Left panel: dust mass versus stellar mass for Taurus Class II objects. Dots and upper limits from Andrews et al. (2013), assuming a dust temperature as T_dust ≈ 25 × (L_⋆/L_⊙)^0.25 K, and the evolutionary models from Baraffe et al. (1998) to calculate the stellar mass. The hexagonal points correspond to the targets reported by Ward-Duong et al. (2018), assuming the same procedure as in Andrews et al. (2013) to calculate the dust disk mass. The position of CIDA 1 is shown by the red square. Right panel: mass accretion rate versus stellar mass for Taurus Class II objects. Dots from Herczeg & Hillenbrand (2008), diamonds from the compilation of Rigliaco et al. (2015). The location of CIDA 1 is shown by the red square. Known TDs as classified by Rigliaco et al. (2015) are identified by blue squares.