  A fundamental question in the study of planetary system demographics is: how
common is the solar system architecture? The primary importance of this
question lies in the potential of planetary systems to create habitable
environments, and dissecting the various components of solar system evolution
that contributed to a sustainable temperate surface for Earth. One important
factor in that respect is volatile delivery to the inner system and the
dependence on giant planets beyond the snow line as scattering agents,
particularly as such cold giant planets are relatively rare. Here, we provide
an investigation of the eccentricity distribution for giant planet populations
both interior and exterior to their system snow lines. We show that the median
eccentricity for cold giants is 0.23, compared with a far more circular orbital
regime for inner planets. We further present the results of a dynamical
simulation that explores the particle scattering potential for a Jupiter analog
in comparison with a Jupiter whose eccentricity matches that of the median cold
giant eccentricity. These simulations demonstrate that the capacity for such an
eccentric cold giant system to scatter volatiles interior to the snow line is
significantly increased compared with the Jupiter analog case, resulting in a
far greater volume of Earth-crossing volatiles. Thus, many of the known systems
with cold giant planets may harbor water worlds interior to the snow line.
