The GW observations and the recent constraints on neutron star radii from Neutron star Interior Composition Explorer (NICER) have provided some constraints on the relationship between total pressure and the matter density. Neither provides an independent constraint on the symmetry energy: the EoS term that arises from the imbalance of neutron and proton composition. The symmetry energy governs the proton fraction, the crust-core phase transition density and pressure, and possible transitions to D matter or to strange matter within neutron stars. I will discuss some experimental efforts to constrain the symmetry energy via experiments where its role can be controlled by varying the n-p imbalance and density of the system. I will discuss some of the results obtained to date and endeavor to put them into context with some of the astrophysical observations.