Star formation and gas flow history of a dwarf irregular galaxy traced by gas-phase and stellar metallicities

TL;DR

This study investigates the star formation and gas flow history of dwarf galaxy NGC 6822 using chemical abundance data, revealing complex evolution involving outflows and possibly gas accretion.

Contribution

It provides a detailed chemical evolution analysis of NGC 6822, highlighting the limitations of simple models and suggesting more complex processes are involved.

Findings

Outflow-dominated models explain gas-phase oxygen abundance and gas fraction.

Metallicity distributions challenge simple chemical evolution models.

Complex star formation and gas flow history inferred from chemical abundance data.

Abstract

Studying the evolution of dwarf galaxies can provide insights into the characteristics of systems that can act as building blocks of massive galaxies. This paper discusses the history of star formation and gas flows (inflow and outflow) of a dwarf irregular galaxy in the Local Group, NGC 6822, from the viewpoint of gas-phase and stellar chemical abundance. Gas-phase oxygen abundance, stellar metallicity distribution and gas fraction data are compared to chemical evolution models in which continuous star formation and gas flows are assumed. If the galaxy is assumed to be a closed or an accretion-dominated system where steeper stellar initial mass functions are allowed, the observed gas-phase oxygen abundance and gas fraction can be explained simultaneously; however metallicity distributions predicted by the models seem to be inconsistent with the observed distribution, which suggests that the star formation, gas flows and/or chemical enrichment are more complex than assumed by the models. When NGC 6822 is assumed to be a system dominated by outflow, the observed values of gas-phase oxygen abundance and gas fraction can be explained, and the metallicity distributions predicted by some of the models are also roughly consistent with the observed distribution in the metallicity range of -2.0<[Fe/H]<-0.5. It should be noted that this result does not necessarily mean that the accretion of gas is completely ruled out. More observables, such as chemical abundance ratios, and detailed modelling may provide deeper insight into the evolution of the system.