We present a detailed chemical abundance analysis of the parent star of the transiting extrasolar planet TrES-1 .
Based on high-resolution Keck/HIRES and HET/HRS spectra , we have determined abundances relative to the Sun for 16 elements ( Na , Mg , Al , Si , Ca , Sc , Ti , V , Cr , Mn , Co , Ni , Cu , Zn , Y , and Ba ) .
The resulting average abundance of < [ X /H ] > = -0.02 \pm 0.06 is in good agreement with initial estimates of solar metallicity based on iron .
We compare the elemental abundances of TrES-1 with those of the sample of stars with planets , searching for possible chemical abundance anomalies .
TrES-1 appears not to be chemically peculiar in any measurable way .
We investigate possible signs of selective accretion of refractory elements in TrES-1 and other stars with planets , and find no statistically significant trends of metallicity [ X /H ] with condensation temperature T _ { c } .
We use published abundances and kinematic information for the sample of planet-hosting stars ( including TrES-1 ) and several statistical indicators to provide an updated classification in terms of their likelihood to belong to either the thin disk or the thick disk of the Milky Way Galaxy .
TrES-1 is found to be a very likely member of the thin disk population .
By comparing \alpha -element abundances of planet hosts and a large control sample of field stars , we also find that metal-rich ( [ Fe/H ] \gtrsim 0.0 ) stars with planets appear to be systematically underabundant in [ \alpha /Fe ] by \approx 0.1 dex with respect to comparison field stars .
The reason for this signature is unclear , but systematic differences in the analysis procedures adopted by different groups can not be ruled out .