  We analyzed the Kepler light curves of four transiting hot Jupiter systems
--- KOI-13, HAT-P-7, TrES-2, and Kepler-76, which show BEaming, Ellipsoidal and
Reflection (BEER) phase modulations. The mass of the four planets can be
estimated from either the beaming or the ellipsoidal amplitude, given the mass
and radius of their parent stars. For KOI-13, HAT-P-7, and Kepler-76 we find
that the beaming-based planetary mass estimate is larger than the mass
estimated from the ellipsoidal amplitude, consistent with previous studies.
This apparent discrepancy may be explained by equatorial superrotation of the
planet atmosphere, which induces an angle shift of the planet
reflection/emission phase modulation, as was suggested for Kepler-76 in the
first paper of this series. We propose a modified BEER model that supports
superrotation, assuming either a Lambertian or geometric reflection/emission
phase function, and provides a photometry-consistent estimate of the planetary
mass. Our analysis shows that for Kepler-76 and HAT-P-7, the Lambertian
superrotation BEER model is highly preferable over an unshifted null model,
while for KOI-13 it is preferable only at a 1.4 sigma level. For TrES-2 we do
not find such preference. For all four systems the Lambertian superrotation
model mass estimates are in excellent agreement with the planetary masses
derived from, or constrained by, radial velocity measurements. This makes the
Lambertian superrotation BEER model a viable tool for estimating the masses of
hot Jupiters from photometry alone. We conclude that hot Jupiter superrotation
may be a common phenomenon that can be detected in the visual light curves of
Kepler.
