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BLACK HOLE CLUMPING. “The medium within the cold disk is turbulent, which causes numerous weak shocks. The disk then fragments into three clumps, which all of which proceed to collapse because thermal pressure and rotational forces cannot counteract the gravitational forces of the clumps.” https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn

BLACK HOLE HALO. “The MMH grows gradually after its rapid growth event, which allows the system to form a rotationally supported disk that is cold (300 K) compared to the surrounding gas (10,000 K).” (MMH = most massive halo). https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn

BLACK HOLE CRITICAL POINT. “The simulations follow the evolution of the target haloes until they reach a density of 10(-15) g cm(-3), at which point it is certain that a collapsed object will form. Both haloes form a gravitationally unstable core.” https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn

BLACK HOLE MERGERS. “We find that major mergers are the dominant mechanism for preventing population III star formation in these haloes.” https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn

FORMATION OF MASSIVE BLACK HOLES. “Most of the accreted matter originates from the parent filament, a major merger and several minor halo mergers. This rapid convergence of matter below the atomic-cooling limit is a prediction of the standard cold dark-matter paradigm, and in conflict with cosmologies that suppress power below the atomic-cooling limit. Nevertheless, rapid convergence is rare, occurring in only about 0.03% of haloes with similar masses and that exist in an large-scale overdense environment.” Worth the effort! https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn

MASSIVE BLACK HOLES. “The MMH grows by a factor of 30 over 30 Myr as it virializes. The LWH experiences two rapid growth events.” (MMH = most massive halo; LWH = Lyman–Werner radiation flux). https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn

COMPLETED MODEL. “We are confident that our simulation follows the complete star-formation history of all collapsed structure, and thus the metal-enrichment history of pre-galactic gas that is vital to determining the conditions for DCBH formation.” (DCBH = direct-collapse black holes). https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn

OBSERVATIONS. “We predict that these DCBHs will evolve to form the population of faint quasars observed at z ≈ 6. This population will be within the reach of the James Webb Space Telescope, which will be able to provide stringent constraints on their number densities that will be directly comparable to our results.” (DCBH = direct-collapse black holes). https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn

SUPERMASSIVE STARS. “SMSs and therefore DCBHs that form in rapidly growing haloes, as proposed here, will be tens of kiloparsecs away from the large-scale overdensity. They will take hundreds of millions of years—a substantial fraction of the age of the Universe at z > 6—to fall into the nearby group of galaxies.” DCBH = direct-collapse black holes; SMSs = supermassive stars). https://www.nature.com/articles/s41586-019-0873-4 View in LinkedIn