In recent years simulations of SMBHs in a cosmological context have been attempting to answer the question whether, given our current understanding of the process, we are able to grow SMBHs from stellar mass seeds to the quasars observed by redshift z=6. The emergent consensus points to the fact that there is in fact enough gas being funnelled from the ISM to the inner few parsecs of the galaxies to feed the black hole at its centre. However, whether enough of this gas is able to shed its angular momentum and reach scales on which an accretion disc starts to form is still open to debate. This poster will show results of new simulations that are able to track the gas from intergalactic scales down to about 0.1, greatly extending the range probed so far.