Typical comparisons between XSL and GSL energy distributions for low metallicity stars with estimated T_eff between 4000 and 5000 K, at R = 500, when adopting the parameters of Arentsen et al. (2019) unchanged. Gravity increases from top to bottom: HD 165195(X0232), HD 1638 (X0258), NGC 68381037 (X0705), LHS 1841 (X0572), LHS 343 (X0906). The discontinuities between the UVB, VIS and NIR segments of the XSL data appear when the general energy distributionis not well matched by the models, because our method scales each arm independently: no other A_V +scaling combination would provide a smaller discrepancy D (Eq. (1)) across all wavelengths. In other words, D would be worse if the UVB, VIS and NIR segments were first merged and A_V was estimated subsequently.