Galactic radial gradients for [Fe/H], [O/H], [Mg/H], and [Si/H] (from top to bottom). Stars in the mid-plane (|z| < −0.4 kpc) with S/N_r > 50 are grouped into radial bins. Only bins containing at least 50 stars are shown, with values and uncertainties computed as the weighted mean and standard deviation of the abundances within each bin. The best-fit linear correlation is shown as a solid line, with its slope in the lower-left corner. The dotted line represents literature results for Galactic radial gradients derived from Classical Cepheids (Trentin et al. 2024).