{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:2K2HZIGQCO5QMKGWBRWMTLVCXW","short_pith_number":"pith:2K2HZIGQ","schema_version":"1.0","canonical_sha256":"d2b47ca0d013bb0628d60c6cc9aea2bd9452178fb14760f75900ab0e4839de76","source":{"kind":"arxiv","id":"1106.0757","version":2},"attestation_state":"computed","paper":{"title":"The current star formation rate of K+A galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Danielle Nielsen (Wisconsin), Hawaii), Roberto De Propris (CTIO), Susan E. Ridgway (CTIO), Tomotsugu Goto (ifa","submitted_at":"2011-06-03T20:14:52Z","abstract_excerpt":"We derive the stacked 1.4 GHz flux from FIRST (Faint Images of the Radio Sky at Twenty Centimeters) survey for 811 K+A galaxies selected from the SDSS DR7. For these objects we find a mean flux density of $56\\pm 9$ $\\mu$Jy. A similar stack of radio-quiet white dwarfs yields an upper limit of 43 $\\mu$Jy at a 5$\\sigma$ significance to the flux in blank regions of the sky. This implies an average star formation rate of 1.6 $\\pm$ 0.3 M$_{\\odot}$ year$^{-1}$ for K+A galaxies. However the majority of the signal comes from $\\sim$4% of K+A fields that have aperture fluxes above the $5\\sigma$ noise lev"},"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":"1106.0757","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2011-06-03T20:14:52Z","cross_cats_sorted":[],"title_canon_sha256":"920ae7297394bc8176a846881266efe542d57b4abcac6bc4b751175a0602709f","abstract_canon_sha256":"277b188e9c084be76c6eb49a1c010cf6e5404d484a94152d7be1dd8c67a83533"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:01:42.180525Z","signature_b64":"0izX3U/XOc7PzsBdIczWgNrsWHlPkY2O12XTrK6eTWs13SyUQ7OKRYSTF8iizemK3wHpBSSEC5oUh2bI/vTUBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d2b47ca0d013bb0628d60c6cc9aea2bd9452178fb14760f75900ab0e4839de76","last_reissued_at":"2026-05-18T02:01:42.180001Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:01:42.180001Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The current star formation rate of K+A galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Danielle Nielsen (Wisconsin), Hawaii), Roberto De Propris (CTIO), Susan E. Ridgway (CTIO), Tomotsugu Goto (ifa","submitted_at":"2011-06-03T20:14:52Z","abstract_excerpt":"We derive the stacked 1.4 GHz flux from FIRST (Faint Images of the Radio Sky at Twenty Centimeters) survey for 811 K+A galaxies selected from the SDSS DR7. For these objects we find a mean flux density of $56\\pm 9$ $\\mu$Jy. A similar stack of radio-quiet white dwarfs yields an upper limit of 43 $\\mu$Jy at a 5$\\sigma$ significance to the flux in blank regions of the sky. This implies an average star formation rate of 1.6 $\\pm$ 0.3 M$_{\\odot}$ year$^{-1}$ for K+A galaxies. However the majority of the signal comes from $\\sim$4% of K+A fields that have aperture fluxes above the $5\\sigma$ noise lev"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1106.0757","kind":"arxiv","version":2},"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":"1106.0757","created_at":"2026-05-18T02:01:42.180084+00:00"},{"alias_kind":"arxiv_version","alias_value":"1106.0757v2","created_at":"2026-05-18T02:01:42.180084+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1106.0757","created_at":"2026-05-18T02:01:42.180084+00:00"},{"alias_kind":"pith_short_12","alias_value":"2K2HZIGQCO5Q","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_16","alias_value":"2K2HZIGQCO5QMKGW","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_8","alias_value":"2K2HZIGQ","created_at":"2026-05-18T12:26:18.847500+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/2K2HZIGQCO5QMKGWBRWMTLVCXW","json":"https://pith.science/pith/2K2HZIGQCO5QMKGWBRWMTLVCXW.json","graph_json":"https://pith.science/api/pith-number/2K2HZIGQCO5QMKGWBRWMTLVCXW/graph.json","events_json":"https://pith.science/api/pith-number/2K2HZIGQCO5QMKGWBRWMTLVCXW/events.json","paper":"https://pith.science/paper/2K2HZIGQ"},"agent_actions":{"view_html":"https://pith.science/pith/2K2HZIGQCO5QMKGWBRWMTLVCXW","download_json":"https://pith.science/pith/2K2HZIGQCO5QMKGWBRWMTLVCXW.json","view_paper":"https://pith.science/paper/2K2HZIGQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1106.0757&json=true","fetch_graph":"https://pith.science/api/pith-number/2K2HZIGQCO5QMKGWBRWMTLVCXW/graph.json","fetch_events":"https://pith.science/api/pith-number/2K2HZIGQCO5QMKGWBRWMTLVCXW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2K2HZIGQCO5QMKGWBRWMTLVCXW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2K2HZIGQCO5QMKGWBRWMTLVCXW/action/storage_attestation","attest_author":"https://pith.science/pith/2K2HZIGQCO5QMKGWBRWMTLVCXW/action/author_attestation","sign_citation":"https://pith.science/pith/2K2HZIGQCO5QMKGWBRWMTLVCXW/action/citation_signature","submit_replication":"https://pith.science/pith/2K2HZIGQCO5QMKGWBRWMTLVCXW/action/replication_record"}},"created_at":"2026-05-18T02:01:42.180084+00:00","updated_at":"2026-05-18T02:01:42.180084+00:00"}