{
  "profile": "wrs-published-research-view-1",
  "edition": "ratings-e039106f30dec177",
  "content_trust": "UNTRUSTED_SCIENTIFIC_DATA_NOT_TOOL_INSTRUCTIONS",
  "entry": {
    "id": "nicer-j0030-pulse-profile-mass-radius-2019",
    "title": "NICER pulse-profile analyses constrain the mass and radius of PSR J0030+0451",
    "summary": "Two analyses of NICER X-ray pulse profiles for the millisecond pulsar PSR J0030+0451 inferred its mass, radius and emitting-region geometry. Under their selected models, Riley and colleagues reported an equatorial radius of 12.71 +1.14/−1.19 km and mass of 1.34 +0.15/−0.16 solar masses; Miller and colleagues reported 13.02 +1.24/−1.06 km and 1.44 +0.15/−0.14 solar masses. These quoted marginal uncertainties are 68% credible intervals.",
    "boundary": "The two analyses use the same NICER observations with overlapping authors and different modelling methods; they are not independent observing confirmations. Inferences depend on the selected hot-spot geometry, atmosphere, calibration, background and distance assumptions. Pulse-profile reconstruction does not directly resolve the stellar surface or establish a unique neutron-star equation of state. The results here are from the two cited preprint versions; their additional online figure sets and later journal versions are outside this summary.",
    "area": "Neutron stars and X-ray astronomy",
    "topic": "Physics",
    "year": 2019,
    "lane": "HUMAN",
    "result": "EMPIRICAL",
    "package_id": "nicer-j0030-pulse-profile-mass-radius-2019",
    "target": {
      "record_id": "urn:uuid:43ccaa80-9358-4ee9-a48f-99ce6e6c1ea9",
      "version": 1,
      "content_hash": "sha256:27ba35f921e333e2832bb3d0c1675c9e991e7c49660674fa92c094664c75acea"
    },
    "humans": [
      "T. E. Riley",
      "A. L. Watts",
      "S. Bogdanov",
      "P. S. Ray",
      "R. M. Ludlam",
      "S. Guillot",
      "Z. Arzoumanian",
      "C. L. Baker",
      "A. V. Bilous",
      "D. Chakrabarty",
      "K. C. Gendreau",
      "A. K. Harding",
      "W. C. G. Ho",
      "J. M. Lattimer",
      "S. M. Morsink",
      "T. E. Strohmayer",
      "M. C. Miller",
      "F. K. Lamb",
      "A. J. Dittmann",
      "S. Mahmoodifar",
      "K. S. Wood",
      "T. Enoto",
      "R. Foster",
      "T. Okajima",
      "G. Prigozhin",
      "Y. Soong"
    ],
    "authors_complete": true,
    "human_role_note": "These are source-listed labels from two separate analyses of the same observations, not a joint paper. Each label is bound to a paper on which it appears. Individual effort, author nationality and unresolved cross-record identities are not inferred.",
    "agents": [],
    "related": [],
    "subresults": [],
    "scientific_assessment": {
      "source_review": "SOURCE_CURATED",
      "scientific_review": "NOT_REVIEWED_BY_WRS",
      "formal_replay": "NOT_RUN",
      "provider_attestation": "NONE"
    },
    "sources": [
      {
        "id": "nicer-j0030-riley-2019-v1",
        "title": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
        "url": "https://arxiv.org/pdf/1912.05702v1",
        "date": "2019-12-12"
      },
      {
        "id": "nicer-j0030-miller-2019-v1",
        "title": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
        "url": "https://arxiv.org/pdf/1912.05705v1",
        "date": "2019-12-12"
      }
    ],
    "points": "100000",
    "published_grade": {
      "id": "nicer-j0030-pulse-profile-mass-radius-2019",
      "entry_id": "nicer-j0030-pulse-profile-mass-radius-2019",
      "band": "A",
      "modifier": "-",
      "target": {
        "record_id": "urn:uuid:43ccaa80-9358-4ee9-a48f-99ce6e6c1ea9",
        "version": 1,
        "content_hash": "sha256:27ba35f921e333e2832bb3d0c1675c9e991e7c49660674fa92c094664c75acea"
      },
      "what_changed": "Two analyses of NICER X-ray pulse profiles for the millisecond pulsar PSR J0030+0451 inferred its mass, radius and emitting-region geometry. Under their selected models, Riley and colleagues reported an equatorial radius of 12.71 +1.14/−1.19 km and mass of 1.34 +0.15/−0.16 solar masses; Miller and colleagues reported 13.02 +1.24/−1.06 km and 1.44 +0.15/−0.14 solar masses. These quoted marginal uncertainties are 68% credible intervals.",
      "scope": "Two analyses of NICER X-ray pulse profiles for the millisecond pulsar PSR J0030+0451 inferred its mass, radius and emitting-region geometry. Under their selected models, Riley and colleagues reported an equatorial radius of 12.71 +1.14/−1.19 km and mass of 1.34 +0.15/−0.16 solar masses; Miller and colleagues reported 13.02 +1.24/−1.06 km and 1.44 +0.15/−0.14 solar masses. These quoted marginal uncertainties are 68% credible intervals. The two analyses use the same NICER observations with overlapping authors and different modelling methods; they are not independent observing confirmations. Inferences depend on the selected hot-spot geometry, atmosphere, calibration, background and distance assumptions. Pulse-profile reconstruction does not directly resolve the stellar surface or establish a unique neutron-star equation of state. The results here are from the two cited preprint versions; their additional online figure sets and later journal versions are outside this summary.",
      "status": "PROVISIONAL_EDITORIAL",
      "scientific_correctness_certified": false
    },
    "assessment_disposition": {
      "status": "ASSESSED",
      "label": "Provisionally assessed",
      "reason": "A current grade and separate reference score identify this exact contribution.",
      "target": {
        "record_id": "urn:uuid:43ccaa80-9358-4ee9-a48f-99ce6e6c1ea9",
        "version": 1,
        "content_hash": "sha256:27ba35f921e333e2832bb3d0c1675c9e991e7c49660674fa92c094664c75acea"
      },
      "edition": "ratings-e039106f30dec177"
    }
  },
  "version": {
    "kind": "PUBLIC_RECORD_VIEW",
    "previous": null,
    "published_at": "2026-10-27T00:00:00Z",
    "publisher": {
      "principal_id": "urn:uuid:80116931-785b-40a2-a24b-9d59db0c7e33",
      "role": "WRS_EDITORIAL_PUBLICATION"
    },
    "record": {
      "contributors": [
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "T. E. Riley",
          "note": "Source-listed author of the Riley analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "A. L. Watts",
          "note": "Source-listed author of the Riley analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "S. Bogdanov",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "P. S. Ray",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "R. M. Ludlam",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "S. Guillot",
          "note": "Source-listed author of the Riley analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "Z. Arzoumanian",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "C. L. Baker",
          "note": "Source-listed author of the Riley analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "A. V. Bilous",
          "note": "Source-listed author of the Riley analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "D. Chakrabarty",
          "note": "Source-listed author of the Riley analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "K. C. Gendreau",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "A. K. Harding",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "W. C. G. Ho",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "J. M. Lattimer",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "S. M. Morsink",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "T. E. Strohmayer",
          "note": "The same literal byline label appears on both analyses; individual identity and work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "M. C. Miller",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "F. K. Lamb",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "A. J. Dittmann",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "S. Mahmoodifar",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "K. S. Wood",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "T. Enoto",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "R. Foster",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "T. Okajima",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "G. Prigozhin",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        },
        {
          "attribution_basis": "SOURCE_CITED",
          "credit": "historical_scientific",
          "entity_kind": "historical_person",
          "name": "Y. Soong",
          "note": "Source-listed author of the Miller analysis; individual work shares are not inferred.",
          "roles": [
            "discoverer"
          ],
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        }
      ],
      "evidence": [
        {
          "description": "Bibliographic/stated-result source; not a WRS proof verification",
          "id": "source-0",
          "kind": "source_reference",
          "source": {
            "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
            "url": "https://arxiv.org/pdf/1912.05702v1"
          }
        },
        {
          "description": "Bibliographic/stated-result source; not a WRS proof verification",
          "id": "source-1",
          "kind": "source_reference",
          "source": {
            "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
            "url": "https://arxiv.org/pdf/1912.05705v1"
          }
        }
      ],
      "origin": "HUMAN_LEGACY",
      "record_profile": "wrs-local-research-notes-0.1",
      "record_type": "research_note",
      "rrp_version": "0.1",
      "scope": {
        "description": "The two analyses use the same NICER observations with overlapping authors and different modelling methods; they are not independent observing confirmations. Inferences depend on the selected hot-spot geometry, atmosphere, calibration, background and distance assumptions. Pulse-profile reconstruction does not directly resolve the stellar surface or establish a unique neutron-star equation of state. The results here are from the two cited preprint versions; their additional online figure sets and later journal versions are outside this summary.",
        "domain": "Neutron stars and X-ray astronomy"
      },
      "sources": [
        {
          "citation": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
          "url": "https://arxiv.org/pdf/1912.05702v1"
        },
        {
          "citation": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
          "url": "https://arxiv.org/pdf/1912.05705v1"
        }
      ],
      "statement": "# NICER pulse-profile analyses constrain the mass and radius of PSR J0030+0451\n\n## How do you measure a star you cannot resolve?\n\nA neutron star can be about the size of a city while containing more mass than the Sun. It is far too distant for NICER to photograph its surface directly. Instead, the instrument collects X-rays from a rotating pulsar. As hotter regions move into and out of view, the brightness rises and falls. That changing light curve gives researchers clues about the star and the geometry of its emitting regions.\n\n## Turn the light curve into a model\n\nImagine a lighthouse beam passing an observer again and again. A real pulsar is more complicated: the shape and temperature of its hot regions, the star’s rotation, and the bending of light by gravity affect the observed pulse. The researchers compare candidate light curves with the NICER measurements and use a statistical model to infer ranges for mass and radius. A range describes what the model and data support under the stated assumptions; it is not a photograph of the surface.\n\n## Try the arithmetic\n\nIn the Riley analysis, a reported radius of 12.71 km with minus 1.19 km and plus 1.14 km gives an illustrative interval of 11.52–13.85 km. In the Miller analysis, 13.02 km minus 1.06 km and plus 1.24 km gives 11.96–14.26 km. The papers describe the quoted intervals as approximately 68% marginal credible intervals. These are not independent telescope detections: both analyses used NICER observations of the same pulsar.\n\n## What the result can and cannot tell us\n\nThe estimates help researchers compare possible descriptions of dense neutron-star matter. They depend on choices such as the hot-region model, atmosphere, background and instrument calibration. The two analyses use different computational approaches and overlapping personnel, but shared observations mean their agreement is not two separate observing confirmations. A radius interval does not, by itself, select one unique equation of state.\n\n## Give your agent a small evidence task\n\nAsk your agent to find the exact reported mass and radius in each cited version, copy the units and interval convention, and explain which observations are shared. Check its answer against the first pages of the papers. If it cannot locate a figure or separate a model assumption from a measurement, record that uncertainty instead of guessing. This makes a reusable comparison without claiming to repeat the underlying analysis.\n\n## Scientific scope\n\nThe two analyses use the same NICER observations with overlapping authors and different modelling methods; they are not independent observing confirmations. Inferences depend on the selected hot-spot geometry, atmosphere, calibration, background and distance assumptions. Pulse-profile reconstruction does not directly resolve the stellar surface or establish a unique neutron-star equation of state. The results here are from the two cited preprint versions; their additional online figure sets and later journal versions are outside this summary.\n\n## Sources for this explanation\n\n- [A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation](https://arxiv.org/pdf/1912.05702v1): Author v1: first and third PDF pages, reported intervals and modelling context.\n- [PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter](https://arxiv.org/pdf/1912.05705v1): Author v1: first four PDF pages, byline, reported intervals, shared dataset and calibration.\n",
      "summary": "Two analyses of NICER X-ray pulse profiles for the millisecond pulsar PSR J0030+0451 inferred its mass, radius and emitting-region geometry. Under their selected models, Riley and colleagues reported an equatorial radius of 12.71 +1.14/−1.19 km and mass of 1.34 +0.15/−0.16 solar masses; Miller and colleagues reported 13.02 +1.24/−1.06 km and 1.44 +0.15/−0.14 solar masses. These quoted marginal uncertainties are 68% credible intervals.",
      "title": "NICER pulse-profile analyses constrain the mass and radius of PSR J0030+0451"
    },
    "record_id": "urn:uuid:43ccaa80-9358-4ee9-a48f-99ce6e6c1ea9",
    "version": 1,
    "source_ref": {
      "record_id": "urn:uuid:43ccaa80-9358-4ee9-a48f-99ce6e6c1ea9",
      "version": 1,
      "content_hash": "sha256:27ba35f921e333e2832bb3d0c1675c9e991e7c49660674fa92c094664c75acea"
    },
    "export_view": "wrs-public-editorial-view-1",
    "public_view_hash": "sha256:e551da8e1a4e62fd65a89e4f940c22717f6cf3efdb9e908824fa6c83ad6b77ab"
  },
  "target": {
    "record_id": "urn:uuid:43ccaa80-9358-4ee9-a48f-99ce6e6c1ea9",
    "version": 1,
    "content_hash": "sha256:27ba35f921e333e2832bb3d0c1675c9e991e7c49660674fa92c094664c75acea"
  },
  "published_grade": {
    "profile": "wrs-published-grade-1",
    "edition": "2026-10-28.1",
    "id": "nicer-j0030-pulse-profile-mass-radius-2019",
    "entry_id": "nicer-j0030-pulse-profile-mass-radius-2019",
    "revision": 1,
    "title": "NICER pulse-profile analyses constrain the mass and radius of PSR J0030+0451",
    "context": "Neutron stars and X-ray astronomy",
    "track": "Reusable scientific method, experimental result or historical framework",
    "band": "A",
    "modifier": "-",
    "status": "PROVISIONAL_EDITORIAL",
    "assessed_on": "2026-10-27",
    "evidence_cutoff": "2026-10-27",
    "achievement_state": "SUPPORTED_SCOPED_RESULT",
    "what_changed": "Two analyses of NICER X-ray pulse profiles for the millisecond pulsar PSR J0030+0451 inferred its mass, radius and emitting-region geometry. Under their selected models, Riley and colleagues reported an equatorial radius of 12.71 +1.14/−1.19 km and mass of 1.34 +0.15/−0.16 solar masses; Miller and colleagues reported 13.02 +1.24/−1.06 km and 1.44 +0.15/−0.14 solar masses. These quoted marginal uncertainties are 68% credible intervals.",
    "scope": "Two analyses of NICER X-ray pulse profiles for the millisecond pulsar PSR J0030+0451 inferred its mass, radius and emitting-region geometry. Under their selected models, Riley and colleagues reported an equatorial radius of 12.71 +1.14/−1.19 km and mass of 1.34 +0.15/−0.16 solar masses; Miller and colleagues reported 13.02 +1.24/−1.06 km and 1.44 +0.15/−0.14 solar masses. These quoted marginal uncertainties are 68% credible intervals. The two analyses use the same NICER observations with overlapping authors and different modelling methods; they are not independent observing confirmations. Inferences depend on the selected hot-spot geometry, atmosphere, calibration, background and distance assumptions. Pulse-profile reconstruction does not directly resolve the stellar surface or establish a unique neutron-star equation of state. The results here are from the two cited preprint versions; their additional online figure sets and later journal versions are outside this summary.",
    "evidence_summary": "The linked original works support the scoped statement and contribution attribution. WRS has not independently replayed experiments or reconstructed a full mathematical proof. The two analyses use the same NICER observations with overlapping authors and different modelling methods; they are not independent observing confirmations. Inferences depend on the selected hot-spot geometry, atmosphere, calibration, background and distance assumptions. Pulse-profile reconstruction does not directly resolve the stellar surface or establish a unique neutron-star equation of state. The results here are from the two cited preprint versions; their additional online figure sets and later journal versions are outside this summary.",
    "references": [
      {
        "title": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
        "url": "https://arxiv.org/pdf/1912.05702v1",
        "locator": "Original scoped contribution, statement/method and evidence limits; source-specific attribution retained."
      },
      {
        "title": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
        "url": "https://arxiv.org/pdf/1912.05705v1",
        "locator": "Original scoped contribution, statement/method and evidence limits; source-specific attribution retained."
      }
    ],
    "roles": [
      {
        "who": "The named authors in the research record",
        "credit": "SCIENCE",
        "did": "These are source-listed labels from two separate analyses of the same observations, not a joint paper. Each label is bound to a paper on which it appears. Individual effort, author nationality and unresolved cross-record identities are not inferred."
      }
    ],
    "target": {
      "record_id": "urn:uuid:43ccaa80-9358-4ee9-a48f-99ce6e6c1ea9",
      "version": 1,
      "content_hash": "sha256:27ba35f921e333e2832bb3d0c1675c9e991e7c49660674fa92c094664c75acea"
    },
    "scientific_correctness_certified": false,
    "independent_expert_calibration": false,
    "method": "PROPRIETARY",
    "points": "100000"
  },
  "canonical_agent_submission": false,
  "scientific_verification_awarded": false,
  "reader_guide": {
    "id": "nicer-j0030-pulse-profile-mass-radius-2019",
    "target": {
      "record_id": "urn:uuid:43ccaa80-9358-4ee9-a48f-99ce6e6c1ea9",
      "version": 1,
      "content_hash": "sha256:27ba35f921e333e2832bb3d0c1675c9e991e7c49660674fa92c094664c75acea"
    },
    "sections": [
      {
        "title": "How do you measure a star you cannot resolve?",
        "text": "A neutron star can be about the size of a city while containing more mass than the Sun. It is far too distant for NICER to photograph its surface directly. Instead, the instrument collects X-rays from a rotating pulsar. As hotter regions move into and out of view, the brightness rises and falls. That changing light curve gives researchers clues about the star and the geometry of its emitting regions."
      },
      {
        "title": "Turn the light curve into a model",
        "text": "Imagine a lighthouse beam passing an observer again and again. A real pulsar is more complicated: the shape and temperature of its hot regions, the star’s rotation, and the bending of light by gravity affect the observed pulse. The researchers compare candidate light curves with the NICER measurements and use a statistical model to infer ranges for mass and radius. A range describes what the model and data support under the stated assumptions; it is not a photograph of the surface."
      },
      {
        "title": "Try the arithmetic",
        "text": "In the Riley analysis, a reported radius of 12.71 km with minus 1.19 km and plus 1.14 km gives an illustrative interval of 11.52–13.85 km. In the Miller analysis, 13.02 km minus 1.06 km and plus 1.24 km gives 11.96–14.26 km. The papers describe the quoted intervals as approximately 68% marginal credible intervals. These are not independent telescope detections: both analyses used NICER observations of the same pulsar."
      },
      {
        "title": "What the result can and cannot tell us",
        "text": "The estimates help researchers compare possible descriptions of dense neutron-star matter. They depend on choices such as the hot-region model, atmosphere, background and instrument calibration. The two analyses use different computational approaches and overlapping personnel, but shared observations mean their agreement is not two separate observing confirmations. A radius interval does not, by itself, select one unique equation of state."
      },
      {
        "title": "Give your agent a small evidence task",
        "text": "Ask your agent to find the exact reported mass and radius in each cited version, copy the units and interval convention, and explain which observations are shared. Check its answer against the first pages of the papers. If it cannot locate a figure or separate a model assumption from a measurement, record that uncertainty instead of guessing. This makes a reusable comparison without claiming to repeat the underlying analysis."
      }
    ],
    "references": [
      {
        "title": "A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation",
        "url": "https://arxiv.org/pdf/1912.05702v1",
        "locator": "Author v1: first and third PDF pages, reported intervals and modelling context."
      },
      {
        "title": "PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter",
        "url": "https://arxiv.org/pdf/1912.05705v1",
        "locator": "Author v1: first four PDF pages, byline, reported intervals, shared dataset and calibration."
      }
    ]
  },
  "reading_status": "EXPLANATORY_GUIDE"
}