Cosmological simulations of intergalactic medium enrichment from galactic outflows

ABSTRACT

We investigate models of self-consistent chemical enrichment of the intergalactic medium (IGM) from  z= 6.0 → 1.5 , based on hydrodynamic simulations of structure formation that explicitly incorporate outflows from star-forming galaxies. Our main result is that outflow parametrizations derived from observations of local starburst galaxies, in particular momentum-driven wind scenarios, provide the best agreement with observations of C iv absorption at  z∼ 2–5 . Such models sufficiently enrich the high-z IGM to produce a global mass density of C iv absorbers that is relatively invariant from  z= 5.5 → 1.5 , in agreement with observations. This occurs despite continual IGM enrichment causing an increase in volume-averaged metallicity by  ∼× 5–10  over this redshift range, because energy input accompanying the enriching outflows causes a drop in the global ionization fraction of C iv. Comparisons to observed C iv column density and linewidth distributions and C iv-based pixel optical depth ratios provide significant constraints on wind models. Our best-fitting outflow models show mean IGM temperatures only slightly above our no-outflow case, metal filling factors of just a few per cent with volume-weighted metallicities around 10⁻³ at  z∼ 3 , significant amounts of collisionally ionized C iv absorption and a metallicity–density relationship that rises rapidly at low overdensities and flattens at higher ones. In general, we find that outflow speeds must be high enough to enrich the low-density IGM at early times but low enough not to overheat it, and concurrently must significantly suppress early star formation while still producing enough early metals. It is therefore non-trivial that locally calibrated momentum-driven wind scenarios naturally yield the desired strength and evolution of outflows, and suggest that such models represent a significant step towards understanding the impact of galactic outflows on galaxies and the IGM across cosmic time.