Journey to the MBH-σ relation: the fate of low-mass black holes in the Universe

By M. Volonteri, P. Natarajan. 2009

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In this paper, we explore the establishment and evolution of the empirical correlation between black hole mass (MBH) and velocity dispersion (σ ) with redshift. We trace the growth and accretion history of massive black holes (MBHs) starting from high-redshift seeds that are planted via physically motivated prescriptions. Two seeding models are explored in this work: ‘light seeds’, derived from Population III remnants, and ‘heavy seeds’, derived from direct gas collapse. Even though the seeds themselves do not satisfy the M BH–σ relation initially, we find that the relation can be established and maintained at all times if self-regulating accretion episodes are associated with major mergers. The massive end of the M BH–σ relation is established early, and lower mass MBHs migrate on to it as hierarchical merging proceeds. How MBHs migrate towards the relation depends critically on the seeding prescription. Light seeds initially lie well below the M BH–σ relation, and MBHs can grow via steady accretion episodes unhindered by self-regulation. In contrast, for the heavy seeding model, MBHs are initially over-massive compared to the empirical correlation, and the host haloes assemble prior to kick-starting the growth of the MBH. We find that the existence of the M BH–σ correlation is purely a reflection of the merging hierarchy of massive dark matter haloes. The slope and scatter of the relation however appear to be a consequence of the seeding mechanism and the self-regulation prescription. We expect flux limited active galactic nucleus surveys to select MBHs that have already migrated on to the M BH–σ relation. Similarly, the Laser Interferometer Space Antenna (LISA) is also likely to be biased towards detecting merging MBHs that preferentially inhabit the M BH–σ . These results are a consequence of major mergers being more common at high redshift for the most massive, biased, galaxies that host MBHs which have already migrated on to the M BH–σ relation. We also predict the existence of a large population of low-mass ‘hidden’ MBHs at high redshift which can easily escape detection. Additionally, we find that if MBH seeds are massive, ∼10 5 M� , the low-mass end of the M BH–σ flattens towards an asymptotic value, creating a characteristic ‘plume’.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/593f1bf7577ca9c15f55db7cea2ed75fdc9f06b3

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CONSTRAINTS ON BLACK HOLE GROWTH, QUASAR LIFETIMES, AND EDDINGTON RATIO DISTRIBUTIONS FROM THE SDSS BROAD-LINE QUASAR BLACK HOLE MASS FUNCTION (2010, result): “…estimates of the mass distribution of SMBH seeds suggest that typical values for the seed mass should be MBH ∼ 105–106 M at z ∼ 10 (Lodato & Natarajan 2007; Pelupessy et al. 2007; Volonteri et al. 2008), and grow to MBH ∼ 108 M by z ∼ 3 (Volonteri & Natarajan 2009), consistent with our results.”
REVISITING THE SCALING RELATIONS OF BLACK HOLE MASSES AND HOST GALAXY PROPERTIES (2012, background): “However, there are currently insufficient data to probe the 30−100 km s−1 range, where scatter in M• could identify the initial formation mechanism for massive black holes (Volonteri et al. 2008; Volonteri & Natarajan 2009).”
What drives the growth of black holes (2011, background): “…it is possible that these late-type systems have never undergone a galaxy major merger, and a non-negligible fraction of the BH mass may be from the massive BH seed formation (e.g., Kormendy & Kennicutt 2004; Volonteri & Natarajan 2009; see §4.3 for the discussion of the formation of massive BHs).”
A ∼50,000 M⊙ SOLAR MASS BLACK HOLE IN THE NUCLEUS OF RGG 118 (2015, background): “Volonteri & Natarajan (2009) found that for BH masses .”
Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, background): “Late type dwarfs are thus the preferred site for the search of pristine black holes (Volonteri and Natarajan, 2009).”
The evolution of massive black holes and their spins in their galactic hosts (2012, methodology): “This population of outliers is also found for instance in the model of Volonteri & Natarajan (2009), but remarkably not in the “two-phase” galaxy-formation model proposed by Cook, Lapi, & Granato (2009); Cook et al. (2010a,b) (see in particular Fig.”
On the correlations between galaxy properties and supermassive black hole mass (2011, background): “Volonteri & Natarajan (2009) investigated through numerical simulations the observational signature of the self-regulated SMBH growth by analysing the mass assembly history of black hole seeds.”
RELATIONS BETWEEN CENTRAL BLACK HOLE MASS AND TOTAL GALAXY STELLAR MASS IN THE LOCAL UNIVERSE (2015, background): “Volonteri & Natarajan (2009) and van Wassenhove et al. (2010) suggested that if BH seeds are massive, e.g., 105 M⊙, as predicted by ‘direct collapse’ models, the low-mass end of the relation between BHs and galaxies (they specifically referred to the correlation with the velocity dispersion, but…”
THE NON-CAUSAL ORIGIN OF THE BLACK-HOLE–GALAXY SCALING RELATIONS (2010, background): “…either explicitly include AGN feedback (e.g. Croton et al. 2006; Robertson et al. 2006; Booth & Schaye 2009; Johansson et al. 2009; Shankar et al. 2009) or couple the merging scenario with a self regulation prescription for BH growth (e.g. Kauffmann & Haehnelt 2000; Volonteri & Natarajan 2009).”
A New Sample of (Wandering) Massive Black Holes in Dwarf Galaxies from High-resolution Radio Observations (2019, background): “…signatures of BH seeding should be strongest in dwarf galaxies, with the BH occupation fraction and scaling relations at low masses varying depending on whether the seeds are light or heavy (Volonteri et al. 2008; Volonteri & Natarajan 2009; van Wassenhove et al. 2010; Ricarte & Natarajan 2018).”
DWARF GALAXIES WITH OPTICAL SIGNATURES OF ACTIVE MASSIVE BLACK HOLES (2013, background): “Studying the scaling relations between BHs and galaxies at low-mass may provide further clues (e.g., Volonteri & Natarajan 2009).”