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Modelling the evolution of mass and spin of supermassive black holes with hydrodynamical simulations

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Supermassive black holes at high redshift (z>6) with masses as large as those in our local Universe are now abundantly observed in large-scale surveys. This questions our understanding of black hole growth in the first Gyrs of cosmological evolution, and how 10^9 Msun of gas can be trapped at the heart of primordial galaxies. I will show how cosmological hydrodynamical simulations can help to design a scenario for feeding those massive beasts, and what problems arise when one wants to take into account the spin of BHs in the global picture.

This talk is part of the Institute of Astronomy Galaxies Discussion Group series.

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