Context : Detailed chemical abundances of volatile and refractory elements have been discussed in the context of terrestrial-planet formation during in past years .

Aims : The HARPS-GTO high-precision planet-search program has provided an extensive database of stellar spectra , which we have inspected in order to select the best-quality spectra available for late type stars .
We study the volatile-to-refractory abundance ratios to investigate their possible relation with the low-mass planetary formation .

Methods : We present a fully differential chemical abundance analysis using high-quality HARPS and UVES spectra of 61 late F- and early G-type main-sequence stars , where 29 are planet hosts and 32 are stars without detected planets .

Results : As for the previous sample of solar analogs , these stars slightly hotter than the Sun also provide very accurate Galactic chemical abundance trends in the metallicity range -0.3 < { [ Fe / H ] } < 0.4 .
Stars with and without planets show similar mean abundance ratios .
Moreover , when removing the Galactic chemical evolution effects , these mean abundance ratios , \Delta { [ X / Fe ] _ { SUN - STARS } } , against condensation temperature tend to exhibit less steep trends with nearly zero or slightly negative slopes .
We have also analyzed a subsample of 26 metal-rich stars , 13 with and 13 without known planets , with spectra at S/N \sim 850 , on average , in the narrow metallicity range 0.04 < { [ Fe / H ] } < 0.19 .
We find the similar , although not equal , abundance pattern with negative slopes for both samples of stars with and without planets .
Using stars at S/N \geq 550 provides equally steep abundance trends with negative slopes for stars both with and without planets .
We revisit the sample of solar analogs to study the abundance patterns of these stars , in particular , 8 stars hosting super-Earth-like planets .
Among these stars having very low-mass planets , only four of them reveal clear increasing abundance trends versus condensation temperature .

Conclusions : Finally , we compared these observed slopes with those predicted using a simple model that enables us to compute the mass of rocks that have formed terrestrial planets in each planetary system .
We do not find any evidence supporting the conclusion that the volatile-to-refractory abundance ratio is related to the presence of rocky planets .