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We have performed cosmo-hydro simulations using the RAMSES code to studyatomic cooling (ACHs) haloes at z=10 with masses 5E7Msun<~M<~2E9Msun. We assumeprimordial gas and H2-cooling and prior star-formation have been suppressed. Weanalysed 19 haloes (gas and DM) at a resolution of ~10 (proper) pc, selectedfrom a total volume of ~2E3 (comoving) Mpc3. This is the largest statisticalhydro-sim. study of ACHs at z>10 to date. We examine the morphology, angularmomentum (AM), thermodynamic, and turbulence of these haloes, in order toassess the prevalence of disks and supermassive black holes (SMBHs). We find nocorrelation between either the magnitude or the direction of the AM of the gasand its parent DM halo. Only 3 haloes form rotationally supported cores. Two ofthe most massive haloes form massive, compact overdense blobs. These blobs havean accretion rate ~0.5 Msun/yr (at a distance of 100 pc), and are possiblesites of SMBH formation. Our results suggest that the degree of rotationalsupport and the fate of the gas in a halo is determined by its large-scaleenvironment and merger history. In particular, the two haloes forming blobs arelocated at knots of the cosmic web, cooled early on, and experienced manymergers. The gas in these haloes is lumpy and highly turbulent, with Mach N. >~5. In contrast, the haloes forming rotationally supported cores are relativelymore isolated, located midway along filaments, cooled more recently, andunderwent fewer mergers. Thus, the gas in these haloes is less lumpy and lessturbulent (Mach <~ 4), and could retain most of its AM. The remaining 14 haloeshave intermediate properties. If verified in a larger sample of haloes and withadditional physics, our results will have implications for observations of thehighest-redshift galaxies and quasars with JWST.

Gas infall into atomic cooling haloes: on the formation of protogalactic disks and supermassive black holes at z > 10