HR diagram for stars in Table 2 (black dots) compared with disk–free TWA objects investigated in Manara et al. (2013b) and Stelzer et al. (2013) (gray diamonds), rescaled to Gaia DR2 distances and Herczeg & Hillenbrand’s (2014) SpT–based T_eff. Filled symbols identify probable TWA members, open symbols targets with disputed membership. Errors on T_eff and log L_⋆ are as in Fig. 3 (y-axis) and Fig. 2 (x-axis), respectively. Left panel: theoretical isochrones from different model grids (Baraffe et al. 2015, dotted blue line; Siess et al. 2000, dash-dot red line; Tognelli et al. 2011, dashed green line; Spada et al. 2013, solid black line; Spada et al. 2017, solid yellow line) are shown for comparison on the diagram. The illustrated isochrone ages are, from top to bottom, 1 Myr, 2 Myr, 5 Myr, 20 Myr, and 100 Myr (the isochrones at 1, 2, and 5 Myr are not available from the models of Spada et al. 2013, and the 5 Myr isochrone is not available from the models of Spada et al. 2017). Right panel: mass tracks from the same model grids are illustrated for comparison. Displayed masses are, from right to left: 0.01 M_⊙, 0.02 M_⊙, 0.05 M_⊙, 0.1 M_⊙, 0.2 M_⊙, 0.4 M_⊙, and 0.6 M_⊙ (Baraffe et al. 2015); 0.1 M_⊙, 0.2 M_⊙, 0.4 M_⊙, 0.6 M_⊙ (Siess et al. 2000; Spada et al. 2013); 0.2 M_⊙, 0.4 M_⊙, 0.6 M_⊙ (Tognelli et al. 2011; Spada et al. 2017).