{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:M2FHL62JEEH4QKZJC6GWUZPPKQ","short_pith_number":"pith:M2FHL62J","schema_version":"1.0","canonical_sha256":"668a75fb49210fc82b29178d6a65ef541f2acb788d7ac813e493418790422614","source":{"kind":"arxiv","id":"0903.4347","version":1},"attestation_state":"computed","paper":{"title":"Suzaku Observation of a Hard Excess in 1H 0419-577: Detection of a Compton-Thick Partial-Covering Absorber","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"J.N.Reeves, K.A.Pounds, L.Miller, S.B.Kraemer, T.J.Turner","submitted_at":"2009-03-25T14:35:52Z","abstract_excerpt":"We present results from a 200 ks Suzaku observation of 1H 0419-577 taken during 2007 July. The source shows a strong excess of counts above 10 keV compared to the extrapolation of models based on previous data in the 0.5-10 keV band. The 'hard excess' in 1H 0419-577 can be explained by the presence of a Compton-thick partial-covering absorber that covers ~ 70% of the source. The Compton-thick gas likely originates from a radius inside of the optical BLR and may form part of a clumpy disk wind. The fluorescent Fe Ka luminosity measured by Suzaku is consistent with that expected from an equatori"},"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":"0903.4347","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-03-25T14:35:52Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"1f74bfceb4c669b1578b4996976e4b9f49d8fed496d4dd3e11c1dd85026dd289","abstract_canon_sha256":"dc527d51f44bd6cf4d0a7b521e6cbe566d8e5853d6a5720770119f4038590958"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:29:15.627250Z","signature_b64":"q0LzsSJeg9GgNH7KVXnPpMl8zFg1HPQ7LdTv+5odCSPe3ngn+AprpYozv81Gks9FXanf2xLdY4ozBPjKLqmtBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"668a75fb49210fc82b29178d6a65ef541f2acb788d7ac813e493418790422614","last_reissued_at":"2026-05-18T04:29:15.626757Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:29:15.626757Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Suzaku Observation of a Hard Excess in 1H 0419-577: Detection of a Compton-Thick Partial-Covering Absorber","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"J.N.Reeves, K.A.Pounds, L.Miller, S.B.Kraemer, T.J.Turner","submitted_at":"2009-03-25T14:35:52Z","abstract_excerpt":"We present results from a 200 ks Suzaku observation of 1H 0419-577 taken during 2007 July. The source shows a strong excess of counts above 10 keV compared to the extrapolation of models based on previous data in the 0.5-10 keV band. The 'hard excess' in 1H 0419-577 can be explained by the presence of a Compton-thick partial-covering absorber that covers ~ 70% of the source. The Compton-thick gas likely originates from a radius inside of the optical BLR and may form part of a clumpy disk wind. The fluorescent Fe Ka luminosity measured by Suzaku is consistent with that expected from an equatori"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0903.4347","kind":"arxiv","version":1},"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":"0903.4347","created_at":"2026-05-18T04:29:15.626835+00:00"},{"alias_kind":"arxiv_version","alias_value":"0903.4347v1","created_at":"2026-05-18T04:29:15.626835+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0903.4347","created_at":"2026-05-18T04:29:15.626835+00:00"},{"alias_kind":"pith_short_12","alias_value":"M2FHL62JEEH4","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_16","alias_value":"M2FHL62JEEH4QKZJ","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_8","alias_value":"M2FHL62J","created_at":"2026-05-18T12:26:00.592388+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.22918","citing_title":"Strong X-ray Variability of I Zwicky 1: Obscuration from Clumpy Accretion-Disk Winds","ref_index":130,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ","json":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ.json","graph_json":"https://pith.science/api/pith-number/M2FHL62JEEH4QKZJC6GWUZPPKQ/graph.json","events_json":"https://pith.science/api/pith-number/M2FHL62JEEH4QKZJC6GWUZPPKQ/events.json","paper":"https://pith.science/paper/M2FHL62J"},"agent_actions":{"view_html":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ","download_json":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ.json","view_paper":"https://pith.science/paper/M2FHL62J","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0903.4347&json=true","fetch_graph":"https://pith.science/api/pith-number/M2FHL62JEEH4QKZJC6GWUZPPKQ/graph.json","fetch_events":"https://pith.science/api/pith-number/M2FHL62JEEH4QKZJC6GWUZPPKQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ/action/storage_attestation","attest_author":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ/action/author_attestation","sign_citation":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ/action/citation_signature","submit_replication":"https://pith.science/pith/M2FHL62JEEH4QKZJC6GWUZPPKQ/action/replication_record"}},"created_at":"2026-05-18T04:29:15.626835+00:00","updated_at":"2026-05-18T04:29:15.626835+00:00"}