{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:2TAFXBYV46ZUHZPZS7EKAX3EFI","short_pith_number":"pith:2TAFXBYV","schema_version":"1.0","canonical_sha256":"d4c05b8715e7b343e5f997c8a05f642a017a8a5658fa65097de3f5e9c22b38ec","source":{"kind":"arxiv","id":"astro-ph/0607438","version":1},"attestation_state":"computed","paper":{"title":"Old open clusters as key tracers of Galactic chemical evolution. I. Fe abundances in NGC 2660, NGC 3960, and Berkeley 32","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.Bragaglia (INAF/Osservatiorio Astronomico di Bologna), E.Carretta (INAF/Osservatiorio Astronomico di Bologna), L.Prisinzano (INAF/Osservatorio Astronomico di Palermo), M.Tosi (INAF/Osservatiorio Astronomico di Bologna), P. Sestito (INAF/Osservatorio Astronomico di Palermo; INAF/Osservatorio Astrofisico di Arcetri; INAF/Osservatiorio Astronomico di Bologna), S. Randich (INAF/Osservatorio Astrofisico di Arcetri)","submitted_at":"2006-07-19T09:51:33Z","abstract_excerpt":"We obtained high-resolution UVES/FLAMES observations of a sample of nine old open clusters spanning a wide range of ages and Galactocentric radii. The goal of the project is to investigate the radial metallicity gradient in the disk, as well as the abundance of key elements (alpha and Fe-peak elements). In this paper we present the results for the metallicity of three clusters: NGC 2660 (age ~1 Gyr, Galactocentric distance of 8.68 kpc), NGC 3960 (~ 1 Gyr, 7.80 kpc), and Be 32 (~6-7 Gyr, 11.30 kpc). For Be 32 and NGC 2660, our study provides the first metallicity determination based on high-res"},"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/0607438","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-07-19T09:51:33Z","cross_cats_sorted":[],"title_canon_sha256":"8e2b44da1b14e0d0efe976a2e8eb8ac9fc22d14eb55db68e455d47969fbc61e9","abstract_canon_sha256":"20d21fb0139cc7a2aa9b3181fcdf25f23253d76708028ec93aab0a655a598750"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:35:03.753823Z","signature_b64":"TUYWdMlGmdVJerPRMtOiqiMc59Jevq0ylmBgqCxfmL2QqShbGaFVE7vxIizNtDBkC4E1uFqXmx8X/iOvWWrVCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d4c05b8715e7b343e5f997c8a05f642a017a8a5658fa65097de3f5e9c22b38ec","last_reissued_at":"2026-05-18T04:35:03.753400Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:35:03.753400Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Old open clusters as key tracers of Galactic chemical evolution. I. Fe abundances in NGC 2660, NGC 3960, and Berkeley 32","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.Bragaglia (INAF/Osservatiorio Astronomico di Bologna), E.Carretta (INAF/Osservatiorio Astronomico di Bologna), L.Prisinzano (INAF/Osservatorio Astronomico di Palermo), M.Tosi (INAF/Osservatiorio Astronomico di Bologna), P. Sestito (INAF/Osservatorio Astronomico di Palermo; INAF/Osservatorio Astrofisico di Arcetri; INAF/Osservatiorio Astronomico di Bologna), S. Randich (INAF/Osservatorio Astrofisico di Arcetri)","submitted_at":"2006-07-19T09:51:33Z","abstract_excerpt":"We obtained high-resolution UVES/FLAMES observations of a sample of nine old open clusters spanning a wide range of ages and Galactocentric radii. The goal of the project is to investigate the radial metallicity gradient in the disk, as well as the abundance of key elements (alpha and Fe-peak elements). In this paper we present the results for the metallicity of three clusters: NGC 2660 (age ~1 Gyr, Galactocentric distance of 8.68 kpc), NGC 3960 (~ 1 Gyr, 7.80 kpc), and Be 32 (~6-7 Gyr, 11.30 kpc). For Be 32 and NGC 2660, our study provides the first metallicity determination based on high-res"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0607438","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":"astro-ph/0607438","created_at":"2026-05-18T04:35:03.753468+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0607438v1","created_at":"2026-05-18T04:35:03.753468+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0607438","created_at":"2026-05-18T04:35:03.753468+00:00"},{"alias_kind":"pith_short_12","alias_value":"2TAFXBYV46ZU","created_at":"2026-05-18T12:25:53.939244+00:00"},{"alias_kind":"pith_short_16","alias_value":"2TAFXBYV46ZUHZPZ","created_at":"2026-05-18T12:25:53.939244+00:00"},{"alias_kind":"pith_short_8","alias_value":"2TAFXBYV","created_at":"2026-05-18T12:25:53.939244+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/2TAFXBYV46ZUHZPZS7EKAX3EFI","json":"https://pith.science/pith/2TAFXBYV46ZUHZPZS7EKAX3EFI.json","graph_json":"https://pith.science/api/pith-number/2TAFXBYV46ZUHZPZS7EKAX3EFI/graph.json","events_json":"https://pith.science/api/pith-number/2TAFXBYV46ZUHZPZS7EKAX3EFI/events.json","paper":"https://pith.science/paper/2TAFXBYV"},"agent_actions":{"view_html":"https://pith.science/pith/2TAFXBYV46ZUHZPZS7EKAX3EFI","download_json":"https://pith.science/pith/2TAFXBYV46ZUHZPZS7EKAX3EFI.json","view_paper":"https://pith.science/paper/2TAFXBYV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0607438&json=true","fetch_graph":"https://pith.science/api/pith-number/2TAFXBYV46ZUHZPZS7EKAX3EFI/graph.json","fetch_events":"https://pith.science/api/pith-number/2TAFXBYV46ZUHZPZS7EKAX3EFI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2TAFXBYV46ZUHZPZS7EKAX3EFI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2TAFXBYV46ZUHZPZS7EKAX3EFI/action/storage_attestation","attest_author":"https://pith.science/pith/2TAFXBYV46ZUHZPZS7EKAX3EFI/action/author_attestation","sign_citation":"https://pith.science/pith/2TAFXBYV46ZUHZPZS7EKAX3EFI/action/citation_signature","submit_replication":"https://pith.science/pith/2TAFXBYV46ZUHZPZS7EKAX3EFI/action/replication_record"}},"created_at":"2026-05-18T04:35:03.753468+00:00","updated_at":"2026-05-18T04:35:03.753468+00:00"}