{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:VMBEOU35QTETYLVUF4VQF4XP3N","short_pith_number":"pith:VMBEOU35","schema_version":"1.0","canonical_sha256":"ab0247537d84c93c2eb42f2b02f2efdb62e32c0551427cb15413f0cf1324d8a9","source":{"kind":"arxiv","id":"1705.08059","version":2},"attestation_state":"computed","paper":{"title":"Baseline Metal Enrichment from Population III Star Formation in Cosmological Volume Simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Jason Jaacks, Robert Thompson, Steven L. Finkelstein, Volker Bromm","submitted_at":"2017-05-23T02:46:15Z","abstract_excerpt":"We utilize the hydrodynamic and N-body code {\\small GIZMO} coupled with our newly developed sub-grid Population~III (Pop~III) Legacy model, designed specifically for cosmological volume simulations, to study the baseline metal enrichment from Pop~III star formation at $z>7$. In this idealized numerical experiment, we only consider Pop~III star formation. We find that our model Pop~III star formation rate density (SFRD), which peaks at $\\sim 10^{-3}\\ {\\rm M_\\odot yr^{-1} Mpc^{-1}}$ near $z\\sim10$, agrees well with previous numerical studies and is consistent with the observed estimates for Pop~"},"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":"1705.08059","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-05-23T02:46:15Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"beb5acfb7f93fc47cfc8d6902ec902ae78964324e19e55f360bc1b9ecf8204f2","abstract_canon_sha256":"58b67a265733cb63c9bcf4379c5fd74f1b9b3b4f999c612d430b988adb8946e8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:25:39.468072Z","signature_b64":"ihQMKVvWw3X2whokSbzbWg4v9f2m458lfhojy3vmiKtpmQKPhaRhP1vqXtHwdsO6Lqd5BQFwxFllAsk2ecd9Bw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ab0247537d84c93c2eb42f2b02f2efdb62e32c0551427cb15413f0cf1324d8a9","last_reissued_at":"2026-05-18T00:25:39.467425Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:25:39.467425Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Baseline Metal Enrichment from Population III Star Formation in Cosmological Volume Simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Jason Jaacks, Robert Thompson, Steven L. Finkelstein, Volker Bromm","submitted_at":"2017-05-23T02:46:15Z","abstract_excerpt":"We utilize the hydrodynamic and N-body code {\\small GIZMO} coupled with our newly developed sub-grid Population~III (Pop~III) Legacy model, designed specifically for cosmological volume simulations, to study the baseline metal enrichment from Pop~III star formation at $z>7$. In this idealized numerical experiment, we only consider Pop~III star formation. We find that our model Pop~III star formation rate density (SFRD), which peaks at $\\sim 10^{-3}\\ {\\rm M_\\odot yr^{-1} Mpc^{-1}}$ near $z\\sim10$, agrees well with previous numerical studies and is consistent with the observed estimates for Pop~"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1705.08059","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":"1705.08059","created_at":"2026-05-18T00:25:39.467519+00:00"},{"alias_kind":"arxiv_version","alias_value":"1705.08059v2","created_at":"2026-05-18T00:25:39.467519+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1705.08059","created_at":"2026-05-18T00:25:39.467519+00:00"},{"alias_kind":"pith_short_12","alias_value":"VMBEOU35QTET","created_at":"2026-05-18T12:31:49.984773+00:00"},{"alias_kind":"pith_short_16","alias_value":"VMBEOU35QTETYLVU","created_at":"2026-05-18T12:31:49.984773+00:00"},{"alias_kind":"pith_short_8","alias_value":"VMBEOU35","created_at":"2026-05-18T12:31:49.984773+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.04740","citing_title":"TDEs on FIRE: Illuminating the Cosmic Evolution of Tidal Disruption Rates","ref_index":105,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15310","citing_title":"Introducing the Lumina project: large-volume radiation-hydrodynamic simulations of the epochs of hydrogen and helium reionization","ref_index":88,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N","json":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N.json","graph_json":"https://pith.science/api/pith-number/VMBEOU35QTETYLVUF4VQF4XP3N/graph.json","events_json":"https://pith.science/api/pith-number/VMBEOU35QTETYLVUF4VQF4XP3N/events.json","paper":"https://pith.science/paper/VMBEOU35"},"agent_actions":{"view_html":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N","download_json":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N.json","view_paper":"https://pith.science/paper/VMBEOU35","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1705.08059&json=true","fetch_graph":"https://pith.science/api/pith-number/VMBEOU35QTETYLVUF4VQF4XP3N/graph.json","fetch_events":"https://pith.science/api/pith-number/VMBEOU35QTETYLVUF4VQF4XP3N/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N/action/storage_attestation","attest_author":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N/action/author_attestation","sign_citation":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N/action/citation_signature","submit_replication":"https://pith.science/pith/VMBEOU35QTETYLVUF4VQF4XP3N/action/replication_record"}},"created_at":"2026-05-18T00:25:39.467519+00:00","updated_at":"2026-05-18T00:25:39.467519+00:00"}