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The Kepler mission has provided exquisite data to perform an ensembleasteroseismic analysis on evolved stars. In this work we systematicallycharacterize solar-like oscillations and granulation for 16,094 oscillating redgiants, using end-of-mission long-cadence data. We produced a homogeneouscatalog of the frequency of maximum power (typical uncertainty$\sigma_{\nu_{\rm max}}$=1.6\%), the mean large frequency separation($\sigma_{\Delta\nu}$=0.6\%), oscillation amplitude ($\sigma_{\rm A}$=4.7\%),granulation power ($\sigma_{\rm gran}$=8.6\%), power excess width ($\sigma_{\rmwidth}$=8.8\%), seismically-derived stellar mass ($\sigma_{\rm M}$=7.8\%),radius ($\sigma_{\rm R}$=2.9\%), and thus surface gravity ($\sigma_{\logg}$=0.01 dex). Thanks to the large red giant sample, we confirm thatred-giant-branch (RGB) and helium-core-burning (HeB) stars collectively differin the distribution of oscillation amplitude, granulation power, and width ofpower excess, which is mainly due to the mass difference. The distribution ofoscillation amplitudes shows an extremely sharp upper edge at fixed $\nu_{\rmmax}$, which might hold clues to understand the excitation and dampingmechanisms of the oscillation modes. We find both oscillation amplitude andgranulation power depend on metallicity, causing a spread of 15\% inoscillation amplitudes and a spread of 25\% in granulation power from[Fe/H]=-0.7 to 0.5 dex. Our asteroseismic stellar properties can be used asreliable distance indicators and age proxies for mapping and dating galacticstellar populations observed by Kepler. They will also provide an excellentopportunity to test asteroseismology using Gaia parallaxes, and liftdegeneracies in deriving atmospheric parameters in large spectroscopic surveyssuch as APOGEE and LAMOST.

Asteroseismology of 16000 Kepler Red Giants: Global Oscillation Parameters, Masses, and Radii