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Using high resolution hydrodynamical cosmological simulations, we study thegas accretion history of low mass halos located in a field-like, low densityenvironment. We track their evolution individually from the early,pre-reionization era, through reionization, and beyond until $z=0$. Beforereionization, low mass halos accrete cool cosmic web gas at a very rapid rate,often reaching the highest gas mass they will ever have. But when reionizationoccurs, we see that almost all halos lose significant quantities of their gascontent, although some respond less quickly than others. We find that theresponse rate is influenced by halo mass first, and secondarily by theirinternal gas density at the epoch of reionization. Reionization also fullyionises the cosmic web gas by z$\sim$6. As a result, the lowest mass halos(M$\sim$10$^6~h^{-1}$M$_\odot$ at $z=6$) can never again re-accrete gas fromthe cosmic web, and by $z\sim5$ have lost all their internal gas to ionisation,resulting in a halt in star formation at this epoch. However, more massivehalos can recover from their gas mass loss, and re-accrete ionised cosmic webgas. We find the efficiency of this re-accretion is a function of halo massfirst, followed by local surrounding gas density. Halos that are closer to thecosmic web structure can accrete denser gas more rapidly. We find that ourlower mass halos have a sweet spot for rapid, dense gas accretion at distancesof roughly 1-5 virial radii from the most massive halos in our sample($>$10$^8~h^{-1}$M$_\odot$), as these tend to be embedded deeply within thecosmic web.

The Gas Accretion History of Low Mass Halos within the Cosmic Web from Cosmological Simulations