Leslie M. MoralesEric L. SandquistGail H. SchaeferChristopher D. FarringtonRobert KlementBedin, L. R.L. R.BedinMattia LibralatoLuca MalavoltaDomenico NardielloJerome A. OroszJohn D. MonnierStefan KrausJean-Baptiste Le BouquinNarsireddy AnuguTheo ten BrummelaarClaire L. DaviesJacob EnnisTyler GardnerCyprien Lanthermann2023-01-202023-01-2020220004-6256http://hdl.handle.net/20.500.12386/32948We observe the brightest member of the Praesepe cluster, ϵ Cnc, to precisely measure the characteristics of the stars in this binary system, en route to a new measurement of the cluster's age. We present spectroscopic radial velocity measurements and interferometric observations of the sky-projected orbit to derive the masses, which we find to be M 1/M = 2.420 ± 0.008 and M 2/M= 2.226 ± 0.004. We place limits on the color-magnitude positions of the stars by using spectroscopic and interferometric luminosity ratios while trying to reproduce the spectral energy distribution of ϵ Cnc. We reexamine the cluster membership of stars at the bright end of the color-magnitude diagram using Gaia data and literature radial velocity information. The binary star data are consistent with an age of 637 ± 19 Myr, as determined from MIST model isochrones. The masses and luminosities of the stars appear to select models with the most commonly used amount of convective core overshooting.STAMPAenArticle10.3847/1538-3881/ac73292-s2.0-85134702286https://doi.org/10.3847/1538-3881/ac7329https://iopscience.iop.org/article/10.3847/1538-3881/ac7329FIS/05 - ASTRONOMIA E ASTROFISICA