{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:WMTCMBQ4JKREXDYR2BDUXKVOHB","short_pith_number":"pith:WMTCMBQ4","schema_version":"1.0","canonical_sha256":"b32626061c4aa24b8f11d0474baaae387cda365a98f8117b2bb48d8b5d0fbf68","source":{"kind":"arxiv","id":"1604.07842","version":2},"attestation_state":"computed","paper":{"title":"Galaxy Properties and UV Escape Fractions During Epoch of Reionization: Results from the Renaissance Simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Brian W. O'Shea, Hao Xu, John H. Wise, Kyungjin Ahn, Michael L. Norman","submitted_at":"2016-04-26T20:16:00Z","abstract_excerpt":"Cosmic reionization is thought to be primarily fueled by the first generations of galaxies. We examine their stellar and gaseous properties, focusing on the star formation rates and the escape of ionizing photons, as a function of halo mass, redshift, and environment using the full suite of the {\\it Renaissance Simulations} with an eye to provide better inputs to global reionization simulations. This suite, carried out with the adaptive mesh refinement code Enzo, is unprecedented in terms of their size and physical ingredients. The simulations probe overdense, average, and underdense regions o"},"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":"1604.07842","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-04-26T20:16:00Z","cross_cats_sorted":[],"title_canon_sha256":"b067a1da335be6800c2caa235f20b26f61bc9b9b389109fcff363462c93a39ab","abstract_canon_sha256":"c0a0b956b3f8a738e68bdf64c1bee6e67cfbf60055a217a4208510bbda744ce5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:55:13.882567Z","signature_b64":"gx3rkHcpM7ywyB6R3oiW8ZZloSvqftAM1XEbMxwU0KIJfmwItwAqd7C7smj2oH1CR5xtnrwU8Bhl5kbMGwM7DQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b32626061c4aa24b8f11d0474baaae387cda365a98f8117b2bb48d8b5d0fbf68","last_reissued_at":"2026-05-18T00:55:13.882153Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:55:13.882153Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Galaxy Properties and UV Escape Fractions During Epoch of Reionization: Results from the Renaissance Simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Brian W. O'Shea, Hao Xu, John H. Wise, Kyungjin Ahn, Michael L. Norman","submitted_at":"2016-04-26T20:16:00Z","abstract_excerpt":"Cosmic reionization is thought to be primarily fueled by the first generations of galaxies. We examine their stellar and gaseous properties, focusing on the star formation rates and the escape of ionizing photons, as a function of halo mass, redshift, and environment using the full suite of the {\\it Renaissance Simulations} with an eye to provide better inputs to global reionization simulations. This suite, carried out with the adaptive mesh refinement code Enzo, is unprecedented in terms of their size and physical ingredients. The simulations probe overdense, average, and underdense regions o"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1604.07842","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":"1604.07842","created_at":"2026-05-18T00:55:13.882207+00:00"},{"alias_kind":"arxiv_version","alias_value":"1604.07842v2","created_at":"2026-05-18T00:55:13.882207+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1604.07842","created_at":"2026-05-18T00:55:13.882207+00:00"},{"alias_kind":"pith_short_12","alias_value":"WMTCMBQ4JKRE","created_at":"2026-05-18T12:30:48.956258+00:00"},{"alias_kind":"pith_short_16","alias_value":"WMTCMBQ4JKREXDYR","created_at":"2026-05-18T12:30:48.956258+00:00"},{"alias_kind":"pith_short_8","alias_value":"WMTCMBQ4","created_at":"2026-05-18T12:30:48.956258+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.14312","citing_title":"An Improved Fit for Linear Halo Bias at High Redshift","ref_index":51,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB","json":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB.json","graph_json":"https://pith.science/api/pith-number/WMTCMBQ4JKREXDYR2BDUXKVOHB/graph.json","events_json":"https://pith.science/api/pith-number/WMTCMBQ4JKREXDYR2BDUXKVOHB/events.json","paper":"https://pith.science/paper/WMTCMBQ4"},"agent_actions":{"view_html":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB","download_json":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB.json","view_paper":"https://pith.science/paper/WMTCMBQ4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1604.07842&json=true","fetch_graph":"https://pith.science/api/pith-number/WMTCMBQ4JKREXDYR2BDUXKVOHB/graph.json","fetch_events":"https://pith.science/api/pith-number/WMTCMBQ4JKREXDYR2BDUXKVOHB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB/action/storage_attestation","attest_author":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB/action/author_attestation","sign_citation":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB/action/citation_signature","submit_replication":"https://pith.science/pith/WMTCMBQ4JKREXDYR2BDUXKVOHB/action/replication_record"}},"created_at":"2026-05-18T00:55:13.882207+00:00","updated_at":"2026-05-18T00:55:13.882207+00:00"}