SIMBAD references

We present a theoretical model to predict the properties of an observed z = 5.72 Lyman α emitter galaxy-C IV absorption pair separated by 1384 comoving kpc h^–1. We use the separation of the pair and an outflow velocity/time travelling argument to demonstrate that the observed galaxy cannot be the source of metals for the C IV absorber. We find a plausible explanation for the metal enrichment in the context of our simulations: a dwarf galaxy with M_* = 1.87 x 10⁹ M_☉ located 119 comoving kpc h^–1 away with a wind velocity of ∼100 km s^–1 launched at z ∼ 7. Such a dwarf (M_UV = -20.5) is fainter than the detection limit of the observed example. In a general analysis of galaxy-C IV absorbers, we find galaxies with - 20.5 <M_UV < -18.8 are responsible for the observed metal signatures. In addition, we find no correlation between the mass of the closest galaxy to the absorber and the distance between them, but a weak anti-correlation between the strength of the absorption and the separation of galaxy-absorber pairs.