Eclipsing binary stars allow derivation of accurate and precise masses and radii. When they reside in star clusters, properties of even higher precision, along with additional information, can be extracted. Asteroseismology of solar-like oscillations offers similar possibilities for single stars. We improve the previously established properties of the Hyades eclipsing binary HD27130 and re-assess the asteroseismic properties of the giant star $epsilon$ Tau. The physical properties of these members of the Hyades are then used to constrain the helium content and age of the cluster. New multi-colour light curves were combined with multi-epoch radial velocities to yield masses and radii of HD27130. $T_{rm eff}$ was derived from spectroscopy and photometry, and verified using the Gaia parallax. We estimate the cluster age from re-evaluated asteroseismic properties of $epsilon$ Tau while using HD27130 to constrain the helium content. The masses and radii, and $T_{rm eff}$ of HD 27130 were found to be $M=1.0245pm0.0024 M_{odot}$, $R=0.9226pm0.015 R_{odot}$, $T_{rm eff}=5650pm50$ K for the primary, and $M=0.7426pm0.0016 M_{odot}$, $R=0.7388pm0.026 R_{odot}$, $T_{rm eff}=4300pm100$ K for the secondary component. Our re-evaluation of $epsilon$ Tau suggests that the previous literature estimates are trustworthy, and that the Hipparcos parallax is more reliable than the Gaia DR2 parallax. The helium content of HD27130 and thus of the Hyades is found to be $Y=0.27$ but with significant model dependence. Correlations with the adopted metallicity results in a robust helium enrichment law with $frac{Delta Y}{Delta Z}$ close to 1.2. We estimate the age of the Hyades to be 0.9 $pm$ 0.1 (stat) $pm$ 0.1 (sys) Gyr in slight tension with recent age estimates based on the cluster white dwarfs. (abridged)
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