{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:TH2A42C7G3RWX46ZGX2GVDZXJE","short_pith_number":"pith:TH2A42C7","schema_version":"1.0","canonical_sha256":"99f40e685f36e36bf3d935f46a8f3749353a41f2f95e8ef17667e955c43bf792","source":{"kind":"arxiv","id":"astro-ph/0606040","version":1},"attestation_state":"computed","paper":{"title":"Fe II Emission in 14 Low-Redshift Quasars: I - Observations","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Kimiaki Kawara, Shinki Oyabu, Toshihiko Tanabe, Yoshiki Matsuoka, Yumihiko Tsuzuki, Yuzuru Yoshii","submitted_at":"2006-06-02T04:18:52Z","abstract_excerpt":"We present the spectra of 14 quasars with a wide coverage of rest wavelengths from 1000 to 7300 A. The redshift ranges from z = 0.061 to 0.555 and the luminosity from M_{B} = -22.69 to -26.32. We describe the procedure of generating the template spectrum of Fe II line emission from the spectrum of a narrow-line Seyfert 1 galaxy I Zw 1 that covers two wavelength regions of 2200-3500 A and 4200-5600 A. Our template Fe II spectrum is semi-empirical in the sense that the synthetic spectrum calculated with the CLOUDY photoionization code is used to separate the Fe II emission from the Mg II line. T"},"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":"astro-ph/0606040","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-06-02T04:18:52Z","cross_cats_sorted":[],"title_canon_sha256":"1dd27f66313591edf598e1ce2141adf6a4146a5df3d3422a23c3c6cc3fdfd925","abstract_canon_sha256":"43fff8a7d9e34b72da4a9e315f1c2add9179f4ed1435b178bea7eb0047c64150"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:19:03.653338Z","signature_b64":"WTxUqeZUqtkEcqyCET/CforhUvXticm9GNM+B4bczIkH+AkgAbV8rDPolAap2oozXo7QDENDlMK4yYd/jiGSBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"99f40e685f36e36bf3d935f46a8f3749353a41f2f95e8ef17667e955c43bf792","last_reissued_at":"2026-07-04T15:19:03.652964Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:19:03.652964Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Fe II Emission in 14 Low-Redshift Quasars: I - Observations","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Kimiaki Kawara, Shinki Oyabu, Toshihiko Tanabe, Yoshiki Matsuoka, Yumihiko Tsuzuki, Yuzuru Yoshii","submitted_at":"2006-06-02T04:18:52Z","abstract_excerpt":"We present the spectra of 14 quasars with a wide coverage of rest wavelengths from 1000 to 7300 A. The redshift ranges from z = 0.061 to 0.555 and the luminosity from M_{B} = -22.69 to -26.32. We describe the procedure of generating the template spectrum of Fe II line emission from the spectrum of a narrow-line Seyfert 1 galaxy I Zw 1 that covers two wavelength regions of 2200-3500 A and 4200-5600 A. Our template Fe II spectrum is semi-empirical in the sense that the synthetic spectrum calculated with the CLOUDY photoionization code is used to separate the Fe II emission from the Mg II line. T"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0606040","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0606040/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"astro-ph/0606040","created_at":"2026-07-04T15:19:03.653022+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0606040v1","created_at":"2026-07-04T15:19:03.653022+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0606040","created_at":"2026-07-04T15:19:03.653022+00:00"},{"alias_kind":"pith_short_12","alias_value":"TH2A42C7G3RW","created_at":"2026-07-04T15:19:03.653022+00:00"},{"alias_kind":"pith_short_16","alias_value":"TH2A42C7G3RWX46Z","created_at":"2026-07-04T15:19:03.653022+00:00"},{"alias_kind":"pith_short_8","alias_value":"TH2A42C7","created_at":"2026-07-04T15:19:03.653022+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2607.00105","citing_title":"AGN radiative feedback as the main regulator of [O III] outflow activity and obscuration in X-ray AGN","ref_index":89,"is_internal_anchor":true},{"citing_arxiv_id":"2606.08782","citing_title":"JWST Absorption-Line Analysis of UV-Bright Galaxies at $z=7.2-10.6$: Early Chemical Enrichment Traced by C, O, Mg, Al, Si, and Fe","ref_index":110,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27195","citing_title":"HALO II: Constraining Hubble constant $H_{0}$ through continuum delay fitting of Fairall 9","ref_index":141,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE","json":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE.json","graph_json":"https://pith.science/api/pith-number/TH2A42C7G3RWX46ZGX2GVDZXJE/graph.json","events_json":"https://pith.science/api/pith-number/TH2A42C7G3RWX46ZGX2GVDZXJE/events.json","paper":"https://pith.science/paper/TH2A42C7"},"agent_actions":{"view_html":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE","download_json":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE.json","view_paper":"https://pith.science/paper/TH2A42C7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0606040&json=true","fetch_graph":"https://pith.science/api/pith-number/TH2A42C7G3RWX46ZGX2GVDZXJE/graph.json","fetch_events":"https://pith.science/api/pith-number/TH2A42C7G3RWX46ZGX2GVDZXJE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE/action/storage_attestation","attest_author":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE/action/author_attestation","sign_citation":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE/action/citation_signature","submit_replication":"https://pith.science/pith/TH2A42C7G3RWX46ZGX2GVDZXJE/action/replication_record"}},"created_at":"2026-07-04T15:19:03.653022+00:00","updated_at":"2026-07-04T15:19:03.653022+00:00"}