GASTRO library I: the simulated chemodynamical properties of several GSE-like stellar halos

TL;DR

This study uses simulated chemodynamical models of Milky Way-like stellar halos to understand how single merger events can produce complex signatures, aiding interpretation of observed galactic substructures.

Contribution

It introduces a set of SPH+$N$-body models exploring the chemodynamical effects of a major merger, highlighting feedback effects and potential misinterpretations of stellar substructures.

Findings

Supernova feedback affects satellite structure and chemodynamical signatures.

Retrograde high-energy stars are the most metal-poor, possibly mimicking separate mergers.

Most bound stars are more metal-rich, suggesting secondary mergers.

Abstract

The Milky Way stellar halo contains relics of ancient mergers that tell the story of our Galaxy's formation. Some of them are identified due to their similarity in energy, actions and chemistry, referred to as the "chemodynamical space", and are often attributed to distinct merger events. It is also known that our Galaxy went through a significant merger event that shaped the local stellar halo during its first Gyr. Previous studies using $N$-body only and cosmological hydrodynamical simulations have shown that such single massive merger can produce several "signatures" in the chemodynamical space, which can potentially be misinterpreted as distinct merger events. Motivated by these, in this work we use a subset of the GASTRO, library which consists of several SPH+$N$-body models of single accretion event in a Milky Way-like galaxy. Here, we study models with orbital properties similar to the main merger event of our Galaxy and explore the implications to known stellar halo substructures. We find that: $i.$ supernova feedback efficiency influences the satellite's structure and orbital evolution, resulting in distinct chemodynamical features for models with the same initial conditions, $ii.$ very retrograde high energy stars are the most metal-poor of the accreted dwarf galaxy and could be misinterpreted as a distinct merger $iii.$ the most bound stars are more metal-rich in our models, the opposite of what is observed in the Milky Way, suggesting a secondary massive merger, and finally $iv.$ our models can reconcile other known substructures to an unique progenitor.