{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:QGVPW5K3Y24VIVOD2HGJCY75SP","short_pith_number":"pith:QGVPW5K3","schema_version":"1.0","canonical_sha256":"81aafb755bc6b95455c3d1cc9163fd93f042428678bb308e463125147db5163f","source":{"kind":"arxiv","id":"2206.03508","version":3},"attestation_state":"computed","paper":{"title":"Supermassive Black Holes at High Redshift are Expected to be Obscured by their Massive Host Galaxies' Inter Stellar Medium","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Comastri, C. Norman, C. Vignali, F. Calura, F. Pozzi, F. Vito, G. Lanzuisi, K. Iwasawa, M. Brusa, M. Mignoli, P. Cox, Q. D'Amato, R. Decarli, R. Gilli, S. Marchesi","submitted_at":"2022-06-07T18:00:02Z","abstract_excerpt":"We combine results from deep ALMA observations of massive ($M_*>10^{10}\\;M_{\\odot}$) galaxies at different redshifts to show that the column density of their inter stellar medium (ISM) rapidly increases towards early cosmic epochs. Our analysis includes objects from the ASPECS and ALPINE large programs, as well as individual observations of $z\\sim 6$ QSO hosts. When accounting for non-detections and correcting for selection effects, we find that the median surface density of the ISM of the massive galaxy population evolves as $\\sim(1+z)^{3.3}$. This means that the ISM column density towards th"},"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":"2206.03508","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2022-06-07T18:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"02e97fe3b36aa58364c1e827340a8ab10afcce649088c2e932f0aa1a232aa436","abstract_canon_sha256":"4f55a010f0f9509a1b45b30e5e07fda520ab8029e28b79d978769bfe463fce62"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:03:25.714176Z","signature_b64":"y2Hfw6wtOOtT30NUUPUwarzwBPqZH91YTfddxedDl6rZHylsJ4C1zn/gScGU0R0IG0XWtEdYzUzE5IPQ9fNGCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"81aafb755bc6b95455c3d1cc9163fd93f042428678bb308e463125147db5163f","last_reissued_at":"2026-07-05T05:03:25.713693Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:03:25.713693Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Supermassive Black Holes at High Redshift are Expected to be Obscured by their Massive Host Galaxies' Inter Stellar Medium","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Comastri, C. Norman, C. Vignali, F. Calura, F. Pozzi, F. Vito, G. Lanzuisi, K. Iwasawa, M. Brusa, M. Mignoli, P. Cox, Q. D'Amato, R. Decarli, R. Gilli, S. Marchesi","submitted_at":"2022-06-07T18:00:02Z","abstract_excerpt":"We combine results from deep ALMA observations of massive ($M_*>10^{10}\\;M_{\\odot}$) galaxies at different redshifts to show that the column density of their inter stellar medium (ISM) rapidly increases towards early cosmic epochs. Our analysis includes objects from the ASPECS and ALPINE large programs, as well as individual observations of $z\\sim 6$ QSO hosts. When accounting for non-detections and correcting for selection effects, we find that the median surface density of the ISM of the massive galaxy population evolves as $\\sim(1+z)^{3.3}$. This means that the ISM column density towards th"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2206.03508","kind":"arxiv","version":3},"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/2206.03508/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":"2206.03508","created_at":"2026-07-05T05:03:25.713752+00:00"},{"alias_kind":"arxiv_version","alias_value":"2206.03508v3","created_at":"2026-07-05T05:03:25.713752+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2206.03508","created_at":"2026-07-05T05:03:25.713752+00:00"},{"alias_kind":"pith_short_12","alias_value":"QGVPW5K3Y24V","created_at":"2026-07-05T05:03:25.713752+00:00"},{"alias_kind":"pith_short_16","alias_value":"QGVPW5K3Y24VIVOD","created_at":"2026-07-05T05:03:25.713752+00:00"},{"alias_kind":"pith_short_8","alias_value":"QGVPW5K3","created_at":"2026-07-05T05:03:25.713752+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.12511","citing_title":"Unification models of Active Galactic Nuclei","ref_index":76,"is_internal_anchor":false},{"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":40,"is_internal_anchor":false},{"citing_arxiv_id":"2606.30734","citing_title":"The Lifetimes of High-redshift Quasars Suggest Magnetic Disk Support","ref_index":13,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP","json":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP.json","graph_json":"https://pith.science/api/pith-number/QGVPW5K3Y24VIVOD2HGJCY75SP/graph.json","events_json":"https://pith.science/api/pith-number/QGVPW5K3Y24VIVOD2HGJCY75SP/events.json","paper":"https://pith.science/paper/QGVPW5K3"},"agent_actions":{"view_html":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP","download_json":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP.json","view_paper":"https://pith.science/paper/QGVPW5K3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2206.03508&json=true","fetch_graph":"https://pith.science/api/pith-number/QGVPW5K3Y24VIVOD2HGJCY75SP/graph.json","fetch_events":"https://pith.science/api/pith-number/QGVPW5K3Y24VIVOD2HGJCY75SP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP/action/storage_attestation","attest_author":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP/action/author_attestation","sign_citation":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP/action/citation_signature","submit_replication":"https://pith.science/pith/QGVPW5K3Y24VIVOD2HGJCY75SP/action/replication_record"}},"created_at":"2026-07-05T05:03:25.713752+00:00","updated_at":"2026-07-05T05:03:25.713752+00:00"}