An updated mass-radius analysis of the 2017-2018 NICER data set of PSR J0030+0451
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| Main Authors: | , , , , , , , , , , , , , |
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| Format: | Preprint |
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2023
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| _version_ | 1866914760750006272 |
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| author | Vinciguerra, Serena Salmi, Tuomo Watts, Anna L. Choudhury, Devarshi Riley, Thomas E. Ray, Paul S. Bogdanov, Slavko Kini, Yves Guillot, Sebastien Chakrabarty, Deepto Ho, Wynn C. G. Huppenkothen, Daniela Morsink, Sharon M. Wadiasingh, Zorawar |
| author_facet | Vinciguerra, Serena Salmi, Tuomo Watts, Anna L. Choudhury, Devarshi Riley, Thomas E. Ray, Paul S. Bogdanov, Slavko Kini, Yves Guillot, Sebastien Chakrabarty, Deepto Ho, Wynn C. G. Huppenkothen, Daniela Morsink, Sharon M. Wadiasingh, Zorawar |
| contents | In 2019 the NICER collaboration published the first mass and radius inferred for PSR J0030+0451, thanks to NICER observations, and consequent constraints on the equation of state characterising dense matter. Two independent analyses found a mass of $\sim 1.3-1.4\,\mathrm{M_\odot}$ and a radius of $\sim 13\,$km. They also both found that the hot spots were all located on the same hemisphere, opposite to the observer, and that at least one of them had a significantly elongated shape. Here we reanalyse, in greater detail, the same NICER data set, incorporating the effects of an updated NICER response matrix and using an upgraded analysis framework. We expand the adopted models and jointly analyse also XMM-Newton data, which enables us to better constrain the fraction of observed counts coming from PSR J0030+0451. Adopting the same models used in previous publications, we find consistent results, although with more stringent inference requirements. We also find a multi-modal structure in the posterior surface. This becomes crucial when XMM-Newton data is accounted for. Including the corresponding constraints disfavors the main solutions found previously, in favor of the new and more complex models. These have inferred masses and radii of $\sim [1.4 \mathrm{M_\odot}, 11.5$ km] and $\sim [1.7 \mathrm{M_\odot}, 14.5$ km], depending on the assumed model. They display configurations that do not require the two hot spots generating the observed X-rays to be on the same hemisphere, nor to show very elongated features, and point instead to the presence of temperature gradients and the need to account for them. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2308_09469 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | An updated mass-radius analysis of the 2017-2018 NICER data set of PSR J0030+0451 Vinciguerra, Serena Salmi, Tuomo Watts, Anna L. Choudhury, Devarshi Riley, Thomas E. Ray, Paul S. Bogdanov, Slavko Kini, Yves Guillot, Sebastien Chakrabarty, Deepto Ho, Wynn C. G. Huppenkothen, Daniela Morsink, Sharon M. Wadiasingh, Zorawar High Energy Astrophysical Phenomena Solar and Stellar Astrophysics Nuclear Theory In 2019 the NICER collaboration published the first mass and radius inferred for PSR J0030+0451, thanks to NICER observations, and consequent constraints on the equation of state characterising dense matter. Two independent analyses found a mass of $\sim 1.3-1.4\,\mathrm{M_\odot}$ and a radius of $\sim 13\,$km. They also both found that the hot spots were all located on the same hemisphere, opposite to the observer, and that at least one of them had a significantly elongated shape. Here we reanalyse, in greater detail, the same NICER data set, incorporating the effects of an updated NICER response matrix and using an upgraded analysis framework. We expand the adopted models and jointly analyse also XMM-Newton data, which enables us to better constrain the fraction of observed counts coming from PSR J0030+0451. Adopting the same models used in previous publications, we find consistent results, although with more stringent inference requirements. We also find a multi-modal structure in the posterior surface. This becomes crucial when XMM-Newton data is accounted for. Including the corresponding constraints disfavors the main solutions found previously, in favor of the new and more complex models. These have inferred masses and radii of $\sim [1.4 \mathrm{M_\odot}, 11.5$ km] and $\sim [1.7 \mathrm{M_\odot}, 14.5$ km], depending on the assumed model. They display configurations that do not require the two hot spots generating the observed X-rays to be on the same hemisphere, nor to show very elongated features, and point instead to the presence of temperature gradients and the need to account for them. |
| title | An updated mass-radius analysis of the 2017-2018 NICER data set of PSR J0030+0451 |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics Nuclear Theory |
| url | https://arxiv.org/abs/2308.09469 |