{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:IOBVZSHQFO4FYVVW5GSXEK4RDL","short_pith_number":"pith:IOBVZSHQ","schema_version":"1.0","canonical_sha256":"43835cc8f02bb85c56b6e9a5722b911af0bcaa1ed6ac218055df8f920899a1c2","source":{"kind":"arxiv","id":"1804.00349","version":1},"attestation_state":"computed","paper":{"title":"The 1.5 Ms Observing Campaign on IRAS 13224-3809: X-ray Spectral Analysis I","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"A. C. Fabian, A. M. Lohfink, B. De Marco, C. Pinto, C.-Y. Chiang, D. J. K. Buisson, D. J. Walton, D. R. Wilkins, E. Kara, E. M. Cackett, F. A. Harrison, G. Miniutti, J. A. Garc\\'ia, J. Jiang, J. M. Miller, L. C. Gallo, M. L. Parker, T. Dauser, W. N. Alston","submitted_at":"2018-04-01T22:08:41Z","abstract_excerpt":"We present a detailed spectral analysis of the recent 1.5\\,Ms XMM-Newton observing campaign on the narrow line Seyfert 1 galaxy IRAS~13224$-$3809, taken simultaneously with 500\\,ks of NuSTAR data. The X-ray lightcurve shows three flux peaks, registering at about 100 times the minimum flux seen during the campaign, and rapid variability with a time scale of kiloseconds. The spectra are well fit with a primary powerlaw continuum, two relativistic-blurred reflection components from the inner accretion disk with very high iron abundance, and a simple blackbody-shaped model for the remaining soft e"},"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":"1804.00349","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2018-04-01T22:08:41Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"75fc7303d8093e89dd922fa18785cd7e2cbd53bb5b8e14119f2e49119502bcea","abstract_canon_sha256":"a2934c49dae6dfc33960d6d04c97435f01d843c3d6704e90ae27c6982510eefb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:18:48.734432Z","signature_b64":"jUluaITeKWV0fJ4W813wOuv2gQTvKI67fMc5OCbtCbCbOLK9IsmvXNFNogzYomH0n8CXdMNkto+PhOZHBYmjDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"43835cc8f02bb85c56b6e9a5722b911af0bcaa1ed6ac218055df8f920899a1c2","last_reissued_at":"2026-05-18T00:18:48.733439Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:18:48.733439Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The 1.5 Ms Observing Campaign on IRAS 13224-3809: X-ray Spectral Analysis I","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"A. C. Fabian, A. M. Lohfink, B. De Marco, C. Pinto, C.-Y. Chiang, D. J. K. Buisson, D. J. Walton, D. R. Wilkins, E. Kara, E. M. Cackett, F. A. Harrison, G. Miniutti, J. A. Garc\\'ia, J. Jiang, J. M. Miller, L. C. Gallo, M. L. Parker, T. Dauser, W. N. Alston","submitted_at":"2018-04-01T22:08:41Z","abstract_excerpt":"We present a detailed spectral analysis of the recent 1.5\\,Ms XMM-Newton observing campaign on the narrow line Seyfert 1 galaxy IRAS~13224$-$3809, taken simultaneously with 500\\,ks of NuSTAR data. The X-ray lightcurve shows three flux peaks, registering at about 100 times the minimum flux seen during the campaign, and rapid variability with a time scale of kiloseconds. The spectra are well fit with a primary powerlaw continuum, two relativistic-blurred reflection components from the inner accretion disk with very high iron abundance, and a simple blackbody-shaped model for the remaining soft e"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1804.00349","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":"1804.00349","created_at":"2026-05-18T00:18:48.733572+00:00"},{"alias_kind":"arxiv_version","alias_value":"1804.00349v1","created_at":"2026-05-18T00:18:48.733572+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1804.00349","created_at":"2026-05-18T00:18:48.733572+00:00"},{"alias_kind":"pith_short_12","alias_value":"IOBVZSHQFO4F","created_at":"2026-05-18T12:32:31.084164+00:00"},{"alias_kind":"pith_short_16","alias_value":"IOBVZSHQFO4FYVVW","created_at":"2026-05-18T12:32:31.084164+00:00"},{"alias_kind":"pith_short_8","alias_value":"IOBVZSHQ","created_at":"2026-05-18T12:32:31.084164+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":151,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL","json":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL.json","graph_json":"https://pith.science/api/pith-number/IOBVZSHQFO4FYVVW5GSXEK4RDL/graph.json","events_json":"https://pith.science/api/pith-number/IOBVZSHQFO4FYVVW5GSXEK4RDL/events.json","paper":"https://pith.science/paper/IOBVZSHQ"},"agent_actions":{"view_html":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL","download_json":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL.json","view_paper":"https://pith.science/paper/IOBVZSHQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1804.00349&json=true","fetch_graph":"https://pith.science/api/pith-number/IOBVZSHQFO4FYVVW5GSXEK4RDL/graph.json","fetch_events":"https://pith.science/api/pith-number/IOBVZSHQFO4FYVVW5GSXEK4RDL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL/action/storage_attestation","attest_author":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL/action/author_attestation","sign_citation":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL/action/citation_signature","submit_replication":"https://pith.science/pith/IOBVZSHQFO4FYVVW5GSXEK4RDL/action/replication_record"}},"created_at":"2026-05-18T00:18:48.733572+00:00","updated_at":"2026-05-18T00:18:48.733572+00:00"}