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Based on high-resolution UVES spectra we found that the radial velocity (RV)dispersion of nine of twelve known young bona fide and candidate brown dwarfsin the Cha I dark cloud is 2.0 km/s, i.e. significantly smaller than the RVdispersion of T Tauri stars in Cha I (3.6 km/s) and only slightly larger thanthe dispersion of the surrounding molecular gas (1.2 km/s) (Mizuno et al.1999). This result indicates that the majority of these brown dwarfs are notejected with high velocity out of a dense region as proposed by some formationscenarios for brown dwarfs. The mean RV values are consistent with the objectsbeing kinematic members of Cha I. The RV dispersion of the T Tauri starsconfined to the Cha I region is based on a compilation of T Tauri stars withknown RVs from the literature plus three T Tauri stars observed with UVES andunpublished RVs for nine T Tauri stars. Time-resolved spectroscopy revealed RVvariations for five out of nine of the bona fide and candidate brown dwarfs inCha I, which could be due to orbiting planets or surface features. Furthermorewe derived rotational velocities vsin(i) and the Lithium 6708 \AA equivalentwidth.Comment: A&A Letter, in pres

UVES spectra of young brown dwarfs in Cha I: Radial and rotational velocities