{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:AV6VARRRBZOV5PFFAUU3ZN3VGQ","short_pith_number":"pith:AV6VARRR","schema_version":"1.0","canonical_sha256":"057d5046310e5d5ebca50529bcb775340c3778718b518b8636ab9d9fa9274c0e","source":{"kind":"arxiv","id":"2605.17455","version":1},"attestation_state":"computed","paper":{"title":"Accretion geometry and spectral evolution in 1A 1118-61: a comparison of the 2009 and 2026 outbursts","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"The cyclotron line energy in 1A 1118-61 stays nearly constant across a factor of 25 luminosity change between its 2009 and 2026 outbursts.","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Aru Beri, Kinjal Roy, Phil Charles, Rahul Sharma","submitted_at":"2026-05-17T13:55:28Z","abstract_excerpt":"We present a detailed spectro-temporal study of the Be X-ray binary pulsar $1A$ $1118-61$ during its brightest recorded outburst in 2026, using \\textit{Swift} and \\textit{NuSTAR} observations, and compare its properties with the 2009 outburst. Coherent pulsations at $\\sim400$ s are detected throughout the outburst, with pulse profiles evolving strongly with energy and luminosity, indicating changes in emission geometry. A transient quasi-periodic oscillation (QPO) at $\\sim$0.11 Hz is observed during the rising phase. The luminosity dependence of the QPO frequency during the current and previou"},"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":true,"formal_links_present":true},"canonical_record":{"source":{"id":"2605.17455","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2026-05-17T13:55:28Z","cross_cats_sorted":[],"title_canon_sha256":"25e2fc2d4d9dd08290da63fcd0638f1d3cc6e329db974a5ffd0651dcf06f9aab","abstract_canon_sha256":"691608e6764ae44b72089a51a6bba6e6583c719668e6e2dd38ff9561e7e637bc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-20T00:04:39.904353Z","signature_b64":"zupZGeHwfV7m9EfwqB5mWNluWPxElQR7HJLWRxFuyIWanCpbcRaPr+hdiAp9wc91LF2biRsuPQ8nsL4HgASZBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"057d5046310e5d5ebca50529bcb775340c3778718b518b8636ab9d9fa9274c0e","last_reissued_at":"2026-05-20T00:04:39.903482Z","signature_status":"signed_v1","first_computed_at":"2026-05-20T00:04:39.903482Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Accretion geometry and spectral evolution in 1A 1118-61: a comparison of the 2009 and 2026 outbursts","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"The cyclotron line energy in 1A 1118-61 stays nearly constant across a factor of 25 luminosity change between its 2009 and 2026 outbursts.","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Aru Beri, Kinjal Roy, Phil Charles, Rahul Sharma","submitted_at":"2026-05-17T13:55:28Z","abstract_excerpt":"We present a detailed spectro-temporal study of the Be X-ray binary pulsar $1A$ $1118-61$ during its brightest recorded outburst in 2026, using \\textit{Swift} and \\textit{NuSTAR} observations, and compare its properties with the 2009 outburst. Coherent pulsations at $\\sim400$ s are detected throughout the outburst, with pulse profiles evolving strongly with energy and luminosity, indicating changes in emission geometry. A transient quasi-periodic oscillation (QPO) at $\\sim$0.11 Hz is observed during the rising phase. The luminosity dependence of the QPO frequency during the current and previou"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"A cyclotron line is detected in the two NuSTAR observations, with its energy remaining nearly constant despite a factor of ~25 change in luminosity; the 2026 outburst is systematically harder and brighter, suggesting significant difference in the accretion structure and emission regions between the two outbursts.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the spectral model of thermal Comptonization fully captures the emission physics without unaccounted components and that the 2009 and 2026 datasets are directly comparable despite possible differences in instrument calibration or outburst coverage.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"The 2026 outburst of 1A 1118-61 is brighter and spectrally harder than in 2009, with constant cyclotron line energy across large luminosity changes and QPO frequency suggesting magnetospheric instabilities.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"The cyclotron line energy in 1A 1118-61 stays nearly constant across a factor of 25 luminosity change between its 2009 and 2026 outbursts.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"3adb2e09a2f378a6678b44a85b80eee409a1aab2860691a19d217b7a5f09ab2f"},"source":{"id":"2605.17455","kind":"arxiv","version":1},"verdict":{"id":"1d69ae0b-1e57-4b4f-96a9-e486ae3878fa","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-19T22:38:21.302085Z","strongest_claim":"A cyclotron line is detected in the two NuSTAR observations, with its energy remaining nearly constant despite a factor of ~25 change in luminosity; the 2026 outburst is systematically harder and brighter, suggesting significant difference in the accretion structure and emission regions between the two outbursts.","one_line_summary":"The 2026 outburst of 1A 1118-61 is brighter and spectrally harder than in 2009, with constant cyclotron line energy across large luminosity changes and QPO frequency suggesting magnetospheric instabilities.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the spectral model of thermal Comptonization fully captures the emission physics without unaccounted components and that the 2009 and 2026 datasets are directly comparable despite possible differences in instrument calibration or outburst coverage.","pith_extraction_headline":"The cyclotron line energy in 1A 1118-61 stays nearly constant across a factor of 25 luminosity change between its 2009 and 2026 outbursts."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2605.17455/integrity.json","findings":[],"available":true,"detectors_run":[{"name":"doi_title_agreement","ran_at":"2026-05-19T23:01:19.582101Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"doi_compliance","ran_at":"2026-05-19T22:51:52.156768Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"claim_evidence","ran_at":"2026-05-19T21:41:57.710064Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"ai_meta_artifact","ran_at":"2026-05-19T21:33:23.663789Z","status":"skipped","version":"1.0.0","findings_count":0}],"snapshot_sha256":"abd6c178769de24a27d5b8505d5c81e74d4d61380c42bb413907fd874d5c1bd2"},"references":{"count":63,"sample":[{"doi":"10.1038/316239a0","year":1985,"title":"Alpar, M. A., & Shaham, J. 1985, Nature, 316, 239, doi: 10.1038/316239a0","work_id":"b1d90f27-1119-4085-8826-aa121f25099a","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1051/0004-6361/201322068","year":1996,"title":"2020, arXiv e-prints, 2010, arXiv:2010.09644 Astropy Collaboration, Robitaille, T","work_id":"aeafa8f2-1c15-4f27-9682-a76b6bf42e2b","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1093/mnras/stac2901","year":2022,"title":"2022, MNRAS, 517, 4138, doi: 10.1093/mnras/stac2901","work_id":"8589a743-5b8d-4d29-9c5c-0da2f01f27ce","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.3847/1538-3881/abd806","year":2021,"title":"Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3","work_id":"11e3916b-515c-4528-8feb-7528b967b896","ref_index":4,"cited_arxiv_id":"2012.05220","is_internal_anchor":true},{"doi":"10.1007/s11214-005-5096-3","year":2005,"title":"Barthelmy, S. D., Barbier, L. M., Cummings, J. R., et al. 2005, Space Sci. Rev., 120, 143, doi: 10.1007/s11214-005-5096-3","work_id":"2b527b24-8522-4a61-8a33-834cce163ab2","ref_index":5,"cited_arxiv_id":"astro-ph/0507410","is_internal_anchor":true}],"resolved_work":63,"snapshot_sha256":"0b997cc7c618a257fce15a851e649fb1c7b45ecb56503070ef151c0971b42bed","internal_anchors":5},"formal_canon":{"evidence_count":2,"snapshot_sha256":"804af887c07b65a5639817d0ba4a2a5c814b52e6b232d56461145e4fca4f99d3"},"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":"2605.17455","created_at":"2026-05-20T00:04:39.903627+00:00"},{"alias_kind":"arxiv_version","alias_value":"2605.17455v1","created_at":"2026-05-20T00:04:39.903627+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2605.17455","created_at":"2026-05-20T00:04:39.903627+00:00"},{"alias_kind":"pith_short_12","alias_value":"AV6VARRRBZOV","created_at":"2026-05-20T00:04:39.903627+00:00"},{"alias_kind":"pith_short_16","alias_value":"AV6VARRRBZOV5PFF","created_at":"2026-05-20T00:04:39.903627+00:00"},{"alias_kind":"pith_short_8","alias_value":"AV6VARRR","created_at":"2026-05-20T00:04:39.903627+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":2,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ","json":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ.json","graph_json":"https://pith.science/api/pith-number/AV6VARRRBZOV5PFFAUU3ZN3VGQ/graph.json","events_json":"https://pith.science/api/pith-number/AV6VARRRBZOV5PFFAUU3ZN3VGQ/events.json","paper":"https://pith.science/paper/AV6VARRR"},"agent_actions":{"view_html":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ","download_json":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ.json","view_paper":"https://pith.science/paper/AV6VARRR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2605.17455&json=true","fetch_graph":"https://pith.science/api/pith-number/AV6VARRRBZOV5PFFAUU3ZN3VGQ/graph.json","fetch_events":"https://pith.science/api/pith-number/AV6VARRRBZOV5PFFAUU3ZN3VGQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ/action/storage_attestation","attest_author":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ/action/author_attestation","sign_citation":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ/action/citation_signature","submit_replication":"https://pith.science/pith/AV6VARRRBZOV5PFFAUU3ZN3VGQ/action/replication_record"}},"created_at":"2026-05-20T00:04:39.903627+00:00","updated_at":"2026-05-20T00:04:39.903627+00:00"}