A. O. Thygesen1,2, S. Frandsen1, H. Bruntt1, T. Kallinger3, M. F. Andersen1, Y. P. Elsworth4, S. Hekker5,4, C. Karoff1, D. Stello6, K. Brogaard7, C. Burke8, D. A. Caldwell8 and J. L. Christiansen8
1 Department of Physics and AstronomyAarhus University, 8000 Aarhus C, Denmark
2 Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
3 Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
4 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
5 Astronomical Institute, “Anton Pannekoek”, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, The Netherlands
6 Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia
7 Department of Physics and Astronomy, University of Victoria, PO Box 3055, Victoria, BC V8W 3P6, Canada
8 SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA
Received: 17 March 2012
Accepted: 23 May 2012
Context. Accurate fundamental parameters of stars are essential for the asteroseismic analysis of data from the NASA Kepler mission.
Aims. We aim at determining accurate atmospheric parameters and the abundance pattern for a sample of 82 red giants that are targets for the Kepler mission.
Methods. We have used high-resolution, high signal-to-noise spectra from three different spectrographs. We used the iterative spectral synthesis method VWA to derive the fundamental parameters from carefully selected high-quality iron lines. After determination of the fundamental parameters, abundances of 13 elements were measured using equivalent widths of the spectral lines.
Results. We identify discrepancies in log g and [Fe/H], compared to the parameters based on photometric indices in the Kepler Input Catalogue (larger than 2.0 dex for log g and [Fe/H] for individual stars). The Teff found from spectroscopy and photometry shows good agreement within the uncertainties. We find good agreement between the spectroscopic log g and the log g derived from asteroseismology. Also, we see indications of a potential metallicity effect on the stellar oscillations.
Conclusions. We have determined the fundamental parameters and element abundances of 82 red giants. The large discrepancies between the spectroscopic log g and [Fe/H] and values in the Kepler Input Catalogue emphasize the need for further detailed spectroscopic follow-up of the Kepler targets in order to produce reliable results from the asteroseismic analysis.
Key words: stars: abundances / stars: fundamental parameters / methods: observational / techniques: spectroscopic
Based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
Reduced spectra are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/543/A160
© ESO, 2012