Distinction of the ablated meteorite samples simulating asteroidal meteor analogs based on the measured relative intensity of Cr I-7, Mg I-2, and Fe I-15 spectral lines. Upper panel: Dependency between Cr I and Fe I line intensity relative to Mg I for all tested meteorites. Regions characteristic of HEDs and chondrites (except for the LL group) are highlighted. The Ragland (weathered LL3.4; Cr/Mg ≈ 25) and Mount Joy (iron; Fe/Mg ≈ 100) meteorites are outside the displayed plot limits. Lower panel: ternary diagram displaying relative intensities of Cr I, Mg I, and Fe I for all samples except the LL group.