bongiorno et al 2012;Nobuta et al 2012;Conroy & White 2013;Aird et al 2013a;Veale et al 2014;Hickox et al 2014;Schulze et al 2015;Trump et al 2015;Jones et al 2016;Bongiorno et al 2016), we assume a broken power law shaped ERDF for both radiatively efficient and inefficient AGN. A broken power law shaped ERDF solves the apparent discrepancy between a Schechter function shaped stellar mass function and an observed broken power law shaped luminosity function.…”

Section: Two Accretion Modesmentioning

confidence: 99%

“…In previous work, the black hole mass function and the corresponding Eddington ratio values have been measured observationally (Heckman et al 2004;McLure & Dunlop 2004;Kollmeier et al 2006;Kauffmann & Heckman 2009;Schulze & Wisotzki 2010;Trump et al 2011;Shen & Kelly 2012;Kelly & Merloni 2012;Nobuta et al 2012;Bongiorno et al 2012;Lusso et al 2012;Aird et al 2012;Schulze et al 2015;Jones et al 2016;Bongiorno et al 2016;Aird et al 2017) and have been studied using a phenomenological approach (Merloni et al 2004;Shankar et al 2004;Yu & Lu 2004;Merloni & Heinz 2008;Hopkins & Hernquist 2009;Shen 2009;Shankar et al 2009;Cao 2010;Li et al 2011;Conroy & White 2013;Shankar et al 2013;Novak 2013;Veale et al 2014;Aversa et al 2015;Caplar et al 2015;Tucci & Volonteri 2016).…”

mentioning

confidence: 99%

AGNs and Their Host Galaxies in the Local Universe: Two Mass-independent Eddington Ratio Distribution Functions Characterize Black Hole Growth

Weigel

Schawinski

Čaplar

et al. 2017

ApJ

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We use a phenomenological model to show that black hole growth in the local Universe (z 0.1) can be described by two separate, mass independent Eddington ratio distribution functions (ERDFs). We assume that black holes can be divided into two independent groups: those with radiatively efficient accretion, primarily hosted by optically blue and green galaxies, and those with radiatively inefficient accretion, which are mainly found in red galaxies. With observed galaxy stellar mass functions as input, we show that the observed AGN luminosity functions can be reproduced by using mass independent, broken power law shaped ERDFs. We use the observed hard X-ray and 1.4 GHz radio luminosity functions to constrain the ERDF for radiatively efficient and inefficient AGN, respectively. We also test alternative ERDF shapes and mass dependent models. Our results are consistent with a mass independent AGN fraction and AGN hosts being randomly drawn from the galaxy population. We argue that the ERDF is not shaped by galaxy-scale effects, but by how efficiently material can be transported from the inner few parsecs to the accretion disc. Our results are incompatible with the simplest form of mass quenching where massive galaxies host higher accretion rate AGN. Furthermore, if reaching a certain Eddington ratio is a sufficient condition for maintenance mode, it can occur in all red galaxies, not just the most massive ones.

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The cosmic growth of the active black hole population at 1 <z <2 in zCOSMOS, VVDS and SDSS

Cited by 100 publications

References 184 publications

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

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

On the Lamppost Model of Accreting Black Holes

AGNs and Their Host Galaxies in the Local Universe: Two Mass-independent Eddington Ratio Distribution Functions Characterize Black Hole Growth

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