{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:WUOIAJAAX6WHIWE37M75Y6OANF","short_pith_number":"pith:WUOIAJAA","schema_version":"1.0","canonical_sha256":"b51c802400bfac74589bfb3fdc79c0697c8ea366a16a64d3ae6af1069fed5f50","source":{"kind":"arxiv","id":"astro-ph/0212121","version":1},"attestation_state":"computed","paper":{"title":"Estimating Star Formation Rates from Infrared and Radio Luminosities: The Origin of the Radio-Infrared Correlation","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Eric F. Bell (MPIA, Heidelberg)","submitted_at":"2002-12-05T07:37:24Z","abstract_excerpt":"I have assembled a diverse sample of galaxies from the literature with far-ultraviolet (FUV), optical, infrared (IR) and radio luminosities to explore the calibration of radio-derived and IR-derived star formation (SF) rates, and the origin of the radio-IR correlation. By comparing the 8-1000 micron IR, which samples dust-reprocessed starlight, with direct stellar FUV emission, I show that the IR traces most of the SF in luminous L* galaxies but traces only a small fraction of the SF in faint ~0.01 L* galaxies. If radio emission were a perfect SF rate indicator, this effect would cause easily "},"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":"astro-ph/0212121","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2002-12-05T07:37:24Z","cross_cats_sorted":[],"title_canon_sha256":"83cce92f46fb4dfe9b3503eddea2310525a8dc7d4b94db143cc25488e9ab7ea6","abstract_canon_sha256":"3f06bbcb77843ef1787ef009176424434c7d0d9e478d9cb9ea5419d01ec7ff8d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:31:21.636526Z","signature_b64":"Sj04f546pzzZ7T/iAeUBoGYIJCcUNyiqI1edM4qc1IzG3PAwNq0fX7Qih5ko8mvOMy2jxfeOn6Pz6vqYlfiyAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b51c802400bfac74589bfb3fdc79c0697c8ea366a16a64d3ae6af1069fed5f50","last_reissued_at":"2026-07-04T16:31:21.636089Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:31:21.636089Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Estimating Star Formation Rates from Infrared and Radio Luminosities: The Origin of the Radio-Infrared Correlation","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Eric F. Bell (MPIA, Heidelberg)","submitted_at":"2002-12-05T07:37:24Z","abstract_excerpt":"I have assembled a diverse sample of galaxies from the literature with far-ultraviolet (FUV), optical, infrared (IR) and radio luminosities to explore the calibration of radio-derived and IR-derived star formation (SF) rates, and the origin of the radio-IR correlation. By comparing the 8-1000 micron IR, which samples dust-reprocessed starlight, with direct stellar FUV emission, I show that the IR traces most of the SF in luminous L* galaxies but traces only a small fraction of the SF in faint ~0.01 L* galaxies. If radio emission were a perfect SF rate indicator, this effect would cause easily "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0212121","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/astro-ph/0212121/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":"astro-ph/0212121","created_at":"2026-07-04T16:31:21.636147+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0212121v1","created_at":"2026-07-04T16:31:21.636147+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0212121","created_at":"2026-07-04T16:31:21.636147+00:00"},{"alias_kind":"pith_short_12","alias_value":"WUOIAJAAX6WH","created_at":"2026-07-04T16:31:21.636147+00:00"},{"alias_kind":"pith_short_16","alias_value":"WUOIAJAAX6WHIWE3","created_at":"2026-07-04T16:31:21.636147+00:00"},{"alias_kind":"pith_short_8","alias_value":"WUOIAJAA","created_at":"2026-07-04T16:31:21.636147+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.06143","citing_title":"Deep far-UV observations of the ELAIS N1 field using AstroSat: Source catalogue, spectral energy distribution modelling and star formation","ref_index":73,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12254","citing_title":"Investigating the young stellar populations and hierarchies in nearby galaxies with the UVIT. II. Presenting the properties of ~25,000 UV-detected star-forming clumps","ref_index":86,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF","json":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF.json","graph_json":"https://pith.science/api/pith-number/WUOIAJAAX6WHIWE37M75Y6OANF/graph.json","events_json":"https://pith.science/api/pith-number/WUOIAJAAX6WHIWE37M75Y6OANF/events.json","paper":"https://pith.science/paper/WUOIAJAA"},"agent_actions":{"view_html":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF","download_json":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF.json","view_paper":"https://pith.science/paper/WUOIAJAA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0212121&json=true","fetch_graph":"https://pith.science/api/pith-number/WUOIAJAAX6WHIWE37M75Y6OANF/graph.json","fetch_events":"https://pith.science/api/pith-number/WUOIAJAAX6WHIWE37M75Y6OANF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF/action/storage_attestation","attest_author":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF/action/author_attestation","sign_citation":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF/action/citation_signature","submit_replication":"https://pith.science/pith/WUOIAJAAX6WHIWE37M75Y6OANF/action/replication_record"}},"created_at":"2026-07-04T16:31:21.636147+00:00","updated_at":"2026-07-04T16:31:21.636147+00:00"}