  Jupiter-mass planets with large semi-major axes ($a > 1.0$ AU) occur at a
higher rate around evolved intermediate mass stars. There is a pronounced
paucity of close-in ($a < 0.6$ AU), intermediate period ($5 < P < 100$ days),
low-mass ($M_{\rm planet} < 0.7M_{\rm Jup} $) planets, known as the `Planet
Desert'. Current radial velocity methods have yet to yield close-in, low-mass
planets around these stars because the planetary signals could be hidden by the
(5-10) m s$^{-1}$ radial velocity variations caused by acoustic oscillations.
We find that by implementing an observing strategy of taking three observations
per night separated by an optimal $\Delta t$, which is a function of the
oscillation periods and amplitudes, we can average over the stellar jitter and
improve our sensitivity to low-mass planets. We find $\Delta t$ can be
approximated using the stellar mass and radius given by the relationship
$\Delta t = $1.79 $(M/M_{\odot})^{-0.82} ~(R/R_{\odot})^{1.92}$. We test our
proposed method by injecting planets into very well sampled data of a subgiant
star, $\gamma$ Cep. We compare the fraction of planets recovered by our method
to the fraction of planets recovered using current radial velocity
observational strategies. We find that our method decreases the RMS of the
stellar jitter due to acoustic oscillations by a factor of three over current
single epoch observing strategies used for subgiant stars. Our observing
strategy provides a means to test whether the Planet Desert extends to lower
mass planets.
