The Most Metal-poor Stars in the Magellanic Clouds are $r$-process Enhanced

TL;DR

This study identifies the most metal-poor stars in the Magellanic Clouds and finds they are significantly enriched in $r$-process elements, revealing insights into the galaxies' early chemical evolution.

Contribution

It provides the first comprehensive abundance analysis of the most metal-poor stars in the Magellanic Clouds, highlighting their $r$-process enhancement compared to the Milky Way.

Findings

Magellanic Clouds' metal-poor stars are $r$-process enhanced.

These stars are similar to Milky Way stars in other elemental abundances.

The $r$-process enhancement is statistically significant.

Abstract

The chemical abundances of a galaxy's metal-poor stellar population can be used to investigate the earliest stages of its formation and chemical evolution. The Magellanic Clouds are the most massive of the Milky Way's satellite galaxies and are thought to have evolved in isolation until their recent accretion by the Milky Way. Unlike the Milky Way's less massive satellites, little is know about the Magellanic Clouds' metal-poor stars. We have used the mid-infrared metal-poor star selection of Schlaufman & Casey (2014) and archival data to target nine LMC and four SMC giants for high-resolution Magellan/MIKE spectroscopy. These nine LMC giants with $-2.4\lesssim[\text{Fe/H}]\lesssim-1.5$ and four SMC giants with $-2.6\lesssim[\text{Fe/H}]\lesssim-2.0$ are the most metal-poor stars in the Magellanic Clouds yet subject to a comprehensive abundance analysis. While we find that at constant metallicity these stars are similar to Milky Way stars in their $\alpha$, light, and iron-peak elemental abundances, both the LMC and SMC are enhanced relative to the Milky Way in the $r$-process element europium. These abundance offsets are highly significant, equivalent to $3.9\sigma$ for the LMC, $2.7\sigma$ for the SMC, and $5.0\sigma$ for the complete Magellanic Cloud sample. We propose that the $r$-process enhancement of the Magellanic Clouds' metal-poor stellar population is a result of the Magellanic Clouds' isolated chemical evolution and long history of accretion from the cosmic web combined with $r$-process nucleosynthesis on a timescale longer than the core-collapse supernova timescale but shorter than or comparable to the thermonuclear (i.e., Type Ia) supernova timescale.