  The vast majority of well studied giant-planet systems, including the Solar
System, are nearly coplanar which implies dissipation within a primordial gas
disk. however, intrinsic instability may lead to planet-planet scattering,
which often produces non-coplanar, eccentric orbits. Planet scattering theories
have been developed to explain observed high eccentricity systems and also hot
Jupiters; thus far their predictions for mutual inclination (I) have barely
been tested. Here we characterize a highly mutually-inclined (I ~ 15-60
degrees), moderately eccentric (e >~ 0.1) giant planet system: Kepler-108. This
system consists of two approximately Saturn-mass planets with periods of ~49
and ~190 days around a star with a wide (~300AU) binary companion in an orbital
configuration inconsistent with a purely disk migration origin.
