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The majority of gas giants (planets of masses $\gtrsim10^2 M_\oplus$) arefound to reside at distances beyond $\sim1$ au from their host stars. Within 1au, the planetary population is dominated by super-Earths of $2-20 M_\oplus$.We show that this dichotomy between inner super-Earths and outer gas giants canbe naturally explained should they form in nearly inviscid disks. In laminardisks, a planet can more easily repel disk gas away from its orbit. Thefeedback torque from the pile-up of gas inside the planet's orbit slows downand eventually halts migration. A pressure bump outside the planet's orbittraps pebbles and solids, starving the core. Gas giants are born cold and staycold: more massive cores are preferentially formed at larger distances, andthey barely migrate under disk feedback. We demonstrate this using 2Dhydrodynamical simulations of disk-planet interaction lasting up to $10^5$years: we track planet migration and pebble accretion until both come to an endby disk feedback. Whether cores undergo runaway gas accretion to become gasgiants or not is determined by computing 1D gas accretion models. Oursimulations show that in an inviscid minimum mass solar nebula, gas giants donot form inside $\sim$0.5 au, nor can they migrate there while the disk ispresent. We also explore the dependence on disk mass, and find that gas giantsform further out in less massive disks.

Inner Super-Earths, Outer Gas Giants: How Pebble Isolation and Migration Feedback Keep Jupiters Cold