Modelling the cosmological co-evolution of supermassive black holes and galaxies – I. BH scaling relations and the AGN luminosity function

Marulli, F.; Bonoli, Silvia; Branchini, E.; Moscardini, L.; Springel, Volker

doi:10.1111/j.1365-2966.2008.12988.x

Cited by 121 publications

(205 citation statements)

References 144 publications

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“…Thus, the number of outliers in the BH-galaxy classical relations could be very high, impacting the demography of local BHs by severely reducing the expected number density of low mass BHs in the local Universe (similar thoughts were also put forward by Gadotti & Kauffmann 2009;Greene et al 2010). This in turn could have a non-negligible repercussion on accretion and merging models that try to tune parameters such as the radiative efficiency and Eddington ratio distributions by matching the full shape of the local BH mass function (e.g., Marulli et al 2008;Shankar et al 2012b). …”

Section: Discussionmentioning

confidence: 99%

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Black holes in pseudobulges: demography and models

Shankar

Marulli

Mathur

et al. 2012

A&A

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Context. There is mounting evidence that a significant fraction of black holes (BHs) today live in late-type galaxies, including bulgeless galaxies and those hosting pseudobulges, and are significantly undermassive with respect to the scaling relations followed by their counterpart BHs in classical bulges of similar stellar (or even bulge) mass. Aims. Here we discuss the predictions of two state-of-the-art hierarchical galaxy formation models in which BHs grow via mergers and, in one, also via disc instability. Our aim is to understand if the wealth of new data on local BH demography is consistent with standard models. Methods. We follow the merger trees of representative subsamples of BHs and compute the fractional contributions of different processes to the final BH mass. Results. We show that the model in which BHs always closely follow the growth of their host bulges, also during late disk instabilities (i.e., bars), produces too narrow a distribution of BHs at fixed stellar mass to account for the numerous low-mass BHs now detected in later-type galaxies. Models with a looser connection between BH growth and bar instability instead predict the existence of a larger number of undermassive BHs, in better agreement with the observations. Conclusions. The scatter in the updated local BH-bulge mass relation (with no restriction on galaxy type) appears to be quite large when including later-type systems, but it can still be managed to be reproduced within current hierarchical models. However, the fuelling of BHs during the late bar-instability mode needs to be better quantified/improved to properly fit the data. We conclude discussing how the possibly large number of BHs in later type galaxies demands for an in-depth revision of the local BH mass function and its modelling.

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Section: Discussionmentioning

confidence: 99%

“…While this type of comparison was pursued several times in the Literature (e.g., Lapi et al 2006;Marulli et al 2008), it was never performed before taking care of differentiating classical and pseudo bulges.…”

Section: Late-type Bulges: Bh Demography Revisitedmentioning

confidence: 99%

Black holes in pseudobulges: demography and models

Shankar

Marulli

Mathur

et al. 2012

A&A

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“…These models range from large cosmological hydrodynamic simulations (Degraf et al 2010;Khandai et al 2014;Hirschmann et al 2014;Sijacki et al 2014;Bachmann et al 2014, Rosas-Guevara et al, in preparation), semianalytical models (Cattaneo et al 2005;Marulli et al 2008;Bonoli et al 2009;Fanidakis et al 2012;Hirschmann et al 2012;Menci et al 2014;Neistein & Netzer 2014) to more phenomenological models (Wyithe & Loeb 2003;Shen 2009;Conroy & White 2013;Veale et al 2014;Caplar et al 2014). However, since these models differ in many details, in particular the trigger mechanisms for AGN activity, no consistent picture on the physics of BH growth can be inferred from these comparisons alone.…”

Section: Comparison To Model Predictionsmentioning

confidence: 99%

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

Schulze

Bongiorno

Gavignaud

et al. 2015

Monthly Notices of the Royal Astronomical Society

100

159

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We present a census of the active black hole population at 1 < z < 2, by constructing the bivariate distribution function of black hole mass and Eddington ratio, employing a maximum likelihood fitting technique. The study of the active black hole mass function (BHMF) and the Eddington ratio distribution function (ERDF) allows us to clearly disentangle the active galactic nuclei (AGN) downsizing phenomenon, present in the AGN luminosity function, into its physical processes of black hole mass downsizing and accretion rate evolution. We are utilizing type-1 AGN samples from three optical surveys (VVDS, zCOSMOS and SDSS), that cover a wide range of 3 dex in luminosity over our redshift interval of interest. We investigate the cosmic evolution of the AGN population as a function of AGN luminosity, black hole mass and accretion rate. Compared to z = 0, we find a distinct change in the shape of the BHMF and the ERDF, consistent with downsizing in black hole mass. The active fraction or duty cycle of type-1 AGN at z ∼ 1.5 is almost flat as a function of black hole mass, while it shows a strong decrease with increasing mass at z = 0. We are witnessing a phase of intense black hole growth, which is largely driven by the onset of AGN activity in massive black holes towards z = 2. We finally compare our results to numerical simulations and semi-empirical models and while we find reasonable agreement over certain parameter ranges, we highlight the need to refine these models in order to match our observations.

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“…Current observations require a correlation of the form M • ∝ M α σ β over a simple correlation with either σ or M at ≥3σ confidence (Hopkins et al 2007a;Hopkins 2008;Marulli et al 2008).…”

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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Modelling the cosmological co-evolution of supermassive black holes and galaxies – I. BH scaling relations and the AGN luminosity function

Cited by 121 publications

References 144 publications

Black holes in pseudobulges: demography and models

Black holes in pseudobulges: demography and models

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

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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