{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:FQ4DWBGVLCDHBM6FRGH3J7PBYH","short_pith_number":"pith:FQ4DWBGV","schema_version":"1.0","canonical_sha256":"2c383b04d5588670b3c5898fb4fde1c1c9050e139f7a7cf9bdf60ea3e219bf64","source":{"kind":"arxiv","id":"1406.6564","version":1},"attestation_state":"computed","paper":{"title":"Abundance analysis for long-period variables II. RGB and AGB stars in the globular cluster 47\\,Tuc","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Bernhard Aringer, Kenneth H. Hinkle, Susanne H\\\"ofner, Thomas Lebzelter, Walter Nowotny","submitted_at":"2014-06-25T13:30:06Z","abstract_excerpt":"Asymptotic giant branch (AGB) stars play a key role in the enrichment of galaxies with heavy elements. Due to their large amplitude variability, the measurement of elemental abundances is a highly challenging task that has not been solved in a satisfactory way yet.\n  Following our previous work we use hydrostatic and dynamical model atmospheres to simulate observed high-resolution near-infrared spectra of 12 variable and non-variable red giants in the globular cluster 47 Tuc. The 47 Tuc red giants are independently well-characterized in important parameters (mass, metallicity, luminosity). The"},"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":"1406.6564","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-06-25T13:30:06Z","cross_cats_sorted":[],"title_canon_sha256":"708d17edd315ec1db441b2ca43cd75364d8516053c97514dff06b4453f8fd827","abstract_canon_sha256":"73ea076c48a0d7884f443ed306997dea246b74fde77df4c41994d721af16dffb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:43:34.747361Z","signature_b64":"MR0EsUNQ2WCOVhZcy8t4RBvY8SspEj8Ysb+qW1/1ve87HNUSZpwzHGS2tgaGwhKHfEHEpb/FTzXybqFirE17BQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2c383b04d5588670b3c5898fb4fde1c1c9050e139f7a7cf9bdf60ea3e219bf64","last_reissued_at":"2026-05-18T02:43:34.746781Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:43:34.746781Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Abundance analysis for long-period variables II. RGB and AGB stars in the globular cluster 47\\,Tuc","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Bernhard Aringer, Kenneth H. Hinkle, Susanne H\\\"ofner, Thomas Lebzelter, Walter Nowotny","submitted_at":"2014-06-25T13:30:06Z","abstract_excerpt":"Asymptotic giant branch (AGB) stars play a key role in the enrichment of galaxies with heavy elements. Due to their large amplitude variability, the measurement of elemental abundances is a highly challenging task that has not been solved in a satisfactory way yet.\n  Following our previous work we use hydrostatic and dynamical model atmospheres to simulate observed high-resolution near-infrared spectra of 12 variable and non-variable red giants in the globular cluster 47 Tuc. The 47 Tuc red giants are independently well-characterized in important parameters (mass, metallicity, luminosity). The"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1406.6564","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":"1406.6564","created_at":"2026-05-18T02:43:34.746851+00:00"},{"alias_kind":"arxiv_version","alias_value":"1406.6564v1","created_at":"2026-05-18T02:43:34.746851+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1406.6564","created_at":"2026-05-18T02:43:34.746851+00:00"},{"alias_kind":"pith_short_12","alias_value":"FQ4DWBGVLCDH","created_at":"2026-05-18T12:28:28.263976+00:00"},{"alias_kind":"pith_short_16","alias_value":"FQ4DWBGVLCDHBM6F","created_at":"2026-05-18T12:28:28.263976+00:00"},{"alias_kind":"pith_short_8","alias_value":"FQ4DWBGV","created_at":"2026-05-18T12:28:28.263976+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":93,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH","json":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH.json","graph_json":"https://pith.science/api/pith-number/FQ4DWBGVLCDHBM6FRGH3J7PBYH/graph.json","events_json":"https://pith.science/api/pith-number/FQ4DWBGVLCDHBM6FRGH3J7PBYH/events.json","paper":"https://pith.science/paper/FQ4DWBGV"},"agent_actions":{"view_html":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH","download_json":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH.json","view_paper":"https://pith.science/paper/FQ4DWBGV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1406.6564&json=true","fetch_graph":"https://pith.science/api/pith-number/FQ4DWBGVLCDHBM6FRGH3J7PBYH/graph.json","fetch_events":"https://pith.science/api/pith-number/FQ4DWBGVLCDHBM6FRGH3J7PBYH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH/action/storage_attestation","attest_author":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH/action/author_attestation","sign_citation":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH/action/citation_signature","submit_replication":"https://pith.science/pith/FQ4DWBGVLCDHBM6FRGH3J7PBYH/action/replication_record"}},"created_at":"2026-05-18T02:43:34.746851+00:00","updated_at":"2026-05-18T02:43:34.746851+00:00"}