We present a fully differential chemical abundance analysis using very high-resolution ( \lambda / \delta \lambda \gtrsim 85 , 000 ) and very high signal-to-noise ( S/N \sim 800 on average ) HARPS and UVES spectra of 7 solar twins and 95 solar analogs , 24 are planet hosts and 71 are stars without detected planets .
The whole sample of solar analogs provide very accurate Galactic chemical evolution trends in the metalliciy range -0.3 < { [ Fe / H ] } < 0.5 .
Solar twins with and without planets show similar mean abundance ratios .
We have also analysed a sub-sample of 28 solar analogs , 14 planet hosts and 14 stars without known planets , with spectra at S/N \sim 850 on average , in the metallicity range 0.14 < { [ Fe / H ] } < 0.36 and find the same abundance pattern for both samples of stars with and without planets .
This result does not depend on either the planet mass , from 7 Earth masses to 17.4 Jupiter masses , or the orbital period of the planets , from 3 to 4300 days .
In addition , we have derived the slope of the abundance ratios as a function of the condensation temperature for each star and again find similar distributions of the slopes for both stars with and without planets .
In particular , the peaks of these two distributions are placed at a similar value but with opposite sign as that expected from a possible signature of terrestial planets .
In particular , two of the planetary systems in this sample , containing each of them a Super-Earth like planet , show slope values very close to these peaks which may suggest that these abundance patterns are not related to the presence of terrestial planets .