  The Dwarf Planet Ceres revealed the presence of ammonia and other unique
properties compared to other asteroids in the main belt which suggests that it
was not formed in situ. We model the early dynamical evolution of the outer
Solar System to study possible dynamical mechanisms to implant a Ceres-sized
planetesimal in the asteroid belt from the trans-Saturnian region. We calculate
that the fraction of the population of Ceres-sized planetesimals that are
captured in the asteroid belt is in the range of 2.8e-5 to 1.2e-3 depending on
the initial location in the outer planetesimal disk. The captured bodies have a
70% probability to have a semimajor axis between 2.5 and 3 au, a 33%
probability to have an eccentricity smaller than 0.2 and a 45% probability to
have an orbital inclination smaller than 10 degrees. Assuming the existence of
3,600 Ceres-size planetesimals in the inner part of the trans-Saturnian disk,
consistent with the estimate of Nesvorny & Vokrouhlicky (2016) for the
trans-Neptunian disk, our estimated capture probability and a final 80%
depletion of the asteroid belt during the subsequent giant planet instability,
lead to capture 1 Ceres in the asteroid belt, with a probability of 15%, 34%,
and 51% to be located in the inner, middle and outer belt respectively.
