The stellar metallicity gradients of Local Group dwarf galaxies

TL;DR

This study analyzes the metallicity gradients of 30 Local Group dwarf galaxies, finding mostly mild negative profiles with little dependence on mass, environment, or star formation history, and compares results with simulations.

Contribution

It provides the largest homogeneous compilation of metallicity gradients in dwarf galaxies and compares observational data with theoretical simulations.

Findings

Most dwarf galaxies show decreasing metallicity with radius.

No correlation between gradients and galaxy mass or environment.

Strongest gradients linked to past merger events.

Abstract

Through a homogeneous analysis of spectroscopic literature data of red giant stars, we determine the radial metallicity profiles of 30 dwarf galaxies in the Local Group. We explore correlations between the calculated metallicity gradients and stellar mass, star formation history and environment, delivering the largest compilation to date of this type. The dwarf galaxies in our sample mostly show metallicity profiles decreasing with radius, with some exhibiting rather steep profiles. The derived metallicity gradients as a function of the half-light radius, $\nabla_{\rm [Fe/H]} (R/R_e)$, show no statistical differences when compared with the galaxies' morphological type, nor with their distance from the Milky Way or M31. No correlations are found with either stellar mass or star formation timescales. In particular, we do not find the linear relationship between $\nabla_{\rm [Fe/H]} (R/R_e)$ and the galaxies' median age $t_{50}$, as instead shown in the literature for a set of simulated systems. The presence of high angular momentum in some of our galaxies does not seem to have an impact on the gradient values. The strongest gradients in our sample are observed in systems that are likely to have experienced a past merger event. By excluding them, the analysed dwarf galaxies show mild gradients ($\sim -0.1$ dex $R_e^{-1}$) with little scatter between them, regardless of their stellar mass, dynamical state, and star formation history. These results are in good agreement with different sets of simulations presented in the literature and analysed using the same method as for the observed sample. The interplay between the multitude of factors that could drive the formation of metallicity gradients in dwarf galaxies likely combine in complex ways to produce in general comparable values.