{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:SWE3PFWJBEJDKGPNPEQ6Q4O7YZ","short_pith_number":"pith:SWE3PFWJ","schema_version":"1.0","canonical_sha256":"9589b796c909123519ed7921e871dfc67933656d88e6db3358365df9cb07c632","source":{"kind":"arxiv","id":"1603.05283","version":1},"attestation_state":"computed","paper":{"title":"Evolution of Thermally Pulsing Asymptotic Giant Branch Stars V: Constraining the Mass Loss and Lifetimes of Intermediate Mass, Low Metallicity AGB Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Alessandro Bressan, Andrew Dolphin, Benjamin F. Williams, Julianne J. Dalcanton, L\\'eo Girardi, Paola Marigo, Philip Rosenfield","submitted_at":"2016-03-16T21:07:41Z","abstract_excerpt":"Thermally-Pulsing Asymptotic Giant Branch (TP-AGB) stars are relatively short lived (less than a few Myr), yet their cool effective temperatures, high luminosities, efficient mass-loss and dust production can dramatically effect the chemical enrichment histories and the spectral energy distributions of their host galaxies. The ability to accurately model TP-AGB stars is critical to the interpretation of the integrated light of distant galaxies, especially in redder wavelengths. We continue previous efforts to constrain the evolution and lifetimes of TP-AGB stars by modeling their underlying st"},"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":"1603.05283","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2016-03-16T21:07:41Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"203df44ee4097ed92391b6c6faee9c4672c6b679adf801f489a79a0478f228e9","abstract_canon_sha256":"49293e1466b461e7de9040fd611f5a600897b0c59f4d03704bc9c48b93b84472"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:13:53.987979Z","signature_b64":"jhOoj28XbksVc+id17ENnoE3ATZNfsAxK9XXp9KnMQg0SCExOx9f8h7aepwSNEwY6LW0XkrcgZSJ8KeVpuCxDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9589b796c909123519ed7921e871dfc67933656d88e6db3358365df9cb07c632","last_reissued_at":"2026-05-18T01:13:53.987248Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:13:53.987248Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evolution of Thermally Pulsing Asymptotic Giant Branch Stars V: Constraining the Mass Loss and Lifetimes of Intermediate Mass, Low Metallicity AGB Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Alessandro Bressan, Andrew Dolphin, Benjamin F. Williams, Julianne J. Dalcanton, L\\'eo Girardi, Paola Marigo, Philip Rosenfield","submitted_at":"2016-03-16T21:07:41Z","abstract_excerpt":"Thermally-Pulsing Asymptotic Giant Branch (TP-AGB) stars are relatively short lived (less than a few Myr), yet their cool effective temperatures, high luminosities, efficient mass-loss and dust production can dramatically effect the chemical enrichment histories and the spectral energy distributions of their host galaxies. The ability to accurately model TP-AGB stars is critical to the interpretation of the integrated light of distant galaxies, especially in redder wavelengths. We continue previous efforts to constrain the evolution and lifetimes of TP-AGB stars by modeling their underlying st"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1603.05283","kind":"arxiv","version":1},"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":"1603.05283","created_at":"2026-05-18T01:13:53.987367+00:00"},{"alias_kind":"arxiv_version","alias_value":"1603.05283v1","created_at":"2026-05-18T01:13:53.987367+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1603.05283","created_at":"2026-05-18T01:13:53.987367+00:00"},{"alias_kind":"pith_short_12","alias_value":"SWE3PFWJBEJD","created_at":"2026-05-18T12:30:44.179134+00:00"},{"alias_kind":"pith_short_16","alias_value":"SWE3PFWJBEJDKGPN","created_at":"2026-05-18T12:30:44.179134+00:00"},{"alias_kind":"pith_short_8","alias_value":"SWE3PFWJ","created_at":"2026-05-18T12:30:44.179134+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.17153","citing_title":"Chemical hints of Population III stars from silicon abundances in massive galaxies","ref_index":289,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ","json":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ.json","graph_json":"https://pith.science/api/pith-number/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/graph.json","events_json":"https://pith.science/api/pith-number/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/events.json","paper":"https://pith.science/paper/SWE3PFWJ"},"agent_actions":{"view_html":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ","download_json":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ.json","view_paper":"https://pith.science/paper/SWE3PFWJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1603.05283&json=true","fetch_graph":"https://pith.science/api/pith-number/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/graph.json","fetch_events":"https://pith.science/api/pith-number/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/action/storage_attestation","attest_author":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/action/author_attestation","sign_citation":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/action/citation_signature","submit_replication":"https://pith.science/pith/SWE3PFWJBEJDKGPNPEQ6Q4O7YZ/action/replication_record"}},"created_at":"2026-05-18T01:13:53.987367+00:00","updated_at":"2026-05-18T01:13:53.987367+00:00"}