{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1361981471294781184.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/2041-8213/ab50c5"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/2041-8213/ab50c5/pdf"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/2041-8213/ab50c5"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1912.05705"}}],"dc:title":[{"@value":"PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>Neutron stars are not only of astrophysical interest, but are also of great interest to nuclear physicists because their attributes can be used to determine the properties of the dense matter in their cores. One of the most informative approaches for determining the equation of state (EoS) of this dense matter is to measure both a star’s equatorial circumferential radius <jats:italic>R</jats:italic>\n                  <jats:sub>\n                     <jats:italic>e</jats:italic>\n                  </jats:sub> and its gravitational mass <jats:italic>M</jats:italic>. Here we report estimates of the mass and radius of the isolated 205.53 Hz millisecond pulsar PSR J0030+0451 obtained using a Bayesian inference approach to analyze its energy-dependent thermal X-ray waveform, which was observed using the <jats:italic>Neutron Star Interior Composition Explorer</jats:italic> (<jats:italic>NICER</jats:italic>). This approach is thought to be less subject to systematic errors than other approaches for estimating neutron star radii. We explored a variety of emission patterns on the stellar surface. Our best-fit model has three oval, uniform-temperature emitting spots and provides an excellent description of the pulse waveform observed using <jats:italic>NICER</jats:italic>. The radius and mass estimates given by this model are <jats:inline-formula>\n                     <jats:tex-math>\n\n</jats:tex-math>\n                  </jats:inline-formula> km and <jats:inline-formula>\n                     <jats:tex-math>\n\n</jats:tex-math>\n                  </jats:inline-formula> (68%). The independent analysis reported in the companion paper by Riley et al. explores different emitting spot models, but finds spot shapes and locations and estimates of <jats:italic>R</jats:italic>\n                  <jats:sub>\n                     <jats:italic>e</jats:italic>\n                  </jats:sub> and <jats:italic>M</jats:italic> that are consistent with those found in this work. We show that our measurements of <jats:italic>R</jats:italic>\n                  <jats:sub>\n                     <jats:italic>e</jats:italic>\n                  </jats:sub> and <jats:italic>M</jats:italic> for PSR J0030+0451 improve the astrophysical constraints on the EoS of cold, catalyzed matter above nuclear saturation density.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380298755601659404","@type":"Researcher","foaf:name":[{"@value":"M. C. Miller"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781197","@type":"Researcher","foaf:name":[{"@value":"F. K. Lamb"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781185","@type":"Researcher","foaf:name":[{"@value":"A. J. Dittmann"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781195","@type":"Researcher","foaf:name":[{"@value":"S. Bogdanov"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781187","@type":"Researcher","foaf:name":[{"@value":"Z. Arzoumanian"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781193","@type":"Researcher","foaf:name":[{"@value":"K. C. Gendreau"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781202","@type":"Researcher","foaf:name":[{"@value":"S. Guillot"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781194","@type":"Researcher","foaf:name":[{"@value":"A. K. Harding"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781196","@type":"Researcher","foaf:name":[{"@value":"W. C. G. Ho"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781186","@type":"Researcher","foaf:name":[{"@value":"J. M. Lattimer"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781204","@type":"Researcher","foaf:name":[{"@value":"R. M. Ludlam"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781184","@type":"Researcher","foaf:name":[{"@value":"S. Mahmoodifar"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781190","@type":"Researcher","foaf:name":[{"@value":"S. M. Morsink"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781200","@type":"Researcher","foaf:name":[{"@value":"P. S. Ray"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781199","@type":"Researcher","foaf:name":[{"@value":"T. E. Strohmayer"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781188","@type":"Researcher","foaf:name":[{"@value":"K. S. Wood"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781201","@type":"Researcher","foaf:name":[{"@value":"T. Enoto"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781198","@type":"Researcher","foaf:name":[{"@value":"R. Foster"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781203","@type":"Researcher","foaf:name":[{"@value":"T. Okajima"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781192","@type":"Researcher","foaf:name":[{"@value":"G. Prigozhin"}]},{"@id":"https://cir.nii.ac.jp/crid/1381981471294781189","@type":"Researcher","foaf:name":[{"@value":"Y. Soong"}]}],"contributor":[{"@id":"https://cir.nii.ac.jp/crid/1893679867726457093","@type":"Researcher","foaf:name":[{"@value":"Institut de recherche en astrophysique et planétologie (IRAP) ; Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3) ; Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP) ; Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)"}]},{"@id":"https://cir.nii.ac.jp/crid/1890021791196400005","@type":"Researcher","foaf:name":[{"@value":"Université Toulouse III - Paul Sabatier (UT3)"}]},{"@id":"https://cir.nii.ac.jp/crid/1890021791196400003","@type":"Researcher","foaf:name":[{"@value":"Institut de recherche en astrophysique et planétologie (IRAP)"}]},{"@id":"https://cir.nii.ac.jp/crid/1893679867726457218","@type":"Researcher","foaf:name":[{"@value":"Centre National d'Études Spatiales [Toulouse] (CNES)"}]},{"@id":"https://cir.nii.ac.jp/crid/1890021791196400001","@type":"Researcher","foaf:name":[{"@value":"Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP)"}]},{"@id":"https://cir.nii.ac.jp/crid/1890021791196400004","@type":"Researcher","foaf:name":[{"@value":"Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3)"}]},{"@id":"https://cir.nii.ac.jp/crid/1890021791196400000","@type":"Researcher","foaf:name":[{"@value":"Centre National d'Études Spatiales Toulouse (CNES)"}]},{"@id":"https://cir.nii.ac.jp/crid/1890021791196400006","@type":"Researcher","foaf:name":[{"@value":"Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales Toulouse (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales Toulouse (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Centre National de la Recherche Scientifique (CNRS)"}]},{"@id":"https://cir.nii.ac.jp/crid/1893679867726457101","@type":"Researcher","foaf:name":[{"@value":"Institut de recherche en astrophysique et planétologie (IRAP) ; Université Toulouse III - Paul Sabatier (UT3) ; Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP) ; Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3) ; Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Centre National de la Recherche Scientifique (CNRS)"}]},{"@id":"https://cir.nii.ac.jp/crid/1890021791196400002","@type":"Researcher","foaf:name":[{"@value":"HEP, INSPIRE"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"20418205"},{"@type":"EISSN","@value":"20418213"}],"prism:publicationName":[{"@value":"The Astrophysical Journal Letters"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2019-12-10","prism:volume":"887","prism:number":"1","prism:startingPage":"L24"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","dc:rights":["https://iopscience.iop.org/page/copyright","https://iopscience.iop.org/info/page/text-and-data-mining"],"url":[{"@id":"https://iopscience.iop.org/article/10.3847/2041-8213/ab50c5/pdf"},{"@id":"https://iopscience.iop.org/article/10.3847/2041-8213/ab50c5"}],"createdAt":"2019-12-12","modifiedAt":"2024-09-06","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Millisecond%20pulsars","dc:title":"Millisecond pulsars"},{"@id":"https://cir.nii.ac.jp/all?q=%5BPHYS.NUCL%5D%20Physics%20%5Bphysics%5D/Nuclear%20Theory%20%5Bnucl-th%5D","dc:title":"[PHYS.NUCL] Physics [physics]/Nuclear Theory [nucl-th]"},{"@id":"https://cir.nii.ac.jp/all?q=High%20Energy%20Astrophysical%20Phenomena%20(astro-ph.HE)","dc:title":"High Energy Astrophysical Phenomena (astro-ph.HE)"},{"@id":"https://cir.nii.ac.jp/all?q=%5BPHYS.NUCL%5DPhysics%20%5Bphysics%5D/Nuclear%20Theory%20%5Bnucl-th%5D","dc:title":"[PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th]"},{"@id":"https://cir.nii.ac.jp/all?q=Nuclear%20Theory","dc:title":"Nuclear Theory"},{"@id":"https://cir.nii.ac.jp/all?q=FOS:%20Physical%20sciences","dc:title":"FOS: Physical sciences"},{"@id":"https://cir.nii.ac.jp/all?q=X-ray%20sources","dc:title":"X-ray sources"},{"@id":"https://cir.nii.ac.jp/all?q=520","dc:title":"520"},{"@id":"https://cir.nii.ac.jp/all?q=Neutron%20stars","dc:title":"Neutron stars"},{"@id":"https://cir.nii.ac.jp/all?q=Nuclear%20Theory%20(nucl-th)","dc:title":"Nuclear Theory (nucl-th)"},{"@id":"https://cir.nii.ac.jp/all?q=Neutron%20star%20cores","dc:title":"Neutron star cores"},{"@id":"https://cir.nii.ac.jp/all?q=%5BPHYS.ASTR%5D%20Physics%20%5Bphysics%5D/Astrophysics%20%5Bastro-ph%5D","dc:title":"[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]"},{"@id":"https://cir.nii.ac.jp/all?q=%5BPHYS.ASTR%5DPhysics%20%5Bphysics%5D/Astrophysics%20%5Bastro-ph%5D","dc:title":"[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20High%20Energy%20Astrophysical%20Phenomena","dc:title":"Astrophysics - High Energy Astrophysical Phenomena"}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050571859110653312","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Quark-hadron crossover equations of state for neutron stars: Constraining the chiral invariant mass in a parity doublet model"}]},{"@id":"https://cir.nii.ac.jp/crid/1050856893077653760","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Coalescence of black hole–neutron star binaries"},{"@value":"Solar flares: Magnetohydrodynamic processes"}]},{"@id":"https://cir.nii.ac.jp/crid/1360009142595970944","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"A New Approach to the Mass and Radius of Neutron Stars with Supernova Neutrinos"}]},{"@id":"https://cir.nii.ac.jp/crid/1360013168736637952","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Enhanced x-ray emission coinciding with giant radio pulses from the Crab Pulsar"}]},{"@id":"https://cir.nii.ac.jp/crid/1360013168761345792","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Magnetohydrodynamic Simulations of Self-Consistent Rotating Neutron Stars with Mixed Poloidal and Toroidal Magnetic Fields"}]},{"@id":"https://cir.nii.ac.jp/crid/1360013168798542336","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Observing Supernova Neutrino Light Curves with Super-Kamiokande. 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