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Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge (supported by UKRI-STFC grants: ST/N005805/1, ST/T003081/1 and ST/X001857/1), and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell' Istruzione, dell' Universita e della Ricerca (MIUR) in the form of the grant "Premiale VLT 2012". The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. D.M. acknowledges financial support from the Agencia Estatal de Investigacion 10.13039/501100011033 of the Ministerio de Ciencia e Innovacion and the ERDF "A way of making Europe" through project PID2019-109522GBC54. F.J.E. acknowledges support from ESA through the Faculty of the European Space Astronomy Centre (ESAC) - Funding reference 4000139151/22/ES/CM. H.M.T. acknowledges financial support from the Agencia Estatal de Investigacion (AEI/10.13039/501100011033) of the Ministerio de Ciencia e Innovacion and the ERDF "A way of making Europe" through project PID2019-109522GB-C51. S.V. gratefully acknowledges the support provided by Fondecyt reg. 1220264 and by the ANID BASAL projects ACE210002 and FB210003. S.M. thanks the COST Action CA18104: MW-Gaia. U.H. acknowledges support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). E.J.A. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (CEX2021-001131-S). T.B. was funded by the project grant no. 2018-04857 from the Swedish Research Council. G.G. acknowledges support by the Collaborative Research Centre SFB 881 (projects A5, A10), Heidelberg University, of the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) and by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement 949173). P.J. acknowledges support from Fondecyt Regular Ladder Number 1231057, Millenium Nucleus ERIS NCN2021_017, Centros ANID Iniciativa Milenio. J.I.G.H. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) project PID2020-117493GB-I00. E.M. acknowledges financial support through a "Margarita Salas" postdoctoral fellowship from Universidad Complutense de Madrid (CT18/22), funded by the Spanish Ministerio de Universidades with NextGeneration EU funds.

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The Gaia-ESO Survey: The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

Publicated to:Astronomy & Astrophysics. 684 A148- - 2024-04-19 684(), DOI: 10.1051/0004-6361/202347558

Authors: Worley, C C; Smiljanic, R; Magrini, L; Frasca, A; Franciosini, E; Montes, D; Feuillet, D K; Tabernero, H M; Hernandez, J I Gonzalez; Villanova, S; Mikolaitis, S; Lind, K; Tautvaisiene, G; Casey, A R; Korn, A J; Bonifacio, P; Soubiran, C; Caffau, E; Guiglion, G; Merle, T; Hourihane, A; Gonneau, A; Francois, P; Randich, S; Gilmore, G; Lewis, J R; Murphy, D N A; Jeffries, R D; Koposov, S E; Blomme, R; Lanzafame, A C; Bensby, T; Bragaglia, A; Alfaro, E J; Walton, N A; Vallenari, A; Prusti, T; Biazzo, K; Jofre, P; Zaggia, S; Heiter, U; Marfil, E; Jimenez-Esteban, F; Albarran, M L Gutierrez; Morbidelli, L

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Abstract

The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted 105 stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high (R similar to 47 000) and GIRAFFE medium (R similar to 20 000) resolution spectra. The analysis of the Gaia-ESO spectra was the work of multiple analysis teams (nodes) within five working groups (WG). The homogenisation of the stellar parameters within WG11 (high resolution observations of FGK stars) and the homogenisation of the stellar parameters within WG10 (medium resolution observations of FGK stars) is described here. In both cases, the homogenisation was carried out using a Bayesian Inference method developed specifically for the Gaia-ESO Survey by WG11. The method was also used for the chemical abundance homogenisation within WG11, however, the WG10 chemical abundance data set was too sparsely populated so basic corrections for each node analysis were employed for the homogenisation instead. The WG10 homogenisation primarily used the cross-match of stars with WG11 as the reference set in both the stellar parameter and chemical abundance homogenisation. In this way the WG10 homogenised results have been placed directly onto the WG11 stellar parameter and chemical abundance scales. The reference set for the metal-poor end was sparse which limited the effectiveness of the homogenisation in that regime. For WG11, the total number of stars for which stellar parameters were derived was 6 231 with typical uncertainties for T-eff, log g and [Fe/H] of 32 K, 0.05 and 0.05 respectively. One or more chemical abundances out of a possible 39 elements were derived for 6 188 of the stars. For WG10, the total number of stars for which stellar parameters were derived was 76 675 with typical uncertainties for T-eff, log g and [Fe/H] of 64 K, 0.15 and 0.07 respectively. One or more chemical abundances out of a possible 30 elements were derived for 64177 of the stars.

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