000005843 001__ 5843
000005843 005__ 20220922130540.0
000005843 0247_ $$2DOI$$a10.1051/0004-6361/202142349
000005843 037__ $$aSCART-2022-0089
000005843 100__ $$aBlomme, R
000005843 245__ $$aThe Gaia-ESO Survey: The analysis of the hot-star spectra
000005843 260__ $$c2022
000005843 520__ $$aContext. The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of six years, spectra of ~105 stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra. Aims. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of the hottest stars (O, B, and A type, with a formal cutoff of Teff > 7000 K) that were observed as part of GES. We present the procedures and techniques that have been applied to the reduced spectra in order to determine the stellar parameters and abundances of these stars. Methods. The procedure used was similar to that of other working groups in GES. A number of groups (called Nodes) each independently analyse the spectra via state-of-the-art techniques and codes. Specific for the analysis in WG13 was the large temperature range covered (Teff ≈ 7000–50 000 K), requiring the use of different analysis codes. Most Nodes could therefore only handle part of the data. Quality checks were applied to the results of these Nodes by comparing them to benchmark stars, and by comparing them to one another. For each star the Node values were then homogenised into a single result: the recommended parameters and abundances. Results. Eight Nodes each analysed part of the data. In total 17 693 spectra of 6462 stars were analysed, most of them in 37 open star clusters. The homogenisation led to stellar parameters for 5584 stars. Abundances were determined for a more limited number of stars. The elements studied are He, C, N, O, Ne, Mg, Al, Si, and Sc. Abundances for at least one of these elements were determined for 292 stars. Conclusions. The hot-star data analysed here, as well as the GES data in general, will be of considerable use in future studies of stellar evolution and open clusters.
000005843 594__ $$aNO
000005843 6531_ $$a surveys 
000005843 6531_ $$a catalogs 
000005843 6531_ $$a stars: fundamental parameters 
000005843 6531_ $$a stars: abundances 
000005843 6531_ $$a stars: early-type 
000005843 6531_ $$a techniques: spectroscopic
000005843 700__ $$aDaflon, S
000005843 700__ $$aGebran, M
000005843 700__ $$aHerrero, A
000005843 700__ $$aLobel, A
000005843 700__ $$aMahy, L
000005843 700__ $$aMartins, F
000005843 700__ $$aMorel, T
000005843 700__ $$aR Berlanas, S
000005843 700__ $$aBlazère, A
000005843 700__ $$aFrémat, Y
000005843 700__ $$aGosset, E
000005843 700__ $$aMaiz Apellaniz, J
000005843 700__ $$aSantos, W
000005843 700__ $$aSemaan, T
000005843 700__ $$aSimon-Diaz, S
000005843 700__ $$aVolpi, D
000005843 700__ $$aHolgado, G
000005843 700__ $$aJiménez-Esteban, F
000005843 700__ $$aF Nieva, M
000005843 700__ $$aPrzybilla, N
000005843 700__ $$aGilmore, G
000005843 700__ $$aRandich, S
000005843 700__ $$aNegueruela, I
000005843 700__ $$aPrusti, T
000005843 700__ $$aVallenari, A
000005843 700__ $$aJ Alfaro, E
000005843 700__ $$aBensby, T
000005843 700__ $$aBragaglia, A
000005843 700__ $$aFlaccomio, E
000005843 700__ $$aFrancois, P
000005843 700__ $$aJ Korn, A
000005843 700__ $$aLanzafame, A
000005843 700__ $$aPancino, E
000005843 700__ $$aSmiljanic, R
000005843 700__ $$aBergemann, M
000005843 700__ $$aCarraro, G
000005843 700__ $$aFranciosini, E
000005843 700__ $$aGonneau, A
000005843 700__ $$aHeiter, U
000005843 700__ $$aHourihane, A
000005843 700__ $$aJofré, P
000005843 700__ $$aMagrini, L
000005843 700__ $$aMorbidelli, L
000005843 700__ $$aG Sacco, G
000005843 700__ $$aC Worley, C
000005843 700__ $$aZaggia, S
000005843 773__ $$nA120$$pAstronomy & Astrophysics$$v661$$y2022
000005843 8560_ $$felodie.brahy@ksb-orb.be
000005843 85642 $$ahttps://www.aanda.org/articles/aa/full_html/2022/05/aa42349-21/aa42349-21.html
000005843 905__ $$apublished in
000005843 980__ $$aREFERD