{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:B7XCZKCXGMHWB6ONP5JCK7752Y","short_pith_number":"pith:B7XCZKCX","schema_version":"1.0","canonical_sha256":"0fee2ca857330f60f9cd7f52257ffdd6288f461d454c5a93f677ebaebf85ee18","source":{"kind":"arxiv","id":"0710.2954","version":2},"attestation_state":"computed","paper":{"title":"Low-Ionization Emission Regions in Quasars: Gas Properties Probed with Broad O I and Ca II Lines","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"K. Kawara, S. Oyabu, Y. Matsuoka","submitted_at":"2007-10-16T05:05:25Z","abstract_excerpt":"We have compiled the emission-line fluxes of O I 8446, O I 11287, and the near-IR Ca II triplet (8579) observed in 11 quasars. These lines are considered to emerge from the same gas as do the Fe II lines in the low-ionized portion of the broad emission line region (BELR). The compiled quasars are distributed over wide ranges of redshift (0.06 < z < 1.08) and of luminosity (-29.8 < M_B < -22.1), thus representing a useful sample to investigate the line-emitting gas properties in various quasar environments. The measured line strengths and velocities, as functions of the quasar properties, are a"},"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":"0710.2954","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-10-16T05:05:25Z","cross_cats_sorted":[],"title_canon_sha256":"2d793ff8865fd786a169f0aa0fd236796d04fc4eee2d234044176d64f7ab1873","abstract_canon_sha256":"d14e974156b391caf8b917e016f12137891e1bb0c0a849fea23658435f531dcc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:29:33.785904Z","signature_b64":"PHDl7Xt9RURIedMHnDClLvcSHLgjEWvGSY5Z2XWl/mKN00dD29gaTxOrtr+Ym+BtKqPmvdYn5fiv9DACW2jVDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0fee2ca857330f60f9cd7f52257ffdd6288f461d454c5a93f677ebaebf85ee18","last_reissued_at":"2026-05-18T04:29:33.785516Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:29:33.785516Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Low-Ionization Emission Regions in Quasars: Gas Properties Probed with Broad O I and Ca II Lines","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"K. Kawara, S. Oyabu, Y. Matsuoka","submitted_at":"2007-10-16T05:05:25Z","abstract_excerpt":"We have compiled the emission-line fluxes of O I 8446, O I 11287, and the near-IR Ca II triplet (8579) observed in 11 quasars. These lines are considered to emerge from the same gas as do the Fe II lines in the low-ionized portion of the broad emission line region (BELR). The compiled quasars are distributed over wide ranges of redshift (0.06 < z < 1.08) and of luminosity (-29.8 < M_B < -22.1), thus representing a useful sample to investigate the line-emitting gas properties in various quasar environments. The measured line strengths and velocities, as functions of the quasar properties, are a"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0710.2954","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":"0710.2954","created_at":"2026-05-18T04:29:33.785584+00:00"},{"alias_kind":"arxiv_version","alias_value":"0710.2954v2","created_at":"2026-05-18T04:29:33.785584+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0710.2954","created_at":"2026-05-18T04:29:33.785584+00:00"},{"alias_kind":"pith_short_12","alias_value":"B7XCZKCXGMHW","created_at":"2026-05-18T12:25:55.427421+00:00"},{"alias_kind":"pith_short_16","alias_value":"B7XCZKCXGMHWB6ON","created_at":"2026-05-18T12:25:55.427421+00:00"},{"alias_kind":"pith_short_8","alias_value":"B7XCZKCX","created_at":"2026-05-18T12:25:55.427421+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.00992","citing_title":"Understanding the Broad-line Region of Active Galactic Nuclei with Photoionization. II. Slim disks, Self-shadowing, and BLR sizes","ref_index":79,"is_internal_anchor":true},{"citing_arxiv_id":"2606.21614","citing_title":"Little Red and Blue Dots: AGN-excited narrow lines, Lyman-$\\alpha$ emission, and resemblance to standard quasars","ref_index":207,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y","json":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y.json","graph_json":"https://pith.science/api/pith-number/B7XCZKCXGMHWB6ONP5JCK7752Y/graph.json","events_json":"https://pith.science/api/pith-number/B7XCZKCXGMHWB6ONP5JCK7752Y/events.json","paper":"https://pith.science/paper/B7XCZKCX"},"agent_actions":{"view_html":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y","download_json":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y.json","view_paper":"https://pith.science/paper/B7XCZKCX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0710.2954&json=true","fetch_graph":"https://pith.science/api/pith-number/B7XCZKCXGMHWB6ONP5JCK7752Y/graph.json","fetch_events":"https://pith.science/api/pith-number/B7XCZKCXGMHWB6ONP5JCK7752Y/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y/action/timestamp_anchor","attest_storage":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y/action/storage_attestation","attest_author":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y/action/author_attestation","sign_citation":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y/action/citation_signature","submit_replication":"https://pith.science/pith/B7XCZKCXGMHWB6ONP5JCK7752Y/action/replication_record"}},"created_at":"2026-05-18T04:29:33.785584+00:00","updated_at":"2026-05-18T04:29:33.785584+00:00"}