  The internal structures and properties of oscillating red-giant stars can be
accurately inferred through their global oscillation modes (asteroseismology).
Based on 1460 days of Kepler observations we perform a thorough asteroseismic
study to probe the stellar parameters and evolutionary stages of three red
giants in eclipsing binary systems. We present the first detailed analysis of
individual 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 the
asteroseismic scaling relations as well as grid-based modelling. As these red
giants are in double-lined eclipsing binaries, it is possible to derive their
independent dynamical masses and radii from the orbital solution and compare it
with the seismically inferred values. For KIC 5640750 we compute the first
spectroscopic orbit based on both components of this system. We use
high-resolution spectroscopic data and light curves of the three systems to
determine up-to-date values of the dynamical stellar parameters. With our
comprehensive set of stellar parameters we explore consistencies between binary
analysis and asteroseismic methods, and test the reliability of the well-known
scaling relations. For the three red giants under study, we find agreement
between dynamical and asteroseismic stellar parameters in cases where the
asteroseismic methods account for metallicity, temperature and mass dependence
as well as surface effects. We are able to attain agreement from the scaling
laws in all three systems if we use $\Delta\nu_{\rm ref,emp} = 130.8 \pm
0.9\,\mu$Hz instead of the usual solar reference value.
