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We use photometric and spectroscopic observations of the eclipsing binary E32in the globular cluster 47 Tuc to derive the masses, radii, and luminosities ofthe component stars. The system has an orbital period of 40.9 d, a markedlyeccentric orbit with e = 0.24, and is shown to be a member of or a recentescaper from the cluster. We obtain Mp = 0.862(5) Msun , Rp = 1.183(3) Rsun ,Lp = 1.65(5) Lsun for the primary and Ms = 0.827(5) Msun , Rs = 1.004(4) Rsun ,Ls = 1.14(4) Lsun for the secondary. Based on these data and on an earlieranalysis of the binary V69 in 47 Tuc we measure the distance to the clusterfrom the distance moduli of the component stars, and, independently, from acolor - surface brightness calibration. We obtain 4.55(3) and 4.50(7) kpc,respectively - values compatible within 1 sigma with recent estimates based onGaia DR2 parallaxes. By comparing the M - R diagram of the two binaries and thecolor-magnitude diagram of 47 Tuc to Dartmouth model isochrones we estimate theage of the cluster to be 12.0 pm 0.5 Gyr, and the helium abundance of thecluster to be Y approx 0.25.

The Cluster Ages Experiment (CASE). VIII. Age and Distance of the Globular Cluster 47 Tuc from the Analysis of Two Detached Eclipsing Binaries