Typical comparisons between XSL and GSL energy distributions for stars with relatively high metallicities and 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 50877 (X0314), BBB SMC 104 (X0504), HD 44391 (X0563), 2MASS J18351420-3438060 (X0698), HD 218566 (X0739), HD 21197 (X0560). As in Fig. C.5, discontinuities between the UVB, VIS, and NIR segments of the XSL data appear when the general energy distribution is not well matched by the models.