On the evolution of the black‐hole/spheroid mass ratio

By R. McLure, Michael J. Jarvis, Thomas Targett, J. Dunlop, P. Best. 2005

148 citations recorded by the source corpus.

We present the results of a study which uses the 3CRR sample of radio-loud active galactic nuclei (AGN) to investigate the evolution of the black-hole:spheroid relation in the most massive early-type galaxies from 0 < z < 2. Radioloud unification is exploited to obtain virial (line-width) black-hole mass estimates from the 3CRR quasars, and stellar mass estimates from the 3CRR radio galaxies, thereby providing black-hole and stellar mass estimates for a single population of early-type galaxies. At low redshift (z < 1) the 3CRR sample is consistent with a black-hole:spheroid ratio ofMbh/Msph ≃ 0.002, in good agreement with that observed locally for quiescent galaxies of similar stellar mass (Msph ≃ 5 × 1011 M⊙). However, over the redshift interval 0 < z < 2 the 3CRR black-hole:spheroid ratio is found to evolve as Mbh/Msph ∝ (1 + z )2.07±0.76, reaching Mbh/Msph ≃ 0.008 by redshift z ≃ 2. This evolution is found to be inconsistent with the local black-hole:spheroid ratio remaining constant at a moderately significant level (98%). If confirmed, the detection of evolution in the 3CRR black-hole:spheroid mass ratio further strengthens the evidence that, at least for massive early-type galaxies, the growth of the central supermassive black hole may be completed before that of the host spheroid. (© 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/70c32d4bb3fae31d9fda53d111582935191667b2

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In Astronomy and Astrophysics

1. D. M. Alexander
2. L. Hernquist
3. P. Hopkins
4. M. Volonteri
5. D. Narayanan
6. R. Dav'e
7. R. Somerville
8. C. Casey

In Nuclear and High Energy Physics

1. A. Merloni
2. D. M. Alexander
3. R. Ivison
4. P. Padovani
5. I. Smail
6. S. Heinz
7. D. Narayanan
8. C. Casey

Citations in the corpus

• The quasar relation through cosmic time – II. Evidence for evolution from z = 3 to the present age (2009, background): “studies suggest that, for a given galaxy mass, black holes in high-z AGN are more massive than their low-z counter-parts (e.g., McLure et al. 2006; Peng et al. 2006a,b).”
• A synthesis model for AGN evolution: supermassive black holes growth and feedback modes (2008, background): “…have recently attempted to push the study of scaling relations toz > 0, despite the large observational biases (Merloni, Rudnick & Di Matteo 2004; McLure et al. 2006; Shields et al. 2006; Peng et al. 2006; Wu 2007; Treu et al. 2007; Salviander et al. 2007; Shen et al. 2008; Schramm, Wisotzki &…”
• EDDINGTON-LIMITED ACCRETION AND THE BLACK HOLE MASS FUNCTION AT REDSHIFT 6 (2010, background): “…tend to show higher than local ratios of MBH/Mstellar at all redshifts; z < 1 (Mathur & Grupe 2005; Woo et al. 2008), 1 < z < 4 (Peng et al. 2006; McLure et al. 2006; Merloni et al. 2010); z > 4 (Walter et al. 2004; Riechers et al. 2008; Wang et al. 2010), whereas studies based on z ≈ 2…”
• Dusty Star Forming Galaxies at High Redshift (2014, background): “They find that SMGs have black-hole masses to galaxy mass ratios 3–5× lower than local relationship (Häring and Rix, 2004), and much lower than other highredshift populations of AGN (McLure et al., 2006; Peng et al., 2006).”
• The stochastic gravitational-wave background from massive black hole binary systems: implications for observations with Pulsar Timing Arrays (2008, methodology): “McLure et al. 2006 found MBH/Mbulge ∝ (1 + z)2, but the normalisation of their best fit to this relation at z = 0 is lower than 0.0014; the relation given by equation (39) is within the error bars given by McLure et al. 2006 for 0.4 < z < 0.8.”
• Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays (2008, methodology): “Figure 3 shows that in the most pessimistic case – TrNA model, that has the sharpest cut–off of the MBHB mass function bright end – a precision of ≈ 5ns should guarantee a positive detection; in the optimistic La-DA case, a precision of ≈ 50ns should be sufficient.”
• Testing the evolutionary link between submillimetre galaxies and quasars: CO observations of QSOs at z∼ 2 (2008, unknown): “Thus our CO survey of z ∼ 2 QSOs appears to support the claim that MBH/Msph for z > 1 AGN is higher than observed locally (e.g. Peng et al. 2006; McLure et al. 2006).”
• Four Quasars above Redshift 6 Discovered by the Canada-France High-z Quasar Survey (2007, background): “…evolution of this relation with redshift is not well known and attempts are now being made to determine the relation up toz = 3 because it is a crucial component of galaxy evolution models (Shields et al. 2003; Adelberger & Steidel 2005; Alexander et al. 2005; Peng et al. 2006; McLure et al. 2006).”
• HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE FORMATION OF MASSIVE EARLY-TYPE GALAXIES (2011, background): “Therefore, the local ratioM•/M⋆ ≈ 2×10 −3 (Marconi & Hunt 2003) between the black hole mass M• and the stellar mass M⋆ of the host ETG should be already in place then (but see also McLure et al. 2006 and Peng et al. 2006).”
• SELF-CONSISTENT MODELS OF THE AGN AND BLACK HOLE POPULATIONS: DUTY CYCLES, ACCRETION RATES, AND THE MEAN RADIATIVE EFFICIENCY (2007, result): “Our conclusions are in marginal agreement with those of McLure et al. (2006) and Shields et al. (2006) and in some disagreement with those of Peng et al. (2006), who find M•/Mstar in gravitationally lensed quasar hosts atz∼ 1−2 a factor∼ 3 above the local value.”
• Dust covering factor, silicate emission, and star formation in luminous QSOs (2007, background): “Indeed, Peng et al. (2006) and McLure et al. (2006) found that, for a given BH mass, QSO hosts at z∼2 are characterized by a stellar mass lower than expected from the local BH-galaxy mass relation.”
• Self-regulated growth of supermassive black holes by a dual jet-heating active galactic nucleus feedback mechanism: methods, tests and implications for cosmological simulations (2011, background): “Despite these difficulties, an increasing amount of data is suggesting that the MBH–Ms relationship shows some positive evolution with redshift (McLure et al. 2006; Peng et al. 2006; Shields et al. 2006; Salviander et al. 2007; Bennert et al. 2010; Decarli et al. 2010; Merloni et al. 2010).”
• Cosmic Evolution of Black Holes and Spheroids. II. Scaling Relations at z = 0.36 (2007, background): “Similar results are obtained by other studies of quasar host galaxies at comparable redshifts (Shields et al. 2006; McLure et al. 2006).”
• EMU: Evolutionary Map of the Universe (2011, background): “These sources provide constraints on the co-evolution of galaxy bulges and central supermassive black holes (Magorrian et al. 1998; McLure et al. 2006), trace (proto-)clusters at early times (e.g. Miley et al. 2006), and may be crucial in determining the impact that powerful radio activity has on…”