{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:NUL7NX4LAUHRKFDPS5AYV6ABW5","short_pith_number":"pith:NUL7NX4L","schema_version":"1.0","canonical_sha256":"6d17f6df8b050f15146f97418af801b7517ed830125752dfb9799a19cc1c0bf7","source":{"kind":"arxiv","id":"1411.2831","version":1},"attestation_state":"computed","paper":{"title":"The Gaia-ESO Survey: CNO abundances in the open clusters Trumpler 20, NGC 4815, and NGC 6705","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Bragaglia, A. Drazdauskas, A. Recio-Blanco, A. Vallenari, C. Lardo, D. Romano, E. Flaccomio, E. Friel, E. Pancino, E. Puzeras, E. Stonkut\\.e, F. Jim\\'enez-Esteban, G. Barisevi\\v{c}ius, G. Carraro, G. Gilmore, G. Tautvai\\v{s}ien\\.e, L. Magrini, L. Moribelli, M. T. Costado, P. de Laverny, P. Donati, P. Jofr\\'e, R. D. Jeffries, R. Smiljanic, S. G. Sousa, S. Randich, S. Zaggia, T. Bensby, T. Masseron, T. Morel, V. Hill, \\v{S}. Mikolaitis, Y. Chorniy","submitted_at":"2014-11-11T14:35:12Z","abstract_excerpt":"Aim of this work is to determine C, N, and O abundances in stars of Galactic open clusters of the Gaia-ESO survey and to compare the observed abundances with those predicted by current stellar and Galactic evolution models. In this pilot paper, we investigate the first three intermediate-age open clusters. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT telescope, were analysed using a differential model atmosphere method. Abundances of carbon were derived using the C2 band heads at 5135 and 5635.5 {\\AA}. The wavelength interval 6470- 6490 {\\AA}, with CN feat"},"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":"1411.2831","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-11-11T14:35:12Z","cross_cats_sorted":[],"title_canon_sha256":"fcc936835a8d74a22205ed8aa5bbb3bd81a58a4f6e03de972b86cfac73fa8f41","abstract_canon_sha256":"ec9084c41cc56bf6ac6dacd5e0afb7285e1323468cfd28ef540e9dc4fd43510c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:31.617853Z","signature_b64":"cQM7+UhBY0yz1RRAPmpCFCZtXVb7CDHb67jInRWdocm/IyeV60FjBcQZRJkT6+fNr42EqViRf3V1hHHfpoMkBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6d17f6df8b050f15146f97418af801b7517ed830125752dfb9799a19cc1c0bf7","last_reissued_at":"2026-05-18T01:41:31.617138Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:31.617138Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Gaia-ESO Survey: CNO abundances in the open clusters Trumpler 20, NGC 4815, and NGC 6705","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Bragaglia, A. Drazdauskas, A. Recio-Blanco, A. Vallenari, C. Lardo, D. Romano, E. Flaccomio, E. Friel, E. Pancino, E. Puzeras, E. Stonkut\\.e, F. Jim\\'enez-Esteban, G. Barisevi\\v{c}ius, G. Carraro, G. Gilmore, G. Tautvai\\v{s}ien\\.e, L. Magrini, L. Moribelli, M. T. Costado, P. de Laverny, P. Donati, P. Jofr\\'e, R. D. Jeffries, R. Smiljanic, S. G. Sousa, S. Randich, S. Zaggia, T. Bensby, T. Masseron, T. Morel, V. Hill, \\v{S}. Mikolaitis, Y. Chorniy","submitted_at":"2014-11-11T14:35:12Z","abstract_excerpt":"Aim of this work is to determine C, N, and O abundances in stars of Galactic open clusters of the Gaia-ESO survey and to compare the observed abundances with those predicted by current stellar and Galactic evolution models. In this pilot paper, we investigate the first three intermediate-age open clusters. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT telescope, were analysed using a differential model atmosphere method. Abundances of carbon were derived using the C2 band heads at 5135 and 5635.5 {\\AA}. The wavelength interval 6470- 6490 {\\AA}, with CN feat"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1411.2831","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":"1411.2831","created_at":"2026-05-18T01:41:31.617253+00:00"},{"alias_kind":"arxiv_version","alias_value":"1411.2831v1","created_at":"2026-05-18T01:41:31.617253+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1411.2831","created_at":"2026-05-18T01:41:31.617253+00:00"},{"alias_kind":"pith_short_12","alias_value":"NUL7NX4LAUHR","created_at":"2026-05-18T12:28:41.024544+00:00"},{"alias_kind":"pith_short_16","alias_value":"NUL7NX4LAUHRKFDP","created_at":"2026-05-18T12:28:41.024544+00:00"},{"alias_kind":"pith_short_8","alias_value":"NUL7NX4L","created_at":"2026-05-18T12:28:41.024544+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5","json":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5.json","graph_json":"https://pith.science/api/pith-number/NUL7NX4LAUHRKFDPS5AYV6ABW5/graph.json","events_json":"https://pith.science/api/pith-number/NUL7NX4LAUHRKFDPS5AYV6ABW5/events.json","paper":"https://pith.science/paper/NUL7NX4L"},"agent_actions":{"view_html":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5","download_json":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5.json","view_paper":"https://pith.science/paper/NUL7NX4L","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1411.2831&json=true","fetch_graph":"https://pith.science/api/pith-number/NUL7NX4LAUHRKFDPS5AYV6ABW5/graph.json","fetch_events":"https://pith.science/api/pith-number/NUL7NX4LAUHRKFDPS5AYV6ABW5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5/action/storage_attestation","attest_author":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5/action/author_attestation","sign_citation":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5/action/citation_signature","submit_replication":"https://pith.science/pith/NUL7NX4LAUHRKFDPS5AYV6ABW5/action/replication_record"}},"created_at":"2026-05-18T01:41:31.617253+00:00","updated_at":"2026-05-18T01:41:31.617253+00:00"}