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The internal structures and properties of oscillating red-giant stars can beaccurately inferred through their global oscillation modes (asteroseismology).Based on 1460 days of Kepler observations we perform a thorough asteroseismicstudy to probe the stellar parameters and evolutionary stages of three redgiants in eclipsing binary systems. We present the first detailed analysis ofindividual oscillation modes of the red-giant components of KIC 8410637,KIC5640750 and KIC9540226. We obtain estimates of their asteroseismic masses,radii, mean densities and logarithmic surface gravities by using theasteroseismic scaling relations as well as grid-based modelling. As these redgiants are in double-lined eclipsing binaries, it is possible to derive theirindependent dynamical masses and radii from the orbital solution and compare itwith the seismically inferred values. For KIC 5640750 we compute the firstspectroscopic orbit based on both components of this system. We usehigh-resolution spectroscopic data and light curves of the three systems todetermine up-to-date values of the dynamical stellar parameters. With ourcomprehensive set of stellar parameters we explore consistencies between binaryanalysis and asteroseismic methods, and test the reliability of the well-knownscaling relations. For the three red giants under study, we find agreementbetween dynamical and asteroseismic stellar parameters in cases where theasteroseismic methods account for metallicity, temperature and mass dependenceas well as surface effects. We are able to attain agreement from the scalinglaws in all three systems if we use $\Delta\nu_{\rm ref,emp} = 130.8 \pm0.9\,\mu$Hz instead of the usual solar reference value.

Oscillating red giants in eclipsing binary systems: empirical reference value for asteroseismic scaling relation