{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:WWUTGBEKQRUD32OGY7W2AO3DC3","short_pith_number":"pith:WWUTGBEK","schema_version":"1.0","canonical_sha256":"b5a933048a84683de9c6c7eda03b6316f71a5222b6e2e0e0fb41a53baf54d6f5","source":{"kind":"arxiv","id":"1810.04357","version":1},"attestation_state":"computed","paper":{"title":"The Slope of the Source-Count Distribution for Fast Radio Bursts","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"C. W. James, J.-P. Macquart, K. W. Bannister, R. D. Ekers, R. M. Shannon","submitted_at":"2018-10-10T04:00:38Z","abstract_excerpt":"The slope of the source-count distribution of fast radio burst (FRB) fluences, $\\alpha$, has been estimated using a variety of methods. Hampering all attempts have been the low number of detected FRBs, and the difficulty of defining a completeness threshold for FRB surveys. In this work, we extend maximum-likelihood methods for estimating $\\alpha$, using detected and threshold signal-to-noise ratios applied to all FRBs in a sample without regard to a completeness threshold. Using this method with FRBs detected by the Parkes radio telescope, we find $\\alpha=-1.18 \\pm 0.24$ (68\\% confidence inte"},"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":"1810.04357","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2018-10-10T04:00:38Z","cross_cats_sorted":[],"title_canon_sha256":"8ce4ca1a144ad19273379acea90527db4f8a5e6f13b28b82b49fc9a9df56b725","abstract_canon_sha256":"92f1f50c1316dd1a6cbaf49fb1bb1aa3a1df7833c1c28375a5644d6c70f8c75c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:59:49.186422Z","signature_b64":"wzy8MMMXhYGWmE9BeDiUFhfwwkO5/CRF6Kb9m9BqnuwRJ8goljyc3YN8KBIslDqArz3IJBOzdKWaAjFgujiTCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b5a933048a84683de9c6c7eda03b6316f71a5222b6e2e0e0fb41a53baf54d6f5","last_reissued_at":"2026-05-17T23:59:49.185971Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:59:49.185971Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Slope of the Source-Count Distribution for Fast Radio Bursts","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"C. W. James, J.-P. Macquart, K. W. Bannister, R. D. Ekers, R. M. Shannon","submitted_at":"2018-10-10T04:00:38Z","abstract_excerpt":"The slope of the source-count distribution of fast radio burst (FRB) fluences, $\\alpha$, has been estimated using a variety of methods. Hampering all attempts have been the low number of detected FRBs, and the difficulty of defining a completeness threshold for FRB surveys. In this work, we extend maximum-likelihood methods for estimating $\\alpha$, using detected and threshold signal-to-noise ratios applied to all FRBs in a sample without regard to a completeness threshold. Using this method with FRBs detected by the Parkes radio telescope, we find $\\alpha=-1.18 \\pm 0.24$ (68\\% confidence inte"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1810.04357","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":"1810.04357","created_at":"2026-05-17T23:59:49.186044+00:00"},{"alias_kind":"arxiv_version","alias_value":"1810.04357v1","created_at":"2026-05-17T23:59:49.186044+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1810.04357","created_at":"2026-05-17T23:59:49.186044+00:00"},{"alias_kind":"pith_short_12","alias_value":"WWUTGBEKQRUD","created_at":"2026-05-18T12:33:01.666342+00:00"},{"alias_kind":"pith_short_16","alias_value":"WWUTGBEKQRUD32OG","created_at":"2026-05-18T12:33:01.666342+00:00"},{"alias_kind":"pith_short_8","alias_value":"WWUTGBEK","created_at":"2026-05-18T12:33:01.666342+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21331","citing_title":"Searching for links between energetic millisecond pulsars and repeating fast radio bursts","ref_index":237,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3","json":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3.json","graph_json":"https://pith.science/api/pith-number/WWUTGBEKQRUD32OGY7W2AO3DC3/graph.json","events_json":"https://pith.science/api/pith-number/WWUTGBEKQRUD32OGY7W2AO3DC3/events.json","paper":"https://pith.science/paper/WWUTGBEK"},"agent_actions":{"view_html":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3","download_json":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3.json","view_paper":"https://pith.science/paper/WWUTGBEK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1810.04357&json=true","fetch_graph":"https://pith.science/api/pith-number/WWUTGBEKQRUD32OGY7W2AO3DC3/graph.json","fetch_events":"https://pith.science/api/pith-number/WWUTGBEKQRUD32OGY7W2AO3DC3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3/action/storage_attestation","attest_author":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3/action/author_attestation","sign_citation":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3/action/citation_signature","submit_replication":"https://pith.science/pith/WWUTGBEKQRUD32OGY7W2AO3DC3/action/replication_record"}},"created_at":"2026-05-17T23:59:49.186044+00:00","updated_at":"2026-05-17T23:59:49.186044+00:00"}