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We use the EAGLE suite of hydrodynamical simulations to analyse accretionrates (and the breakdown of their constituent channels) onto haloes over cosmictime, comparing the behaviour of baryons and dark matter (DM). We alsoinvestigate the influence of sub-grid baryon physics on halo-scale inflow,specifically the consequences of modelling radiative cooling, as well asfeedback from stars and active galactic nuclei (AGN). We find that variationsin halo baryon fractions at fixed mass (particularly their circum-galacticmedium gas content) are very well correlated with variations in the baryonfraction of accreting matter, which we show to be heavily suppressed by stellarfeedback in low-mass haloes, $M_{\rm halo}\lesssim10^{11.5}M_{\odot}$. Breakingdown accretion rates into first infall, recycled, transfer and mergercomponents, we show that baryons are much more likely to be smoothly accretedthan to have originated from mergers when compared to DM, finding (averagedacross halo mass) a merger contribution of $\approx6\%$ for baryons, and$\approx15\%$ for DM at $z\approx0$. We also show that the breakdown of inflowinto different channels is strongly dependent on sub-grid physics, particularlythe contribution of recycled accretion (accreting matter that has beenpreviously ejected from progenitor haloes). Our findings highlight the dualrole that baryonic feedback plays in regulating the evolution of galaxies andhaloes: by (i) directly removing gas from haloes, and (ii) suppressing gasinflow to haloes.

The impact of stellar and AGN feedback on halo-scale baryonic and dark matter accretion in the EAGLE simulations