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| Main Authors: | , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2026
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2602.23743 |
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| _version_ | 1866914356353040384 |
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| author | Kini, Yves Mauviard, Lucien Salmi, Tuomo Watts, Anna L. Guillot, Sebastien Dorsman, Bas Choudhury, Devarshi González-Caniulef, Denis Hoogkamer, Mariska Huppenkothen, Daniela Kazantsev, Christine Kerr, Matthew Nissanke, Samaya Ray, Paul S. Stammler, Pierre Vinciguerra, Serena |
| author_facet | Kini, Yves Mauviard, Lucien Salmi, Tuomo Watts, Anna L. Guillot, Sebastien Dorsman, Bas Choudhury, Devarshi González-Caniulef, Denis Hoogkamer, Mariska Huppenkothen, Daniela Kazantsev, Christine Kerr, Matthew Nissanke, Samaya Ray, Paul S. Stammler, Pierre Vinciguerra, Serena |
| contents | 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--radius was 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 significantly reduces the discrepancy between the hot spot models. The inferred mass and radius are $M = 1.43^{+0.20}_{-0.17}\,M_\odot$ and $R_{\rm eq} = 12.68^{+1.31}_{-1.04}$ km (68% credible intervals), reducing the tension with the results from other sources. In addition, the inferred hot spot configurations suggest the presence of intra-spot temperature gradients. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2602_23743 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | A NICER View of PSR J0030+0451: Updated Constraints from Six Years of NICER Observations Kini, Yves Mauviard, Lucien Salmi, Tuomo Watts, Anna L. Guillot, Sebastien Dorsman, Bas Choudhury, Devarshi González-Caniulef, Denis Hoogkamer, Mariska Huppenkothen, Daniela Kazantsev, Christine Kerr, Matthew Nissanke, Samaya Ray, Paul S. Stammler, Pierre Vinciguerra, Serena High Energy Astrophysical Phenomena 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--radius was 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 significantly reduces the discrepancy between the hot spot models. The inferred mass and radius are $M = 1.43^{+0.20}_{-0.17}\,M_\odot$ and $R_{\rm eq} = 12.68^{+1.31}_{-1.04}$ km (68% credible intervals), reducing the tension with the results from other sources. In addition, the inferred hot spot configurations suggest the presence of intra-spot temperature gradients. |
| title | A NICER View of PSR J0030+0451: Updated Constraints from Six Years of NICER Observations |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2602.23743 |