{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:CRLXR6V7ECFPLVLAWVOQ2OLUPC","short_pith_number":"pith:CRLXR6V7","schema_version":"1.0","canonical_sha256":"145778fabf208af5d560b55d0d3974789caca30fd9c59db859d775f1ceff2650","source":{"kind":"arxiv","id":"2209.13321","version":1},"attestation_state":"computed","paper":{"title":"A panchromatic view of infrared quasars: excess star formation and radio emission in the most heavily obscured systems","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Agnese Del Moro, Andrea Lapi, Antonis Georgakakis, Brivael Laloux, Carolina Andonie, Carolin Villforth, Chris Harrison, David M. Alexander, David Rosario, Francesco Shankar, Gabriela Calistro Rivera, Grayson Petter, James Petley, Leah K. Morabito, Mathilda Avirett-Mackenzie, Sotiria Fotopoulou","submitted_at":"2022-09-27T11:54:17Z","abstract_excerpt":"To understand the Active Galactic Nuclei (AGN) phenomenon and their impact on the evolution of galaxies, a complete AGN census is required; however, finding heavily obscured AGNs is observationally challenging. Here we use the deep and extensive multi-wavelength data in the COSMOS field to select a complete sample of 578 infrared (IR) quasars ($L_{\\rm AGN,IR}>10^{45}\\rm \\: erg\\: s^{-1}$) at $z<3$, with minimal obscuration bias, using detailed UV-to-far IR spectral energy distribution (SED) fitting. We complement our SED constraints with X-ray and radio observations to further investigate the p"},"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":"2209.13321","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2022-09-27T11:54:17Z","cross_cats_sorted":[],"title_canon_sha256":"58c8a3b0297aeb1643279e6d09cb077c6ee0266e6d789d6026b027f8d46e5f2e","abstract_canon_sha256":"6bb82b461c5a6430e431370bceaa334f5202ea3c1e6759c5ced1c6815f47686c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:05:09.803032Z","signature_b64":"Jp8dzor2r6EHqFqNl/LWqBPilxGQNErff4gGakkbE4rKqLdhkw5v/t5Q/BdNpmP0cYO3PY7cl5b7VtYjlGkwAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"145778fabf208af5d560b55d0d3974789caca30fd9c59db859d775f1ceff2650","last_reissued_at":"2026-07-05T05:05:09.802464Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:05:09.802464Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A panchromatic view of infrared quasars: excess star formation and radio emission in the most heavily obscured systems","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Agnese Del Moro, Andrea Lapi, Antonis Georgakakis, Brivael Laloux, Carolina Andonie, Carolin Villforth, Chris Harrison, David M. Alexander, David Rosario, Francesco Shankar, Gabriela Calistro Rivera, Grayson Petter, James Petley, Leah K. Morabito, Mathilda Avirett-Mackenzie, Sotiria Fotopoulou","submitted_at":"2022-09-27T11:54:17Z","abstract_excerpt":"To understand the Active Galactic Nuclei (AGN) phenomenon and their impact on the evolution of galaxies, a complete AGN census is required; however, finding heavily obscured AGNs is observationally challenging. Here we use the deep and extensive multi-wavelength data in the COSMOS field to select a complete sample of 578 infrared (IR) quasars ($L_{\\rm AGN,IR}>10^{45}\\rm \\: erg\\: s^{-1}$) at $z<3$, with minimal obscuration bias, using detailed UV-to-far IR spectral energy distribution (SED) fitting. We complement our SED constraints with X-ray and radio observations to further investigate the p"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2209.13321","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/2209.13321/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":"2209.13321","created_at":"2026-07-05T05:05:09.802521+00:00"},{"alias_kind":"arxiv_version","alias_value":"2209.13321v1","created_at":"2026-07-05T05:05:09.802521+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2209.13321","created_at":"2026-07-05T05:05:09.802521+00:00"},{"alias_kind":"pith_short_12","alias_value":"CRLXR6V7ECFP","created_at":"2026-07-05T05:05:09.802521+00:00"},{"alias_kind":"pith_short_16","alias_value":"CRLXR6V7ECFPLVLA","created_at":"2026-07-05T05:05:09.802521+00:00"},{"alias_kind":"pith_short_8","alias_value":"CRLXR6V7","created_at":"2026-07-05T05:05:09.802521+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.00105","citing_title":"AGN radiative feedback as the main regulator of [O III] outflow activity and obscuration in X-ray AGN","ref_index":224,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC","json":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC.json","graph_json":"https://pith.science/api/pith-number/CRLXR6V7ECFPLVLAWVOQ2OLUPC/graph.json","events_json":"https://pith.science/api/pith-number/CRLXR6V7ECFPLVLAWVOQ2OLUPC/events.json","paper":"https://pith.science/paper/CRLXR6V7"},"agent_actions":{"view_html":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC","download_json":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC.json","view_paper":"https://pith.science/paper/CRLXR6V7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2209.13321&json=true","fetch_graph":"https://pith.science/api/pith-number/CRLXR6V7ECFPLVLAWVOQ2OLUPC/graph.json","fetch_events":"https://pith.science/api/pith-number/CRLXR6V7ECFPLVLAWVOQ2OLUPC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC/action/storage_attestation","attest_author":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC/action/author_attestation","sign_citation":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC/action/citation_signature","submit_replication":"https://pith.science/pith/CRLXR6V7ECFPLVLAWVOQ2OLUPC/action/replication_record"}},"created_at":"2026-07-05T05:05:09.802521+00:00","updated_at":"2026-07-05T05:05:09.802521+00:00"}