APOGEE-2S Mg-Al anti-correlation of the Metal-Poor Globular Cluster NGC 2298

TL;DR

This study analyzes elemental abundances and radial velocities of stars in the metal-poor globular cluster NGC 2298 using high-resolution near-infrared spectra, revealing multiple stellar populations and chemical abundance patterns.

Contribution

First detailed chemical abundance analysis of NGC 2298 using APOGEE-2S data, confirming multiple populations and Mg-Al anti-correlation in this cluster.

Findings

No intrinsic Fe spread detected in NGC 2298.

Confirmed Al-enhanced population anti-correlated with Mg.

Cluster shows typical alpha-element overabundance for its metallicity.

Abstract

We present detailed elemental abundances and radial velocities of stars in the metal-poor globular cluster (GC) NGC 2298, based on near-infrared high-resolution ($R\sim$ 22,500) spectra of twelve members obtained during the second phase of the Apache Point Observatory Galactic Evolution Experiment (APOGEE-2) at Las Campanas Observatory as part of the seventeenth Data Release (DR 17) of the Sloan Digital Sky Survey IV (SDSS-IV). We employ the Brussels Automatic Code for Characterizing High accuracy Spectra (\texttt{BACCHUS}) software to investigate abundances for a variety of species including $\alpha$-elements (Mg, Si, and Ca), the odd-Z element Al, and iron-peak elements (Fe and Ni) located in the innermost regions of NGC 2298. We find a mean and median metallicity [Fe/H] $ = -1.76$ and $-1.75$, respectively, with a star-to-star spread of 0.14 dex, compatible with the internal measurement errors. Thus, we find no evidence for an intrinsic Fe abundance spread in NGC 2298. The typical $\alpha-$element enrichment in NGC 2298 is overabundant relative to the Sun, and follows the trend of other metal-poor GCs. We confirm the existence of an Al-enhanced population in this cluster, which is clearly anti-correlated with Mg, indicating the prevalence of the multiple-population phenomenon in NGC 2298.