{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1999:QNC2MFAOOLU2DAHIRV4C3T56QU","short_pith_number":"pith:QNC2MFAO","schema_version":"1.0","canonical_sha256":"8345a6140e72e9a180e88d782dcfbe8538d3417257e512822a0568a42a5fa1a0","source":{"kind":"arxiv","id":"astro-ph/9902377","version":1},"attestation_state":"computed","paper":{"title":"The distribution of absorbing column densities among Seyfert 2 galaxies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G. Risaliti, M. Salvati, R. Maiolino","submitted_at":"1999-02-26T16:05:00Z","abstract_excerpt":"We use hard X-ray data for an \"optimal\" sample of Seyfert 2 galaxies to derive the distribution of the gaseous absorbing column densities among obscured active nuclei in the local Universe. Of all Seyfert 2 galaxies in the sample, 75% are heavily obscured (N_H > 10^23 cm^-2) and about half are Compton thick (N_H > 10^24 cm^-2). Intermediate type 1.8-1.9 Seyferts are characterized by an average N_H much lower than \"strict\" Seyfert 2s. No correlation is found between N_H and the intrinsic luminosity of the nuclear source. This N_H distribution has important consequences for the synthesis of the "},"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/9902377","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1999-02-26T16:05:00Z","cross_cats_sorted":[],"title_canon_sha256":"5cd6adfc636d0411f461d7ede2f949aa335ca70f5ed1cb3d17ed1a9b2fa0b614","abstract_canon_sha256":"37123452482c3b9be31d1db4d95a748dbb2dbd88bb44dd7dd87e27b7ea862757"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:10:44.667590Z","signature_b64":"02v+vusGTPDRSA0MGS/HNIk8unx9xteBZqd21PzDb4JyvUkloPb/p6ZxjZCQYkUTm+b1AFAsVsHYZlCTLPNXAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8345a6140e72e9a180e88d782dcfbe8538d3417257e512822a0568a42a5fa1a0","last_reissued_at":"2026-07-04T16:10:44.667214Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:10:44.667214Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The distribution of absorbing column densities among Seyfert 2 galaxies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G. Risaliti, M. Salvati, R. Maiolino","submitted_at":"1999-02-26T16:05:00Z","abstract_excerpt":"We use hard X-ray data for an \"optimal\" sample of Seyfert 2 galaxies to derive the distribution of the gaseous absorbing column densities among obscured active nuclei in the local Universe. Of all Seyfert 2 galaxies in the sample, 75% are heavily obscured (N_H > 10^23 cm^-2) and about half are Compton thick (N_H > 10^24 cm^-2). Intermediate type 1.8-1.9 Seyferts are characterized by an average N_H much lower than \"strict\" Seyfert 2s. No correlation is found between N_H and the intrinsic luminosity of the nuclear source. This N_H distribution has important consequences for the synthesis of the "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9902377","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/9902377/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/9902377","created_at":"2026-07-04T16:10:44.667272+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9902377v1","created_at":"2026-07-04T16:10:44.667272+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9902377","created_at":"2026-07-04T16:10:44.667272+00:00"},{"alias_kind":"pith_short_12","alias_value":"QNC2MFAOOLU2","created_at":"2026-07-04T16:10:44.667272+00:00"},{"alias_kind":"pith_short_16","alias_value":"QNC2MFAOOLU2DAHI","created_at":"2026-07-04T16:10:44.667272+00:00"},{"alias_kind":"pith_short_8","alias_value":"QNC2MFAO","created_at":"2026-07-04T16:10:44.667272+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.06844","citing_title":"First detection of ultra-fast outflows in a quiescent galaxy","ref_index":7,"is_internal_anchor":true},{"citing_arxiv_id":"2606.20800","citing_title":"No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST-PRIMER MIRI and NIRCam","ref_index":85,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU","json":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU.json","graph_json":"https://pith.science/api/pith-number/QNC2MFAOOLU2DAHIRV4C3T56QU/graph.json","events_json":"https://pith.science/api/pith-number/QNC2MFAOOLU2DAHIRV4C3T56QU/events.json","paper":"https://pith.science/paper/QNC2MFAO"},"agent_actions":{"view_html":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU","download_json":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU.json","view_paper":"https://pith.science/paper/QNC2MFAO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9902377&json=true","fetch_graph":"https://pith.science/api/pith-number/QNC2MFAOOLU2DAHIRV4C3T56QU/graph.json","fetch_events":"https://pith.science/api/pith-number/QNC2MFAOOLU2DAHIRV4C3T56QU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU/action/storage_attestation","attest_author":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU/action/author_attestation","sign_citation":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU/action/citation_signature","submit_replication":"https://pith.science/pith/QNC2MFAOOLU2DAHIRV4C3T56QU/action/replication_record"}},"created_at":"2026-07-04T16:10:44.667272+00:00","updated_at":"2026-07-04T16:10:44.667272+00:00"}