{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:3B4I2EXF7GDV7P3KUIIQGHI7AW","short_pith_number":"pith:3B4I2EXF","schema_version":"1.0","canonical_sha256":"d8788d12e5f9875fbf6aa211031d1f058609db69894eaa264a94c72e80f7a7de","source":{"kind":"arxiv","id":"1107.3148","version":1},"attestation_state":"computed","paper":{"title":"\"Revealing a Population of Heavily Obscured Active Galactic Nuclei at z=0.5-1 in the Chandra Deep Field-South","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"A.C. Fabian, A. Comastri, B.D. Lehmer, B. Luo, C. Vignali, D.A. Rafferty, D.M. Alexander, D.P. Schneider, F.E. Bauer, M. Brusa, R. Gilli, W.N. Brandt, Y.Q. Xue","submitted_at":"2011-07-15T20:00:02Z","abstract_excerpt":"(abridged) We identify a numerically significant population of heavily obscured AGNs at z~0.5-1 in the Chandra Deep Field-South (CDF-S) and Extended Chandra Deep Field-South by selecting 242 X-ray undetected objects with infrared-based star formation rates (SFRs) substantially higher (a factor of 3.2 or more) than their SFRs determined from the UV after correcting for dust extinction. An X-ray stacking analysis of 23 candidates in the central CDF-S region using the 4 Ms Chandra data reveals a hard X-ray signal with an effective power-law photon index of Gamma=0.6_{-0.4}^{+0.3}, indicating a si"},"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":"1107.3148","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-07-15T20:00:02Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"cae1793d9805f66d1adb0a5e42dd67e58fffdd5c5439b587c4a8b76b43c3bbb9","abstract_canon_sha256":"dd5b8f03801091822a28960a2065fb7208deb5d182fd162bc423f2b1e7553824"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:01:16.034057Z","signature_b64":"5/aGocbBqsivOq2wHME2A/JFRkZVszvSoPjYEOTB296dknLRYOqbpXhN4lHRYtjDyJ0lhWzEfGGEJOg44gz8BQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d8788d12e5f9875fbf6aa211031d1f058609db69894eaa264a94c72e80f7a7de","last_reissued_at":"2026-05-18T02:01:16.033214Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:01:16.033214Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"\"Revealing a Population of Heavily Obscured Active Galactic Nuclei at z=0.5-1 in the Chandra Deep Field-South","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"A.C. Fabian, A. Comastri, B.D. Lehmer, B. Luo, C. Vignali, D.A. Rafferty, D.M. Alexander, D.P. Schneider, F.E. Bauer, M. Brusa, R. Gilli, W.N. Brandt, Y.Q. Xue","submitted_at":"2011-07-15T20:00:02Z","abstract_excerpt":"(abridged) We identify a numerically significant population of heavily obscured AGNs at z~0.5-1 in the Chandra Deep Field-South (CDF-S) and Extended Chandra Deep Field-South by selecting 242 X-ray undetected objects with infrared-based star formation rates (SFRs) substantially higher (a factor of 3.2 or more) than their SFRs determined from the UV after correcting for dust extinction. An X-ray stacking analysis of 23 candidates in the central CDF-S region using the 4 Ms Chandra data reveals a hard X-ray signal with an effective power-law photon index of Gamma=0.6_{-0.4}^{+0.3}, indicating a si"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1107.3148","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":"1107.3148","created_at":"2026-05-18T02:01:16.033334+00:00"},{"alias_kind":"arxiv_version","alias_value":"1107.3148v1","created_at":"2026-05-18T02:01:16.033334+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1107.3148","created_at":"2026-05-18T02:01:16.033334+00:00"},{"alias_kind":"pith_short_12","alias_value":"3B4I2EXF7GDV","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_16","alias_value":"3B4I2EXF7GDV7P3K","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_8","alias_value":"3B4I2EXF","created_at":"2026-05-18T12:26:18.847500+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":139,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW","json":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW.json","graph_json":"https://pith.science/api/pith-number/3B4I2EXF7GDV7P3KUIIQGHI7AW/graph.json","events_json":"https://pith.science/api/pith-number/3B4I2EXF7GDV7P3KUIIQGHI7AW/events.json","paper":"https://pith.science/paper/3B4I2EXF"},"agent_actions":{"view_html":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW","download_json":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW.json","view_paper":"https://pith.science/paper/3B4I2EXF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1107.3148&json=true","fetch_graph":"https://pith.science/api/pith-number/3B4I2EXF7GDV7P3KUIIQGHI7AW/graph.json","fetch_events":"https://pith.science/api/pith-number/3B4I2EXF7GDV7P3KUIIQGHI7AW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW/action/storage_attestation","attest_author":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW/action/author_attestation","sign_citation":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW/action/citation_signature","submit_replication":"https://pith.science/pith/3B4I2EXF7GDV7P3KUIIQGHI7AW/action/replication_record"}},"created_at":"2026-05-18T02:01:16.033334+00:00","updated_at":"2026-05-18T02:01:16.033334+00:00"}