{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1998:YNDQYPVSHUFOTBIYC6VUAHM7DR","short_pith_number":"pith:YNDQYPVS","schema_version":"1.0","canonical_sha256":"c3470c3eb23d0ae9851817ab401d9f1c7a62012c99a65871bd039361c3652358","source":{"kind":"arxiv","id":"astro-ph/9805327","version":1},"attestation_state":"computed","paper":{"title":"Star Formation Rates in Faint Radio Galaxies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Hopkins, B. Mobasher, L. Cram, M. Rowan-Robinson","submitted_at":"1998-05-27T03:16:07Z","abstract_excerpt":"The decimetric radio continuum luminosity of a star-forming galaxy appears to be directly proportional to the rate of formation of supernovae in the galaxy. Since decimetric radiation does not suffer significant extinction and is not directive, radio luminosities may thus provide a particularly straightforward way to determine the current rate of star formation. Using a sample of over 700 local galaxies we confirm the utility of the radio luminosity as a measure of star formation rate by showing concordance with the rates predicted by U-band, H-alpha, and far-infrared luminosites. We also show"},"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/9805327","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1998-05-27T03:16:07Z","cross_cats_sorted":[],"title_canon_sha256":"54a8fea3be0ae902f036e39c78c5929c250688597068ce32c4fe9b5402f19bd0","abstract_canon_sha256":"870138e453a096cf9e33984cd62031f98885678112ba2d7abc807ab378b88f3b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:51:57.244096Z","signature_b64":"wyiRHZQ6IDEdH+K6RG4AGUkoLROsD1n3AbP2EXs8UM+uf6z/ZDSePcNc/6M7ivBXGrVVg0jtrD5bk1b2a6pBAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c3470c3eb23d0ae9851817ab401d9f1c7a62012c99a65871bd039361c3652358","last_reissued_at":"2026-07-04T15:51:57.243717Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:51:57.243717Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Star Formation Rates in Faint Radio Galaxies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Hopkins, B. Mobasher, L. Cram, M. Rowan-Robinson","submitted_at":"1998-05-27T03:16:07Z","abstract_excerpt":"The decimetric radio continuum luminosity of a star-forming galaxy appears to be directly proportional to the rate of formation of supernovae in the galaxy. Since decimetric radiation does not suffer significant extinction and is not directive, radio luminosities may thus provide a particularly straightforward way to determine the current rate of star formation. Using a sample of over 700 local galaxies we confirm the utility of the radio luminosity as a measure of star formation rate by showing concordance with the rates predicted by U-band, H-alpha, and far-infrared luminosites. We also show"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9805327","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/9805327/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/9805327","created_at":"2026-07-04T15:51:57.243780+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9805327v1","created_at":"2026-07-04T15:51:57.243780+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9805327","created_at":"2026-07-04T15:51:57.243780+00:00"},{"alias_kind":"pith_short_12","alias_value":"YNDQYPVSHUFO","created_at":"2026-07-04T15:51:57.243780+00:00"},{"alias_kind":"pith_short_16","alias_value":"YNDQYPVSHUFOTBIY","created_at":"2026-07-04T15:51:57.243780+00:00"},{"alias_kind":"pith_short_8","alias_value":"YNDQYPVS","created_at":"2026-07-04T15:51:57.243780+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03543","citing_title":"A MIGHTEE robust measurement of the star formation rate-radio correlation","ref_index":63,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR","json":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR.json","graph_json":"https://pith.science/api/pith-number/YNDQYPVSHUFOTBIYC6VUAHM7DR/graph.json","events_json":"https://pith.science/api/pith-number/YNDQYPVSHUFOTBIYC6VUAHM7DR/events.json","paper":"https://pith.science/paper/YNDQYPVS"},"agent_actions":{"view_html":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR","download_json":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR.json","view_paper":"https://pith.science/paper/YNDQYPVS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9805327&json=true","fetch_graph":"https://pith.science/api/pith-number/YNDQYPVSHUFOTBIYC6VUAHM7DR/graph.json","fetch_events":"https://pith.science/api/pith-number/YNDQYPVSHUFOTBIYC6VUAHM7DR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR/action/storage_attestation","attest_author":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR/action/author_attestation","sign_citation":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR/action/citation_signature","submit_replication":"https://pith.science/pith/YNDQYPVSHUFOTBIYC6VUAHM7DR/action/replication_record"}},"created_at":"2026-07-04T15:51:57.243780+00:00","updated_at":"2026-07-04T15:51:57.243780+00:00"}