Deciphering the Milky Way's star formation at cosmic noon with high proper-motion stars: A precursor to the merger-driven starburst

TL;DR

This study investigates the impact of the Gaia-Sausage/Enceladus merger on the Milky Way's star formation history by analyzing high proper-motion stars' chemical and dynamical signatures, revealing distinct stellar populations and their origins.

Contribution

It identifies a new chemically distinct stellar component linked to the GSE merger, providing insights into in situ star formation triggered by galaxy collisions.

Findings

Low-$$ stars with GSE-like kinematics show bimodality in [Na/Fe] and [Al/Fe].

A population ratio of approximately 1:10 between certain stars and GSE debris was estimated.

Low-$$ high-Na stars formed in a compact, gas-rich environment from the GSE progenitor.

Abstract

Evidence suggests that the Milky Way (MW) underwent a major collision with the Gaia-Sausage/Enceladus (GSE) dwarf galaxy around cosmic noon. While GSE has since been fully disrupted, it brought in ex situ stars and dynamically heated in situ stars into the halo. In addition, the gas-rich merger may have triggered a burst of in situ star formation, potentially giving rise to a chemically distinct stellar component. We investigated the region of phase space where stars formed during the GSE merger likely reside, and retain distinct chemical and dynamical signatures. Building on our previous investigation of metallicity ([Fe/H]) and vertical angular momentum ($L_Z$) distributions, we analysed spectroscopic samples from GALAH, APOGEE, SDSS, and LAMOST, combined with Gaia kinematics. We focused on high proper-motion stars as effective tracers of the phase-space volume likely influenced by the GSE merger. To correct for selection effects, we incorporated metallicity estimates derived from SDSS and SMSS photometry. Our analysis reveals that low-$\alpha$ stars with GSE-like kinematics exhibit bimodality in [Na/Fe] and [Al/Fe] at $-1.0 \lesssim {\rm [Fe/H]} \lesssim -0.4$. One group follows the low light-element abundances of GSE stars, while another exhibits enhanced values. These low-$\alpha$, high-Na stars have eccentric orbits but are more confined to the inner MW. Eos overlaps with a high-eccentricity subset of these stars, implying that it constitutes a smaller structure nested within the broader population. After correcting for sampling biases, we estimated a population ratio of approximately 1:10 between the low-$\alpha$, high-Na stars and the GSE debris. These results suggest that the low-$\alpha$, high-Na stars formed in a compact region, likely fuelled by gas from the GSE progenitor, analogous to clumpy star-forming clouds seen in high-redshift galaxies.