A NICER view of the 1.4 solar-mass edge-on pulsar PSR J0614-3329
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866911311070232576 |
|---|---|
| author | Mauviard, Lucien Guillot, Sebastien Salmi, Tuomo Choudhury, Devarshi Dorsman, Bas González-Caniulef, Denis Hoogkamer, Mariska Huppenkothen, Daniela Kazantsev, Christine Kini, Yves Olive, Jean-Francois Stammler, Pierre Watts, Anna L. Mendes, Melissa Rutherford, Nathan Schwenk, Achim Svensson, Isak Bogdanov, Slavko Kerr, Matthew Ray, Paul S. Guillemot, Lucas Cognard, Ismaël Theureau, Gilles |
| author_facet | Mauviard, Lucien Guillot, Sebastien Salmi, Tuomo Choudhury, Devarshi Dorsman, Bas González-Caniulef, Denis Hoogkamer, Mariska Huppenkothen, Daniela Kazantsev, Christine Kini, Yves Olive, Jean-Francois Stammler, Pierre Watts, Anna L. Mendes, Melissa Rutherford, Nathan Schwenk, Achim Svensson, Isak Bogdanov, Slavko Kerr, Matthew Ray, Paul S. Guillemot, Lucas Cognard, Ismaël Theureau, Gilles |
| contents | Four neutron star radius measurements have already been obtained by modeling the X-ray pulses of rotation-powered millisecond pulsars observed by the Neutron Star Interior Composition ExploreR (NICER). We report here the radius measurement of PSR J0614-3329 employing the same method with NICER and XMM-Newton data using Bayesian Inference. For all different models tested, including one with unrestricted inclination prior, we retrieve very similar non-antipodal hot regions geometries and radii. For the preferred model, we infer an equatorial radius of $R_{\rm eq}=10.29^{+1.01}_{-0.86}\,$km for a mass of $M=1.44^{+0.06}_{-0.07} \, M_{\odot}$ (median values with equal-tailed $68\%$ credible interval), the latter being essentially constrained from radio timing priors obtained by MeerKAT. A more complex model, fitting the data equally well, resulted in a consistent inferred radius. We find that, for all different models, the pulse emission originates from two hot regions, one at the pole and the other at the equator. The resulting radius constraint is consistent with previous X-ray and gravitational wave measurements of neutron stars in the same mass range. Equation of state inferences, including previous NICER and gravitational wave results, slightly soften the equation of state with PSR J0614$-$3329 included and shift the allowed mass-radius region toward lower radii by $\sim 300\,$m, which is compatible with previous analyses to within less than one standard deviation. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2506_14883 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A NICER view of the 1.4 solar-mass edge-on pulsar PSR J0614-3329 Mauviard, Lucien Guillot, Sebastien Salmi, Tuomo Choudhury, Devarshi Dorsman, Bas González-Caniulef, Denis Hoogkamer, Mariska Huppenkothen, Daniela Kazantsev, Christine Kini, Yves Olive, Jean-Francois Stammler, Pierre Watts, Anna L. Mendes, Melissa Rutherford, Nathan Schwenk, Achim Svensson, Isak Bogdanov, Slavko Kerr, Matthew Ray, Paul S. Guillemot, Lucas Cognard, Ismaël Theureau, Gilles High Energy Astrophysical Phenomena Solar and Stellar Astrophysics Nuclear Theory Four neutron star radius measurements have already been obtained by modeling the X-ray pulses of rotation-powered millisecond pulsars observed by the Neutron Star Interior Composition ExploreR (NICER). We report here the radius measurement of PSR J0614-3329 employing the same method with NICER and XMM-Newton data using Bayesian Inference. For all different models tested, including one with unrestricted inclination prior, we retrieve very similar non-antipodal hot regions geometries and radii. For the preferred model, we infer an equatorial radius of $R_{\rm eq}=10.29^{+1.01}_{-0.86}\,$km for a mass of $M=1.44^{+0.06}_{-0.07} \, M_{\odot}$ (median values with equal-tailed $68\%$ credible interval), the latter being essentially constrained from radio timing priors obtained by MeerKAT. A more complex model, fitting the data equally well, resulted in a consistent inferred radius. We find that, for all different models, the pulse emission originates from two hot regions, one at the pole and the other at the equator. The resulting radius constraint is consistent with previous X-ray and gravitational wave measurements of neutron stars in the same mass range. Equation of state inferences, including previous NICER and gravitational wave results, slightly soften the equation of state with PSR J0614$-$3329 included and shift the allowed mass-radius region toward lower radii by $\sim 300\,$m, which is compatible with previous analyses to within less than one standard deviation. |
| title | A NICER view of the 1.4 solar-mass edge-on pulsar PSR J0614-3329 |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics Nuclear Theory |
| url | https://arxiv.org/abs/2506.14883 |