  We report here an analysis of the physical stellar parameters of the giant
star HD185351 using Kepler short-cadence photometry, optical and near infrared
interferometry from CHARA, and high-resolution spectroscopy. Asteroseismic
oscillations detected in the Kepler short-cadence photometry combined with an
effective temperature calculated from the interferometric angular diameter and
bolometric flux yield a mean density, rho_star = 0.0130 +- 0.0003 rho_sun and
surface gravity, logg = 3.280 +- 0.011. Combining the gravity and density we
find Rstar = 5.35 +- 0.20 Rsun and Mstar = 1.99 +- 0.23 Msun. The trigonometric
parallax and CHARA angular diameter give a radius Rstar = 4.97 +- 0.07 Rsun.
This smaller radius,when combined with the mean stellar density, corresponds to
a stellar mass Mstar = 1.60 +- 0.08 Msun, which is smaller than the
asteroseismic mass by 1.6-sigma. We find that a larger mass is supported by the
observation of mixed modes in our high-precision photometry, the spacing of
which is consistent only for Mstar =~ 1.8 Msun. Our various and independent
mass measurements can be compared to the mass measured from interpolating the
spectroscopic parameters onto stellar evolution models, which yields a
model-based mass M_star = 1.87 +- 0.07 Msun. This mass agrees well with the
asteroseismic value,but is 2.6-sigma higher than the mass from the combination
of asteroseismology and interferometry. The discrepancy motivates future
studies with a larger sample of giant stars. However, all of our mass
measurements are consistent with HD185351 having a mass in excess of 1.5 Msun.
