{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:NV3WU55VTPSSG4FDNFPVRHI4AR","short_pith_number":"pith:NV3WU55V","schema_version":"1.0","canonical_sha256":"6d776a77b59be52370a3695f589d1c045997be404a21715029f2e2380ee17ca3","source":{"kind":"arxiv","id":"astro-ph/0610740","version":2},"attestation_state":"computed","paper":{"title":"Can we use Gamma Ray Bursts to probe high redshift star-formation?","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"D. Guetta, F. Fiore, L.A. Antonelli, S. Piranomonte, V. D'Elia","submitted_at":"2006-10-25T07:21:34Z","abstract_excerpt":"We present a detailed analysis of the selection effects that plague GRB observations. We find that these effects may partially explain the different redshift distributions between BeppoSax/HETE2 and Swift bursts. It is mandatory to consider these effects to determine the redshift evolution of GRBs."},"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/0610740","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-10-25T07:21:34Z","cross_cats_sorted":[],"title_canon_sha256":"33cbc930f989b9f58eee89c284d546027bc949b70067772965bf4189a5f5cd59","abstract_canon_sha256":"7060925fb657c8f28a4047ff2aa79c76cc5c2f2776c9dde3d92588b6824b0d3f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:36:20.824150Z","signature_b64":"Dde3n1TDxgRF3BBtXQlqgxxh9c+tsbjHABZPgkwiVIMe/xlrYLkiQS07uM1TMta1kzWdhtvVfUNBxZMTw5wtCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6d776a77b59be52370a3695f589d1c045997be404a21715029f2e2380ee17ca3","last_reissued_at":"2026-05-18T04:36:20.823735Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:36:20.823735Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Can we use Gamma Ray Bursts to probe high redshift star-formation?","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"D. Guetta, F. Fiore, L.A. Antonelli, S. Piranomonte, V. D'Elia","submitted_at":"2006-10-25T07:21:34Z","abstract_excerpt":"We present a detailed analysis of the selection effects that plague GRB observations. We find that these effects may partially explain the different redshift distributions between BeppoSax/HETE2 and Swift bursts. It is mandatory to consider these effects to determine the redshift evolution of GRBs."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0610740","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":"astro-ph/0610740","created_at":"2026-05-18T04:36:20.823790+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0610740v2","created_at":"2026-05-18T04:36:20.823790+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0610740","created_at":"2026-05-18T04:36:20.823790+00:00"},{"alias_kind":"pith_short_12","alias_value":"NV3WU55VTPSS","created_at":"2026-05-18T12:25:54.717736+00:00"},{"alias_kind":"pith_short_16","alias_value":"NV3WU55VTPSSG4FD","created_at":"2026-05-18T12:25:54.717736+00:00"},{"alias_kind":"pith_short_8","alias_value":"NV3WU55V","created_at":"2026-05-18T12:25:54.717736+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/NV3WU55VTPSSG4FDNFPVRHI4AR","json":"https://pith.science/pith/NV3WU55VTPSSG4FDNFPVRHI4AR.json","graph_json":"https://pith.science/api/pith-number/NV3WU55VTPSSG4FDNFPVRHI4AR/graph.json","events_json":"https://pith.science/api/pith-number/NV3WU55VTPSSG4FDNFPVRHI4AR/events.json","paper":"https://pith.science/paper/NV3WU55V"},"agent_actions":{"view_html":"https://pith.science/pith/NV3WU55VTPSSG4FDNFPVRHI4AR","download_json":"https://pith.science/pith/NV3WU55VTPSSG4FDNFPVRHI4AR.json","view_paper":"https://pith.science/paper/NV3WU55V","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0610740&json=true","fetch_graph":"https://pith.science/api/pith-number/NV3WU55VTPSSG4FDNFPVRHI4AR/graph.json","fetch_events":"https://pith.science/api/pith-number/NV3WU55VTPSSG4FDNFPVRHI4AR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NV3WU55VTPSSG4FDNFPVRHI4AR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NV3WU55VTPSSG4FDNFPVRHI4AR/action/storage_attestation","attest_author":"https://pith.science/pith/NV3WU55VTPSSG4FDNFPVRHI4AR/action/author_attestation","sign_citation":"https://pith.science/pith/NV3WU55VTPSSG4FDNFPVRHI4AR/action/citation_signature","submit_replication":"https://pith.science/pith/NV3WU55VTPSSG4FDNFPVRHI4AR/action/replication_record"}},"created_at":"2026-05-18T04:36:20.823790+00:00","updated_at":"2026-05-18T04:36:20.823790+00:00"}