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A NICER View of PSR J0030+0451: Updated Constraints from 6 yr of NICER Observations
Yves Kini (University of Amsterdam), Lucien Mauviard (Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse), Tuomo Salmi (University of Helsinki), Anna L. Watts (University of Amsterdam), Sébastien Guillot (Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse), Bas Dorsman (University of Amsterdam), Devarshi Choudhury (University of Amsterdam), Denis González–Caniulef (Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse), Mariska Hoogkamer (University of Amsterdam), Daniela Huppenkothen (University of Amsterdam), Christine Kazantsev (Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse), Matthew T. Kerr, S. Nissanke (University of Potsdam, Deutsches Elektronen-Synchrotron DESY), Paul S. Ray, Pierre Stammler (Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse), S. Vinciguerra
Résumé : Abstract Pulse-profile modeling of rotation-powered millisecond pulsars targeted by NICER has enabled mass–radius constraints of several neutron star sources, with implications for the dense-matter equation of state. For the bright isolated pulsar PSR J0030+0451, the inferred mass and radius were previously found to depend strongly on the assumed hot-spot model. These hot-spot models yielded different mass–radius constraints, with the statistically preferred model exhibiting some mild tension with results inferred for PSR J0437−4715, PSR J0614−3329, and GW170817. We present an updated pulse-profile analysis of PSR J0030+0451 using new NICER observations obtained between 2017 July to 2023 January, increasing the number of X-ray counts by about 50% compared to previous analyses. We jointly analyze the NICER data with archival XMM-Newton observations to better constrain the source spectrum and background. The new analysis, using more conservative nested-sampling settings together with the new NICER observations, significantly reduces the discrepancy between the hot-spot models. The inferred mass and radius are M = 1.4 3 − 0.17 + 0.20 M ⊙ and R eq = 12.6 8 − 1.04 + 1.31 km (68% credible intervals), reducing the tension with the results from other sources. In addition, the inferred hot-spot configurations suggest the presence of intraspot temperature gradients.