000002153 001__ 2153
000002153 005__ 20160706145943.0
000002153 0247_ $$2DOI$$a10.1051/0004-6361/201423619
000002153 037__ $$aASTROimport-310
000002153 100__ $$aSacco, G. G.
000002153 245__ $$aThe Gaia-ESO Survey: processing FLAMES-UVES spectra
000002153 260__ $$c2014
000002153 520__ $$aThe Gaia-ESO Survey is a large public spectroscopic survey that aims to derive radial velocities and fundamental parameters of about 105 Milky Way stars in the field and in clusters. Observations are carried out with the multi-object optical spectrograph FLAMES, using simultaneously the medium-resolution (R ~ 20 000) GIRAFFE spectrograph and the high-resolution (R ~ 47 000) UVES spectrograph. In this paper we describe the methods and the software used for the data reduction, the derivation of the radial velocities, and the quality control of the FLAMES-UVES spectra. Data reduction has been performed using a workflow specifically developed for this project. This workflow runs the ESO public pipeline optimizing the data reduction for the Gaia-ESO Survey, automatically performs sky subtraction, barycentric correction and normalisation, and calculates radial velocities and a first guess of the rotational velocities. The quality control is performed using the output parameters from the ESO pipeline, by a visual inspection of the spectra and by the analysis of the signal-to-noise ratio of the spectra. Using the observations of the first 18 months, specifically targets observed multiple times at different epochs, stars observed with both GIRAFFE and UVES, and observations of radial velocity standards, we estimated the precision and the accuracy of the radial velocities. The statistical error on the radial velocities is s ~ 0.4 km s-1 and is mainly due to uncertainties in the zero point of the wavelength calibration. However, we found a systematic bias with respect to the GIRAFFE spectra (~0.9 km s-1) and to the radial velocities of the standard stars (~0.5 km s-1) retrieved from the literature. This bias will be corrected in the future data releases, when a common zero point for all the set-ups and instruments used for the survey is be established. Based on observations made with the ESO/VLT, at Paranal Observatory, under programme 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey).
000002153 700__ $$aMorbidelli, L.
000002153 700__ $$aFranciosini, E.
000002153 700__ $$aMaiorca, E.
000002153 700__ $$aRandich, S.
000002153 700__ $$aModigliani, A.
000002153 700__ $$aGilmore, G.
000002153 700__ $$aAsplund, M.
000002153 700__ $$aBinney, J.
000002153 700__ $$aBonifacio, P.
000002153 700__ $$aDrew, J.
000002153 700__ $$aFeltzing, S.
000002153 700__ $$aFerguson, A.
000002153 700__ $$aJeffries, R.
000002153 700__ $$aMicela, G.
000002153 700__ $$aNegueruela, I.
000002153 700__ $$aPrusti, T.
000002153 700__ $$aRix, H.-W.
000002153 700__ $$aVallenari, A.
000002153 700__ $$aAlfaro, E.
000002153 700__ $$aAllende Prieto, C.
000002153 700__ $$aBabusiaux, C.
000002153 700__ $$aBensby, T.
000002153 700__ $$aBlomme, R.
000002153 700__ $$aBragaglia, A.
000002153 700__ $$aFlaccomio, E.
000002153 700__ $$aFrancois, P.
000002153 700__ $$aHambly, N.
000002153 700__ $$aIrwin, M.
000002153 700__ $$aKoposov, S.
000002153 700__ $$aKorn, A.
000002153 700__ $$aLanzafame, A.
000002153 700__ $$aPancino, E.
000002153 700__ $$aRecio-Blanco, A.
000002153 700__ $$aSmiljanic, R.
000002153 700__ $$aVan Eck, S.
000002153 700__ $$aWalton, N.
000002153 700__ $$aBergemann, M.
000002153 700__ $$aCostado, M. T.
000002153 700__ $$ade Laverny, P.
000002153 700__ $$aHeiter, U.
000002153 700__ $$aHill, V.
000002153 700__ $$aHourihane, A.
000002153 700__ $$aJackson, R.
000002153 700__ $$aJofre, P.
000002153 700__ $$aLewis, J.
000002153 700__ $$aLind, K.
000002153 700__ $$aLardo, C.
000002153 700__ $$aMagrini, L.
000002153 700__ $$aMasseron, T.
000002153 700__ $$aPrisinzano, L.
000002153 700__ $$aWorley, C.
000002153 773__ $$cA113$$pAstronomy and Astrophysics$$v565$$y2014
000002153 85642 $$ahttp://esoads.eso.org/abs/2014A%26A...565A.113S
000002153 905__ $$apublished in
000002153 980__ $$aREFERD