{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:3TVE7TTP6UOOIYLA4ENANN25OC","short_pith_number":"pith:3TVE7TTP","schema_version":"1.0","canonical_sha256":"dcea4fce6ff51ce46160e11a06b75d70bae34683843226eaab08e616d5ac0cb7","source":{"kind":"arxiv","id":"astro-ph/0603313","version":1},"attestation_state":"computed","paper":{"title":"Why X-ray--Selected AGN Appear Optically Dull","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) CSIC), A. Alonso-Herrero (2), G. H. Rieke (1), J. L. Donley (1), J. R. Rigby (1), P. G. P\\'erez-Gonz\\'alez (1) ((1) Steward Observatory","submitted_at":"2006-03-13T17:50:23Z","abstract_excerpt":"We investigate why half of X-ray--selected active galactic nuclei (AGN) in deep surveys lack signs of accretion in their optical spectra. The majority of these ``optically--dull'' AGN are no more than 6 times fainter than their host galaxies in rest-frame R-band; as such, AGN lines are unlikely to be overwhelmed by stellar continuum in at least half the sample. We find that optically--dull AGN have the mid--infrared emission and L(x)/L(IR) ratios characteristic of local Seyferts, suggesting that the cause of optical dullness is not missing UV--optical continua. We compare the morphologies of 2"},"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/0603313","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-03-13T17:50:23Z","cross_cats_sorted":[],"title_canon_sha256":"63ee133ec9acfa3c6f43f5bd461f9f109cf10d7a8e3d1a9dd668e8bdae443e56","abstract_canon_sha256":"84d8ff4cd5fd3c8eb20b0cb0748a0eccb8e9b01a3674416b881ffd7e4fa55e77"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:18:14.324675Z","signature_b64":"fDO9AAyloPzamJWt5wl1cVE2Z/F1oYneFaZuAfjycO5ZSfhSzcPaIU2RSAdve+4L/yVXIzD6+IiDj3rxnbJ6Dw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"dcea4fce6ff51ce46160e11a06b75d70bae34683843226eaab08e616d5ac0cb7","last_reissued_at":"2026-05-18T04:18:14.323935Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:18:14.323935Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Why X-ray--Selected AGN Appear Optically Dull","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) CSIC), A. Alonso-Herrero (2), G. H. Rieke (1), J. L. Donley (1), J. R. Rigby (1), P. G. P\\'erez-Gonz\\'alez (1) ((1) Steward Observatory","submitted_at":"2006-03-13T17:50:23Z","abstract_excerpt":"We investigate why half of X-ray--selected active galactic nuclei (AGN) in deep surveys lack signs of accretion in their optical spectra. The majority of these ``optically--dull'' AGN are no more than 6 times fainter than their host galaxies in rest-frame R-band; as such, AGN lines are unlikely to be overwhelmed by stellar continuum in at least half the sample. We find that optically--dull AGN have the mid--infrared emission and L(x)/L(IR) ratios characteristic of local Seyferts, suggesting that the cause of optical dullness is not missing UV--optical continua. We compare the morphologies of 2"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0603313","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":"astro-ph/0603313","created_at":"2026-05-18T04:18:14.324059+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0603313v1","created_at":"2026-05-18T04:18:14.324059+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0603313","created_at":"2026-05-18T04:18:14.324059+00:00"},{"alias_kind":"pith_short_12","alias_value":"3TVE7TTP6UOO","created_at":"2026-05-18T12:25:53.939244+00:00"},{"alias_kind":"pith_short_16","alias_value":"3TVE7TTP6UOOIYLA","created_at":"2026-05-18T12:25:53.939244+00:00"},{"alias_kind":"pith_short_8","alias_value":"3TVE7TTP","created_at":"2026-05-18T12:25:53.939244+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.17993","citing_title":"Nuclear Activity and Host Galaxy Properties of Low-Luminosity AGN Identified from VLA Observations","ref_index":27,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC","json":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC.json","graph_json":"https://pith.science/api/pith-number/3TVE7TTP6UOOIYLA4ENANN25OC/graph.json","events_json":"https://pith.science/api/pith-number/3TVE7TTP6UOOIYLA4ENANN25OC/events.json","paper":"https://pith.science/paper/3TVE7TTP"},"agent_actions":{"view_html":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC","download_json":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC.json","view_paper":"https://pith.science/paper/3TVE7TTP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0603313&json=true","fetch_graph":"https://pith.science/api/pith-number/3TVE7TTP6UOOIYLA4ENANN25OC/graph.json","fetch_events":"https://pith.science/api/pith-number/3TVE7TTP6UOOIYLA4ENANN25OC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC/action/storage_attestation","attest_author":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC/action/author_attestation","sign_citation":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC/action/citation_signature","submit_replication":"https://pith.science/pith/3TVE7TTP6UOOIYLA4ENANN25OC/action/replication_record"}},"created_at":"2026-05-18T04:18:14.324059+00:00","updated_at":"2026-05-18T04:18:14.324059+00:00"}