Effect of microturbulent velocity on the derived FeI abundances for two representative stars in the sample, SV Vul and X Pup. Each panel shows the abundance distributions obtained by adopting three different values of ξ: 3.3 km s⁻¹ (pink histogram with the black Gaussian fit), 2.3 km s⁻¹ (red), and 4.3 km s⁻¹ (blue). In all cases, the resulting differences are smaller than 0.1 dex and lie within the typical abundance uncertainties, supporting the robustness of using a fixed ξ in our analysis.