Volume 570, October 2014
|Number of page(s)||14|
|Section||Catalogs and data|
|Published online||20 October 2014|
The AMBRE project: Parameterisation of FGK-type stars from the ESO:HARPS archived spectra
1 Laboratoire Lagrange (UMR 7293), Université de Nice-Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, BP 4229, 06304 Nice Cedex 4, France
2 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
3 European Southern Observatory, Karl-Schwarzschild-Straße 2, 85748 Garching bei München, Germany
4 INAF − Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, Italy
5 Dipartimento di Fisica e Astronomia, Vicolo Osservatorio 2, 35122 Padova, Italy
Received: 6 March 2014
Accepted: 26 August 2014
Context. The AMBRE project is a collaboration between the European Southern Observatory (ESO) and the Observatoire de la Côte d’Azur (OCA). It has been established to determine the stellar atmospheric parameters of the archived spectra of four ESO spectrographs.
Aims. The analysis of the ESO:HARPS archived spectra for the determination of their atmospheric parameters (effective temperature, surface gravity, global metallicities, and abundance of α-elements over iron) is presented. The sample being analysed (AMBRE:HARPS) covers the period from 2003 to 2010 and is comprised of 126 688 scientific spectra corresponding to ~17 218 different stars.
Methods. For the analysis of the AMBRE:HARPS spectral sample, the automated pipeline developed for the analysis of the AMBRE:FEROS archived spectra has been adapted to the characteristics of the HARPS spectra. Within the pipeline, the stellar parameters are determined by the MATISSE algorithm, which has been developed at OCA for the analysis of large samples of stellar spectra in the framework of galactic archaeology. In the present application, MATISSE uses the AMBRE grid of synthetic spectra, which covers FGKM-type stars for a range of gravities and metallicities.
Results. We first determined the radial velocity and its associated error for the ~15% of the AMBRE:HARPS spectra, for which this velocity had not been derived by the ESO:HARPS reduction pipeline. The stellar atmospheric parameters and the associated chemical index [α/Fe] with their associated errors have then been estimated for all the spectra of the AMBRE:HARPS archived sample. Based on key quality criteria, we accepted and delivered the parameterisation of 93 116 (74% of the total sample) spectra to ESO. These spectra correspond to ~10 706 stars; each are observed between one and several hundred times. This automatic parameterisation of the AMBRE:HARPS spectra shows that the large majority of these stars are cool main-sequence dwarfs with metallicities greater than −0.5 dex (as expected, given that HARPS has been extensively used for planet searches around GK-stars).
Key words: astronomical databases: miscellaneous / stars: fundamental parameters / stars: abundances / techniques: spectroscopic / methods: data analysis
© ESO, 2014
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