{"paper":{"title":"Gaia FGK Benchmark Stars - Metallicity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"A. Mucciarelli, A. Recio-Blanco, A. Vallenari, C. C. Worley, C. Lardo, C. Soubiran, D. Montes, E. Pancino, H. Tabernero, J. I. Gonzalez-Hernandez, J. Sobeck, K. Lind, L. Magrini, M. Bergemann, Paula Jofre, P. de Laverny, R. Sordo, S. Blanco-Cuaresma, S. G. Sousa, S. Van Eck, T. Cantat-Gaudin, T. Masseron, T. Nordlander, U. Heiter, V. Hill","submitted_at":"2013-09-04T16:48:38Z","abstract_excerpt":"To calibrate automatic pipelines that determine atmospheric parameters of stars, one needs a sample of stars -- ``benchmark stars'' -- with well defined parameters to be used as a reference We provide a detailed documentation of the determination of the iron abundance of the 34 FGK-type benchmark stars selected to be the pillars for calibration of the one billion Gaia stars. They cover a wide range of temperatures, surface gravities and metallicities. Up to seven different methods were used to analyze an observed spectral library of high resolution and high signal-to-noise ratio. The metallici"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1309.1099","kind":"arxiv","version":2},"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"}