Comparison between the posterior distributions obtained for the assumption that GW170817 is a NS–NS or NS–BH merger, without (left panel) and with (right panel) the NICER measurements of PSR J0030+0451. Here we only show results for the PP model. The lines show the connected 95% credible regions at a given energy density ε. The black lines show the same credible regions when the posterior distribution is only informed by the 2.14 M_⊙ pulsar. The lower right inset illustrates the evolution of the Kullback–Leibler divergence with energy density ε and indicates that GW170817 is slightly more constraining for the EOS when assumed to be a NS–NS merger.