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The giant planet occurrence rate rises with orbital period out to at least$\sim$300 days. Large-scale planetary migration through the disk has long beensuspected to be the physical origin of this feature, as the timescale ofstandard Type I migration in a standard solar nebula is longer farther from thestar. These calculations also find that typical Jupiter-bearing cores shuttletowards the disk inner edge on timescales orders of magnitude shorter than thegas disk lifetime. The presence of gas giants at myriad distances requiresmechanisms to slow large-scale migration. We revisit the migration paradigm byderiving model occurrence rate profiles from migration of cores, mass growth bygas accretion, and planetary gap opening. We show explicitly that the formertwo processes occur in tandem. Radial transport of planets can slow downsignificantly once deep gaps are carved out by their interaction with disk gas.Disks are more easily perturbed closer to the star, so accounting for gapopening flattens the final orbital period distribution. To recover the observedrise in occurrence rate, gas giants need to be more massive farther out, whichis naturally achieved if their envelopes are dust-free. The range of massgradients we find to reconcile the observed occurrence rate of Jupiters is tooabrupt to account for the mass-period distribution of low-eccentricity giantplanets, challenging disk migration as the dominant origin channel of hot andwarm Jupiters. Future efforts in characterizing the unbiased mass distributionwill place stronger constraints on predictions from migration theory.

Can Large-Scale Migration Explain the Giant Planet Occurrence Rate?