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Given the potential of ensemble asteroseismology for understandingfundamental properties of large numbers of stars, it is critical to determinethe accuracy of the scaling relations on which these measurements are based.From several powerful validation techniques, all indications so far show thatstellar radius estimates from the asteroseismic scaling relations are accurateto within a few percent. Eclipsing binary systems hosting at least one starwith detectable solar-like oscillations constitute the ideal test objects forvalidating asteroseismic radius and mass inferences. By combiningradial-velocity measurements and photometric time series of eclipses, it ispossible to determine the masses and radii of each component of a double-linedspectroscopic binary. We report the results of a four-year radial-velocitysurvey performed with the \'echelle spectrometer of the Astrophysical ResearchConsortium's 3.5-m telescope and the APOGEE spectrometer at Apache PointObservatory. We compare the masses and radii of 10 red giants obtained bycombining radial velocities and eclipse photometry with the estimates from theasteroseismic scaling relations. We find that the asteroseismic scalingrelations overestimate red-giant radii by about 5% on average and masses byabout 15% for stars at various stages of red-giant evolution. Systematicoverestimation of mass leads to underestimation of stellar age, which can haveimportant implications for ensemble asteroseismology used for Galactic studies.As part of a second objective, where asteroseismology is used for understandingbinary systems, we confirm that oscillations of red giants in close binariescan be suppressed enough to be undetectable, an hypothesis that was proposed ina previous work.

Testing the asteroseismic scaling relations for Red Giants with Eclipsing Binaries Observed by Kepler