{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:H2Q2IMWCM3Z4BDYXOXMYA7ASEK","short_pith_number":"pith:H2Q2IMWC","schema_version":"1.0","canonical_sha256":"3ea1a432c266f3c08f1775d9807c122280afcec18150aae14ae5d2afdc01b272","source":{"kind":"arxiv","id":"0908.0386","version":2},"attestation_state":"computed","paper":{"title":"What broad emission lines tell us about how active galactic nuclei work","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"C. Martin Gaskell","submitted_at":"2009-08-04T05:58:34Z","abstract_excerpt":"I review progress made in understanding the nature of the broad-line region (BLR) of active galactic nuclei (AGNs) and the role BLRs play in the AGN phenomenon. The high equivalent widths of the lines imply a high BLR covering factor, and the absence of clear evidence for absorption by the BLR means that the BLR has a flattened distribution and that we always view it near pole-on. The BLR gas is strongly self-shielding near the equatorial plane. Velocity-resolved reverberation mapping has long strongly excluded significant outflow of the BLR and shows instead that the predominant motions are K"},"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":"0908.0386","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-08-04T05:58:34Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"255c64c41f7aa58ac21ce66aa520d4a5f3014731c4ae3e308e27baf10645b329","abstract_canon_sha256":"b461826ddb6ab2fd9b4114091063f9b808d8cbde049c8407340c4493780ee159"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:12:44.930030Z","signature_b64":"d+07f07dtmy0XjjGQS2lR2aqJdolJ0B/LQfUkGZWfXYfGiCvZJU/MeAORbSrquK7GOtwkXEM+SR8M9XKNaoOCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3ea1a432c266f3c08f1775d9807c122280afcec18150aae14ae5d2afdc01b272","last_reissued_at":"2026-05-18T02:12:44.929543Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:12:44.929543Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"What broad emission lines tell us about how active galactic nuclei work","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"C. Martin Gaskell","submitted_at":"2009-08-04T05:58:34Z","abstract_excerpt":"I review progress made in understanding the nature of the broad-line region (BLR) of active galactic nuclei (AGNs) and the role BLRs play in the AGN phenomenon. The high equivalent widths of the lines imply a high BLR covering factor, and the absence of clear evidence for absorption by the BLR means that the BLR has a flattened distribution and that we always view it near pole-on. The BLR gas is strongly self-shielding near the equatorial plane. Velocity-resolved reverberation mapping has long strongly excluded significant outflow of the BLR and shows instead that the predominant motions are K"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0908.0386","kind":"arxiv","version":2},"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":"0908.0386","created_at":"2026-05-18T02:12:44.929617+00:00"},{"alias_kind":"arxiv_version","alias_value":"0908.0386v2","created_at":"2026-05-18T02:12:44.929617+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0908.0386","created_at":"2026-05-18T02:12:44.929617+00:00"},{"alias_kind":"pith_short_12","alias_value":"H2Q2IMWCM3Z4","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_16","alias_value":"H2Q2IMWCM3Z4BDYX","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_8","alias_value":"H2Q2IMWC","created_at":"2026-05-18T12:25:59.703012+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03291","citing_title":"Physically motivated AGN emissivity profiles and their effects on quasar microlensing signatures. 1. Multi-epoch accretion disc size inference","ref_index":179,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK","json":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK.json","graph_json":"https://pith.science/api/pith-number/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/graph.json","events_json":"https://pith.science/api/pith-number/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/events.json","paper":"https://pith.science/paper/H2Q2IMWC"},"agent_actions":{"view_html":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK","download_json":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK.json","view_paper":"https://pith.science/paper/H2Q2IMWC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0908.0386&json=true","fetch_graph":"https://pith.science/api/pith-number/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/graph.json","fetch_events":"https://pith.science/api/pith-number/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/action/storage_attestation","attest_author":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/action/author_attestation","sign_citation":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/action/citation_signature","submit_replication":"https://pith.science/pith/H2Q2IMWCM3Z4BDYXOXMYA7ASEK/action/replication_record"}},"created_at":"2026-05-18T02:12:44.929617+00:00","updated_at":"2026-05-18T02:12:44.929617+00:00"}