Insights into the chemical composition of the metal-poor Milky Way halo globular cluster NGC 6426

TL;DR

This study provides a detailed chemical composition analysis of four red giant stars in the metal-poor globular cluster NGC 6426, revealing insights into its enrichment history and elemental abundances.

Contribution

It introduces a new semi-automated tool, EWCODE, for measuring equivalent widths and offers detailed abundance measurements for 22 elements in NGC 6426.

Findings

NGC 6426 has a mean [Fe/H] of -2.34 dex, consistent with previous studies.

The cluster shows alpha-element enhancement typical of the Milky Way halo.

Evidence suggests enrichment from hypernovae and possibly multiple stellar populations.

Abstract

We present our detailed spectroscopic analysis of the chemical composition of four red giant stars in the halo globular cluster NGC 6426. We obtained high-resolution spectra using the Magellan2/MIKE spectrograph, from which we derived equivalent widths and subsequently computed abundances of 24 species of 22 chemical elements. For the purpose of measuring equivalent widths, we developed a new semi-automated tool, called EWCODE. We report a mean Fe content of [Fe/H] = -2.34$\pm$0.05 dex (stat.) in accordance with previous studies. At a mean $\alpha$-abundance of [(Mg,Si,Ca)/3 Fe] = 0.39$\pm$0.03 dex, NGC 6426 falls on the trend drawn by the Milky Way halo and other globular clusters at comparably low metallicities. The distribution of the lighter $\alpha$-elements as well as the enhanced ratio [Zn/Fe] = 0.39 dex could originate from hypernova enrichment of the pre-cluster medium. We find tentative evidence for a spread in the elements Mg, Si, and Zn, indicating an enrichment scenario, where ejecta of evolved massive stars of a slightly older population polluted a newly born younger one. The heavy element abundances in this cluster fit well into the picture of metal-poor globular clusters, which in that respect appear to be remarkably homogeneous. The pattern of the neutron-capture elements heavier than Zn point towards an enrichment history governed by the r-process with only little -if any- sign of s-process contributions. This finding is supported by the striking similarity of our program stars to the metal-poor field star HD 108317.