{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:IXRUY4NAKFMS3HSFWYXHBYWBFX","short_pith_number":"pith:IXRUY4NA","schema_version":"1.0","canonical_sha256":"45e34c71a051592d9e45b62e70e2c12ddde6e0e043bbd6e9cd459ba08a94a0e2","source":{"kind":"arxiv","id":"1912.00934","version":1},"attestation_state":"computed","paper":{"title":"Cosmic evolution of star-forming galaxies to $z \\simeq 1.8$ in the faint low-frequency radio source population","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. R. Taylor, C.H. Ishwara-Chandra, C. Mancuso, E. F. Ocran, I. Prandoni, M. Prescott, M. Vaccari","submitted_at":"2019-12-02T17:01:31Z","abstract_excerpt":"We study the properties of star-forming galaxies selected at 610 MHz with the GMRT in a survey covering $\\sim$1.86 deg$^2$ down to a noise of $\\sim$7.1\\,$\\mu$Jy / beam. These were identified by combining multiple classification diagnostics: optical, X-ray, infrared and radio data.\n  Of the 1685 SFGs from the GMRT sample, 496 have spectroscopic redshifts whereas 1189 have photometric redshifts. We find that the IRRC of star-forming galaxies, quantified by the infrared-to-1.4 GHz radio luminosity ratio $\\rm{q_{IR}}$, decreases with increasing redshift: $\\rm{q_{IR}\\,=\\,2.86\\pm0.04(1\\,+\\,z)^{-0.20"},"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":"1912.00934","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2019-12-02T17:01:31Z","cross_cats_sorted":[],"title_canon_sha256":"29590e75b89517582798513159ad31de168c90623560dd090f97bfbc1de7eb87","abstract_canon_sha256":"1e5a7b6b8ea493d5dcf77adaf2c7c31e68a4b0b0e225a17c721cc7fbfaabec97"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:31:34.710916Z","signature_b64":"kSKUKxFVdRkfsIJsUBOrh0C5pfSujmJTJPoJdGsgvGnqPQ4MRTMtRju5mUiH4KHk+dd7cDXrQdr5DSVkLM+kBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"45e34c71a051592d9e45b62e70e2c12ddde6e0e043bbd6e9cd459ba08a94a0e2","last_reissued_at":"2026-07-05T00:31:34.710564Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:31:34.710564Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cosmic evolution of star-forming galaxies to $z \\simeq 1.8$ in the faint low-frequency radio source population","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. R. Taylor, C.H. Ishwara-Chandra, C. Mancuso, E. F. Ocran, I. Prandoni, M. Prescott, M. Vaccari","submitted_at":"2019-12-02T17:01:31Z","abstract_excerpt":"We study the properties of star-forming galaxies selected at 610 MHz with the GMRT in a survey covering $\\sim$1.86 deg$^2$ down to a noise of $\\sim$7.1\\,$\\mu$Jy / beam. These were identified by combining multiple classification diagnostics: optical, X-ray, infrared and radio data.\n  Of the 1685 SFGs from the GMRT sample, 496 have spectroscopic redshifts whereas 1189 have photometric redshifts. We find that the IRRC of star-forming galaxies, quantified by the infrared-to-1.4 GHz radio luminosity ratio $\\rm{q_{IR}}$, decreases with increasing redshift: $\\rm{q_{IR}\\,=\\,2.86\\pm0.04(1\\,+\\,z)^{-0.20"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1912.00934","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/1912.00934/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":"1912.00934","created_at":"2026-07-05T00:31:34.710625+00:00"},{"alias_kind":"arxiv_version","alias_value":"1912.00934v1","created_at":"2026-07-05T00:31:34.710625+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1912.00934","created_at":"2026-07-05T00:31:34.710625+00:00"},{"alias_kind":"pith_short_12","alias_value":"IXRUY4NAKFMS","created_at":"2026-07-05T00:31:34.710625+00:00"},{"alias_kind":"pith_short_16","alias_value":"IXRUY4NAKFMS3HSF","created_at":"2026-07-05T00:31:34.710625+00:00"},{"alias_kind":"pith_short_8","alias_value":"IXRUY4NA","created_at":"2026-07-05T00:31:34.710625+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"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":103,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX","json":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX.json","graph_json":"https://pith.science/api/pith-number/IXRUY4NAKFMS3HSFWYXHBYWBFX/graph.json","events_json":"https://pith.science/api/pith-number/IXRUY4NAKFMS3HSFWYXHBYWBFX/events.json","paper":"https://pith.science/paper/IXRUY4NA"},"agent_actions":{"view_html":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX","download_json":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX.json","view_paper":"https://pith.science/paper/IXRUY4NA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1912.00934&json=true","fetch_graph":"https://pith.science/api/pith-number/IXRUY4NAKFMS3HSFWYXHBYWBFX/graph.json","fetch_events":"https://pith.science/api/pith-number/IXRUY4NAKFMS3HSFWYXHBYWBFX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX/action/storage_attestation","attest_author":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX/action/author_attestation","sign_citation":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX/action/citation_signature","submit_replication":"https://pith.science/pith/IXRUY4NAKFMS3HSFWYXHBYWBFX/action/replication_record"}},"created_at":"2026-07-05T00:31:34.710625+00:00","updated_at":"2026-07-05T00:31:34.710625+00:00"}