THE ASSEMBLY OF SUPERMASSIVE BLACK HOLES AT HIGH REDSHIFTS

By Takamitsu L. Tanaka, Zoltán Haiman. 2008

227 citations recorded by the source corpus.

The supermassive black holes (SMBHs) massive enough (≳ few ×109 M☉) to power the bright redshift z ≈ 6 quasars observed in the Sloan Digital Sky Survey (SDSS) are thought to have assembled by mergers and/or gas accretion from less massive “seed” BHs. If the seeds are the ∼102 M☉ remnant BHs from the first generation of stars, they must be in place well before redshift z = 6, and must avoid being ejected from their parent protogalaxies by the large (several ×102 km s−1) kicks they suffer from gravitational-radiation-induced recoil during mergers with other BHs. We simulate the SMBH mass function at redshift z > 6 using dark matter halo merger trees, coupled with a prescription for the halo occupation fraction, accretion histories, and radial recoil trajectories of the growing BHs. Our purpose is (1) to map out plausible scenarios for successful assembly of the z ≈ 6 quasar BHs by exploring a wide region of parameter space, and (2) to predict the rate of low-frequency gravitational wave events detectable by the Laser Interferometer Space Antenna (LISA) for each such scenario. Our main findings are as follows: (1) ∼100 M☉ seed BHs can grow into the SDSS quasar BHs without super-Eddington accretion, but only if they form in minihalos at z ≳ 30 and subsequently accrete ≳60% of the time; (2) the scenarios with optimistic assumptions required to explain the SDSS quasar BHs overproduce the mass density in lower mass (few ×105 M☉ ≲ Mbh≲ few × 107 M☉) BHs by a factor of 102–103, unless seeds stop forming, or accrete at a severely diminished rates or duty cycles (e.g., due to feedback), at z ≲ 20–30. We also present several successful assembly models and their LISA detection rates, including a “maximal” model that gives the highest rate (∼30 yr−1 at z = 6) without overproducing the total SMBH density.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f971c504be44a0d8eee21ab91a483b49a39fbb08

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Citations in the corpus

Hyper-Eddington accretion flows on to massive black holes (2015, background): “In any of these cases, seed BHs with ∼ 102−5 M⊙ still need to grow by subsequent accretion and mergers up c© 0000 RAS 2 to SMBHs with ∼ 109 M⊙ by z > 6 (e.g. Tanaka & Haiman 2009).”
Supermassive black hole formation by direct collapse: keeping protogalactic gas H2 free in dark matter haloes with virial temperatures Tvir > rsim 104 K (2009, background): “This requires a preferential suppression of BH growth in low–mass halos, plausibly due to negative feedback effects acting on these halos (Bromley et al. 2004; Tanaka & Haiman 2009).”
Ubiquitous seeding of supermassive black holes by direct collapse (2012, background): “Mergers of Pop III seed BHs at high redshifts can also, in principle, build up supermassive BHs (Tanaka & Haiman 2009), although slingshot effectsand merger time scales pose problems for this scenario (see e.g.th reviews by Natarajan 2011; Volonteri 2010, and references therein).”
Formation of supermassive black holes (2010, background): “How could the seed massive black holes have grown rapidly enough within this short timespan is still an open question (e.g., Haiman, 2004; Shapiro, 2005; Volonteri and Rees, 2006; Tanaka and Haiman, 2009).”
SUPER-CRITICAL GROWTH OF MASSIVE BLACK HOLES FROM STELLAR-MASS SEEDS (2014, background): “…et al. 2003), these could grow into billion-solar-mass holes by z ∼ 7 only if all the following conditions were fullfilled: 1) seeds were present early on, at z ∼ > 20; 2) gas accretion continued more or less uninterrupted at the Eddington rate for ∼> 0.6 Gyr; and 3) ǫ < 0.1 (Tanaka & Haiman 2009).”
Black hole formation in the early Universe (2013, background): “…for the formation of massive black holes have been suggested (Rees 1978; Djorgovski et al. 2008; Begelman & Shlosman 2009; Regan & Haehnelt 2009b; Tanaka & Haiman 2009; Volonteri 2010; Haiman 2012; Johnson et al. 2012, 2013; Choi, Shlosman & Begelman 2013; Melia 2013; Prieto, Jimenez & Haiman…”
Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes (2018, background): “…more worrying question, is the extent to which a massive seed black hole can continue growing without merger events in an isolated halo (e.g., Tanaka & Haiman 2009) Though still uncertain, progress on this front may come soon from the search for IMBH relics in the low-redshift Universe (see…”
Formation of Supermassive Black Hole Seeds (2016, background): “However, the gravitational recoil velocities are about the order of ∼ 1000 km/s which are much larger than the escape velocity of halos (10 km/s) and therefore lead to the ejection of BHs from the shallow DM potentials at earlier comic times (Haiman 2004; Tanaka & Haiman 2009).”
Self-Interacting Dark Matter from a Non-Abelian Hidden Sector (2014, background): “[97] T.”