“Rapid-Fire” Spectroscopy of Kepler Solar-Like Oscillators
The NASA Kepler mission has been continuously monitoring the same field of the sky since the successful launch in March 2009, providing high-quality stellar lightcurves that are excellent data for asteroseismology, far superior to any other observations available at the present. In order to make a meaningful analysis and interpretation of the asteroseismic data, accurate fundamental parameters for the observed stars are needed. The currently available parameters are quite uncertain as illustrated by e.g. Thygesen et al. (A&A 543:A160, 2012), who found deviations as extreme as 2 dex in [Fe/H] and logg, compared to catalogue values. Thus, additional follow-up observations for these targets are needed in order to put firm limits on the parameter space investigated by the asteroseismic modellers. Here, we propose a method for deriving accurate metallicities of main sequence and subgiant solar-like oscillators from medium resolution spectra with a moderate S/N. The method takes advantage of the additional constraints on the fundamental parameters, available from asteroseismology and multi-color photometry. The approach enables us to reduce the analysis overhead significantly when doing spectral synthesis, which in turn will increases the efficiency of follow-up observations.
The authors would like to thank the entire Kepler-team for their continued effort to ensure the success of this mission. AOT acknowledges support from Sonderforschungsbereich SFB 881 “The Milky Way System” (subproject A5) of the German Research Foundation (DFG). SB acknowledges NSF grant AST-1105930. WJC acknowledges the financial support of the UK Science and Technology Facilities Council (STFC). This research took advantage of the SIMBAD and VIZIER databases at the CDS, Strasbourg (France), and NASA’s Astrophysics Data System Bibliographic Services. Funding for this Discovery mission is provided by NASA’s Science Mission Directorate.
- Bruntt, H., Basu, S., Smalley, B., et al. 2012, MNRAS, 423, 122 (HB12)Google Scholar