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Neutron stars are not only of astrophysical interest, but are also of greatinterest to nuclear physicists, because their attributes can be used todetermine the properties of the dense matter in their cores. One of the mostinformative approaches for determining the equation of state of this densematter is to measure both a star's equatorial circumferential radius $R_e$ andits gravitational mass $M$. Here we report estimates of the mass and radius ofthe isolated 205.53 Hz millisecond pulsar PSR J0030+0451 obtained using aBayesian inference approach to analyze its energy-dependent thermal X-raywaveform, which was observed using the Neutron Star Interior CompositionExplorer (NICER). This approach is thought to be less subject to systematicerrors than other approaches for estimating neutron star radii. We explored avariety of emission patterns on the stellar surface. Our best-fit model hasthree oval, uniform-temperature emitting spots and provides an excellentdescription of the pulse waveform observed using NICER. The radius and massestimates given by this model are $R_e = 13.02^{+1.24}_{-1.06}$ km and $M =1.44^{+0.15}_{-0.14}\ M_\odot$ (68%). The independent analysis reported in thecompanion paper by Riley et al. (2019) explores different emitting spot models,but finds spot shapes and locations and estimates of $R_e$ and $M$ that areconsistent with those found in this work. We show that our measurements of$R_e$ and $M$ for PSR J0030$+$0451 improve the astrophysical constraints on theequation of state of cold, catalyzed matter above nuclear saturation density.

PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter