{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:MMWHSL5B3GYFPNOIMQKPOV6OPO","short_pith_number":"pith:MMWHSL5B","schema_version":"1.0","canonical_sha256":"632c792fa1d9b057b5c86414f757ce7bac7ed88989a8ebe634118e9a873542d5","source":{"kind":"arxiv","id":"1412.4108","version":1},"attestation_state":"computed","paper":{"title":"AGB Sodium Abundances in the Globular Cluster 47 Tucanae (NGC 104)","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Albert A. Zijlstra, Catherine A. Pilachowski, Christian I. Johnson, Edward Olszewski, Iain McDonald, Ian Thompson, Jeffrey D. Crane, John I. Bailey III, Maria J. Cordero, Mario Mateo, Stephen A. Shectman","submitted_at":"2014-12-12T20:47:57Z","abstract_excerpt":"A recent analysis comparing the [Na/Fe] distributions of red giant branch (RGB) and asymptotic giant branch (AGB) stars in the Galactic globular cluster NGC 6752 found that the ratio of Na-poor to Na-rich stars changes from 30:70 on the RGB to 100:0 on the AGB. The surprising paucity of Na-rich stars on the AGB in NGC 6752 warrants additional investigations to determine if the failure of a significant fraction of stars to ascend the AGB is an attribute common to all globular clusters. Therefore, we present radial velocities, [Fe/H], and [Na/Fe] abundances for 35 AGB stars in the Galactic globu"},"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":"1412.4108","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-12-12T20:47:57Z","cross_cats_sorted":[],"title_canon_sha256":"358c980185e7847281a0f949c8d78b2839e616395309404bc0a9ec297242bd01","abstract_canon_sha256":"519057b2e7eb58e9a348877bdb04c9a113b696fae8d5412748467e181ba9f2ac"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:19.523486Z","signature_b64":"4b+5ZYW4GF5wB3lX/lmwC4bePBKDTK1uKqVbjxa3CNWPxsZ9dEtYvMVo01hSJDT4G0DSGjwSErQTyfvXiw1LCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"632c792fa1d9b057b5c86414f757ce7bac7ed88989a8ebe634118e9a873542d5","last_reissued_at":"2026-05-18T01:41:19.522818Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:19.522818Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"AGB Sodium Abundances in the Globular Cluster 47 Tucanae (NGC 104)","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Albert A. Zijlstra, Catherine A. Pilachowski, Christian I. Johnson, Edward Olszewski, Iain McDonald, Ian Thompson, Jeffrey D. Crane, John I. Bailey III, Maria J. Cordero, Mario Mateo, Stephen A. Shectman","submitted_at":"2014-12-12T20:47:57Z","abstract_excerpt":"A recent analysis comparing the [Na/Fe] distributions of red giant branch (RGB) and asymptotic giant branch (AGB) stars in the Galactic globular cluster NGC 6752 found that the ratio of Na-poor to Na-rich stars changes from 30:70 on the RGB to 100:0 on the AGB. The surprising paucity of Na-rich stars on the AGB in NGC 6752 warrants additional investigations to determine if the failure of a significant fraction of stars to ascend the AGB is an attribute common to all globular clusters. Therefore, we present radial velocities, [Fe/H], and [Na/Fe] abundances for 35 AGB stars in the Galactic globu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1412.4108","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":"1412.4108","created_at":"2026-05-18T01:41:19.522928+00:00"},{"alias_kind":"arxiv_version","alias_value":"1412.4108v1","created_at":"2026-05-18T01:41:19.522928+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1412.4108","created_at":"2026-05-18T01:41:19.522928+00:00"},{"alias_kind":"pith_short_12","alias_value":"MMWHSL5B3GYF","created_at":"2026-05-18T12:28:38.356838+00:00"},{"alias_kind":"pith_short_16","alias_value":"MMWHSL5B3GYFPNOI","created_at":"2026-05-18T12:28:38.356838+00:00"},{"alias_kind":"pith_short_8","alias_value":"MMWHSL5B","created_at":"2026-05-18T12:28:38.356838+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.09205","citing_title":"Tracing the s-Process: Spectroscopic Insights into Chemical Abundances in O- and C-rich Evolved Stars","ref_index":94,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO","json":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO.json","graph_json":"https://pith.science/api/pith-number/MMWHSL5B3GYFPNOIMQKPOV6OPO/graph.json","events_json":"https://pith.science/api/pith-number/MMWHSL5B3GYFPNOIMQKPOV6OPO/events.json","paper":"https://pith.science/paper/MMWHSL5B"},"agent_actions":{"view_html":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO","download_json":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO.json","view_paper":"https://pith.science/paper/MMWHSL5B","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1412.4108&json=true","fetch_graph":"https://pith.science/api/pith-number/MMWHSL5B3GYFPNOIMQKPOV6OPO/graph.json","fetch_events":"https://pith.science/api/pith-number/MMWHSL5B3GYFPNOIMQKPOV6OPO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO/action/storage_attestation","attest_author":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO/action/author_attestation","sign_citation":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO/action/citation_signature","submit_replication":"https://pith.science/pith/MMWHSL5B3GYFPNOIMQKPOV6OPO/action/replication_record"}},"created_at":"2026-05-18T01:41:19.522928+00:00","updated_at":"2026-05-18T01:41:19.522928+00:00"}