{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:IWEL75IGLGIT2AAT5JKYT444BU","short_pith_number":"pith:IWEL75IG","schema_version":"1.0","canonical_sha256":"4588bff50659913d0013ea5589f39c0d3265ec314502f8ab3c86202cd9649eea","source":{"kind":"arxiv","id":"2605.13232","version":1},"attestation_state":"computed","paper":{"title":"Revisiting the 2021 Outburst of the BHC MAXI J1803-298 Using NICER, NuSTAR, and Insight-HXMT Data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"LFQPOs in MAXI J1803-298 arise from the dynamically evolving inner accretion flow.","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Kaushik Chatterjee, Sujoy K. Nath","submitted_at":"2026-05-13T09:20:37Z","abstract_excerpt":"We present a broadband spectral and timing study of the black hole candidate MAXI J1803-298 during its 2021 outburst using simultaneous observations from NICER, NuSTAR, and Insight-HXMT. The combined multi-instrument coverage allows us to investigate the evolution of low-frequency quasi-periodic oscillations (LFQPOs) together with the spectral properties of the source over a wide energy range. During the early observation epoch, the source exhibits a hard or hard-intermediate spectral state dominated by Comptonized emission with reflection features. Spectral modeling within the framework of th"},"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":"2605.13232","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2026-05-13T09:20:37Z","cross_cats_sorted":[],"title_canon_sha256":"92687ff9100d2e6ba3b3f7899c75d1f07edc9e25727cb7b1fc11ef86e0cf9a56","abstract_canon_sha256":"c20155eb9038910b77462d1193e1816c717da22b2225327a2ed4075cc0dba557"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:44:49.578776Z","signature_b64":"a+tPVI0hFARX7fFVNZsM09AwCcvKpM4G7qz6KkE0ib98iJSu0KbjJGDmmh73U7udkqYEbfXaW80FEuHCPBFFAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4588bff50659913d0013ea5589f39c0d3265ec314502f8ab3c86202cd9649eea","last_reissued_at":"2026-05-18T02:44:49.578344Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:44:49.578344Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Revisiting the 2021 Outburst of the BHC MAXI J1803-298 Using NICER, NuSTAR, and Insight-HXMT Data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"LFQPOs in MAXI J1803-298 arise from the dynamically evolving inner accretion flow.","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Kaushik Chatterjee, Sujoy K. Nath","submitted_at":"2026-05-13T09:20:37Z","abstract_excerpt":"We present a broadband spectral and timing study of the black hole candidate MAXI J1803-298 during its 2021 outburst using simultaneous observations from NICER, NuSTAR, and Insight-HXMT. The combined multi-instrument coverage allows us to investigate the evolution of low-frequency quasi-periodic oscillations (LFQPOs) together with the spectral properties of the source over a wide energy range. During the early observation epoch, the source exhibits a hard or hard-intermediate spectral state dominated by Comptonized emission with reflection features. Spectral modeling within the framework of th"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"The combined spectral and timing results support a scenario in which LFQPOs in MAXI J1803-298 arise from the dynamically evolving inner accretion flow.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the two-component advective flow (TCAF) model accurately captures the accretion geometry and yields an unbiased independent black hole mass estimate from the fitted shock location and flow parameters.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Multi-instrument observations of MAXI J1803-298 link LFQPOs to the evolving inner Comptonizing accretion flow in the hard state, with TCAF modeling yielding a black hole mass estimate.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"LFQPOs in MAXI J1803-298 arise from the dynamically evolving inner accretion flow.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"f1c158180899b745321ea4ca8827b391c189672c0c9ce43f7a8237b1729c6464"},"source":{"id":"2605.13232","kind":"arxiv","version":1},"verdict":{"id":"f101e5ef-c532-4374-8794-98db5c24ea98","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-14T18:46:21.664093Z","strongest_claim":"The combined spectral and timing results support a scenario in which LFQPOs in MAXI J1803-298 arise from the dynamically evolving inner accretion flow.","one_line_summary":"Multi-instrument observations of MAXI J1803-298 link LFQPOs to the evolving inner Comptonizing accretion flow in the hard state, with TCAF modeling yielding a black hole mass estimate.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the two-component advective flow (TCAF) model accurately captures the accretion geometry and yields an unbiased independent black hole mass estimate from the fitted shock location and flow parameters.","pith_extraction_headline":"LFQPOs in MAXI J1803-298 arise from the dynamically evolving inner accretion flow."},"references":{"count":3,"sample":[{"doi":"","year":2015,"title":"A., Cook, R., et al","work_id":"679dc9a7-1f83-4441-bfe6-3c95650afecc","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1088/0004-637x/800/2/109","year":2022,"title":"A., Cook, R., et al","work_id":"ac5aa908-305c-442d-b5b3-b30580ce64ae","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2018,"title":"1989, in Timing Neutron Stars: proceedings of the NA TO Advanced Study Institute on Timing Neutron Stars held April 4-15, 27 Xu, Y ., & Harrison, F","work_id":"63efc0ca-06fc-4837-aca5-38a3faa6d76b","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":3,"snapshot_sha256":"e8d8b66f8285ff10c5a0e1d8421ad34aa0bb1e5b146b052115cdf254fcfce9a0","internal_anchors":0},"formal_canon":{"evidence_count":2,"snapshot_sha256":"c33aa56ae4e25c4a1a2dbc9a4ebc743cbe373395ff295bbac069e04c84f7463f"},"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":"2605.13232","created_at":"2026-05-18T02:44:49.578413+00:00"},{"alias_kind":"arxiv_version","alias_value":"2605.13232v1","created_at":"2026-05-18T02:44:49.578413+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2605.13232","created_at":"2026-05-18T02:44:49.578413+00:00"},{"alias_kind":"pith_short_12","alias_value":"IWEL75IGLGIT","created_at":"2026-05-18T12:33:37.589309+00:00"},{"alias_kind":"pith_short_16","alias_value":"IWEL75IGLGIT2AAT","created_at":"2026-05-18T12:33:37.589309+00:00"},{"alias_kind":"pith_short_8","alias_value":"IWEL75IG","created_at":"2026-05-18T12:33:37.589309+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/IWEL75IGLGIT2AAT5JKYT444BU","json":"https://pith.science/pith/IWEL75IGLGIT2AAT5JKYT444BU.json","graph_json":"https://pith.science/api/pith-number/IWEL75IGLGIT2AAT5JKYT444BU/graph.json","events_json":"https://pith.science/api/pith-number/IWEL75IGLGIT2AAT5JKYT444BU/events.json","paper":"https://pith.science/paper/IWEL75IG"},"agent_actions":{"view_html":"https://pith.science/pith/IWEL75IGLGIT2AAT5JKYT444BU","download_json":"https://pith.science/pith/IWEL75IGLGIT2AAT5JKYT444BU.json","view_paper":"https://pith.science/paper/IWEL75IG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2605.13232&json=true","fetch_graph":"https://pith.science/api/pith-number/IWEL75IGLGIT2AAT5JKYT444BU/graph.json","fetch_events":"https://pith.science/api/pith-number/IWEL75IGLGIT2AAT5JKYT444BU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IWEL75IGLGIT2AAT5JKYT444BU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IWEL75IGLGIT2AAT5JKYT444BU/action/storage_attestation","attest_author":"https://pith.science/pith/IWEL75IGLGIT2AAT5JKYT444BU/action/author_attestation","sign_citation":"https://pith.science/pith/IWEL75IGLGIT2AAT5JKYT444BU/action/citation_signature","submit_replication":"https://pith.science/pith/IWEL75IGLGIT2AAT5JKYT444BU/action/replication_record"}},"created_at":"2026-05-18T02:44:49.578413+00:00","updated_at":"2026-05-18T02:44:49.578413+00:00"}