{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:NI2G53SZHAGRHGP7D5KQDBQ7NU","short_pith_number":"pith:NI2G53SZ","schema_version":"1.0","canonical_sha256":"6a346eee59380d1399ff1f5501861f6d29d2f21f319ba3c98aaf8af776e92aa3","source":{"kind":"arxiv","id":"1506.04796","version":2},"attestation_state":"computed","paper":{"title":"Lyman-Werner UV Escape Fractions from Primordial Halos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Anna T. P. Schauer, Daniel J. Whalen, Ralf S. Klessen, Simon C. O. Glover","submitted_at":"2015-06-15T23:01:02Z","abstract_excerpt":"Population III stars can regulate star formation in the primordial Universe in several ways. They can ionize nearby halos, and even if their ionizing photons are trapped by their own halos, their Lyman-Werner (LW) photons can still escape and destroy H$_2$ in other halos, preventing them from cooling and forming stars. LW escape fractions are thus a key parameter in cosmological simulations of early reionization and star formation but have not yet been parametrized for realistic halos by halo or stellar mass. To do so, we perform radiation hydrodynamical simulations of LW UV escape from 9--120"},"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":"1506.04796","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2015-06-15T23:01:02Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"a1569fad8c87f0866c261d1877cde99a2021ae75074c92e8c411038c8bcd9300","abstract_canon_sha256":"9f886795748d0d6460b6352acf287ec41b24cd5c4283e4e50d6c78d67c180795"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:29:45.703097Z","signature_b64":"VBSylPbp35QllzoQ5HhnGmAmHmzgAxNV5Gn2LGHCKnIDj+yGYvXVXYKjBN+pbb1w0SXsrrCICAtsKmk3oPwnCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6a346eee59380d1399ff1f5501861f6d29d2f21f319ba3c98aaf8af776e92aa3","last_reissued_at":"2026-05-18T01:29:45.702583Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:29:45.702583Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Lyman-Werner UV Escape Fractions from Primordial Halos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Anna T. P. Schauer, Daniel J. Whalen, Ralf S. Klessen, Simon C. O. Glover","submitted_at":"2015-06-15T23:01:02Z","abstract_excerpt":"Population III stars can regulate star formation in the primordial Universe in several ways. They can ionize nearby halos, and even if their ionizing photons are trapped by their own halos, their Lyman-Werner (LW) photons can still escape and destroy H$_2$ in other halos, preventing them from cooling and forming stars. LW escape fractions are thus a key parameter in cosmological simulations of early reionization and star formation but have not yet been parametrized for realistic halos by halo or stellar mass. To do so, we perform radiation hydrodynamical simulations of LW UV escape from 9--120"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1506.04796","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":"1506.04796","created_at":"2026-05-18T01:29:45.702666+00:00"},{"alias_kind":"arxiv_version","alias_value":"1506.04796v2","created_at":"2026-05-18T01:29:45.702666+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1506.04796","created_at":"2026-05-18T01:29:45.702666+00:00"},{"alias_kind":"pith_short_12","alias_value":"NI2G53SZHAGR","created_at":"2026-05-18T12:29:32.376354+00:00"},{"alias_kind":"pith_short_16","alias_value":"NI2G53SZHAGRHGP7","created_at":"2026-05-18T12:29:32.376354+00:00"},{"alias_kind":"pith_short_8","alias_value":"NI2G53SZ","created_at":"2026-05-18T12:29:32.376354+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"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":99,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU","json":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU.json","graph_json":"https://pith.science/api/pith-number/NI2G53SZHAGRHGP7D5KQDBQ7NU/graph.json","events_json":"https://pith.science/api/pith-number/NI2G53SZHAGRHGP7D5KQDBQ7NU/events.json","paper":"https://pith.science/paper/NI2G53SZ"},"agent_actions":{"view_html":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU","download_json":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU.json","view_paper":"https://pith.science/paper/NI2G53SZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1506.04796&json=true","fetch_graph":"https://pith.science/api/pith-number/NI2G53SZHAGRHGP7D5KQDBQ7NU/graph.json","fetch_events":"https://pith.science/api/pith-number/NI2G53SZHAGRHGP7D5KQDBQ7NU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU/action/storage_attestation","attest_author":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU/action/author_attestation","sign_citation":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU/action/citation_signature","submit_replication":"https://pith.science/pith/NI2G53SZHAGRHGP7D5KQDBQ7NU/action/replication_record"}},"created_at":"2026-05-18T01:29:45.702666+00:00","updated_at":"2026-05-18T01:29:45.702666+00:00"}