Papers › The ASTRID simulation: the evolution of Supermassive Black Holes
The ASTRID simulation: the evolution of Supermassive Black Holes
Yueying Ni, Tiziana Di Matteo, Simeon Bird, Rupert Croft, Yu Feng, Nianyi Chen, Michael Tremmel, Colin DeGraf, Yin Li
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We present the evolution of black holes (BHs) and their relationship with their host galaxies in Astrid, a large-volume cosmological hydrodynamical simulation with box size 250 h⁻¹ Mpc containing 2×5500³ particles evolved to z=3. Astrid statistically models BH gas accretion and AGN feedback to their environments, applies a power-law distribution for BH seed mass M_(sd), uses a dynamical friction model for BH dynamics and executes a physical treatment of BH mergers. The BH population is broadly consistent with empirical constraints on the BH mass function, the bright end of the luminosity functions, and the time evolution of BH mass and accretion rate density. The BH mass and accretion exhibit a tight correlation with host stellar mass and star formation rate. We trace BHs seeded before z>10 down to z=3, finding that BHs carry virtually no imprint of the initial M_(sd) except those with the smallest M_(sd), where less than 50\% of them have doubled in mass. Gas accretion is the dominant channel for BH growth compared to BH mergers. With dynamical friction, Astrid predicts a significant delay for BH mergers after the first encounter of a BH pair, with a typical elapse time of about 200 Myrs. There are in total 4.5 ×10⁵ BH mergers in Astrid at z>3, ∼10³ of which have X-ray detectable EM counterparts: a bright kpc scale dual AGN with L_X>10⁴³ erg/s. BHs with M_(BH) ∼10⁷⁻⁸ M_⊙ experience the most frequent mergers. Galaxies that host BH mergers are unbiased tracers of the overall M_(BH) - M_* relation. Massive (>10¹¹ M_⊙) galaxies have a high occupation number (>10) of BHs, and hence host the majority of BH mergers.
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