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We analyze the dust morphology of 29 transition disks (TDs) observed withALMA at (sub-) millimeter-emission. We perform the analysis in the visibilityplane to characterize the total flux, cavity size, and shape of the ring-likestructure. First, we found that the $M_{\rm{dust}}-M_\star$ relation is muchflatter for TDs than the observed trends from samples of class II sources indifferent star forming regions. This relation demonstrates that cavities openin high (dust) mass disks, independent of the stellar mass. The flatness ofthis relation contradicts the idea that TDs are a more evolved set of disks.Two potential reasons (not mutually exclusive) may explain this flat relation:the emission is optically thick or/and millimeter-sized particles are trappedin a pressure bump. Second, we discuss our results of the cavity size and ringwidth in the context of different physical processes for cavity formation.Photoevaporation is an unlikely leading mechanism for the origin of the cavityof any of the targets in the sample. Embedded giant planets or dead zonesremain as potential explanations. Although both models predict correlationsbetween the cavity size and the ring shape for different stellar and diskproperties, we demonstrate that with the current resolution of theobservations, it is difficult to obtain these correlations. Future observationswith higher angular resolution observations of TDs with ALMA will help todiscern between different potential origins of cavities in TDs.

Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating dust trapping and the origin of the cavities