{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:TEWIDRLX7WAWHDBMJY2CQ5SROP","short_pith_number":"pith:TEWIDRLX","schema_version":"1.0","canonical_sha256":"992c81c577fd81638c2c4e3428765173f0c0ee4d98e4f23de9a21c276511ab96","source":{"kind":"arxiv","id":"1901.03516","version":2},"attestation_state":"computed","paper":{"title":"Long gamma-ray burst rate at very high redshift","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Katsuaki Asano, Tomoya Kinugawa, Yuichi Harikane","submitted_at":"2019-01-11T09:10:30Z","abstract_excerpt":"Future missions for long gammma-ray burst (GRB) observations at high redshift such as HiZ-GUNDAM and THESEUS will provide clue to the star formation history in our universe. In this paper focusing on high redshift (z>8) GRBs, we calculate the detection rate of long GRBs by future observations, considering both Population (Pop) I&II stars and Pop III stars as GRB progenitors. For the Pop I&II star formation rate (SFR), we adopt an up-to-date model of high-redshift SFR based on the halo mass function and dark matter accretion rate obtained from cosmological simulations. We show that the Pop I&II"},"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":"1901.03516","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2019-01-11T09:10:30Z","cross_cats_sorted":[],"title_canon_sha256":"4dbbc65c8844d87d7feb25579c92b521cf0790566461e65f5a6b2c58c4b9e294","abstract_canon_sha256":"babc45ba4bc0f5af9f29febf63b4ddea66f3802d155504d348d556bfef0567c1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:42:24.725922Z","signature_b64":"BIuFtyWXM2g9zdO7D5QrzzKxdAqxd180Av+U0dWk58G+mxKjrmaTcIwElQ+nxW4QpTHhiaAlUWRTKXUinzDTDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"992c81c577fd81638c2c4e3428765173f0c0ee4d98e4f23de9a21c276511ab96","last_reissued_at":"2026-05-17T23:42:24.725284Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:42:24.725284Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Long gamma-ray burst rate at very high redshift","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Katsuaki Asano, Tomoya Kinugawa, Yuichi Harikane","submitted_at":"2019-01-11T09:10:30Z","abstract_excerpt":"Future missions for long gammma-ray burst (GRB) observations at high redshift such as HiZ-GUNDAM and THESEUS will provide clue to the star formation history in our universe. In this paper focusing on high redshift (z>8) GRBs, we calculate the detection rate of long GRBs by future observations, considering both Population (Pop) I&II stars and Pop III stars as GRB progenitors. For the Pop I&II star formation rate (SFR), we adopt an up-to-date model of high-redshift SFR based on the halo mass function and dark matter accretion rate obtained from cosmological simulations. We show that the Pop I&II"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1901.03516","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":"1901.03516","created_at":"2026-05-17T23:42:24.725398+00:00"},{"alias_kind":"arxiv_version","alias_value":"1901.03516v2","created_at":"2026-05-17T23:42:24.725398+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1901.03516","created_at":"2026-05-17T23:42:24.725398+00:00"},{"alias_kind":"pith_short_12","alias_value":"TEWIDRLX7WAW","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_16","alias_value":"TEWIDRLX7WAWHDBM","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_8","alias_value":"TEWIDRLX","created_at":"2026-05-18T12:33:27.125529+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/TEWIDRLX7WAWHDBMJY2CQ5SROP","json":"https://pith.science/pith/TEWIDRLX7WAWHDBMJY2CQ5SROP.json","graph_json":"https://pith.science/api/pith-number/TEWIDRLX7WAWHDBMJY2CQ5SROP/graph.json","events_json":"https://pith.science/api/pith-number/TEWIDRLX7WAWHDBMJY2CQ5SROP/events.json","paper":"https://pith.science/paper/TEWIDRLX"},"agent_actions":{"view_html":"https://pith.science/pith/TEWIDRLX7WAWHDBMJY2CQ5SROP","download_json":"https://pith.science/pith/TEWIDRLX7WAWHDBMJY2CQ5SROP.json","view_paper":"https://pith.science/paper/TEWIDRLX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1901.03516&json=true","fetch_graph":"https://pith.science/api/pith-number/TEWIDRLX7WAWHDBMJY2CQ5SROP/graph.json","fetch_events":"https://pith.science/api/pith-number/TEWIDRLX7WAWHDBMJY2CQ5SROP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TEWIDRLX7WAWHDBMJY2CQ5SROP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TEWIDRLX7WAWHDBMJY2CQ5SROP/action/storage_attestation","attest_author":"https://pith.science/pith/TEWIDRLX7WAWHDBMJY2CQ5SROP/action/author_attestation","sign_citation":"https://pith.science/pith/TEWIDRLX7WAWHDBMJY2CQ5SROP/action/citation_signature","submit_replication":"https://pith.science/pith/TEWIDRLX7WAWHDBMJY2CQ5SROP/action/replication_record"}},"created_at":"2026-05-17T23:42:24.725398+00:00","updated_at":"2026-05-17T23:42:24.725398+00:00"}