{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:ULZWGXBFS6I6JZXQ3UQTYALAFE","short_pith_number":"pith:ULZWGXBF","schema_version":"1.0","canonical_sha256":"a2f3635c259791e4e6f0dd213c016029020befa7f83d7960a3abf24b2d5aa4d7","source":{"kind":"arxiv","id":"1211.6440","version":1},"attestation_state":"computed","paper":{"title":"Herschel-ATLAS/GAMA: a difference between star-formation rates in strong-line and weak-line radio galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Cooray, A. Dariush, A. S. G. Robotham, D. J. B. Smith, D. Thomas, E. E. Rigby, E. M. Sadler, E. Valiante, G. de Zotti, I. K. Baldry, J. A. Stevens, J. H. Y. Ching, J. Liske, J. S. Virdee, L. Dunne, M. Baes, M. J. Hardcastle, M. J. Jarvis, M. J. Michalowski, O. Steele, R. Hopwood, S. Brough, S. Driver, S. Dye, S. Eales, S. Maddox, S. M. Croom, T. Mauch","submitted_at":"2012-11-27T21:00:24Z","abstract_excerpt":"We have constructed a sample of radio-loud objects with optical spectroscopy from the Galaxy and Mass Assembly (GAMA) project over the Herschel-ATLAS Phase 1 fields. Classifying the radio sources in terms of their optical spectra, we find that strong-emission-line sources (`high-excitation radio galaxies') have, on average, a factor ~4 higher 250-micron Herschel luminosity than weak-line (`low-excitation') radio galaxies and are also more luminous than magnitude-matched radio-quiet galaxies at the same redshift. Using all five H-ATLAS bands, we show that this difference in luminosity between t"},"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":"1211.6440","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-11-27T21:00:24Z","cross_cats_sorted":[],"title_canon_sha256":"01c4426fa6af9b8cae358ae98aea6cb02a3d54718ce6d877402de783a218de43","abstract_canon_sha256":"a2d9d3ba13e8cce9a69609b5ec4f570ed6c80502771abb2a39e85a06c675c2ac"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:52:54.169091Z","signature_b64":"izvFGBfy8G4aIyxpkJxyNyo79mRCe3q7FPm1Qb8vmHiy7ZiswLMZv+V+07AOb6SzB6aAV7Lu5gtZk/LhjEu7Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a2f3635c259791e4e6f0dd213c016029020befa7f83d7960a3abf24b2d5aa4d7","last_reissued_at":"2026-05-18T01:52:54.168446Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:52:54.168446Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Herschel-ATLAS/GAMA: a difference between star-formation rates in strong-line and weak-line radio galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Cooray, A. Dariush, A. S. G. Robotham, D. J. B. Smith, D. Thomas, E. E. Rigby, E. M. Sadler, E. Valiante, G. de Zotti, I. K. Baldry, J. A. Stevens, J. H. Y. Ching, J. Liske, J. S. Virdee, L. Dunne, M. Baes, M. J. Hardcastle, M. J. Jarvis, M. J. Michalowski, O. Steele, R. Hopwood, S. Brough, S. Driver, S. Dye, S. Eales, S. Maddox, S. M. Croom, T. Mauch","submitted_at":"2012-11-27T21:00:24Z","abstract_excerpt":"We have constructed a sample of radio-loud objects with optical spectroscopy from the Galaxy and Mass Assembly (GAMA) project over the Herschel-ATLAS Phase 1 fields. Classifying the radio sources in terms of their optical spectra, we find that strong-emission-line sources (`high-excitation radio galaxies') have, on average, a factor ~4 higher 250-micron Herschel luminosity than weak-line (`low-excitation') radio galaxies and are also more luminous than magnitude-matched radio-quiet galaxies at the same redshift. Using all five H-ATLAS bands, we show that this difference in luminosity between t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1211.6440","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":"1211.6440","created_at":"2026-05-18T01:52:54.168568+00:00"},{"alias_kind":"arxiv_version","alias_value":"1211.6440v1","created_at":"2026-05-18T01:52:54.168568+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1211.6440","created_at":"2026-05-18T01:52:54.168568+00:00"},{"alias_kind":"pith_short_12","alias_value":"ULZWGXBFS6I6","created_at":"2026-05-18T12:27:23.164592+00:00"},{"alias_kind":"pith_short_16","alias_value":"ULZWGXBFS6I6JZXQ","created_at":"2026-05-18T12:27:23.164592+00:00"},{"alias_kind":"pith_short_8","alias_value":"ULZWGXBF","created_at":"2026-05-18T12:27:23.164592+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE","json":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE.json","graph_json":"https://pith.science/api/pith-number/ULZWGXBFS6I6JZXQ3UQTYALAFE/graph.json","events_json":"https://pith.science/api/pith-number/ULZWGXBFS6I6JZXQ3UQTYALAFE/events.json","paper":"https://pith.science/paper/ULZWGXBF"},"agent_actions":{"view_html":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE","download_json":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE.json","view_paper":"https://pith.science/paper/ULZWGXBF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1211.6440&json=true","fetch_graph":"https://pith.science/api/pith-number/ULZWGXBFS6I6JZXQ3UQTYALAFE/graph.json","fetch_events":"https://pith.science/api/pith-number/ULZWGXBFS6I6JZXQ3UQTYALAFE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE/action/storage_attestation","attest_author":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE/action/author_attestation","sign_citation":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE/action/citation_signature","submit_replication":"https://pith.science/pith/ULZWGXBFS6I6JZXQ3UQTYALAFE/action/replication_record"}},"created_at":"2026-05-18T01:52:54.168568+00:00","updated_at":"2026-05-18T01:52:54.168568+00:00"}