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Recent analyses of samples from asteroid (162173) Ryugu returned by JAXA'sHayabusa2 mission suggest that Ryugu and CI chondrites formed in the sameregion of the protoplanetary disk, in a reservoir that was isolated from thesource regions of other carbonaceous (C-type) asteroids. Here we conduct$N$-body simulations in which CI planetesimals are assumed to have formed inthe Uranus/Neptune zone at $\sim15$--25 au from the Sun. We show that CIplanetesimals are scattered by giant planets toward the asteroid belt wheretheir orbits can be circularized by aerodynamic gas drag. We find that thedynamical implantation of CI asteroids from $\sim15$--25 au is very efficientwith $\sim 5$\% of $\sim 100$-km planetesimals reaching stable orbits in theasteroid belt by the end of the protoplanetary gas disk lifetime. Theefficiency is reduced when planetesimal ablation is accounted for. Theimplanted population subsequently evolved by collisions and was depleted bydynamical instabilities. The model can explain why CIs are isotopicallydistinct from other C-type asteroids which presumably formed at $\sim5$--10 au.

Isotopic Trichotomy of Main Belt Asteroids from Implantation of Outer Solar System Planetesimals