{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:QB5Q6YLJ46NP5J7TUG62WYNJLW","short_pith_number":"pith:QB5Q6YLJ","schema_version":"1.0","canonical_sha256":"807b0f6169e79afea7f3a1bdab61a95db05e2af313a0eba9b7fffd9658324dea","source":{"kind":"arxiv","id":"1409.0568","version":1},"attestation_state":"computed","paper":{"title":"Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Bayo, A. Bragaglia, A. C. Lanzafame, A. Ferguson, A. Frasca, A. Hourihane, A. J. Korn, A. M. Serenelli, A. Mucciarelli, A. Recio-Blanco, A. Vallenari, B. Edvardsson, C. Allende Prieto, C. Babusiaux, C. C. Worley, C. J. Hansen, C. Lardo, C. Martayan, C. Munoz, C. Soubiran, D. Geisler, D. Montes, E. Alfaro, E. Caffau, E. Delgado-Mena, E. Flaccomio, E. Franciosini, E. Friel, E. Maiorca, E. Pancino, E. Puzeras, F. Damiani, G. Barisevicius, G. Carraro, G. Gilmore, G. Guiglion, G. Marconi, G. Micela, G. Ruchti, G. Sacco, G. Tautvaisiene, H. G. Ludwig, H. Jonsson, H. R. Jacobson, H. Tabernero, H-W. Rix, I. Negueruela, I. San Roman, J. Binney, J. Drew, J. I. Gonzalez Hernandez, J. Lewis, K. Biazzo, K. Lind, L. Magrini, L. Monaco, L. Morbidelli, L. Pasquini, L. Prisinzano, L. Sbordone, L. Spina, M. Asplund, M. Bergemann, M. Irwin, M. Steffen, M. T. Costado, M. Valentini, M. Weber, N. C. Santos, N. Ryde, N. Walton, P. Bonifacio, P. de Laverny, P. Donati, P. Francois, P. Gruyters, P. Jofre, R. Blomme, R. Jackson, R. Jeffries, R. Smiljanic, R. Sordo, S. Blanco-Cuaresma, S. Duffau, S. Feltzing, S. G. Sousa, S. Koposov, S. Mikolaitis, S. Randich, S. Van Eck, S. Villanova, S. Zaggia, T. Bensby, T. Cantat-Gaudin, T. Masseron, T. Morel, T. Nordlander, T. Prusti, U. Heiter, V. Hill, V. Zh. Adibekyan, Y. Chorniy","submitted_at":"2014-09-01T21:19:36Z","abstract_excerpt":"The Gaia-ESO Survey is obtaining high-quality spectroscopic data for about 10^5 stars using FLAMES at the VLT. UVES high-resolution spectra are being collected for about 5000 FGK-type stars. These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-to-method dispersion) and accuracy (biases with respect to the reference values) of the final parameters. These results are part of"},"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":"1409.0568","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-09-01T21:19:36Z","cross_cats_sorted":[],"title_canon_sha256":"86f5f1c2eea6aa580259bb8a12989112dadbcd9ea9b0952ce6c70fde52349c5b","abstract_canon_sha256":"7be59d0d7102f3e158211b43ceb0e1f77b4af551fc26cbd9a46ce1651ec30b39"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:38:38.724128Z","signature_b64":"drRawFo5+nYqXUvCPxDX5JERQGmQo3WORJ0G0yUJlegQ2k0h1lEFm5Y5npwbjYdbzqsSVnRNZxeyUGrmRsI/AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"807b0f6169e79afea7f3a1bdab61a95db05e2af313a0eba9b7fffd9658324dea","last_reissued_at":"2026-05-18T02:38:38.723631Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:38:38.723631Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Bayo, A. Bragaglia, A. C. Lanzafame, A. Ferguson, A. Frasca, A. Hourihane, A. J. Korn, A. M. Serenelli, A. Mucciarelli, A. Recio-Blanco, A. Vallenari, B. Edvardsson, C. Allende Prieto, C. Babusiaux, C. C. Worley, C. J. Hansen, C. Lardo, C. Martayan, C. Munoz, C. Soubiran, D. Geisler, D. Montes, E. Alfaro, E. Caffau, E. Delgado-Mena, E. Flaccomio, E. Franciosini, E. Friel, E. Maiorca, E. Pancino, E. Puzeras, F. Damiani, G. Barisevicius, G. Carraro, G. Gilmore, G. Guiglion, G. Marconi, G. Micela, G. Ruchti, G. Sacco, G. Tautvaisiene, H. G. Ludwig, H. Jonsson, H. R. Jacobson, H. Tabernero, H-W. Rix, I. Negueruela, I. San Roman, J. Binney, J. Drew, J. I. Gonzalez Hernandez, J. Lewis, K. Biazzo, K. Lind, L. Magrini, L. Monaco, L. Morbidelli, L. Pasquini, L. Prisinzano, L. Sbordone, L. Spina, M. Asplund, M. Bergemann, M. Irwin, M. Steffen, M. T. Costado, M. Valentini, M. Weber, N. C. Santos, N. Ryde, N. Walton, P. Bonifacio, P. de Laverny, P. Donati, P. Francois, P. Gruyters, P. Jofre, R. Blomme, R. Jackson, R. Jeffries, R. Smiljanic, R. Sordo, S. Blanco-Cuaresma, S. Duffau, S. Feltzing, S. G. Sousa, S. Koposov, S. Mikolaitis, S. Randich, S. Van Eck, S. Villanova, S. Zaggia, T. Bensby, T. Cantat-Gaudin, T. Masseron, T. Morel, T. Nordlander, T. Prusti, U. Heiter, V. Hill, V. Zh. Adibekyan, Y. Chorniy","submitted_at":"2014-09-01T21:19:36Z","abstract_excerpt":"The Gaia-ESO Survey is obtaining high-quality spectroscopic data for about 10^5 stars using FLAMES at the VLT. UVES high-resolution spectra are being collected for about 5000 FGK-type stars. These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-to-method dispersion) and accuracy (biases with respect to the reference values) of the final parameters. These results are part of"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1409.0568","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":"1409.0568","created_at":"2026-05-18T02:38:38.723705+00:00"},{"alias_kind":"arxiv_version","alias_value":"1409.0568v1","created_at":"2026-05-18T02:38:38.723705+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1409.0568","created_at":"2026-05-18T02:38:38.723705+00:00"},{"alias_kind":"pith_short_12","alias_value":"QB5Q6YLJ46NP","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_16","alias_value":"QB5Q6YLJ46NP5J7T","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_8","alias_value":"QB5Q6YLJ","created_at":"2026-05-18T12:28:43.426989+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.11594","citing_title":"Empirical colour--effective temperature relations in the SDSS system from IRFM temperatures of GALAH and APOGEE stars","ref_index":5,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW","json":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW.json","graph_json":"https://pith.science/api/pith-number/QB5Q6YLJ46NP5J7TUG62WYNJLW/graph.json","events_json":"https://pith.science/api/pith-number/QB5Q6YLJ46NP5J7TUG62WYNJLW/events.json","paper":"https://pith.science/paper/QB5Q6YLJ"},"agent_actions":{"view_html":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW","download_json":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW.json","view_paper":"https://pith.science/paper/QB5Q6YLJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1409.0568&json=true","fetch_graph":"https://pith.science/api/pith-number/QB5Q6YLJ46NP5J7TUG62WYNJLW/graph.json","fetch_events":"https://pith.science/api/pith-number/QB5Q6YLJ46NP5J7TUG62WYNJLW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW/action/storage_attestation","attest_author":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW/action/author_attestation","sign_citation":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW/action/citation_signature","submit_replication":"https://pith.science/pith/QB5Q6YLJ46NP5J7TUG62WYNJLW/action/replication_record"}},"created_at":"2026-05-18T02:38:38.723705+00:00","updated_at":"2026-05-18T02:38:38.723705+00:00"}