  Red-giant stars are an incredible source of information for testing models of
stellar evolution, as asteroseismology has opened up a window into their
interiors. Such insights are a direct result of the unprecedented data from
space missions Kepler and CoRoT as well as recent theoretical advances.
Eclipsing binaries are also fundamental astrophysical objects, and when coupled
with asteroseismology, binaries would provide two independent methods to obtain
masses and radii and exciting opportunities to develop highly constrained
stellar models. The possibility of discovering pulsating red giants in
eclipsing binary systems is therefore an important goal that could potentially
offer very robust characterization of these systems. Hitherto, only 1 case has
been discovered with Kepler. We cross-correlated the detected red-giant and
eclipsing-binary catalogs from Kepler data to find candidate systems.
Light-curve modeling and mean asteroseismic properties are combined to yield
measurements of periods, masses, radii, temperatures, eclipse timing
variations, core rotation rates, and red-giant evolutionary state. After
elimination of false positives, out of the 70 systems common to the red-giant
and eclipsing-binary catalogs we find 13 new strong candidates that are
pulsating red giants in eclipsing binaries, and 10 more that are pulsating red
giants in hierarchical triple systems. The systems span a range of orbital
eccentricities, periods, and spectral types for the red-giant companion. One
case even suggests a system composed of two red-giants. The discovery of
pulsating red giants in multiple systems provides exciting test beds for
precise astrophysical modeling, and follow-up spectroscopic observations of the
candidate systems are encouraged.
