Issue |
A&A
Volume 661, May 2022
|
|
---|---|---|
Article Number | A120 | |
Number of page(s) | 26 | |
Section | Catalogs and data | |
DOI | https://doi.org/10.1051/0004-6361/202142349 | |
Published online | 24 May 2022 |
The Gaia-ESO Survey: The analysis of the hot-star spectra
1
Royal Observatory of Belgium,
Ringlaan 3,
1180
Brussels,
Belgium
e-mail: Ronny.Blomme@oma.be
2
Observatório Nacional/MCTIC,
R. Gal. José Cristino 77, São Cristovão,
20921-400
Rio de Janeiro/RJ,
Brazil
3
Department of Chemistry and Physics, Saint Mary’s College,
Notre Dame,
IN
46556,
USA
4
Instituto de Astrofísica de Canarias,
38205
La Laguna,
Tenerife,
Spain
5
Departamento de Astrofísica, Universidad de La Laguna,
38206
La Laguna,
Tenerife,
Spain
6
Instituut voor Sterrenkunde,
KU Leuven, Celestijnlaan 200D, Bus 2401,
3001
Leuven,
Belgium
7
Space Sciences, Technologies, and Astrophysics Research (STAR) Institute, Université de Liège, Quartier Agora,
Bât B5c, allée du 6 août, 19c,
4000
Liège,
Belgium
8
LUPM-UMR 5299, CNRS & Université Montpellier,
Place Eugene Bataillon,
34095
Montpellier Cedex 05,
France
9
Departamento de Física Aplicada, Facultad de Ciencias, Universidad de Alicante,
Carretera de San Vicente s/n,
03690
San Vicente del Raspeig,
Spain
10
Centre National d’Etudes Spatiales,
Toulouse,
France
11
Centro de Astrobiología, CSIC-INTA, Campus ESAC,
Camino bajo del castillo s/n, 28 692,
Villanueva de la Cañada,
Spain
12
Observatoire de Genève, Université de Genève,
Chemin Pegasi 51,
1290
Versoix,
Switzerland
13
Departamento de Astrofísica, Centro de Astrobiología (CSICINTA), ESAC Campus,
Camino Bajo del Castillo s/n,
28692
Villanueva de la Cañada,
Madrid,
Spain
14
Institut für Astro- und Teilchenphysik, Universität Innsbruck,
Technikerstr. 25/8,
6020
Innsbruck,
Austria
15
Institute of Astronomy, University of Cambridge,
Madingley Road,
Cambridge
CB3 0HA,
UK
16
INAF – Osservatorio Astrofisico di Arcetri,
Largo E. Fermi 5,
50125
Firenze,
Italy
17
ESA, ESTEC,
Keplerlaan 1, PO Box 299
2200
AG Noordwijk,
The Netherlands
18
INAF – Padova Observatory,
Vicolo dell’Osservatorio 5,
35122
Padova,
Italy
19
Instituto de Astrofísica de Andalucía (CSIC),
Glorieta de la Astronomía s/n,
Granada
18008,
Spain
20
Lund Observatory, Department of Astronomy and Theoretical Physics,
Box 43,
221 00
Lund,
Sweden
21
INAF – Osservatorio di Astrofisica e Scienza dello Spazio,
via P. Gobetti 93/3,
40129
Bologna,
Italy
22
INAF – Osservatorio Astronomico di Palermo,
Piazza del Parlamento 1,
90134
Palermo,
Italy
23
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot,
5 place Jules Janssen,
92190
Meudon,
France
24
Observational Astrophysics, Division of Astronomy and Space Physics, Department of Physics and Astronomy, Uppsala University,
Box 516,
751 20
Uppsala,
Sweden
25
Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Università di Catania,
via S. Sofia 78,
95123
Catania,
Italy
26
Space Science Data Center – Agenzia Spaziale Italiana,
via del Politecnico, s.n.c.,
00133
Roma,
Italy
27
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences,
ul. Bartycka 18,
00-716
Warsaw,
Poland
28
Max-Planck Institut für Astronomie,
Königstuhl 17,
69117
Heidelberg,
Germany
29
Niels Bohr International Academy, Niels Bohr Institute,
Blegdamsvej 17,
2100
Copenhagen,
Denmark
30
Dipartimento di Fisica e Astronomia, Università di Padova,
Vicolo dell’Osservatorio 3,
35122
Padova,
Italy
31
Núcleo de Astronomía, Facultad de Ingeniería y Ciencias, Universidad Diego Portales,
Av. Ejército 441,
Santiago,
Chile
Received:
1
October
2021
Accepted:
15
February
2022
Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of six years, spectra of ~105 stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra.
Aims. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of the hottest stars (O, B, and A type, with a formal cutoff of Teff > 7000 K) that were observed as part of GES. We present the procedures and techniques that have been applied to the reduced spectra in order to determine the stellar parameters and abundances of these stars.
Methods. The procedure used was similar to that of other working groups in GES. A number of groups (called Nodes) each independently analyse the spectra via state-of-the-art techniques and codes. Specific for the analysis in WG13 was the large temperature range covered (Teff ≈ 7000–50 000 K), requiring the use of different analysis codes. Most Nodes could therefore only handle part of the data. Quality checks were applied to the results of these Nodes by comparing them to benchmark stars, and by comparing them to one another. For each star the Node values were then homogenised into a single result: the recommended parameters and abundances.
Results. Eight Nodes each analysed part of the data. In total 17 693 spectra of 6462 stars were analysed, most of them in 37 open star clusters. The homogenisation led to stellar parameters for 5584 stars. Abundances were determined for a more limited number of stars. The elements studied are He, C, N, O, Ne, Mg, Al, Si, and Sc. Abundances for at least one of these elements were determined for 292 stars.
Conclusions. The hot-star data analysed here, as well as the GES data in general, will be of considerable use in future studies of stellar evolution and open clusters.
Key words: surveys / catalogs / stars: fundamental parameters / stars: abundances / stars: early-type / techniques: spectroscopic
© ESO 2022
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