  In D-term inflation models, Affleck-Dine baryogenesis produces isocurvature
density fluctuations. These can be perturbations in the baryon number, or, in
the case where the present neutralino density comes directly from B-ball decay,
perturbations in the number of dark matter neutralinos. The latter case results
in a large enhancement of the isocurvature perturbation. The requirement that
the deviation of the adiabatic perturbations from scale invariance due to the
Affleck-Dine field is not too large then imposes a lower bound on the magnitude
of the isocurvature fluctuation of about $10^{-2}$ times the adiabatic
perturbation. This should be observable by MAP and PLANCK.
