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; Wolff, Michael T.

doi:10.3847/1538-4357/acfb83

Cited by 36 publications

(26 citation statements)

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“…The calculation is carried out with the EOS constraint result of the GP model (As shown in Figure 1, the results of the three reconstruction methods are well consistent with each other). Different from the direct inference results only with the NICER and XMM-Newton data (i.e., the almost "separated" counter regions marked by the dashed solid lines that are adopted from Vinciguerra et al 2024), for the ST+PDT and PDT-U models our inferred mass and radius of PSR J0030 +0451 are well consistent with each other. This is anticipated since both models yield rather similar , although the PDT-U model has a larger error bar than that of the ST+PDT model, which is why the inferred mass for the former is more uncertain than the latter.…”

Section: Resultscontrasting

confidence: 98%

“…We would also remark that our current results are also consistent with the initial mass/radius inference results with the X-ray data published in Riley et al (2019) and Miller et al (2019). Note that when adopting the same models used in Riley et al (2019) and Miller et al (2019), Vinciguerra et al (2024 found consistent results, although with more stringent inference requirements. Now we estimate the tidal deformability, moment of inertia, and gravitational BE of PSR J0030+0451.…”

Section: Resultssupporting

confidence: 91%

“…Now we estimate the tidal deformability, moment of inertia, and gravitational BE of PSR J0030+0451. The estimated Λ are The red area represents the results obtained using the GP model, the blue area represents the results obtained using the FFNN method, the green area represents the results obtained using the PWLS method, and the yellow and gray filled areas, respectively, represent the results from the ST+PDT and PDT-U models used by Vinciguerra et al (2024). The regions are for the 68% credible level.…”

Section: Resultsmentioning

confidence: 99%

“…One of the targets of the NICER mission, PSR J0030+0451, is very close to Earth, has very bright X-ray radiation, and has long been considered an excellent target for measuring mass and radius using the X-ray profile modeling method. However, the recent reanalysis (Vinciguerra et al 2024) found that, based on more general assumptions and treatments, the mass and radius results for PSR J0030+0451 strongly depend on the adopted hot spot model. This means that the current high-precision X-ray data alone is still not sufficient to fully determine the mass and radius of the isolated NS PSR J0030+0451.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…However, recent studies by the NICER team suggest that these initial measurements require a reassessment (Vinciguerra et al 2024). Adopting more general assumptions and integrating data from the XMM-Newton detector, these authors have found that current data can only precisely constrain the ratio of mass to radius (the compactness of NS, = M R  ) for PSR J0030+0451 rather than accurately determining its mass and radius separately.…”

Section: Introductionmentioning

confidence: 99%

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Bulk Properties of PSR J0030+0451 Inferred with the Compactness Measurement of NICER

Luo,

Tang,

Han

et al. 2024

ApJ

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In 2019, the Neutron star Interior Composition ExploreR (NICER) mission released its findings on the mass and radius of the isolated neutron star (INS) PSR J0030+0451, revealing a mass of approximately 1.4 solar masses (M ⊙) and a radius near 13 km. However, the recent reanalysis by the NICER collaboration suggests that the available data primarily yield a precise inference of the compactness for this source while the resulting mass and radius are strongly model-dependent and diverse (the 68.3% credible regions just overlap slightly for the ST+PDT and PDT-U models). By integrating this compactness data with the equation of state (EOS) refined by our latest investigations, we have deduced the mass and radius for PSR J0030+0451, delivering estimates of M = 1.48 − 0.10 + 0.09 M ⊙ and R = 12.38 − 0.70 + 0.51 km for the compactness found in the ST+PDT model, alongside M = 1.47 − 0.20 + 0.14 M ⊙ and R = 12.37 − 0.69 + 0.50 km for the compactness in the PDT-U model. These two groups of results are well consistent with each other and the direct X-ray data inference within the ST+PDT model seems to be favored. Additionally, we have calculated the tidal deformability, moment of inertia, and gravitational binding energy for this neutron star. Furthermore, employing these refined EOS models, we have updated mass–radius estimates for three INSs with established gravitational redshifts.

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Section: Resultscontrasting

confidence: 98%

Section: Resultssupporting

confidence: 91%

Section: Resultsmentioning

confidence: 99%

Section: Conclusion and Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Bulk Properties of PSR J0030+0451 Inferred with the Compactness Measurement of NICER

Luo,

Tang,

Han

et al. 2024

ApJ

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Gravity experiments with radio pulsars

Freire,

Wex

2024

Living Rev Relativ

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The discovery of the first pulsar in a binary star system, the Hulse–Taylor pulsar, 50 years ago opened up an entirely new field of experimental gravity. For the first time it was possible to investigate strong-field and radiative aspects of the gravitational interaction. Continued observations of the Hulse–Taylor pulsar eventually led, among other confirmations of the predictions of general relativity (GR), to the first evidence for the reality of gravitational waves. In the meantime, many more radio pulsars have been discovered that are suitable for testing GR and its alternatives. One particularly remarkable binary system is the Double Pulsar, which has far surpassed the Hulse–Taylor pulsar in several respects. In addition, binary pulsar-white dwarf systems have been shown to be particularly suitable for testing alternative gravitational theories, as they often predict strong dipolar gravitational radiation for such asymmetric systems. A rather unique pulsar laboratory is the pulsar in a hierarchical stellar triple, that led to by far the most precise confirmation of the strong-field version of the universality of free fall. Using radio pulsars, it could be shown that additional aspects of the Strong Equivalence Principle apply to the dynamics of strongly self-gravitating bodies, like the local position and local Lorentz invariance of the gravitational interaction. So far, GR has passed all pulsar tests with flying colours, while at the same time many alternative gravity theories have either been strongly constrained or even falsified. New telescopes, instrumentation, timing and search algorithms promise a significant improvement of the existing tests and the discovery of (qualitatively) new, more relativistic binary systems.

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Two black widow pulsars in the optical and X-rays

Bobakov,

Kirichenko,

Zharikov

et al. 2024

A&A

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Two millisecond pulsars, PSR J1513$-$2550 and PSR J2017$-$1614, with spin periods of about 2.1 and 2.3 ms were recently discovered in the radio and gamma -rays and classified as black widow pulsars in tight binary stellar systems with orbital periods of about 4.3 and 2.3 h. Our goals are to reveal the fundamental parameters of both systems and their binary components using multi-wavelength observations. We carried out the first time-series multi-band optical photometry of the objects with the 2.1-metre telescope of the Observatorio Astron\'omico Nacional San Pedro M\'artir, the 6.5-metre telescope, and the 10.4-metre Gran Telescopio Canarias. To derive the parameters of both systems, we fitted the obtained light curves with a model assuming heating of the companion by the pulsar. We also analysed archival X-ray data obtained with the observatory. For the first time, we firmly identified J1513$-$2550 in the optical and both pulsars in X-rays. The optical light curves of both systems have a single peak per orbital period with a peak-to-peak amplitude of $ magnitudes. The J2017$-$1614 light curves are symmetric, while J1513$-$2550 demonstrates strong asymmetry whose nature remains unclear. We constrained the orbital inclinations, pulsar masses, companion temperatures and masses, and the distances to both systems. We also conclude that J2017$-$1614 may contain a massive neutron star of 2.4pm 0.6 The X-ray spectra of both sources can be fitted by power laws with parameters typical of black widow systems.

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An Updated Mass–Radius Analysis of the 2017–2018 NICER Data Set of PSR J0030+0451

Cited by 36 publications

References 50 publications

Bulk Properties of PSR J0030+0451 Inferred with the Compactness Measurement of NICER

Bulk Properties of PSR J0030+0451 Inferred with the Compactness Measurement of NICER

Gravity experiments with radio pulsars

Two black widow pulsars in the optical and X-rays

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