{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2001:FSQPL6RG3KARC5BUULU2WXP7PM","short_pith_number":"pith:FSQPL6RG","schema_version":"1.0","canonical_sha256":"2ca0f5fa26da81117434a2e9ab5dff7b00b356664c619f098990f5c4b81581f3","source":{"kind":"arxiv","id":"astro-ph/0110697","version":2},"attestation_state":"computed","paper":{"title":"On the properties of massive Population III stars and metal-free stellar populations","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Daniel Schaerer (OMP, Toulouse)","submitted_at":"2001-10-31T13:46:10Z","abstract_excerpt":"We present realistic models for massive Population III stars and stellar populations based on non-LTE model atmospheres, recent stellar evolution tracks and up-to-date evolutionary synthesis models, to study their spectral properties, including their dependence on age, star formation history, and IMF. (..) The main results regarding integrated stellar populations are: * For young bursts and the case of a constant SFR, nebular continuous emission - neglected in previous studies - dominates the spectrum redward of Lyman-alpha (...). Therefore predicted emission line equivalent widths are conside"},"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/0110697","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2001-10-31T13:46:10Z","cross_cats_sorted":[],"title_canon_sha256":"466e5e0d73482001a695a57358a0ca4d1de4cf54cbbc2a266cdd87fe27c6c39b","abstract_canon_sha256":"9bd25bf2309b3b12f7b2c08f367f26822c723e36586d29093aa07120747d00a7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:24:23.408701Z","signature_b64":"30D5plWlwwyYbntdWrGVWoXbhzwmBB4lxz6qKBG87q0sHBV9MsCThfnKMO2RX700x+ftd8PLQ6tZc7HEj2CYDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2ca0f5fa26da81117434a2e9ab5dff7b00b356664c619f098990f5c4b81581f3","last_reissued_at":"2026-07-04T16:24:23.408214Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:24:23.408214Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the properties of massive Population III stars and metal-free stellar populations","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Daniel Schaerer (OMP, Toulouse)","submitted_at":"2001-10-31T13:46:10Z","abstract_excerpt":"We present realistic models for massive Population III stars and stellar populations based on non-LTE model atmospheres, recent stellar evolution tracks and up-to-date evolutionary synthesis models, to study their spectral properties, including their dependence on age, star formation history, and IMF. (..) The main results regarding integrated stellar populations are: * For young bursts and the case of a constant SFR, nebular continuous emission - neglected in previous studies - dominates the spectrum redward of Lyman-alpha (...). Therefore predicted emission line equivalent widths are conside"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0110697","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0110697/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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/0110697","created_at":"2026-07-04T16:24:23.408267+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0110697v2","created_at":"2026-07-04T16:24:23.408267+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0110697","created_at":"2026-07-04T16:24:23.408267+00:00"},{"alias_kind":"pith_short_12","alias_value":"FSQPL6RG3KAR","created_at":"2026-07-04T16:24:23.408267+00:00"},{"alias_kind":"pith_short_16","alias_value":"FSQPL6RG3KARC5BU","created_at":"2026-07-04T16:24:23.408267+00:00"},{"alias_kind":"pith_short_8","alias_value":"FSQPL6RG","created_at":"2026-07-04T16:24:23.408267+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2606.30750","citing_title":"A Pixel-by-Pixel Path to Population III Discovery with JWST","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2606.29903","citing_title":"High-Redshift Signatures from the Cosmic Dawn and the Epoch of Reionization","ref_index":1,"is_internal_anchor":true},{"citing_arxiv_id":"2606.00205","citing_title":"Ultraviolet diversity of Little Red Dots as a probe for direct-collapse black hole ages","ref_index":265,"is_internal_anchor":true},{"citing_arxiv_id":"2606.00219","citing_title":"21cmEMUv3: a hybrid diffusion-LSTM emulator of 21cmFAST summary observables","ref_index":23,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18097","citing_title":"Effects of formation channels and gravitational lensing on stochastic gravitational wave background","ref_index":63,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM","json":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM.json","graph_json":"https://pith.science/api/pith-number/FSQPL6RG3KARC5BUULU2WXP7PM/graph.json","events_json":"https://pith.science/api/pith-number/FSQPL6RG3KARC5BUULU2WXP7PM/events.json","paper":"https://pith.science/paper/FSQPL6RG"},"agent_actions":{"view_html":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM","download_json":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM.json","view_paper":"https://pith.science/paper/FSQPL6RG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0110697&json=true","fetch_graph":"https://pith.science/api/pith-number/FSQPL6RG3KARC5BUULU2WXP7PM/graph.json","fetch_events":"https://pith.science/api/pith-number/FSQPL6RG3KARC5BUULU2WXP7PM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM/action/storage_attestation","attest_author":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM/action/author_attestation","sign_citation":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM/action/citation_signature","submit_replication":"https://pith.science/pith/FSQPL6RG3KARC5BUULU2WXP7PM/action/replication_record"}},"created_at":"2026-07-04T16:24:23.408267+00:00","updated_at":"2026-07-04T16:24:23.408267+00:00"}