{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:2JKLAMMNXIIARFGIKMEHQJ4AF2","short_pith_number":"pith:2JKLAMMN","schema_version":"1.0","canonical_sha256":"d254b0318dba100894c853087827802ea8c47155c299638c98145d4038e95ab6","source":{"kind":"arxiv","id":"2408.09351","version":1},"attestation_state":"computed","paper":{"title":"The Fast Radio Burst Population Energy Distribution","license":"http://creativecommons.org/licenses/by-sa/4.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"A. C. Gordon, A.T. Deller, C. Flynn, C.W. James, E.M. Sadler, J-P. Macquart, K.W. Bannister, L. Marnoch, M. Glowacki, R.B. Wayth, R.D. Ekers, R.M. Shannon, S.D. Ryder, W.R. Arcus","submitted_at":"2024-08-18T04:19:02Z","abstract_excerpt":"We examine the energy distribution of the fast radio burst (FRB) population using a well-defined sample of 63 FRBs from the ASKAP radio telescope, 28 of which are localised to a host galaxy. We apply the luminosity-volume ($V/V_{\\mathrm{max}}$) test to examine the distribution of these transient sources, accounting for cosmological and instrumental effects, and determine the energy distribution for the sampled population over the redshift range $0.01 \\lesssim z \\lesssim 1.02$. We find the distribution between $10^{23}$ and $10^{26}$J Hz$^{-1}$ to be consistent with both a pure power-law with d"},"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":"2408.09351","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-sa/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-08-18T04:19:02Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"44bf79633a1475c43ac4a35351df415bc8b4c1f29a00f73d334084544b1ec7a2","abstract_canon_sha256":"f8f701809da4468c97289d3ab790b2391354e0d17c5a75a4596447040a52552d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:59:51.362720Z","signature_b64":"sxFy5nBmBMqMZYEqtmoZNXfdwpWD7x7G5T9NjBBRg2xLcrGqh/x4wme04Lb86dLDAYUNIiQmyWKQdyI/FWjeBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d254b0318dba100894c853087827802ea8c47155c299638c98145d4038e95ab6","last_reissued_at":"2026-07-05T09:59:51.362287Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:59:51.362287Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Fast Radio Burst Population Energy Distribution","license":"http://creativecommons.org/licenses/by-sa/4.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"A. C. Gordon, A.T. Deller, C. Flynn, C.W. James, E.M. Sadler, J-P. Macquart, K.W. Bannister, L. Marnoch, M. Glowacki, R.B. Wayth, R.D. Ekers, R.M. Shannon, S.D. Ryder, W.R. Arcus","submitted_at":"2024-08-18T04:19:02Z","abstract_excerpt":"We examine the energy distribution of the fast radio burst (FRB) population using a well-defined sample of 63 FRBs from the ASKAP radio telescope, 28 of which are localised to a host galaxy. We apply the luminosity-volume ($V/V_{\\mathrm{max}}$) test to examine the distribution of these transient sources, accounting for cosmological and instrumental effects, and determine the energy distribution for the sampled population over the redshift range $0.01 \\lesssim z \\lesssim 1.02$. We find the distribution between $10^{23}$ and $10^{26}$J Hz$^{-1}$ to be consistent with both a pure power-law with d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2408.09351","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/2408.09351/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":"2408.09351","created_at":"2026-07-05T09:59:51.362344+00:00"},{"alias_kind":"arxiv_version","alias_value":"2408.09351v1","created_at":"2026-07-05T09:59:51.362344+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2408.09351","created_at":"2026-07-05T09:59:51.362344+00:00"},{"alias_kind":"pith_short_12","alias_value":"2JKLAMMNXIIA","created_at":"2026-07-05T09:59:51.362344+00:00"},{"alias_kind":"pith_short_16","alias_value":"2JKLAMMNXIIARFGI","created_at":"2026-07-05T09:59:51.362344+00:00"},{"alias_kind":"pith_short_8","alias_value":"2JKLAMMN","created_at":"2026-07-05T09:59:51.362344+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2510.09463","citing_title":"Generalized Distributions of Host Dispersion Measures in the Fast Radio Burst Cosmology","ref_index":102,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2","json":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2.json","graph_json":"https://pith.science/api/pith-number/2JKLAMMNXIIARFGIKMEHQJ4AF2/graph.json","events_json":"https://pith.science/api/pith-number/2JKLAMMNXIIARFGIKMEHQJ4AF2/events.json","paper":"https://pith.science/paper/2JKLAMMN"},"agent_actions":{"view_html":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2","download_json":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2.json","view_paper":"https://pith.science/paper/2JKLAMMN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2408.09351&json=true","fetch_graph":"https://pith.science/api/pith-number/2JKLAMMNXIIARFGIKMEHQJ4AF2/graph.json","fetch_events":"https://pith.science/api/pith-number/2JKLAMMNXIIARFGIKMEHQJ4AF2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2/action/storage_attestation","attest_author":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2/action/author_attestation","sign_citation":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2/action/citation_signature","submit_replication":"https://pith.science/pith/2JKLAMMNXIIARFGIKMEHQJ4AF2/action/replication_record"}},"created_at":"2026-07-05T09:59:51.362344+00:00","updated_at":"2026-07-05T09:59:51.362344+00:00"}