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The atmospheric parameters of the components of the 16Cygni binary system, inwhich the secondary has a gas giant planet detected, are measured accuratelyusing high quality observational data. Abundances relative to solar areobtained for 25 elements with a mean error of 0.023 dex. The fact that 16CygAhas about four times more lithium than 16CygB is normal considering theslightly different masses of the stars. The abundance patterns of 16CygA and B,relative to iron, are typical of that observed in most of the so-called solartwin stars, with the exception of the heavy elements (Z>30), which can,however, be explained by Galactic chemical evolution. Differential (A-B)abundances are measured with even higher precision (0.018 dex, on average). Wefind that 16CygA is more metal-rich than 16CygB by 0.041+/-0.007 dex. On anelement-to-element basis, no correlation between the A-B abundance differencesand dust condensation temperature (Tc) is detected. Based on these results, weconclude that if the process of planet formation around 16CygB is responsiblefor the observed abundance pattern, the formation of gas giants produces aconstant downwards shift in the photospheric abundance of metals, without a Tccorrelation. The latter would be produced by the formation of terrestrialplanets instead, as suggested by other recent works on precise elementalabundances. Nevertheless, a scenario consistent with these observationsrequires the convective envelopes of 1 Msun stars to reach their present-daysizes about three times quicker than predicted by standard stellar evolutionmodels.

Elemental abundance differences in the 16 Cygni binary system: a signature of gas giant planet formation?