  Population studies of Kepler's multi-planet systems have revealed a
surprising degree of structure in their underlying architectures. Information
from a detected transiting planet can be combined with a population model to
make predictions about the presence and properties of additional planets in the
system. Using a statistical model for the distribution of planetary systems (He
et al. 2020; arXiv:2007.14473), we compute the conditional occurrence of
planets as a function of the period and radius of Kepler-detectable planets.
About half ($0.52 \pm 0.03$) of the time, the detected planet is not the planet
with the largest semi-amplitude $K$ in the system, so efforts to measure the
mass of the transiting planet with radial velocity (RV) follow-up will have to
contend with additional planetary signals in the data. We simulate RV
observations to show that assuming a single-planet model to measure the $K$ of
the transiting planet often requires significantly more observations than in
the ideal case with no additional planets, due to the systematic errors from
unseen planet companions. Our results show that planets around 10-day periods
with $K$ close to the single-measurement RV precision ($\sigma_{1,\rm obs}$)
typically require $\sim 100$ observations to measure their $K$ to within 20%
error. For a next generation RV instrument achieving $\sigma_{1,\rm obs} = 10$
cm/s, about $\sim 200$ ($600$) observations are needed to measure the $K$ of a
transiting Venus in a Kepler-like system to better than 20% (10%) error, which
is $\sim 2.3$ times as many as what would be necessary for a Venus without any
planetary companions.
