{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:ZW633BGYG47QIMZSWFMFC5J565","short_pith_number":"pith:ZW633BGY","schema_version":"1.0","canonical_sha256":"cdbdbd84d8373f043332b15851753df7542eb1d7aa0ca4a077078f6e7cc81654","source":{"kind":"arxiv","id":"1204.2535","version":1},"attestation_state":"computed","paper":{"title":"Modeling the Fe K Line Profiles in Type I AGN with a Compton-Thick Disk Wind","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"A. R. Patrick, J. N. Reeves, K. S. Long, L. Miller, M. M. Tatum, S. A. Sim, T. J. Turner","submitted_at":"2012-04-11T19:52:17Z","abstract_excerpt":"We have modeled a small sample of Seyfert galaxies that were previously identified as having simple X-ray spectra with little intrinsic absorption. The sources in this sample all contain moderately broad components of Fe K-shell emission and are ideal candidates for testing the applicability of a Compton-thick accretion-disk wind model to AGN emission components. Viewing angles through the wind allow the observer to see the absorption signature of the gas, whereas face-on viewing angles allow the observer to see the scattered light from the wind. We find that the Fe K emission line profiles ar"},"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":"1204.2535","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-04-11T19:52:17Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"25971fa455d12e681ff7d0c7ce7360f0a9be7971e69e717e99146f64ed25a89e","abstract_canon_sha256":"ba6dd0249d2697890dd2a56f1b4f5822d699fc96e64f8377ccd983f11467c4b0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:54:37.028421Z","signature_b64":"NspTtnmFfIGS1EGTtbhtq8daev8+QYdAGwUx82oWgP7MxZfNCoWNzQZSui8vrBlrXG0h4Yd+VFyAWDaOYlTJCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cdbdbd84d8373f043332b15851753df7542eb1d7aa0ca4a077078f6e7cc81654","last_reissued_at":"2026-05-18T03:54:37.027888Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:54:37.027888Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Modeling the Fe K Line Profiles in Type I AGN with a Compton-Thick Disk Wind","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"A. R. Patrick, J. N. Reeves, K. S. Long, L. Miller, M. M. Tatum, S. A. Sim, T. J. Turner","submitted_at":"2012-04-11T19:52:17Z","abstract_excerpt":"We have modeled a small sample of Seyfert galaxies that were previously identified as having simple X-ray spectra with little intrinsic absorption. The sources in this sample all contain moderately broad components of Fe K-shell emission and are ideal candidates for testing the applicability of a Compton-thick accretion-disk wind model to AGN emission components. Viewing angles through the wind allow the observer to see the absorption signature of the gas, whereas face-on viewing angles allow the observer to see the scattered light from the wind. We find that the Fe K emission line profiles ar"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1204.2535","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":"1204.2535","created_at":"2026-05-18T03:54:37.027967+00:00"},{"alias_kind":"arxiv_version","alias_value":"1204.2535v1","created_at":"2026-05-18T03:54:37.027967+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1204.2535","created_at":"2026-05-18T03:54:37.027967+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZW633BGYG47Q","created_at":"2026-05-18T12:27:30.460161+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZW633BGYG47QIMZS","created_at":"2026-05-18T12:27:30.460161+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZW633BGY","created_at":"2026-05-18T12:27:30.460161+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565","json":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565.json","graph_json":"https://pith.science/api/pith-number/ZW633BGYG47QIMZSWFMFC5J565/graph.json","events_json":"https://pith.science/api/pith-number/ZW633BGYG47QIMZSWFMFC5J565/events.json","paper":"https://pith.science/paper/ZW633BGY"},"agent_actions":{"view_html":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565","download_json":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565.json","view_paper":"https://pith.science/paper/ZW633BGY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1204.2535&json=true","fetch_graph":"https://pith.science/api/pith-number/ZW633BGYG47QIMZSWFMFC5J565/graph.json","fetch_events":"https://pith.science/api/pith-number/ZW633BGYG47QIMZSWFMFC5J565/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565/action/storage_attestation","attest_author":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565/action/author_attestation","sign_citation":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565/action/citation_signature","submit_replication":"https://pith.science/pith/ZW633BGYG47QIMZSWFMFC5J565/action/replication_record"}},"created_at":"2026-05-18T03:54:37.027967+00:00","updated_at":"2026-05-18T03:54:37.027967+00:00"}