{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:KGYFBGMTPI2TYG6AFMJ2O7CWKV","short_pith_number":"pith:KGYFBGMT","schema_version":"1.0","canonical_sha256":"51b05099937a353c1bc02b13a77c5655453860963048c6554fe926bdbce66c29","source":{"kind":"arxiv","id":"1609.06328","version":2},"attestation_state":"computed","paper":{"title":"Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Andrew G. Lyne, Ben W. Stappers, C.-Y. Ng, Iain A. Steele, Jules P. Halpern, Malcolm J. Coe, Tyrel J. Johnson, Wynn C. G. Ho","submitted_at":"2016-09-20T20:01:06Z","abstract_excerpt":"The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in a decades-long orbit with the Be star MT91 213, with the pulsar moving rapidly towards periastron. This binary shares many similar characteristics with the previously unique binary system PSR B1259-63/LS 2883. Here, we describe radio, X-ray, and optical monitoring of PSR J2032+4127/MT91 213. Our extended orbital phase coverage in radio, supplemented with Fermi gamma-ray data, allows us to update and refine the orbital period to 45-50 yr and time of periastron passage to 2017 November. We analyse archival and recent Chand"},"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":"1609.06328","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2016-09-20T20:01:06Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"2d0d855fa8a7868ad635a4939f7c7bbf8af89e38bf94aedf125897f21627c388","abstract_canon_sha256":"7b2686f6643b90ee02dc37874882e3087f2a62a4747d0be75e69a70d5ecba06f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:01:21.990469Z","signature_b64":"O2kNfKAcDP94IWG9lYOjBoDzxjP3hK09ZwULIoYk8mQBFCyqQGiYr8A7MDCbCNdfWl7vQiv+wzMJyglQH0JbAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"51b05099937a353c1bc02b13a77c5655453860963048c6554fe926bdbce66c29","last_reissued_at":"2026-05-18T01:01:21.989874Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:01:21.989874Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Andrew G. Lyne, Ben W. Stappers, C.-Y. Ng, Iain A. Steele, Jules P. Halpern, Malcolm J. Coe, Tyrel J. Johnson, Wynn C. G. Ho","submitted_at":"2016-09-20T20:01:06Z","abstract_excerpt":"The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in a decades-long orbit with the Be star MT91 213, with the pulsar moving rapidly towards periastron. This binary shares many similar characteristics with the previously unique binary system PSR B1259-63/LS 2883. Here, we describe radio, X-ray, and optical monitoring of PSR J2032+4127/MT91 213. Our extended orbital phase coverage in radio, supplemented with Fermi gamma-ray data, allows us to update and refine the orbital period to 45-50 yr and time of periastron passage to 2017 November. We analyse archival and recent Chand"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1609.06328","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":""},"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":"1609.06328","created_at":"2026-05-18T01:01:21.989957+00:00"},{"alias_kind":"arxiv_version","alias_value":"1609.06328v2","created_at":"2026-05-18T01:01:21.989957+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1609.06328","created_at":"2026-05-18T01:01:21.989957+00:00"},{"alias_kind":"pith_short_12","alias_value":"KGYFBGMTPI2T","created_at":"2026-05-18T12:30:25.849896+00:00"},{"alias_kind":"pith_short_16","alias_value":"KGYFBGMTPI2TYG6A","created_at":"2026-05-18T12:30:25.849896+00:00"},{"alias_kind":"pith_short_8","alias_value":"KGYFBGMT","created_at":"2026-05-18T12:30:25.849896+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.08175","citing_title":"How many VHE gamma-ray binaries with young pulsars can be observed?","ref_index":53,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV","json":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV.json","graph_json":"https://pith.science/api/pith-number/KGYFBGMTPI2TYG6AFMJ2O7CWKV/graph.json","events_json":"https://pith.science/api/pith-number/KGYFBGMTPI2TYG6AFMJ2O7CWKV/events.json","paper":"https://pith.science/paper/KGYFBGMT"},"agent_actions":{"view_html":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV","download_json":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV.json","view_paper":"https://pith.science/paper/KGYFBGMT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1609.06328&json=true","fetch_graph":"https://pith.science/api/pith-number/KGYFBGMTPI2TYG6AFMJ2O7CWKV/graph.json","fetch_events":"https://pith.science/api/pith-number/KGYFBGMTPI2TYG6AFMJ2O7CWKV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV/action/storage_attestation","attest_author":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV/action/author_attestation","sign_citation":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV/action/citation_signature","submit_replication":"https://pith.science/pith/KGYFBGMTPI2TYG6AFMJ2O7CWKV/action/replication_record"}},"created_at":"2026-05-18T01:01:21.989957+00:00","updated_at":"2026-05-18T01:01:21.989957+00:00"}