  The last five years have seen remarkable progress in our quest to determine
the equation of state of neutron rich matter. Recent advances across the
theoretical, experimental, and observational landscape have been incorporated
in a Bayesian framework to refine existing covariant energy density functionals
previously calibrated by the properties of finite nuclei. In particular,
constraints on the maximum neutron star mass from pulsar timing, on stellar
radii from the NICER mission, on tidal deformabilities from the LIGO-Virgo
collaboration, and on the dynamics of pure neutron matter as predicted from
chiral effective field theories, have resulted in significant refinements to
the models, particularly to those predicting a stiff symmetry energy. Still,
even after these improvements, we find challenging to reproduce simultaneously
the neutron skin thickness of both ${}^{208}$Pb and ${}^{48}$Ca recently
reported by the PREX/CREX collaboration.
