  Maximizing the scientific return of Roman requires focusing on the scientific
discovery space opened up by Roman relative to the ground: i.e., planets in
wide orbits (log s > 0.4), the smallest mass-ratio planets (log q < -4.5), and
free-floating planet candidates (especially those with thetaE < 1 uas).
However, capitalizing on that leverage requires not just detecting such planets
but characterizing them sufficiently that they can be used in a statistical
analysis. In particular, the signals from all three categories are all prone to
light curve degeneracies that may lead to ambiguities in the planet mass-ratio
q, separation s, and the size of the source rho (used to measure thetaE and
constrain the host mass). Bound planets may also have light curves that are
degenerate with models that include a second source rather than a planet. The
most immediate need for designing the Roman Galactic Bulge Time Domain Survey
is a detailed simulation of wide-orbit and small planetary perturbations to
investigate how well the planet perturbations will be characterized. These
investigations and related trade-studies must be done in order to maximize
Roman's ability to take advantage of new parameter space.
