Observational evidence for a connection between supermassive black holes and dark matter haloes

Baes, M.; Buyle, Pieter; Hau, G. K. T.; Dejonghe, Herwig

doi:10.1046/j.1365-8711.2003.06680.x

Cited by 157 publications

(238 citation statements)

References 39 publications

Supporting

Mentioning

215

Contrasting

Order By: Relevance

“…The M BH -σ relation, together with the observed correlation between outer circular velocity and central velocity dispersion measured by several groups (e.g., Ferrarese 2002;Baes et al 2003;Pizzella et al 2005;Buyle et al 2006), implies a mean correlation between BH mass and the mass or virial velocity of the host galaxy's dark matter halo, although with a possibly large scatter (e.g., Ho 2007aHo , 2007b. Recent observational studies have attempted to constrain the evolution of the BHs and their host galaxies, by measuring the M BH -σ relation at 0 < z 3, finding only tentative evidence for larger BHs at fixed velocity dispersion or stellar mass (e.g., McLure et al 2006;Peng et al 2006;Shields et al 2006;Treu et al 2007;Shankar et al 2009a) with respect to what is observed locally.…”

Section: Introductionmentioning

confidence: 69%

On the Radiative Efficiencies, Eddington Ratios, and Duty Cycles of Luminous High-Redshift Quasars

Shankar¹,

Crocce²,

Miralda-Escudé³

et al. 2010

ApJ

134

184

View full text Add to dashboard Cite

We investigate the characteristic radiative efficiency , Eddington ratio λ, and duty cycle P 0 of high-redshift active galactic nuclei (AGNs), drawing on measurements of the AGN luminosity function at z = 3-6 and, especially, on recent measurements of quasar clustering at z = 3-4.5 from the Sloan Digital Sky Survey. The free parameters of our models are , λ, and the normalization, scatter, and redshift evolution of the relation between black hole (BH) mass M BH and halo virial velocity V vir . We compute the luminosity function from the implied growth of the BH mass function and the quasar correlation length from the bias of the host halos. We test our adopted formulae for the halo mass function and halo bias against measurements from the large N-body simulation developed by the MICE collaboration. The strong clustering of AGNs observed at z = 3 and, especially, at z = 4 implies that massive BHs reside in rare, massive dark matter halos. Reproducing the observed luminosity function then requires high efficiency and/or low Eddington ratio λ, with a lower limit (based on 2σ agreement with the measured z = 4 correlation length)0.7λ/(1 + 0.7λ), implying 0.17 for λ > 0.25. Successful models predict high duty cycles, P 0 ∼ 0.2, 0.5, and 0.9 at z = 3.1, 4.5, and 6, respectively, and they require that the fraction of halo baryons locked in the central BH is much larger than the locally observed value. The rapid drop in the abundance of the massive and rare host halos at z > 7 implies a proportionally rapid decline in the number density of luminous quasars, much stronger than simple extrapolations of the z = 3-6 luminosity function would predict. For example, our most successful model predicts that the highest redshift quasar in the sky with true bolometric luminosity L > 10 47.5 erg s −1 should be at z ∼ 7.5, and that all quasars with higher apparent luminosities would have to be magnified by lensing.

show abstract

Section: Introductionmentioning

confidence: 69%

On the Radiative Efficiencies, Eddington Ratios, and Duty Cycles of Luminous High-Redshift Quasars

Shankar¹,

Crocce²,

Miralda-Escudé³

et al. 2010

ApJ

134

184

View full text Add to dashboard Cite

show abstract

“…In the absence of an explicit bulge-disk decomposition from the surface photometry, we can get an orderof-magnitude estimate of the bulge luminosity using the morphological type of the galaxy and its total luminosity. We adopt the empirical relation given in Simien & de Vaucouleurs (1986) to estimate the contribution of the disk to the total luminosity of a disk galaxy: If Ϫ3 ≤ T ≤ 7, then Dm p 0.324(T ϩ bul , where T is the numerical a tight correlation with the stellar velocity dispersion in spiral galaxies in which extended rotation curves are available (Ferrarese 2002;Baes et al 2003;Courteau et al 2007). As part of the SINGS data deliveries, Ha rotation curves are available for NGC 3621 (Daigle et al 2006).…”

Section: Estimating the Bolometric Luminosity Of The Agn And Limits Omentioning

confidence: 99%

The Discovery of an Active Galactic Nucleus in the Late-Type Galaxy NGC 3621: Spitzer Spectroscopic Observations

Satyapal

Vega

Heckman

et al. 2007

ApJ

116

139

View full text Add to dashboard Cite

We report the discovery of an active galactic nucleus (AGN) in the nearby SAd galaxy NGC 3621 using Spitzer high spectral resolution observations. These observations reveal the presence of [Ne v] 14 and 24 mm emission that is centrally concentrated and peaks at the position of the near-infrared nucleus. Using the [Ne v] line luminosity, we estimate that the nuclear bolometric luminosity of the AGN is ∼ ergs s Ϫ1 , which, 41 5 # 10 based on the Eddington limit, corresponds to a lower mass limit of the black hole of ∼ M , . Using an 3 4 # 10 order-of-magnitude estimate for the bulge mass based on the Hubble type of the galaxy, we find that this lower mass limit does not put a strain on the well-known relationship between the black hole mass and the host galaxy's stellar velocity dispersion established in predominantly early-type galaxies. Multiwavelength follow-up observations of NGC 3621 are required to obtain more precise estimates of the bulge mass, black hole mass, accretion rate, and nuclear bolometric luminosity. The discovery reported here adds to the growing evidence that a black hole can form and grow in a galaxy with no or minimal bulge.

show abstract

“…1 in Baes et al 2003) and ignored in our calculation. Equation (41) may not hold for < 80 km s À1 , which corresponds to BH mass P4 Â 10 6 M according to the BH mass-velocity dispersion relation below (eq.…”

Section: The Local Bh Mass Function and Qso Luminosity Function Obtaimentioning

confidence: 99%

Constraints on QSO Models from a Relation between the QSO Luminosity Function and the Local Black Hole Mass Function

2004

ApJ

140

View full text Add to dashboard Cite

QSOs are believed to be powered by accretion onto massive black holes (BHs). In this paper, assuming that each central BH in nearby galaxies has experienced the QSO phase and ignoring BH mergers, we establish a relation between the QSO luminosity function (LF) and the local BH mass function (MF). The QSOLF is jointly controlled by the luminosity evolution of individual QSOs and the triggering history of the accretion onto seed BHs. By comparing the time integral of the QSOLF with that inferred from local BHs, we separate the effect of the luminosity evolution of individual QSOs from the effect of the triggering history. Assuming that the nuclear luminosity evolution includes two phases (first increasing at the Eddington luminosity with growth of BHs and then declining), we find that observations are generally consistent with the expected relation between the QSOLF and the local BHMF and obtain the following constraints on QSO models and BH growth: (i) The QSO mass-toenergy efficiency should be k0.1. (ii) The lifetime (defined directly through the luminosity evolution of individual QSOs here) should be k4 Â 10 7 yr. The characteristic declining timescale in the second phase should be significantly shorter than the Salpeter timescale Sp , and BH growth should not be dominated by the second phase. (iii) The ratio of obscured QSOs/AGNs to optically bright QSOs should be not larger than 7 at M B $ À23 and 3 at M B $ À26 if ¼ 0:31, and not larger than 1 at M B $ À23 and negligible at M B $ À26 if ¼ 0:1. (iv) It is unlikely that most QSOs are accreting at super-Eddington luminosities. We point out that it is hard to accurately estimate the value of the QSO lifetime from the QSOLF and/or the local BHMF, if it is longer than a certain value (e.g., $4 Sp in this study). We discuss the importance of accurate measurements of the intrinsic scatter in the BH mass and velocity dispersion relation of local galaxies and the scatter in the bolometric correction of QSOs. We also discuss some possible applications of the work in this paper, such as to the study of the demography of QSOs and the demography of normal galaxies at intermediate redshift.

show abstract

Observational evidence for a connection between supermassive black holes and dark matter haloes

Cited by 157 publications

References 39 publications

On the Radiative Efficiencies, Eddington Ratios, and Duty Cycles of Luminous High-Redshift Quasars

On the Radiative Efficiencies, Eddington Ratios, and Duty Cycles of Luminous High-Redshift Quasars

The Discovery of an Active Galactic Nucleus in the Late-Type Galaxy NGC 3621: Spitzer Spectroscopic Observations

Constraints on QSO Models from a Relation between the QSO Luminosity Function and the Local Black Hole Mass Function

Contact Info

Product

Resources

About