Major mergers of haloes, the growth of massive black holes and the evolving luminosity function of quasars

Hatziminaoglou, E.; Mathez, G.; Solanes, J. M.; Manrique, Alberto; Salvador-Solé, E.

doi:10.1046/j.1365-8711.2003.06704.x

Cited by 27 publications

(35 citation statements)

References 67 publications

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“…Consequently, the bright AGNs stop radiating as quasars, and remain in the more quiescent radio phase. This has a major impact in the global AGN emissivities because bright AGNs have the largest bolometric luminosity (e.g., Hatziminaoglou et al 2003). However, massive MBHs keep on growing through dry mergers and less massive ones through wet mergers of low-mass galaxies that still harbor gas.…”

Section: Reliability Of the Modelmentioning

confidence: 99%

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CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

Salvador-Solé

Manrique

Guzmán

et al. 2016

ApJ

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We combine observational data on a dozen independent cosmic properties at high-z with the information on reionization drawn from the spectra of distant luminous sources and the cosmic microwave background (CMB) to constrain the interconnected evolution of galaxies and the intergalactic medium since the dark ages. The only acceptable solutions are concentrated in two narrow sets. In one of them reionization proceeds in two phases: a first one driven by Population III stars, completed atz 10, and after a short recombination period a second one driven by normal galaxies, completed atz 6. In the other set both kinds of sources work in parallel until full reionization atz 6. The best solution with double reionization gives excellent fits to all the observed cosmic histories, but the CMB optical depth is 3σ larger than the recent estimate from the Planck data. Alternatively, the best solution with single reionization gives less good fits to the observed star formation rate density and cold gas mass density histories, but the CMB optical depth is consistent with that estimate. We make several predictions, testable with future observations, that should discriminate between the two reionization scenarios. As a byproduct our models provide a natural explanation to some characteristic features of the cosmic properties at high-z, as well as to the origin of globular clusters.

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Section: Reliability Of the Modelmentioning

confidence: 99%

“…In Equation (11)  AGN is the so-called quasar-mode AGN heating efficiency, and á ñ L is the AGN bolometric luminosity L(t), averaged over the typical duration (t = 0.15 Gyr; acc Kelly et al 2010) of one such enlightening episodes. The bolometric light curve is modeled according to Hatziminaoglou et al (2003) through the expression…”

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confidence: 99%

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

Salvador-Solé

Manrique

Guzmán

et al. 2016

ApJ

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“…Investigations of how quasar X-ray parameters depend on black hole mass, M BH , and accretion rate relative to the Eddington rate,ṁ, offer important constraints on models of the disk/corona system. There have been attempts to link the evolution of SMBHs to analytic and semianalytic models of structure formation (e.g., Kauffmann & Haehnelt 2000;Hatziminaoglou et al 2003;Bromley et al 2004), where black holes grow by accreting gas funneled toward the center during a galaxy merger until feedback energy from the SMBH expels gas and shuts off the accretion process (e.g., Silk & Rees 1998;Fabian 1999;Wyithe & Loeb 2003;Begelman & Nath 2005). This self-regulated growth of black holes has recently been successfully applied in smoothed particle hydrodynamics simulations Springel et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Observational Constraints on the Dependence of Radio‐Quiet Quasar X‐Ray Emission on Black Hole Mass and Accretion Rate

Kelly

Bechtold

Trump

et al. 2008

ASTROPHYS J SUPPL S

126

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In this work we use a sample of 318 radio-quiet quasars (RQQs) to investigate the dependence of the ratio of optical/UV flux to X-ray flux, ox , and the X-ray photon index, À X , on black hole mass, UV relative to Eddington luminosity, and X-ray relative to Eddington luminosity. Our sample is drawn from the literature, with X-ray data from ROSAT and Chandra, and optical data mostly from the SDSS; 153 of these sources have estimates of À X from Chandra. We estimate M BH using standard estimates derived from the H, Mg ii, and C iv broad emission lines. Our sample spans a broad range in black hole mass (10 6 P M BH /M P 10 10 ), redshift (0 < z < 4:8), and luminosity (10 43 P kL k (2500 8)½ergs s À1 P 10 48 ). We find that ox increases with increasing M BH and L UV /L Edd and decreases with increasing L X /L Edd . In addition, we confirm the correlation seen in previous studies between À X and M BH and both L UV /L Edd and L X /L Edd ; however, we also find evidence that the dependence of À X of these quantities is not monotonic, changing sign at M BH $ 3 ; 10 8 M . We argue that the ox correlations imply that the fraction of bolometric luminosity emitted by the accretion disk, as compared to the corona, increases with increasing accretion rate relative to the Eddington rate,ṁ. In addition, we argue that the À X trends are caused by a dependence of X-ray spectral index onṁ. We discuss our results within the context of accretion models with Comptonizing corona and discuss the implications of the ox correlations for quasar feedback. To date, this is the largest study of the dependence of RQQ X-ray parameters on black hole mass and related quantities, and the first to attempt to correct for the large statistical uncertainty in the broad-line mass estimates.

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“…It is thus clear that the growth of the BH and the evolution of the host galaxy are related, so it is generally assumed that their co-evolution is mainly the result of merger events within the hierarchical scenario of large Postdoctoral Fellow of the Japan Society for the Promotion of Science. structure formation (Haehnelt et al 1998;Kaufman & Heahnelt 2000;Menou et al 2001;Hatziminaoglou et al 2003).…”

Section: Introduction and Rationalementioning

confidence: 99%

Super-Eddington accretion rates in Narrow Line Seyfert 1 galaxies

Collin¹,

Kawaguchi²

2004

A&A

125

102

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Abstract. We use the BH masses deduced from the empirical relation of Kaspi et al. (2000) between the size of the Broad Line Region (BLR) of Active Galactic Nuclei (AGN) and the optical luminosity, to compute their accretion rates in four samples of AGN, assuming that the optical luminosity is provided by the accretion disc. We show that Narrow Line Seyfert Galaxies 1 (NLS1s) accrete at super-Eddington rates, while their luminosity stays of the order of the Eddington limit. We take into account the possibility of a non-viscous energy release inversely proportional to the square of the distance in the gravitationally unstable region of the disc emitting a fraction of the optical luminosity. It leads to a smaller accretion rate and to a redder continuum than a standard disc, which agrees better with the observations. The observed bolometric luminosities appear to saturate at a few times the Eddington luminosity for super-Eddington accretion rates, as predicted by slim disc models. They favor a Kerr BH rather than a Schwarzschild one. Even when the accretion rate is super-Eddington, it stays always of the order of a few M /yr, irrespective of the BH mass, indicating that the growing of the BH is mass-supply-limited and therefore regulated by an exterior mechanism, and not Eddington-limited. The mass of the BH increases by one order of magnitude in a few 10 7 years, a time smaller than that necessary for changing the bulge mass. This is in agreement with recent claims that the BHs of NLS1s do not follow the same black hole -bulge relation as other galaxies. Since they represent about 10% of AGN up to a redshift of 0.5, these "super-active" phases should play an important role in shaping the mass function of local BHs. We finally discuss the possibility that the masses could be systematically underestimated due to an inclination effect, and we conclude that this could indeed be the case, and that the accretion rates could thus be strongly overestimated in a small fraction of objects, possibly explaining the existence of apparently extremely high accretors.

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Major mergers of haloes, the growth of massive black holes and the evolving luminosity function of quasars

Cited by 27 publications

References 67 publications

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

Observational Constraints on the Dependence of Radio‐Quiet Quasar X‐Ray Emission on Black Hole Mass and Accretion Rate

Super-Eddington accretion rates in Narrow Line Seyfert 1 galaxies

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