# Discovery of a new stellar sub-population residing in the (inner) stellar halo of the Milky Way

## TL;DR

This paper reports the discovery of a new stellar sub-population in the Milky Way's inner halo, characterized by metal-poor giant stars with anomalously high silicon levels and globular cluster-like abundance ratios, suggesting past accretion events.

## Contribution

It identifies a unique chemically distinct stellar group in the inner halo, linking their properties to dissolved globular clusters and past accretion history.

## Key findings

- Stars have high [Si,Al/Fe] ratios similar to globular clusters.
- Most stars follow inner halo-like, retrograde orbits.
- Chemical signatures indicate origins from dissolved globular clusters.

## Abstract

We report the discovery of a unique collection of metal-poor giant-stars, that exhibit anomalously high levels of $^{28}$Si, clearly above typical Galactic levels. Our sample spans a narrow range of metallicities, peaking at $-1.07\pm 0.06$, and exhibit abundance ratios of [Si,Al/Fe] that are as extreme as those observed in Galactic globular clusters (GCs), and Mg is slightly less overabundant. In almost all the sources we used, the elemental abundances were re-determined from high-resolution spectra, which were re-analyzed assuming LTE. Thus, we compiled the main element families, namely the light elements (C, N), $\alpha-$elements (O, Mg, Si), iron-peak element (Fe), $\textit{s}-$process elements (Ce, Nd), and the light odd-Z element (Al). We also provide dynamical evidence that most of these stars lie on tight (inner)halo-like and retrograde orbits passing through the bulge. Such kinds of objects have been found in present-day halo GCs, providing the clearest chemical signature of past accretion events in the (inner) stellar halo of the Galaxy, formed possibly as the result of dissolved halo GCs. Their chemical composition is, in general, similar to that of typical GCs population, although several differences exist.