{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:5PHQQST26JRMPWFDNWK6VXEF6N","short_pith_number":"pith:5PHQQST2","schema_version":"1.0","canonical_sha256":"ebcf084a7af262c7d8a36d95eadc85f34b5fe4e3e514e6c74b8a7874a4c81258","source":{"kind":"arxiv","id":"2405.13889","version":2},"attestation_state":"computed","paper":{"title":"The Intrabinary Shock and Companion Star of Redback Pulsar J2215+5135","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Andrew G. Sullivan, Roger W. Romani","submitted_at":"2024-05-22T18:00:47Z","abstract_excerpt":"PSR J2215+5135 (J2215) is a `redback' spider pulsar, where the intrabinary shock (IBS) wraps around the pulsar rather than the stellar-mass companion. Spider orbital light curves are modulated, dominated by their binary companion thermal emission in the optical bands and by IBS synchrotron emission in the X-rays. We report on new XMM-Newton X-ray and U-band observations of J2215. We produce orbital light curves and use them to model the system properties. Our best-fit optical light model gives a neutron star mass $M_{NS}=1.98\\pm0.08$ M$_\\odot$, lower than previously reported. However, uncertai"},"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":"2405.13889","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-05-22T18:00:47Z","cross_cats_sorted":["astro-ph.SR","nucl-th"],"title_canon_sha256":"278cf5db62a43e4a2594424dfdacc46e534a3c3e2e511f8f27f3b030358d3715","abstract_canon_sha256":"6bb491f5b72ce16c4d63600479e6a1c0de9c4c3b20cd7fe09d317750c708f87c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:02:40.764330Z","signature_b64":"9TZv9enxMHYerlRjv0tpOJGd/dshmJ657rbm5W0vehamgOvwu+8ibhJs38h5pitkh/Ip9i0Y/KVc/WG1ohSCDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ebcf084a7af262c7d8a36d95eadc85f34b5fe4e3e514e6c74b8a7874a4c81258","last_reissued_at":"2026-07-05T09:02:40.763826Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:02:40.763826Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Intrabinary Shock and Companion Star of Redback Pulsar J2215+5135","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Andrew G. Sullivan, Roger W. Romani","submitted_at":"2024-05-22T18:00:47Z","abstract_excerpt":"PSR J2215+5135 (J2215) is a `redback' spider pulsar, where the intrabinary shock (IBS) wraps around the pulsar rather than the stellar-mass companion. Spider orbital light curves are modulated, dominated by their binary companion thermal emission in the optical bands and by IBS synchrotron emission in the X-rays. We report on new XMM-Newton X-ray and U-band observations of J2215. We produce orbital light curves and use them to model the system properties. Our best-fit optical light model gives a neutron star mass $M_{NS}=1.98\\pm0.08$ M$_\\odot$, lower than previously reported. However, uncertai"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2405.13889","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/2405.13889/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":"2405.13889","created_at":"2026-07-05T09:02:40.763894+00:00"},{"alias_kind":"arxiv_version","alias_value":"2405.13889v2","created_at":"2026-07-05T09:02:40.763894+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2405.13889","created_at":"2026-07-05T09:02:40.763894+00:00"},{"alias_kind":"pith_short_12","alias_value":"5PHQQST26JRM","created_at":"2026-07-05T09:02:40.763894+00:00"},{"alias_kind":"pith_short_16","alias_value":"5PHQQST26JRMPWFD","created_at":"2026-07-05T09:02:40.763894+00:00"},{"alias_kind":"pith_short_8","alias_value":"5PHQQST2","created_at":"2026-07-05T09:02:40.763894+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.20111","citing_title":"Hybrid stars with hyperons: structure based on QCD sum rule coupling constants","ref_index":63,"is_internal_anchor":false},{"citing_arxiv_id":"2606.02966","citing_title":"Sensitivity of the Neutron Star Equation of State Inferences to Mass and Radius Measurements","ref_index":47,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N","json":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N.json","graph_json":"https://pith.science/api/pith-number/5PHQQST26JRMPWFDNWK6VXEF6N/graph.json","events_json":"https://pith.science/api/pith-number/5PHQQST26JRMPWFDNWK6VXEF6N/events.json","paper":"https://pith.science/paper/5PHQQST2"},"agent_actions":{"view_html":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N","download_json":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N.json","view_paper":"https://pith.science/paper/5PHQQST2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2405.13889&json=true","fetch_graph":"https://pith.science/api/pith-number/5PHQQST26JRMPWFDNWK6VXEF6N/graph.json","fetch_events":"https://pith.science/api/pith-number/5PHQQST26JRMPWFDNWK6VXEF6N/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N/action/storage_attestation","attest_author":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N/action/author_attestation","sign_citation":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N/action/citation_signature","submit_replication":"https://pith.science/pith/5PHQQST26JRMPWFDNWK6VXEF6N/action/replication_record"}},"created_at":"2026-07-05T09:02:40.763894+00:00","updated_at":"2026-07-05T09:02:40.763894+00:00"}