What question did this study set out to answer?

To investigate the individual abundances of metal-poor M dwarfs and their implications for Galactic history.

June 10, 2026Open Access

Tracing Galactic History through Metal-Poor M Dwarfs in the Solar Vicinity

Key Points

To investigate the individual abundances of metal-poor M dwarfs and their implications for Galactic history.
Analyzed 19 metal-poor M dwarfs with [Fe/H]=−1.0 to −2.0 dex and Teff ∼3650–4000 K.
Derived elemental abundances using MARCS model atmospheres and Turbospectrum analysis.
Utilized the Toomre diagram to assess Galactic dynamics.
Most stars exhibit halo-like abundance patterns in the [Mg/Fe]–[Fe/H] plane.
Identified three likely members associated with the Gaia-Enceladus/Sausage event.
Highlighted additional candidates related to Sequoia and other halo substructures.

Abstract

We present individual abundances of C, O, Mg, Al, Si, K,Ca, Ti, and Fe for 19 metal-poor M dwarfs observed byAPOGEE. The sample spans Fe/H=−1.0 to −2.0 dex andTeff ∼3650–4000 K. Abundances were derived through aclassical analysis using MARCS model atmospheres, thelatest APOGEE line list, and Turbospectrum. Most stars showhalo-like abundance patterns in the Mg/Fe–Fe/H plane,supported by their Galactic dynamics from the Toomrediagram. Since all targets are located in the solarneighborhood, within 340 pc, they may be remnants ofdisrupted globular clusters or accreted satellite galaxies.We identify three likely Gaia-Enceladus/Sausage members,with additional candidates associated with Sequoia andother halo substructures.

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