Characterization of Kepler early-type targets

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Abstract
Stellar pulsation offers a unique opportunity to constrain the intrinsic parameters of stars and unveil their inner structure. The Kepler satellite is collecting an enormous amount of data of unprecedent photometric precision, which will allow us to test theory and obtain a very precise tomography of stellar interiors. We attempt to determine the stars' fundamental parameters Teff, log g, v sin i, and luminosity needed for computing asteroseismic models and interpreting Kepler data. We report spectroscopic observations of 23 early-type Kepler asteroseismic targets, 13 other stars in the Kepler field, that had not been selected to be observed. We measured the radial velocity by performing a cross-correlation with template spectra to help us identify non-single stars. Spectral synthesis was performed to derive the stellar parameters of our target stars, and the state-of-the-art LTE atmospheric models were computed. For all the stars of our sample, we derived the radial velocity, Teff, log g, v sin i, and luminosities. For 12 stars, we performed a detailed abundance analysis of 20 species, for 16, we could derive only the [Fe/H] ratio. A spectral classification was also performed for 17 stars in the sample. We identify two double-lined spectroscopic binaries, HIP96299 and HIP98551, the former of which is an already known eclipsing binary, and two single-lined spectroscopic binaries, HIP 97254 and HIP 97724. We also report two suspected spectroscopic binaries, HIP92637 and HIP96762, and the detection of a possible variability in the radial velocity of HIP 96277. Two of our program stars are chemically peculiar, namely HIP93941, which we classify as B2 He-weak, and HIP96210, which we classify as B6 HgMn. Finally, we find that HIP93522, HIP93941, HIP93943, HIP96210 and HIP96762, are very slow rotators which makes them very interesting and promising targets for asteroseismic modeling.
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