Fig. 7: Effect of different measurements—interpolation.
From: Strongly interacting matter exhibits deconfined behavior in massive neutron stars
Model comparison showing the effect of different measurements on the \({c}_{{{{{{{{\rm{s}}}}}}}},4}^{2}\) parameterization. The first column shows the CIs of various quantities with an EoS parameterization that does not have any astrophysical measurements (prior). The second column shows the Bayesian posterior densities for EoS conditioned with the ≈ 2M⊙ radio pulsar mass measurements. The third column shows the calculations with pulsar masses and tidal deformabilities from GW170817, as well as the assumption that a BH was formed in GW170817. The fourth column shows the calculation with pulsar masses, tidal deformabilities, the assumption that a BH was formed in GW170817, and X-ray measurements. Other quantities and symbols are as in Fig. 5.
