Evolution of active galaxies: black-hole mass–bulge relations for narrow line objects

Mathur, S.; Kuraszkiewicz, Joanna

doi:10.1016/s1384-1076(01)00058-6

Cited by 149 publications

(187 citation statements)

References 38 publications

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“…However, we know that, at least at low redshift, the SMBH-bulge mass relation is unlikely to be universal (Mathur et al 2001Graham et al 2011, and references therein). Furthermore, Batcheldor (2010) suggest that selection effects are important in shaping the SMBH-bulge mass relation.…”

Section: Error Budgetsmentioning

confidence: 99%

Faint high-redshift AGN in theChandradeep field south: the evolution of the AGN luminosity function and black hole demography

Fiore

Puccetti²,

Grazian

et al. 2011

A&A

156

172

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Context. We present detection and analysis of faint X-ray sources in the Chandra deep field south (CDFS) using the 4 Ms Chandra observation. Aims. We place constraints on active galactic nuclei (AGN) luminosity functions at z = 3-7, its cosmological evolution, and highredshift black hole and AGN demography. Methods. We use a new detection algorithm, using the entire three-dimensional data-cube (position and energy), and searching for X-ray counts at the position of high-z galaxies in the GOODS-South survey.Results. This optimized technique results in the identification of 54 AGN at z > 3, 29 of which are new detections. Applying stringent completeness criteria, we derive AGN luminosity functions in the redshift bins 3-4, 4-5, and >5.8 and for 42.75 < log L(2-10 keV) < 44.5. We combine this data with the luminous AGN luminosity functions from optical surveys and find that the evolution of the high-z, wide luminosity range luminosity function can be modeled by pure luminosity evolution with L * decreasing from 6.6 × 10 44 erg/s at z = 3 to L * = 2 × 10 44 erg/s at z = 6. We compare the high-z luminosity function with the predictions of theoretical models using galaxy interactions as AGN triggering mechanism. We find that these models are broadly able to reproduce the high-z AGN luminosity functions. Closer agreement is found when we assume a minimum dark matter halo mass for black hole formation and growth. We compare our AGN luminosity functions with galaxy mass functions to derive the high-z AGN duty cycle, using observed Eddington ratio distributions to derive black hole masses. We find that the duty cycle increases with galaxy stellar mass and redshift by a factor of 10-30 from z = 0.25 to z = 4-5. We also report the detection of a large fraction of highly obscured, Compton thick AGN at z > 3 (18 +17 −10 %). Their optical counterparts do not show any reddening and we thus conclude that the size of the X-ray absorber is likely smaller than the dust sublimation radius. We finally report the discovery of a highly star-forming galaxy at z = 3.47, arguing that its X-ray luminosity is likely dominated by stellar sources. If confirmed, this would be one of the farthest objects in which stellar sources have been detected in X-rays.

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Section: Error Budgetsmentioning

confidence: 99%

Faint high-redshift AGN in theChandradeep field south: the evolution of the AGN luminosity function and black hole demography

Fiore

Puccetti²,

Grazian

et al. 2011

A&A

156

172

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“…All the data and the models have been converted to a common Chabrier (2003) (2012) and Sani et al (2011) report BH masses from multiple sources (please see their papers for details). Finally, we also add another two BH masses from Woo et al (2010) and Mathur et al (2001). Different authors have used different techniques to estimate BH (and bulge) masses, and each technique has its own set of errors.…”

Section: Datamentioning

confidence: 99%

“…Different observations now question that BH-host correlations indeed appear as tight as previously claimed for all types of galaxies (e.g., Hu 2008;Graham 2008;Gültekin et al 2009;Graham & Li 2009). Significant outliers exist (e.g., Mathur et al 2001;Grupe & Mathur 2004;Watson et al 2007), BHs are currently observed also in the centres of bulgeless galaxies (e.g., Ghosh et al 2008;Satyapal et al 2009;Araya salvo et al 2012), and the AGN-starformation correlations disappear for all but highest luminosity AGNs (Shao et al 2010;Grier et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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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“…In practice, however, width of the [OIII] emission line is often used in stead of stellar velocity dispersion due to observational difficulty of the latter. Using such an approach several groups of authors explored the M BH − σ * relation for NLS1s recently, with conflicting results: Mathur et al (2001), Grupe & Mathur (2004), Bian & Zhao (2004), and Botte et al (2004) found that NLS1s showed a systematically lower M BH /M bulge ratio than normal broad line AGNs, while Wang & Lu (2001), Wandel (2002 did not find a clear difference between the two. The difference may be attributed, at least partly, to the different line widths used by the different authors.…”

Section: Black Hole-bulge Relation In Nls1smentioning

confidence: 99%

A Comprehensive Study of 2000 Narrow Line Seyfert 1 Galaxies from the Sloan Digital Sky Survey. I. The Sample

Zhou

Wang

Yuan

et al. 2006

ASTROPHYS J SUPPL S

308

316

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This is the first paper in a series dedicated to the study of the emission-line and continuum properties of narrow line Seyfert 1 galaxies (NLS1s). We carried out a systematic search for NLS1s from objects assigned as "QSOs" or "galaxies" in the spectroscopic sample of the Sloan Digital Sky Survey Data Release 3 (SDSS DR3) by a careful modeling of their emission lines and continua. The result is a uniform sample comprising ∼ 2 000 NLS1. This sample dramatically increases the number of known NLS1 by a factor of ∼ 10 over previous compilations. This paper presents the parameters of the prominent emission lines and continua, which were measured accurately with typical uncertainties < 10%. Taking advantage of such an unprecedented large and uniform sample with accurately measured spectral parameters, we carried out various statistical analysis, some of which were only possible for the first time. The main results found are as follows.(1) Within the overall Seyfert 1 population, the incidence of NLS1s is strongly dependent on the optical, X-ray, and radio luminosities as well as the radioloudness. The fraction of NLS1 peaks around SDSS g-band absolute magnitude M g ∼ −22 m in the optical and ∼ 10 43.2 erg s −1 in the soft X-ray band, and decreases quickly as the radio-loudness increases. (2) On average the relative FeII emission, R 4570 = F eII(4434 − 4684)/Hβ, in NLS1s is about twice that in normal AGNs, and is anti-correlated with the broad component width of the Balmer emission lines. (3) The well-known anti-correlation between the width of broad low-ionization lines and the soft X-ray spectral slope for broad line AGNs extends down to F W HM ∼ 1 000 km s −1 in NLS1s, but the trend appears to

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Evolution of active galaxies: black-hole mass–bulge relations for narrow line objects

Cited by 149 publications

References 38 publications

Faint high-redshift AGN in theChandradeep field south: the evolution of the AGN luminosity function and black hole demography

Faint high-redshift AGN in theChandradeep field south: the evolution of the AGN luminosity function and black hole demography

Black holes in pseudobulges: demography and models

A Comprehensive Study of 2000 Narrow Line Seyfert 1 Galaxies from the Sloan Digital Sky Survey. I. The Sample

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