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atomic and molecular data), improved analysis methods, and improved criteria to define the final recommended parameters.At the end of each cycle an internal data release (i DR) is produced and made available within the Gaia-ESO consortium for scientific validation.For example, the paucity of Fe lines in the HR15N spectral range makes it difficult to derive 100 Myr) and is one of a series describing the Gaia-ESO survey in preparation of its first release of advanced data products.Other papers in this series will discuss the Gaia-ESO scientific goals, observations strategies, team organisation, target selection strategy, data release schedule, data reduction, analysis of OBA-type and FGK-type stars not in the fields of young open clusters, non-standard objects and outliers, external calibration, and the survey-wide homogenisation process. 2 we present the data analysed in the first two Gaia-ESO internal data releases. 3 we outline the principles and general strategies of the Gaia-ESO PMS analysis.The Medusa mode of the fibre-fed system is used throughout the survey, allowing the simultaneous allocation of 132 and 8 fibres feeding GIRAFFE and UVES, respectively, with about 20 (GIRAFFE) and 1 (UVES) fibres used to observe the sky background spectrum.The GIRAFFE/HR15N setup covers the H, and [Fe/H] diagnostics in this wavelength range are poorer than in other settings and still not satisfactorily reproduced by theoretical models.The internal precision of these quantities was estimated by inter-comparing the results obtained by these different methods, while the accuracy was estimated by comparison with independent external data, such as effective temperature and surface gravity derived from angular diameter measurements, on a sample of benchmarks stars.
The memberships of these young clusters, including stars not clearly showing the T Tauri distinctive features, will be discussed in other Gaia-ESO science verification papers (e.g. The Gaia-ESO consortium is set up in several working groups (WGs).
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal mag, systematically covering all the main components of the Milky Way and providing the first homogeneous overview of the distributions of kinematics and chemical element abundances in the Galaxy.
Observations of young open clusters, in particular, are giving new insights into their initial structure, kinematics, and their subsequent evolution. This paper describes the analysis of UVES and GIRAFFE spectra acquired in the fields of young clusters whose population includes pre-main sequence (PMS) stars.
The analysis of PMS stars is carried out by WG12, to which six nodes contributed: INAF–Osservatorio Astrofisico di Arcetri, Centro de Astrofisica de Universidade do Porto (CAUP), Università di Catania and INAF–Osservatorio Astrofisico di Catania (OACT), INAF–Osservatorio Astronomico di Palermo (OAPA), Universidad Complutense de Madrid (UCM), and the Eidgenössische Technische Hochschule Zürich (ETH).
The main input to the Gaia-ESO PMS spectrum analysis consists of UVES and GIRAFFE spectra of cool stars in the field of young open clusters.Specific strategies were implemented to resolve problems of fast rotation, accretion signatures, chromospheric activity, and veiling. The analysis carried out on spectra acquired in young cluster fields during the first 18 months of observations, up to June 2013, is presented in preparation of the first release of advanced data products.