{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:PUHWNB2ZGBAJ2RNHWFO4O6XHQX","short_pith_number":"pith:PUHWNB2Z","schema_version":"1.0","canonical_sha256":"7d0f66875930409d45a7b15dc77ae785de88aedf64939e7b417e4a0db5a2ce9e","source":{"kind":"arxiv","id":"2411.08104","version":1},"attestation_state":"computed","paper":{"title":"Radio-AGN activity across the galaxy population: dependence on stellar mass, star-formation rate, and redshift","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"A. L. Patrick, B. Mingo, C. Tasse, D. J. B. Smith, G. K. Miley, H. J. A. R\\\"ottgering, I. Prandoni, K. J. Duncan, K. Ma{\\l}ek, M. I. Arnaudova, M. J. Hardcastle, M. Magliocchetti, P. Haskell, P. N. Best, R. K. Cochrane, R. Kondapally, S. Das, T. Holc, W. L. Williams","submitted_at":"2024-11-12T19:00:01Z","abstract_excerpt":"We characterise the co-evolution of radio-loud AGN and their galaxies by mapping the dependence of radio-loud AGN activity on stellar mass and star-formation rate (SFR) across cosmic time (out to $z \\sim 1.5$). Deep LOFAR radio observations are combined with large galaxy samples to study the incidence of radio-loud AGN across the galaxy population; the AGN are further split into low-excitation radio galaxies (LERGs) and high-excitation radio galaxies (HERGs). We find that LERG activity occurs over a wide range of SFRs, whereas HERGs are typically found in galaxies with ongoing star formation. "},"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":"2411.08104","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2024-11-12T19:00:01Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"1c0fe9f5e78aec673f6a4ddefb49d889cbaf1bd39c38d4457a60916b672386ff","abstract_canon_sha256":"d0369877f2b4cd647adc335d54ee35276dbc6a8f2e6e564dd41508d66d9f6be0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:34:41.567306Z","signature_b64":"8ZNPaGJotsOaIiMKe65kFJzhYVRgSSBZiWkkn2doH+ccSCETWZlH7/1Scewtibj0DVb54qRUICcuMt9bF0pDCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7d0f66875930409d45a7b15dc77ae785de88aedf64939e7b417e4a0db5a2ce9e","last_reissued_at":"2026-07-05T09:34:41.566797Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:34:41.566797Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Radio-AGN activity across the galaxy population: dependence on stellar mass, star-formation rate, and redshift","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"A. L. Patrick, B. Mingo, C. Tasse, D. J. B. Smith, G. K. Miley, H. J. A. R\\\"ottgering, I. Prandoni, K. J. Duncan, K. Ma{\\l}ek, M. I. Arnaudova, M. J. Hardcastle, M. Magliocchetti, P. Haskell, P. N. Best, R. K. Cochrane, R. Kondapally, S. Das, T. Holc, W. L. Williams","submitted_at":"2024-11-12T19:00:01Z","abstract_excerpt":"We characterise the co-evolution of radio-loud AGN and their galaxies by mapping the dependence of radio-loud AGN activity on stellar mass and star-formation rate (SFR) across cosmic time (out to $z \\sim 1.5$). Deep LOFAR radio observations are combined with large galaxy samples to study the incidence of radio-loud AGN across the galaxy population; the AGN are further split into low-excitation radio galaxies (LERGs) and high-excitation radio galaxies (HERGs). We find that LERG activity occurs over a wide range of SFRs, whereas HERGs are typically found in galaxies with ongoing star formation. "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2411.08104","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/2411.08104/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":"2411.08104","created_at":"2026-07-05T09:34:41.566862+00:00"},{"alias_kind":"arxiv_version","alias_value":"2411.08104v1","created_at":"2026-07-05T09:34:41.566862+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2411.08104","created_at":"2026-07-05T09:34:41.566862+00:00"},{"alias_kind":"pith_short_12","alias_value":"PUHWNB2ZGBAJ","created_at":"2026-07-05T09:34:41.566862+00:00"},{"alias_kind":"pith_short_16","alias_value":"PUHWNB2ZGBAJ2RNH","created_at":"2026-07-05T09:34:41.566862+00:00"},{"alias_kind":"pith_short_8","alias_value":"PUHWNB2Z","created_at":"2026-07-05T09:34:41.566862+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07818","citing_title":"The DESI View of the Faint Radio Source Population in LoTSS DR2","ref_index":53,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX","json":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX.json","graph_json":"https://pith.science/api/pith-number/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/graph.json","events_json":"https://pith.science/api/pith-number/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/events.json","paper":"https://pith.science/paper/PUHWNB2Z"},"agent_actions":{"view_html":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX","download_json":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX.json","view_paper":"https://pith.science/paper/PUHWNB2Z","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2411.08104&json=true","fetch_graph":"https://pith.science/api/pith-number/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/graph.json","fetch_events":"https://pith.science/api/pith-number/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/action/storage_attestation","attest_author":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/action/author_attestation","sign_citation":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/action/citation_signature","submit_replication":"https://pith.science/pith/PUHWNB2ZGBAJ2RNHWFO4O6XHQX/action/replication_record"}},"created_at":"2026-07-05T09:34:41.566862+00:00","updated_at":"2026-07-05T09:34:41.566862+00:00"}