  It is now accepted that the Solar system's youth was a dynamic and chaotic
time. The giant planets migrated significant distances to reach their current
locations, and evidence of that migration's influence on the Solar system
abounds. That migration's pace, and the distance over which it occurred, is
still heavily debated. Some models feature systems in which the giant planets
were initially in an extremely compact configuration, in which Uranus and
Neptune are chaotically scattered into the outer Solar system. Others feature
architectures that were initially more relaxed, and smoother, more sedate
migration. To determine which of these scenarios best represents the formation
of our Solar system, we must turn to the structure of the system's small body
populations, in which the scars of that migration are still clearly visible.
  We present the first results of a program investigating the effect of giant
planet migration on the reservoirs of small bodies that existed at that time.
As the planets migrate, they stir these reservoirs, scattering vast numbers of
small bodies onto dynamically unstable orbits in the outer Solar system. The
great majority of those bodies are rapidly removed from the system, through
collisions and ejections, but a small number become captured as planetary
Trojans or irregular satellites. Others are driven by the migration, leading to
a significant sculpting of the asteroid belt and trans-Neptunian region.
  The capture and retention efficiencies to these stable reservoirs depend on
the particular migration scenario used. Advocates of chaotic migration from an
initially compact scenario argue that smoother, more sedate migration cannot
explain the observed populations of Trojans and irregular satellites. Our
results draw a strikingly different picture, revealing that such smooth
migration is perfectly capable of reproducing the observed populations.
