{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1999:FB5MUYU7NFDQ4Z7B2R5LU2ZHIR","short_pith_number":"pith:FB5MUYU7","schema_version":"1.0","canonical_sha256":"287aca629f69470e67e1d47aba6b27447f0b0a23a920f03fb7a8b01b2a13d601","source":{"kind":"arxiv","id":"astro-ph/9903399","version":1},"attestation_state":"computed","paper":{"title":"The Dynamics and Light Curves of Beamed Gamma Ray Burst Afterglows","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"James E. Rhoads (Kitt Peak National Observatory)","submitted_at":"1999-03-25T22:22:18Z","abstract_excerpt":"The energy requirements of gamma ray bursts have in past been poorly constrained because of three major uncertainties: The distances to bursts, the degree of burst beaming, and the efficiency of gamma ray production. The first of these has been resolved, with both indirect evidence (the distribution of bursts in flux and position) and direct evidence (redshifted absorption features in the afterglow spectrum of GRB 970508) pointing to cosmological distances. We now wish to address the second uncertainty. Afterglows allow a statistical test of beaming, described in an earlier paper. In this pape"},"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":"astro-ph/9903399","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1999-03-25T22:22:18Z","cross_cats_sorted":[],"title_canon_sha256":"cc277e17e3a1f48b0611737d43dd8b095a4c137b3b6ee75b334bcd5ed677fc08","abstract_canon_sha256":"06c847b936980c2599dc4055633024e9f10055606a39cf39ce97186689d1d508"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:20:41.011963Z","signature_b64":"zztgXIBFOik2HgrBsIIZyPZPGZ9AXiFob1Nx65Mt/cj4DQ/mcZPUBbiSYeUfpyKHXWxma7iVb3/fQ48P3PM4CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"287aca629f69470e67e1d47aba6b27447f0b0a23a920f03fb7a8b01b2a13d601","last_reissued_at":"2026-07-04T15:20:41.011572Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:20:41.011572Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Dynamics and Light Curves of Beamed Gamma Ray Burst Afterglows","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"James E. Rhoads (Kitt Peak National Observatory)","submitted_at":"1999-03-25T22:22:18Z","abstract_excerpt":"The energy requirements of gamma ray bursts have in past been poorly constrained because of three major uncertainties: The distances to bursts, the degree of burst beaming, and the efficiency of gamma ray production. The first of these has been resolved, with both indirect evidence (the distribution of bursts in flux and position) and direct evidence (redshifted absorption features in the afterglow spectrum of GRB 970508) pointing to cosmological distances. We now wish to address the second uncertainty. Afterglows allow a statistical test of beaming, described in an earlier paper. In this pape"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9903399","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/astro-ph/9903399/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":"astro-ph/9903399","created_at":"2026-07-04T15:20:41.011629+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9903399v1","created_at":"2026-07-04T15:20:41.011629+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9903399","created_at":"2026-07-04T15:20:41.011629+00:00"},{"alias_kind":"pith_short_12","alias_value":"FB5MUYU7NFDQ","created_at":"2026-07-04T15:20:41.011629+00:00"},{"alias_kind":"pith_short_16","alias_value":"FB5MUYU7NFDQ4Z7B","created_at":"2026-07-04T15:20:41.011629+00:00"},{"alias_kind":"pith_short_8","alias_value":"FB5MUYU7","created_at":"2026-07-04T15:20:41.011629+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2607.01820","citing_title":"Polarization Architecture of Steady GRMHD Jets from the Horizon to Infinity","ref_index":85,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28267","citing_title":"Early Optical Follow-up of Gamma-Ray Bursts: The Critical Role of Robotic Telescopes","ref_index":122,"is_internal_anchor":true},{"citing_arxiv_id":"2606.05146","citing_title":"Early Multiwavelength Observations of AT 2026fgk: The Luminous Afterglow to Sub-luminous GRB 260310A, Identified Independently of a Gamma-ray Trigger","ref_index":123,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10011","citing_title":"A Multi-Wavelength View of the First Type Ic-BL Supernova with an Einstein Probe X-ray Shock Breakout","ref_index":21,"is_internal_anchor":true},{"citing_arxiv_id":"2606.24329","citing_title":"EP251023a: A fast X-ray transient featuring a magnetar-powered optical internal plateau followed by a steep decay","ref_index":13,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR","json":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR.json","graph_json":"https://pith.science/api/pith-number/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/graph.json","events_json":"https://pith.science/api/pith-number/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/events.json","paper":"https://pith.science/paper/FB5MUYU7"},"agent_actions":{"view_html":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR","download_json":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR.json","view_paper":"https://pith.science/paper/FB5MUYU7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9903399&json=true","fetch_graph":"https://pith.science/api/pith-number/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/graph.json","fetch_events":"https://pith.science/api/pith-number/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/action/storage_attestation","attest_author":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/action/author_attestation","sign_citation":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/action/citation_signature","submit_replication":"https://pith.science/pith/FB5MUYU7NFDQ4Z7B2R5LU2ZHIR/action/replication_record"}},"created_at":"2026-07-04T15:20:41.011629+00:00","updated_at":"2026-07-04T15:20:41.011629+00:00"}