Metallicity distributions of low-α stars with |L_Z|< 600 kpc km s⁻¹. Two Gaussian components were used to model the observed distribution: a broad one representing accreted stars from GSE (dashed line), and another capturing the secondary peak linked to the LAHN population. The sum of both components is shown as a solid line. Error bars reflect uncertainties due to variations in the α-based classification (see text).