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Eclipsing binary stars allow derivation of accurate and precise masses andradii. When they reside in star clusters, properties of even higher precision,along with additional information, can be extracted. Asteroseismology ofsolar-like oscillations offers similar possibilities for single stars. Weimprove the previously established properties of the Hyades eclipsing binaryHD27130 and re-assess the asteroseismic properties of the giant star $\epsilon$Tau. The physical properties of these members of the Hyades are then used toconstrain the helium content and age of the cluster. New multi-colour lightcurves were combined with multi-epoch radial velocities to yield masses andradii of HD27130. $T_{\rm eff}$ was derived from spectroscopy and photometry,and verified using the Gaia parallax. We estimate the cluster age fromre-evaluated asteroseismic properties of $\epsilon$ Tau while using HD27130 toconstrain the helium content. The masses and radii, and $T_{\rm eff}$ of HD27130 were found to be $M=1.0245\pm0.0024 M_{\odot}$, $R=0.9226\pm0.015R_{\odot}$, $T_{\rm eff}=5650\pm50$ K for the primary, and $M=0.7426\pm0.0016M_{\odot}$, $R=0.7388\pm0.026 R_{\odot}$, $T_{\rm eff}=4300\pm100$ K for thesecondary component. Our re-evaluation of $\epsilon$ Tau suggests that theprevious literature estimates are trustworthy, and that the Hipparcos parallaxis more reliable than the Gaia DR2 parallax. The helium content of HD27130 andthus of the Hyades is found to be $Y=0.27$ but with significant modeldependence. Correlations with the adopted metallicity results in a robusthelium enrichment law with $\frac{\Delta Y}{\Delta Z}$ close to 1.2. Weestimate the age of the Hyades to be 0.9 $\pm$ 0.1 (stat) $\pm$ 0.1 (sys) Gyrin slight tension with recent age estimates based on the cluster white dwarfs.(abridged)

Properties of the Hyades, the eclipsing binary HD27130, and the oscillating red giant $\epsilon$ Tau