HR diagram of the Lupus star-forming region with the Baraffe et al. (2015) and Siess et al. (2000) evolutionary models. The solid and dashed lines represent isochrones and tracks, respectively, with the corresponding ages (in Myr) and masses (in M_⊙) indicated in each panel. The most massive star in our sample (HR 5999) is not shown to improve the visibility of the low-mass range that includes the other stars in our sample. The error bars are smaller than the size of the symbols.