We present preliminary results of a brown dwarf (BD) detection in a ˜1000 star sample monitored with the ongoing PennState-Toruń Centre for Astronomy Planet Search. Contrary to most other projects, our sample contains a substantial fraction of evolved stars ranging from sub-giants up to bright giants, allowing us to study companions to stars more massive than ˜1.5 M⊙. For Main Sequence stars, this limit is set by effective temperature and rotation velocity. Our relatively long list of about a dozen candidates suggests that the BD frequency may rise with stellar mass as it does in the case of planets \citep{lm2007}.