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Observational evidence suggests that some very large supermassive black holes(SMBHs) already existed less than 1 Gyr after the Big Bang. Explaining theformation and growth of the 'seeds' of these SMBHs is quite challenging. Weexplore the formation of such seeds in the direct collapse scenario. Using 3Dhydrodynamical simulations, we investigate the impact of turbulence androtation on the fragmentation behavior of collapsing primordial gas in thepresence of a strong UV radiation background, which keeps the gas hot.Additionally, we explore different ways in which the collapsing gas may be ableto stay hot, and thus limit fragmentation. Using a one-zone model, we examinethe interplay between magnetic fields, turbulence, and a UV radiationbackground.  Feedback processes from stars and black holes shape the interstellar medium(ISM) out of which new generations of luminous objects form. To understand theproperties of these objects, e.g. the stellar initial mass function, it isvital to have knowledge of the chemical and thermodynamical properties of thefeedback-regulated ISM. To better understand the chemo-thermal state andfragmentation behavior of gas in high-redshift galaxies, we updated, improved,and extended a photodissociation region code. Our computational code, PDR-Zz,is described in detail. Using this code, a grid of models is run, covering asizable range in physical properties. This allows us to systematically explorethe overall impact of various feedback effects, both radiative and chemical, onthe chemical and thermal balance of the gas in different physical regimes.

Matter of Life & Death: The impact of environmental conditions on the origins of stars and supermassive black holes