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We perform cosmological simulations of the intergalactic medium (IGM) atredshift z ~ 3 using the numerical gravity-hydrodynamics codes GADGET-3 andEnzo for the purpose of modelling the gaseous environments of galaxies. Weidentify haloes in the simulations using three different algorithms. Differentrank orderings of the haloes by mass result, introducing a limiting factor inidentifying haloes with observed galaxies. We also compare the physicalproperties of the gas between the two codes, focussing primarily on the gasoutside the virial radius, motivated by recent HI absorption measurements ofthe gas around z ~ 2 - 3 galaxies. The internal dispersion velocities of thegas in the haloes have converged for a box size of 30 comoving Mpc, but thecentre-of-mass peculiar velocities of the haloes have not up to a box size of60 comoving Mpc. The density and temperature of the gas within theinstantaneous turn-around radii of the haloes are adequately captured for boxsizes 30 Mpc on a side, but the results are highly sensitive to the treatmentof unresolved, rapidly cooling gas, with the gas mass fraction within thevirial radius severely depleted by star formation in the GADGET-3 simulations.Convergence of the gas peculiar velocity field on large scales requires a boxsize of at least 60 Mpc. Outside the turn-around radius, the physical state ofthe gas agrees to 30 percent or better both with box size and betweensimulation methods. We conclude that generic IGM simulations make accuratepredictions for the intergalactic gas properties beyond the halo turn-aroundradii, but the gas properties on smaller scales are highly dependent on starformation and feedback implementations.

Gas around galaxy haloes: methodology comparisons using hydrodynamical simulations of the intergalactic medium