M_dust−M_⋆ relation in different star-forming regions (colors) and for the disks with resolved cavities or transition disks (TDs, open circles) and disks with structures (full triangles, see appendix). The values for the slope and intercept for the different star forming regions are taken from Pascucci et al. (2016), except for σ-Orionis, which values are from Ansdell et al. (2017). From fitting this relation for TDs and disk with structures, we used log₁₀ (M_dust∕M_⊕) = βlog₁₀(M_⋆∕M_⊙) + α, and we obtained and and a Pearson coefficient of 0.50. The fit takes into account the uncertainties of the data, which are dominated by the 10% of uncertainty from flux calibration.