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Context: Intermediate-Mass stars are often overlooked as they are notsupernova progenitors but still host convective cores and complex atmosphereswhich require computationally expensive treatment. Due to this, there is ageneral lack of such stars modelled by state of the art stellar structure andevolution codes. Aims: This paper aims to use high-quality spectroscopy toupdate the dynamically obtained stellar parameters and produce a newevolutionary assessment of the bright B0.5+B0.5 and B5V+B5V binary systems CWCep and U Oph. Methods: We use new spectroscopy obtained with the Hermesspectrograph to revisit the photometric binary solution of the two systems. Theupdated mass ratio and effective temperatures are incorporated to obtain newdynamical masses for the primary and secondary. With these, we performisochrone-cloud based evolutionary modelling to investigate the core propertiesof these stars. Results: We report the first abundances for CW Cep and U Oph aswell as report an updated dynamical solution for both systems. We find that wecannot uniquely constrain the amount of core boundary mixing in any of thestars we consider. Instead, we report their core masses and compare our resultsto previous studies. Conclusions: We find that the per-cent level precision onfundamental stellar quantities are accompanied with core mass estimates tobetween ~ 5-15%. We find that differences in analysis techniques can lead tosubstantially different evolutionary mode

Modelling of the B-type binaries CW Cep and U Oph: A critical view on dynamical masses, core boundary mixing, and core mass