Context : Chemical abundances of light elements as beryllium in planet-host stars allow us to study the planet formation scenarios and/or investigate possible surface pollution processes .

Aims : We present here an extension of previous beryllium abundance studies .
The complete sample consists of 70 stars hosting planets and 30 stars without known planetary companions .
The aim of this paper is to further assess the trends found in previous studies with less number of objects .
This will provide more information on the processes of depletion and mixing of light elements in the interior of late type stars , and will provide possible explanations for the abundance differences between stars that host planets and “ single ” stars .

Methods : Using high resolution UVES spectra , we measure beryllium abundances of 26 stars that host planets and 1 “ single ” star mainly using the \lambda 3131.065 Å Be ii line , by fitting synthetic spectra to the observational data .
We also compile beryllium abundance measurements of 44 stars hosting planets and 29 “ single ” stars from the literature , resulting in a final sample of 100 objects .

Results : We confirm that the beryllium content is roughly the same in stars hosting planets and in “ single ” stars at temperatures T _ { eff } \gtrsim 5700 K. The sample is still small for T _ { eff } \lesssim 5500 K , but it seems that the scatter in Be abundances of dwarf stars is slightly higher at these cooler temperatures .

Conclusions : We search for distinctive characteristics of planet hosts through correlations of Be abundance versus Li abundance , age , metallicity and oxygen abundance .
These could provide some insight in the formation and evolution of planetary systems , but we did not find any clear correlation .