Insights into Pre-Enrichment of Star Clusters and Self-Enrichment of Dwarf Galaxies from their Intrinsic Metallicity Dispersions

TL;DR

This study reveals that star clusters and dwarf galaxies have binomial metallicity distributions with distinct correlations between their mean metallicity and dispersion, explained by inhomogeneous chemical evolution models, highlighting differences in pre-enrichment and self-enrichment processes.

Contribution

The paper demonstrates that linear metallicity distributions in star clusters and dwarf galaxies are binomial and can be modeled with inhomogeneous chemical evolution, distinguishing their enrichment histories.

Findings

Star clusters and dwarf galaxies show binomial metallicity distributions.

Offset in the $\sigma(Z)^2$ vs. $ar{Z}$ plot differentiates clusters from galaxies.

Model links metallicity dispersion to enrichment processes.

Abstract

Star clusters are known to have smaller intrinsic metallicity spreads than dwarf galaxies due to their shorter star formation timescales. Here we use individual spectroscopic [Fe/H] measurements of stars in 19 Local Group dwarf galaxies, 13 Galactic open clusters, and 49 globular clusters to show that star cluster and dwarf galaxy linear metallicity distributions are binomial in form, with all objects showing strong correlations between their mean linear metallicity $\bar{Z}$ and intrinsic spread in metallicity $\sigma(Z)^{2}$. A plot of $\sigma(Z)^{2}$ versus $\bar{Z}$ shows that the correlated relationships are offset for the dwarf galaxies from the star clusters. The common binomial nature of these linear metallicity distributions can be explained with a simple inhomogeneous chemical evolution model (e.g., Oey 2000), where the star cluster and dwarf galaxy behaviour in the $\sigma(Z)^{2}-\bar{Z}$ diagram is reproduced in terms of the number of enrichment events, covering fraction, and intrinsic size of the enriched regions. The inhomogeneity of the self-enrichment sets the slope for the observed dwarf galaxy $\sigma(Z)^{2}-\bar{Z}$ correlation. The offset of the star cluster sequence from that of the dwarf galaxies is due to pre-enrichment, and the slope of the star cluster sequence represents the remnant signature of the self-enriched history of their host galaxies. The offset can be used to separate star clusters from dwarf galaxies without a priori knowledge of their luminosity or dynamical mass. The application of the inhomogeneous model to the $\sigma(Z)^{2}-\bar{Z}$ relationship provides a numerical formalism to connect the self-enrichment and pre-enrichment between star clusters and dwarf galaxies using physically motivated chemical enrichment parameters.