Abstract
The Gaia-ESO Survey is a public spectroscopic survey that targeted ≲105 stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (Teff ∼ 30 000-52 000 K) all the way to K-M (-3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
| Original language | English |
|---|---|
| Article number | A129 |
| Number of pages | 33 |
| Journal | Astronomy & Astrophysics |
| Volume | 676 |
| DOIs | |
| Publication status | Published - 1 Aug 2023 |
Keywords
- Galaxy: stellar content
- Methods: data analysis
- Methods: statistical
- Stars: abundances
- Stars: fundamental parameters
- Techniques: spectroscopic
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In: Astronomy & Astrophysics, Vol. 676, A129, 01.08.2023.
Research output: Contribution to journal › Article › Research › peer-review
TY - JOUR
T1 - The Gaia-ESO Survey
T2 - Homogenisation of stellar parameters and elemental abundances
AU - Hourihane, A.
AU - François, P.
AU - Worley, C. C.
AU - Magrini, L.
AU - Gonneau, A.
AU - Casey, A. R.
AU - Gilmore, G.
AU - Randich, S.
AU - Sacco, G. G.
AU - Recio-Blanco, A.
AU - Korn, A. J.
AU - Allende Prieto, C.
AU - Smiljanic, R.
AU - Blomme, R.
AU - Bragaglia, A.
AU - Walton, N. A.
AU - Van Eck, S.
AU - Bensby, T.
AU - Lanzafame, A.
AU - Frasca, A.
AU - Franciosini, E.
AU - Damiani, F.
AU - Lind, K.
AU - Bergemann, M.
AU - Bonifacio, P.
AU - Hill, V.
AU - Lobel, A.
AU - Montes, D.
AU - Feuillet, D. K.
AU - Tautvaišiene, G.
AU - Guiglion, G.
AU - Tabernero, H. M.
AU - González Hernández, J. I.
AU - Gebran, M.
AU - Van Der Swaelmen, M.
AU - Mikolaitis, S.
AU - Daflon, S.
AU - Merle, T.
AU - Morel, T.
AU - Lewis, J. R.
AU - González Solares, E. A.
AU - Murphy, D. N.A.
AU - Jeffries, R. D.
AU - Jackson, R. J.
AU - Feltzing, S.
AU - Prusti, T.
AU - Carraro, G.
AU - Biazzo, K.
AU - Prisinzano, L.
AU - Jofré, P.
AU - Zaggia, S.
AU - Drazdauskas, A.
AU - Stonkuté, E.
AU - Marfil, E.
AU - Jiménez-Esteban, F.
AU - Mahy, L.
AU - Gutiérrez Albarrán, M. L.
AU - Berlanas, S. R.
AU - Santos, W.
AU - Morbidelli, L.
AU - Spina, L.
AU - Minkevičiūte, R.
N1 - Funding Information: Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes 188.B-3002, 193.B-0936, and 197.B-1074. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, 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’Università 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. L. Magrini and M. Van der Swaelmen acknowledge support by the WEAVE Italian consortium, and by the INAF Grant “Checs”. A.J. Korn acknowledges support by the Swedish National Space Agency (SNSA). A. Lobel acknowledges support in part by the Belgian Federal Science Policy Office under contract no. BR/143/A2/BRASS and by the European Union Framework Programme for Research and Innovation Horizon 2020 (2014-2020) under the Marie Sklodowska-Curie grant Agreement No. 823734. D.K. Feuillet was partly supported by grant no. 2016-03412 from the Swedish Research Council. D. Montes acknowledges financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovation through project PID2019-109522GB-C54 /AEI/10.13039/501100011033. E. Marfil acknowledges financial support from the European Regional Development Fund (ERDF) and the Gob-ierno de Canarias through project ProID2021010128. J.I. Gonzalez Hernandez acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) project PID2020-117493GB-I00. M. Bergemann is supported through the Lise Meitner grant from the Max Planck Society and acknowledges support by the Collaborative Research centre SFB 881 (projects A5, A10), Heidelberg University, of the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation). This project has received funding from the European Research Council (ERC) under the European Union, Horizon 2020 research and innovation programme (Grant agreement No. 949173). P. Jofré acknowledges financial support of FONDECYT Regular 1200703 as well as Nucleo Mile-nio ERIS NCN2021_017. R. Smiljanic acknowledges support from the National Science Centre, Poland (2014/15/B/ST/03981). S.R. Berlanas acknowledges support by MCIN/AEI/10.13039/501100011033 (contract FJC 2020-045785-I) and NextGeneration EU/PRTR and MIU (UNI/551/2021) through grant Margarita Salas-ULL. T. Bensby acknowledges financial support by grant No. 2018-04857 from the Swedish Research Council. T. Merle is supported by a grant from the Foundation ULB. T. Morel are grateful to Belgian F.R.S.-FNRS for support, and are also indebted for an ESA/PRODEX Belspo contract related to the Gaia Data Processing and Analysis Consortium and for support through an ARC grant for Concerted Research Actions financed by the Federation Wallonie-Brussels. W. Santos acknowledges FAPERJ for a Ph.D. fellowship. H.M. Tabernero acknowledges financial support from the Agencia Estatal de Investigation of the Ministerio de Ciencia, Innovation through project PID2019-109522GB-C51/AEI/10.13039/501100011033. Publisher Copyright: © 2023 The Authors.
PY - 2023/8/1
Y1 - 2023/8/1
N2 - The Gaia-ESO Survey is a public spectroscopic survey that targeted ≲105 stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (Teff ∼ 30 000-52 000 K) all the way to K-M (-3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
AB - The Gaia-ESO Survey is a public spectroscopic survey that targeted ≲105 stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (Teff ∼ 30 000-52 000 K) all the way to K-M (-3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
KW - Galaxy: stellar content
KW - Methods: data analysis
KW - Methods: statistical
KW - Stars: abundances
KW - Stars: fundamental parameters
KW - Techniques: spectroscopic
UR - http://www.scopus.com/inward/record.url?scp=85169927389&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202345910
DO - 10.1051/0004-6361/202345910
M3 - Article
AN - SCOPUS:85169927389
SN - 0004-6361
VL - 676
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
M1 - A129
ER -