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We use the SPHINX suite of high-resolution cosmological radiationhydrodynamics simulations to study how spatially and temporally inhomogeneousreionization impacts the baryonic content of dwarf galaxies and cosmicfilaments. The SPHINX simulations simultaneously model an inhomogeneousreionization, follow the escape of ionising radiation from thousands ofgalaxies, and resolve haloes well below the atomic cooling threshold. Thismakes them an ideal tool for examining how reionization impacts star formationand the gas content of dwarf galaxies. We compare simulations with and withoutstellar radiation to isolate the effects of radiation feedback from that ofsupernova, cosmic expansion, and numerical resolution. We find that the gascontent of cosmic filaments can be reduced by more than 80% followingreionization. The gas inflow rates into haloes with $M_{vir}<10^8M_{\odot}$ arestrongly affected and are reduced by more than an order of magnitude comparedto the simulation without reionization. A significant increase in gas outflowrates is found for halo masses $M_{vir}<7\times10^7M_{\odot}$. Our simulationsshow that inflow suppression, rather than photoevaporation, is the dominantmechanism by which the baryonic content of high-redshift dwarf galaxies isregulated. At fixed redshift and halo mass, there is a large scatter in thehalo baryon fractions that is entirely dictated by the timing of reionizationin the local region surrounding a halo which can change by $\Delta z>3$ atfixed mass. Finally, although the gas content of high-redshift dwarf galaxiesis significantly impacted by reionization, we find that most haloes with$M_{vir}<10^8M_{\odot}$ can remain self-shielded and form stars long afterreionization, until their local gas reservoir is depleted, suggesting thatlocal group dwarf galaxies do not necessarily exhibit star formation historiesthat peak prior to $z=6$...

How to Quench a Dwarf Galaxy: The Impact of Inhomogeneous Reionization on Dwarf Galaxies and Cosmic Filaments