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Recent ALMA observations have identified a variety of dust gaps inprotoplanetary disks, which are commonly interpreted to be generated byunobserved planets. Predicting mass of such embedded planets is of fundamentalimportance in comparing those disk architectures with the observed diversity ofexoplanets. The prediction, however, depends on the assumption that whether thesame gap structure exists in the dust component alone or in the gas componentas well. We assume a planet can only open a gap in the gas component when itsmass exceeds the pebble isolation mass by considering the core accretionscenario. We then propose two criteria to distinguish if a gap is opened in thedust disk alone or the gas gap as well when observation data on the gas profileis not available. We apply the criteria to 35 disk systems with a total of 55gaps compiled from previous studies, and classify each gap into four differentgroups. The classification of the observed gaps allows us to predict the massof embedded planets in a consistent manner with the pebble isolation mass. Wefind that outer gaps are mostly dust alone, while inner gaps are more likely tobe associated with a gas gap as well. The distribution of such embedded planetsis very different from the architecture of the observed planetary systems,suggesting that the significant inward migration is required in theirevolution.

Architecture of planetary systems predicted from protoplanetary disks observed with ALMA I: mass of the possible planets embedded in the dust gap