{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:VNCUVEAPOQK2Y4BI43WCTLLHBN","short_pith_number":"pith:VNCUVEAP","schema_version":"1.0","canonical_sha256":"ab454a900f7415ac7028e6ec29ad670b46585e48194f40ddd8a5fff14136238e","source":{"kind":"arxiv","id":"1005.0373","version":1},"attestation_state":"computed","paper":{"title":"The X-ray to [Ne V]3426 flux ratio: discovering heavily obscured AGN in the distant Universe","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Comastri, C. Vignali, G. Zamorani, K. Iwasawa, M. Mignoli, R. Gilli","submitted_at":"2010-05-03T18:58:05Z","abstract_excerpt":"We investigate the possibility of using the ratio between the 2-10 keV flux and the [Ne V]3426 emission line flux (X/NeV) as a diagnostic diagram to discover heavily obscured, possibly Compton-Thick Active Galactic Nuclei (AGN) up to z~1.5. First, we calibrate a relation between X/NeV and the cold absorbing column density N_H using a sample of 74 bright, nearby Seyferts with both X-ray and [Ne V] data available in the literature. Similarly to what is found for the X-ray to [O III]5007 flux ratio (X/OIII), we found that the X/NeV ratio decreases towards large column densities. Essentially all l"},"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":"1005.0373","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2010-05-03T18:58:05Z","cross_cats_sorted":[],"title_canon_sha256":"c7117a345cc61645e6f0c4c19c2cee2c1aaeec5fc302652f232ee55e7ecd8d75","abstract_canon_sha256":"0c3e5b62bf993fae8fbf0303e23d216b99221fef3a017b3dde581e8b879a647f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:07:43.462938Z","signature_b64":"Y7Siu4KV5MNp2C0f0kpNR5EMcJbJTkIb3IFppnTyDWF/x8ZnDK6XmrlHmMz2DjMVBs8CKAQT8zTvcsHsVuB/Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ab454a900f7415ac7028e6ec29ad670b46585e48194f40ddd8a5fff14136238e","last_reissued_at":"2026-05-18T02:07:43.461974Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:07:43.461974Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The X-ray to [Ne V]3426 flux ratio: discovering heavily obscured AGN in the distant Universe","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Comastri, C. Vignali, G. Zamorani, K. Iwasawa, M. Mignoli, R. Gilli","submitted_at":"2010-05-03T18:58:05Z","abstract_excerpt":"We investigate the possibility of using the ratio between the 2-10 keV flux and the [Ne V]3426 emission line flux (X/NeV) as a diagnostic diagram to discover heavily obscured, possibly Compton-Thick Active Galactic Nuclei (AGN) up to z~1.5. First, we calibrate a relation between X/NeV and the cold absorbing column density N_H using a sample of 74 bright, nearby Seyferts with both X-ray and [Ne V] data available in the literature. Similarly to what is found for the X-ray to [O III]5007 flux ratio (X/OIII), we found that the X/NeV ratio decreases towards large column densities. Essentially all l"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1005.0373","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":"1005.0373","created_at":"2026-05-18T02:07:43.462098+00:00"},{"alias_kind":"arxiv_version","alias_value":"1005.0373v1","created_at":"2026-05-18T02:07:43.462098+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1005.0373","created_at":"2026-05-18T02:07:43.462098+00:00"},{"alias_kind":"pith_short_12","alias_value":"VNCUVEAPOQK2","created_at":"2026-05-18T12:26:15.391820+00:00"},{"alias_kind":"pith_short_16","alias_value":"VNCUVEAPOQK2Y4BI","created_at":"2026-05-18T12:26:15.391820+00:00"},{"alias_kind":"pith_short_8","alias_value":"VNCUVEAP","created_at":"2026-05-18T12:26:15.391820+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.17040","citing_title":"PEARLS: JWST Counterparts of Micro-Jy Radio Sources in the NEP Time Domain Field. II. All Four Spokes","ref_index":84,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN","json":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN.json","graph_json":"https://pith.science/api/pith-number/VNCUVEAPOQK2Y4BI43WCTLLHBN/graph.json","events_json":"https://pith.science/api/pith-number/VNCUVEAPOQK2Y4BI43WCTLLHBN/events.json","paper":"https://pith.science/paper/VNCUVEAP"},"agent_actions":{"view_html":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN","download_json":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN.json","view_paper":"https://pith.science/paper/VNCUVEAP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1005.0373&json=true","fetch_graph":"https://pith.science/api/pith-number/VNCUVEAPOQK2Y4BI43WCTLLHBN/graph.json","fetch_events":"https://pith.science/api/pith-number/VNCUVEAPOQK2Y4BI43WCTLLHBN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN/action/storage_attestation","attest_author":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN/action/author_attestation","sign_citation":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN/action/citation_signature","submit_replication":"https://pith.science/pith/VNCUVEAPOQK2Y4BI43WCTLLHBN/action/replication_record"}},"created_at":"2026-05-18T02:07:43.462098+00:00","updated_at":"2026-05-18T02:07:43.462098+00:00"}