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Super-massive black holes (SMBHs) with $M_{\bullet} \sim 10^9 $ M$_{\odot}$at $z>6$ likely originate from massive seed black holes (BHs). We investigatethe consequences of seeding SMBHs with direct collapse BHs (DCBHs)($M_{\bullet}=10^{4-6}\, \mathrm{M}_\odot$) on proto-galactic disc growth. Weshow that even in the absence of direct feedback effects, the growth of seedBHs reduces the development of gravitational instabilities in host galaxydiscs, suppressing star formation and confining stars to a narrow ring in thedisc and leading to galaxies at $z \sim 6$ which lie above the local BH-stellarmass relation. The relative magnitude of cosmic and BH accretion rates governsthe evolution of the BH-stellar mass relation. For typical DCBH formationepochs, $z_{\rm{i}} \sim 10$, we find star formation is inhibited in haloesgrowing at the average rate predicted by $\Lambda$CDM which host BHs capable ofreaching $M_{\bullet}\sim 10^9 \, \mathrm{M}_{\odot}$ by $z\gtrsim6$. Slowergrowing BHs cause a delay in the onset of star formation; a $M_{\bullet} \sim10^6 $ M$_{\odot}$ seed growing at $0.25$ times the Eddington limit will delaystar formation by $\sim100$ Myr. This delay is reduced by a factor of $\sim10$if the halo growth rate is increased by $\sim 0.6\, \sigma$. Our resultssuggest that SMBHs seeded by DCBHs and their host galaxies form in separateprogenitor haloes. In the absence of subsequent mergers, higher than averagecosmic accretion or earlier seed formation ($z_{\rm i} \sim 20$) are requiredto place the evolving BH on the local BH-stellar mass relation by $z=6$.

How Black Holes Stop Their Host Galaxy from Growing Without AGN Feedback