Chemodynamics of the Milky Way and disc formation history: insight from the RAVE and Gaia-ESO surveys

TL;DR

This paper uses data from RAVE and Gaia-ESO surveys to analyze the chemo-dynamical properties of Milky Way stars, revealing evidence of radial migration and characterizing the thick and thin discs to inform galaxy evolution models.

Contribution

It presents the first direct evidence of radial migration in the thin disc and provides detailed chemo-dynamical characterization of the Galaxy's disc components.

Findings

Evidence for radial migration in the thin disc

Chemo-dynamical differences between thick and thin discs

Challenges for models to reproduce observed chemo-dynamical properties

Abstract

Multi-object spectrographs have opened a new window on the analyses of the chemo-dynamical properties of old Milky Way stars. These analyses allow us to trace back the internal mechanisms and the external factors that have influenced the evolution of our Galaxy, and therefore understand fundamental aspects of galaxy evolution in general. Here, we present recent results from the RAdial Velocity Experiment (RAVE) and the Gaia-ESO survey. These surveys explore the Milky Way properties in different ways, in terms of sample size and selection, magnitude range, and spectral resolution. We focus here on (i) the first direct detection of evidence for radial migration within the thin disc, providing insight into the history of spiral structure of the Milky Way, and (ii) the chemo-dynamical characterisation of the metal-weak thick and thin discs, for which chemo-dynamical models still have difficulties in reproducing.