{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:WAGHLIM2UH367BCS5U27WQM2CT","short_pith_number":"pith:WAGHLIM2","schema_version":"1.0","canonical_sha256":"b00c75a19aa1f7ef8452ed35fb419a14e71cfde768a69b004b2f50ad7b7e6ac8","source":{"kind":"arxiv","id":"2403.06409","version":1},"attestation_state":"computed","paper":{"title":"Observational Properties of AGN Obscuration During the Peak of Accretion Growth","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Angel Ruiz, Bovornpratch Vijarnwannaluk, Ektoras Pouliasis, Elias Koulouridis, Ioannis Georgantopoulos, Kohei Ichikawa, Malte Schramm, Marcin Sawicki, Masayuki Akiyama, Naoki Matsumoto, Stephen Gwyn, Yoshihiro Ueda, Yoshiki Matsuoka, Yoshiki Toba","submitted_at":"2024-03-11T03:43:42Z","abstract_excerpt":"We investigated the gas obscuration and host galaxy properties of active galactic nuclei (AGN) during the peak of cosmic accretion growth of supermassive black holes (SMBHs) at redshift 0.8-1.8 using X-ray detected AGN with mid-infrared and far-infrared detection. The sample was classified as type-1 and type-2 AGN using optical spectral and morphological classification while the host galaxy properties were estimated with multiwavelength SED fitting. For type-1 AGN, the black hole mass was determined from MgII emission lines while the black hole mass of type-2 AGN was inferred from the host gal"},"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":"2403.06409","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2024-03-11T03:43:42Z","cross_cats_sorted":[],"title_canon_sha256":"7ee9e3b388fc1a111c3f84b65f570f572f42b2278adfbf720e8fc47bac50eea7","abstract_canon_sha256":"5cf7566c144a880be6d4af7cef3ad9e9140759495ca300f7483d132afffcab95"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:54:37.643734Z","signature_b64":"3DawdPyEHtGF8fE6kw9frhmb2d+UI+m42gx5NeKPYvHY25O6qwMk5z95Vor9V5rE5ojqJlYBf8ucLqnWT5fYCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b00c75a19aa1f7ef8452ed35fb419a14e71cfde768a69b004b2f50ad7b7e6ac8","last_reissued_at":"2026-07-05T07:54:37.643240Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:54:37.643240Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Observational Properties of AGN Obscuration During the Peak of Accretion Growth","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Angel Ruiz, Bovornpratch Vijarnwannaluk, Ektoras Pouliasis, Elias Koulouridis, Ioannis Georgantopoulos, Kohei Ichikawa, Malte Schramm, Marcin Sawicki, Masayuki Akiyama, Naoki Matsumoto, Stephen Gwyn, Yoshihiro Ueda, Yoshiki Matsuoka, Yoshiki Toba","submitted_at":"2024-03-11T03:43:42Z","abstract_excerpt":"We investigated the gas obscuration and host galaxy properties of active galactic nuclei (AGN) during the peak of cosmic accretion growth of supermassive black holes (SMBHs) at redshift 0.8-1.8 using X-ray detected AGN with mid-infrared and far-infrared detection. The sample was classified as type-1 and type-2 AGN using optical spectral and morphological classification while the host galaxy properties were estimated with multiwavelength SED fitting. For type-1 AGN, the black hole mass was determined from MgII emission lines while the black hole mass of type-2 AGN was inferred from the host gal"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2403.06409","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/2403.06409/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":"2403.06409","created_at":"2026-07-05T07:54:37.643298+00:00"},{"alias_kind":"arxiv_version","alias_value":"2403.06409v1","created_at":"2026-07-05T07:54:37.643298+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2403.06409","created_at":"2026-07-05T07:54:37.643298+00:00"},{"alias_kind":"pith_short_12","alias_value":"WAGHLIM2UH36","created_at":"2026-07-05T07:54:37.643298+00:00"},{"alias_kind":"pith_short_16","alias_value":"WAGHLIM2UH367BCS","created_at":"2026-07-05T07:54:37.643298+00:00"},{"alias_kind":"pith_short_8","alias_value":"WAGHLIM2","created_at":"2026-07-05T07:54:37.643298+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.12076","citing_title":"X-ray luminosity function of Compton-thick AGN in the early Universe (z > 3). Robustness and biases of the CTK population","ref_index":96,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT","json":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT.json","graph_json":"https://pith.science/api/pith-number/WAGHLIM2UH367BCS5U27WQM2CT/graph.json","events_json":"https://pith.science/api/pith-number/WAGHLIM2UH367BCS5U27WQM2CT/events.json","paper":"https://pith.science/paper/WAGHLIM2"},"agent_actions":{"view_html":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT","download_json":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT.json","view_paper":"https://pith.science/paper/WAGHLIM2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2403.06409&json=true","fetch_graph":"https://pith.science/api/pith-number/WAGHLIM2UH367BCS5U27WQM2CT/graph.json","fetch_events":"https://pith.science/api/pith-number/WAGHLIM2UH367BCS5U27WQM2CT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT/action/storage_attestation","attest_author":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT/action/author_attestation","sign_citation":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT/action/citation_signature","submit_replication":"https://pith.science/pith/WAGHLIM2UH367BCS5U27WQM2CT/action/replication_record"}},"created_at":"2026-07-05T07:54:37.643298+00:00","updated_at":"2026-07-05T07:54:37.643298+00:00"}