# Theoretical study of an LAE-CIV absorption pair at z = 5.7

## TL;DR

This theoretical study models a high-redshift galaxy-CIV absorption pair, demonstrating that nearby dwarf galaxies likely caused the observed metal enrichment through outflows, with implications for understanding early universe metal distribution.

## Contribution

The paper introduces a novel theoretical framework linking galaxy properties and outflows to CIV absorption features at high redshift, explaining metal enrichment origins.

## Key findings

- Dwarf galaxy at 119 cMpc/h can explain observed metals.
- Galaxies with -20.5 < M_UV < -18.8 are responsible for metals.
- No correlation between galaxy mass and proximity to absorber.

## Abstract

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.