{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:CZSGSTS7FUWTUUWRA44274JYGZ","short_pith_number":"pith:CZSGSTS7","schema_version":"1.0","canonical_sha256":"1664694e5f2d2d3a52d10739aff138365d7e23f5e16b82a1a276fd7bea57d0f1","source":{"kind":"arxiv","id":"1003.4271","version":1},"attestation_state":"computed","paper":{"title":"No Evolution in the IR-Radio Relation for IR-Luminous Galaxies at z<2 in the COSMOS Field","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"C. L. Carilli, D. B. Sanders, D. T. Frayer, E. Le Floc'h, E. Murphy, E. Schinnerer, G. Helou, H. Aussel, J. Kartaltepe, Mark T. Sargent, M. Salvato, O. Ilbert, P. Oesch, V. Smolcic","submitted_at":"2010-03-22T20:28:53Z","abstract_excerpt":"Previous observational studies of the infrared (IR)-radio relation out to high redshift employed any detectable star forming systems at a given redshift within the restricted area of cosmological survey fields. Consequently, the evolution inferred relies on a comparison between the average IR/radio properties of (i) very IR-luminous high-z sources and (ii) more heterogeneous low(er)-z samples that often lack the strongest IR emitters. In this report we consider populations of objects with comparable luminosities over the last 10 Gyr by taking advantage of deep IR (esp. Spitzer 24 micron) and V"},"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":"1003.4271","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2010-03-22T20:28:53Z","cross_cats_sorted":[],"title_canon_sha256":"d3c9d290eb97861b1c54c1109e9dceca14f8f976b3e3a70cd2e3a0a776246930","abstract_canon_sha256":"a970b01a49bd9cb159240d27db0796d866415d605e098bee1b0b884513ddba31"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:08:24.435583Z","signature_b64":"bRN98t2h7EQrSMDVuZt4CCh57rqYXfNxf8DhAbi12U7v2oZA48EvG/idbjXrh2JQO2UoxdDwyjI+Bgyt2P4GCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1664694e5f2d2d3a52d10739aff138365d7e23f5e16b82a1a276fd7bea57d0f1","last_reissued_at":"2026-05-18T02:08:24.434724Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:08:24.434724Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"No Evolution in the IR-Radio Relation for IR-Luminous Galaxies at z<2 in the COSMOS Field","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"C. L. Carilli, D. B. Sanders, D. T. Frayer, E. Le Floc'h, E. Murphy, E. Schinnerer, G. Helou, H. Aussel, J. Kartaltepe, Mark T. Sargent, M. Salvato, O. Ilbert, P. Oesch, V. Smolcic","submitted_at":"2010-03-22T20:28:53Z","abstract_excerpt":"Previous observational studies of the infrared (IR)-radio relation out to high redshift employed any detectable star forming systems at a given redshift within the restricted area of cosmological survey fields. Consequently, the evolution inferred relies on a comparison between the average IR/radio properties of (i) very IR-luminous high-z sources and (ii) more heterogeneous low(er)-z samples that often lack the strongest IR emitters. In this report we consider populations of objects with comparable luminosities over the last 10 Gyr by taking advantage of deep IR (esp. Spitzer 24 micron) and V"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1003.4271","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":"1003.4271","created_at":"2026-05-18T02:08:24.434867+00:00"},{"alias_kind":"arxiv_version","alias_value":"1003.4271v1","created_at":"2026-05-18T02:08:24.434867+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1003.4271","created_at":"2026-05-18T02:08:24.434867+00:00"},{"alias_kind":"pith_short_12","alias_value":"CZSGSTS7FUWT","created_at":"2026-05-18T12:26:06.534383+00:00"},{"alias_kind":"pith_short_16","alias_value":"CZSGSTS7FUWTUUWR","created_at":"2026-05-18T12:26:06.534383+00:00"},{"alias_kind":"pith_short_8","alias_value":"CZSGSTS7","created_at":"2026-05-18T12:26:06.534383+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.19658","citing_title":"The PARADIGM Project II: Characterising Nuclear and Diffuse Radio Components in Local U/LIRGs","ref_index":300,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ","json":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ.json","graph_json":"https://pith.science/api/pith-number/CZSGSTS7FUWTUUWRA44274JYGZ/graph.json","events_json":"https://pith.science/api/pith-number/CZSGSTS7FUWTUUWRA44274JYGZ/events.json","paper":"https://pith.science/paper/CZSGSTS7"},"agent_actions":{"view_html":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ","download_json":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ.json","view_paper":"https://pith.science/paper/CZSGSTS7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1003.4271&json=true","fetch_graph":"https://pith.science/api/pith-number/CZSGSTS7FUWTUUWRA44274JYGZ/graph.json","fetch_events":"https://pith.science/api/pith-number/CZSGSTS7FUWTUUWRA44274JYGZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ/action/storage_attestation","attest_author":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ/action/author_attestation","sign_citation":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ/action/citation_signature","submit_replication":"https://pith.science/pith/CZSGSTS7FUWTUUWRA44274JYGZ/action/replication_record"}},"created_at":"2026-05-18T02:08:24.434867+00:00","updated_at":"2026-05-18T02:08:24.434867+00:00"}