{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:BJMALE3UXVP3M6TBT6QCCXY6QS","short_pith_number":"pith:BJMALE3U","schema_version":"1.0","canonical_sha256":"0a58059374bd5fb67a619fa0215f1e848ba48e4855bdec6197b6352cc6cf4fca","source":{"kind":"arxiv","id":"2502.09147","version":2},"attestation_state":"computed","paper":{"title":"PSR J1231-1411 revisited: Pulse Profile Analysis of X-ray Observation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Ang Li, Fang-Jun Lu, Han-Long Peng, Hua Feng, Juan Zhang, Liang Zhang, Lian Tao, Li-Ming Song, Liqiang Qi, Mingyu Ge, Shijie Zheng, Shuang-Nan Zhang, Shu Zhang, Wentao Ye, Yupeng Xu, Zheng-Wei Li, Zhen Zhang","submitted_at":"2025-02-13T10:22:56Z","abstract_excerpt":"One of the primary goals of Neutron Star Interior Composition Explorer (NICER)-like X-ray missions is to impose stringent constraints on the neutron star equation of state by precisely measuring their masses and radii. NICER has recently expanded the dataset of inferred mass-radius relations for neutron stars, including four rotation-powered millisecond pulsars PSR J0030+0451, PSR J0740+6620, PSR J0437-4715, and PSR J1231-1411. In this work, the mass-radius relation and X-ray emitting region properties of PSR J1231-1411 are inferred with an independent pulse profile modeling based on the spher"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2502.09147","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2025-02-13T10:22:56Z","cross_cats_sorted":["nucl-th"],"title_canon_sha256":"57fbe108bf2c9a5f15063fd4f4cfeae5964ba6c75290a8276b033331750250aa","abstract_canon_sha256":"3f1972099a0a9de107ba90e91f7f2dfed91388f66ee3cd7dcd6b0133ae280d03"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:15:26.509099Z","signature_b64":"0GIIyuMbSPegT3tlOws6iT+/pbh9T6OqbB9TK95zfMnIhZfMZCaKN9bP8qT80FMILWCtxjPBEyQbLsVzxzXtAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0a58059374bd5fb67a619fa0215f1e848ba48e4855bdec6197b6352cc6cf4fca","last_reissued_at":"2026-07-05T10:15:26.508530Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:15:26.508530Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"PSR J1231-1411 revisited: Pulse Profile Analysis of X-ray Observation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Ang Li, Fang-Jun Lu, Han-Long Peng, Hua Feng, Juan Zhang, Liang Zhang, Lian Tao, Li-Ming Song, Liqiang Qi, Mingyu Ge, Shijie Zheng, Shuang-Nan Zhang, Shu Zhang, Wentao Ye, Yupeng Xu, Zheng-Wei Li, Zhen Zhang","submitted_at":"2025-02-13T10:22:56Z","abstract_excerpt":"One of the primary goals of Neutron Star Interior Composition Explorer (NICER)-like X-ray missions is to impose stringent constraints on the neutron star equation of state by precisely measuring their masses and radii. NICER has recently expanded the dataset of inferred mass-radius relations for neutron stars, including four rotation-powered millisecond pulsars PSR J0030+0451, PSR J0740+6620, PSR J0437-4715, and PSR J1231-1411. In this work, the mass-radius relation and X-ray emitting region properties of PSR J1231-1411 are inferred with an independent pulse profile modeling based on the spher"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2502.09147","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2502.09147/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"2502.09147","created_at":"2026-07-05T10:15:26.508589+00:00"},{"alias_kind":"arxiv_version","alias_value":"2502.09147v2","created_at":"2026-07-05T10:15:26.508589+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2502.09147","created_at":"2026-07-05T10:15:26.508589+00:00"},{"alias_kind":"pith_short_12","alias_value":"BJMALE3UXVP3","created_at":"2026-07-05T10:15:26.508589+00:00"},{"alias_kind":"pith_short_16","alias_value":"BJMALE3UXVP3M6TB","created_at":"2026-07-05T10:15:26.508589+00:00"},{"alias_kind":"pith_short_8","alias_value":"BJMALE3U","created_at":"2026-07-05T10:15:26.508589+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.21435","citing_title":"Is the coexistence of strange quark stars and hadronic stars favored by astrophysical data? A Bayesian analysis","ref_index":126,"is_internal_anchor":false},{"citing_arxiv_id":"2605.14447","citing_title":"Bayesian analysis of density profile of light dark matter elucidating the properties of dark matter admixed neutron stars in the presence of hyperons","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2605.05005","citing_title":"Characterizing the quark-hadron mixed phase in compact star cores : sensitivity to nuclear saturation and quark-model parameters at finite-temperature","ref_index":50,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS","json":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS.json","graph_json":"https://pith.science/api/pith-number/BJMALE3UXVP3M6TBT6QCCXY6QS/graph.json","events_json":"https://pith.science/api/pith-number/BJMALE3UXVP3M6TBT6QCCXY6QS/events.json","paper":"https://pith.science/paper/BJMALE3U"},"agent_actions":{"view_html":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS","download_json":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS.json","view_paper":"https://pith.science/paper/BJMALE3U","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2502.09147&json=true","fetch_graph":"https://pith.science/api/pith-number/BJMALE3UXVP3M6TBT6QCCXY6QS/graph.json","fetch_events":"https://pith.science/api/pith-number/BJMALE3UXVP3M6TBT6QCCXY6QS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS/action/storage_attestation","attest_author":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS/action/author_attestation","sign_citation":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS/action/citation_signature","submit_replication":"https://pith.science/pith/BJMALE3UXVP3M6TBT6QCCXY6QS/action/replication_record"}},"created_at":"2026-07-05T10:15:26.508589+00:00","updated_at":"2026-07-05T10:15:26.508589+00:00"}