{"paper":{"title":"Revisiting the Galactic age-metallicity relation from wide white dwarf-main-sequence binaries","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"The age-metallicity relation in the Galactic disk shows large intrinsic scatter at all ages.","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Alberto Rebassa-Mansergas, Iset Tejero-G\\'omez, Roberto Raddi","submitted_at":"2026-04-17T10:57:37Z","abstract_excerpt":"The age-metallicity relation (AMR) is a fundamental observational constraint for understanding the chemical evolution of the Galaxy. As reliable cosmochronometers, white dwarfs in binary systems with main sequence companions (WD+MS binaries) provide excellent laboratories to study this relation, since both components are expected to be coeval. We construct a sample of widely separated WD+MS binaries using data from the third data release of the Gaia mission in order to investigate the AMR of the Galactic disk. The sample is identified using photometric measurements and parallaxes of both compo"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We derive the AMR from several sub-samples of WD+MS that use independent measurements of [Fe/H] abundances and consistently find a large dispersion in [Fe/H] at all ages. This behaviour agrees with previous determinations of the AMR based on both WD+MS binaries and samples of isolated stars.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the white dwarf and main-sequence components in wide binaries are coeval so that white dwarf cooling ages accurately represent the system age, and that the compiled [Fe/H] values from the main-sequence companions faithfully reflect the birth metallicity of the system.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Wide WD+MS binaries from Gaia show large intrinsic scatter in [Fe/H] at all ages for the Galactic disk AMR, agreeing with prior studies and indicating complex chemical evolution.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"The age-metallicity relation in the Galactic disk shows large intrinsic scatter at all ages.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"f09adb1fd35833353bea2a333793faa2b3bcca70f30035c9fee850c6ba1a64b3"},"source":{"id":"2604.15939","kind":"arxiv","version":1},"verdict":{"id":"0893be24-3896-464b-b540-8ba9d8ff0f04","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T07:58:53.620483Z","strongest_claim":"We derive the AMR from several sub-samples of WD+MS that use independent measurements of [Fe/H] abundances and consistently find a large dispersion in [Fe/H] at all ages. This behaviour agrees with previous determinations of the AMR based on both WD+MS binaries and samples of isolated stars.","one_line_summary":"Wide WD+MS binaries from Gaia show large intrinsic scatter in [Fe/H] at all ages for the Galactic disk AMR, agreeing with prior studies and indicating complex chemical evolution.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the white dwarf and main-sequence components in wide binaries are coeval so that white dwarf cooling ages accurately represent the system age, and that the compiled [Fe/H] values from the main-sequence companions faithfully reflect the birth metallicity of the system.","pith_extraction_headline":"The age-metallicity relation in the Galactic disk shows large intrinsic scatter at all ages."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.15939/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":56,"sample":[{"doi":"","year":2015,"title":"Althaus, L. G., Camisassa, M. E., Miller Bertolami, M. M., Córsico, A. H., & García-Berro, E. 2015, A&A, 576, A9","work_id":"a522e7b7-924a-45da-ba9b-7d9e7c3e6616","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2023,"title":"2023, A&A, 678, A158","work_id":"8b1be293-dda7-484a-8973-bab998d7162a","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2021,"title":"Barrientos, M. & Chanamé, J. 2021, ApJ, 923, 181","work_id":"379fb3dc-a047-425c-8b4a-15a33a22c5aa","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2019,"title":"Camisassa, M. E., Althaus, L. G., Córsico, A. H., et al. 2019, A&A, 625, A87","work_id":"3d03c159-2946-4c7d-9353-eb6340f984c3","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2016,"title":"Camisassa, M. E., Althaus, L. G., Córsico, A. H., et al. 2016, ApJ, 823, 158","work_id":"582b4c3d-7f2c-43a6-8431-e749efe25fa3","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":56,"snapshot_sha256":"caf07e97bffe2a09ba255651a7c588c92fc9073f9f46711a3524a985fe6f4211","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"}