  We present a global analysis of KOI-977, one of the planet host candidates
detected by {\it Kepler}. Kepler Input Catalog (KIC) reports that KOI-977 is a
red giant, for which few close-in planets have been discovered. Our global
analysis involves spectroscopic and asteroseismic determinations of stellar
parameters (e.g., mass and radius) and radial velocity (RV) measurements. Our
analyses reveal that KOI-977 is indeed a red giant in the red clump, but its
estimated radius ($\gtrsim 20R_\odot=0.093$ AU) is much larger than
KOI-977.01's orbital distance ($\sim 0.027$ AU) estimated from its period
($P_\mathrm{orb}\sim 1.35$ days) and host star's mass. RV measurements show a
small variation, which also contradicts the amplitude of ellipsoidal variations
seen in the light-curve folded with KOI-977.01's period. Therefore, we conclude
that KOI-977.01 is a false positive, meaning that the red giant, for which we
measured the radius and RVs, is different from the object that produces the
transit-like signal (i.e., an eclipsing binary). On the basis of this
assumption, we also perform a light-curve analysis including the modeling of
transits/eclipses and phase-curve variations, adopting various values for the
dilution factor $D$, which is defined as the flux ratio between the red giant
and eclipsing binary. Fitting the whole folded light-curve as well as
individual transits in the short cadence data simultaneously, we find that the
estimated mass and radius ratios of the eclipsing binary are consistent with
those of a solar-type star and a late-type star (e.g., an M dwarf) for
$D\gtrsim 20$.
