  When low- and intermediate-mass stars evolve off the main sequence, they
expand and cool into the red giant stages of evolution, which include those
associated with shell H burning (the red giant branch), core He burning (the
red clump), and shell He burning (the asymptotic giant branch). The majority of
red giants have masses $< 2 M_\odot$, and red giants more massive than this are
often excluded from major studies. Here we present a study of the highest-mass
stars ($M > 3.0 M_\odot$) in the Kepler sample of 16,000 red giants. We begin
by re-estimating their global seismic properties with new light curves,
highlighting the differences between using the SAP and PDCSAP light curves
provided by Kepler. We use the re-estimated properties to derive new mass
estimates for the stars, ending with a final sample of 48 confirmed high-mass
stars. We explore their oscillation envelopes, confirming the trends found in
recent works such as low mean mode amplitude and wide envelopes. We find,
through probabilistic means, that our sample is likely all core He burning
stars. We measure their dipole and quadrupole mode visibilities and confirm
that the dipole mode visibility tends to decrease with mass.
