Theoretical study of an LAE-CIV absorption pair at z = 5.7
  We present a theoretical model to predict the properties of an observed $z =$
5.72 Lyman $\alpha$ emitter galaxy - CIV absorption pair separated by 1384
comoving kpc/h. 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 CIV absorber. We find a plausible explanation for the
metal enrichment in the context of our simulations: a dwarf galaxy with
$M_{\star} =$ 1.87 $\times$ 10$^{9} M_{\odot}$ located 119 comoving kpc/h away
with a wind velocity of $\sim$ 100 km/s launched at $z \sim$ 7. Such a dwarf
($M_{\text{UV}} =$ - 20.5) is fainter than the detection limit of the observed
example. In a general analysis of galaxy - CIV absorbers, we find galaxies with
-20.5 $< M_{\text{UV}} <$ - 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.
