  The Gaia-ESO survey is a large public spectroscopic survey aimed at
investigating the origin and formation history of our Galaxy by collecting
spectroscopy of representative samples (about 10^5 Milky Way stars) of all
Galactic stellar populations, in the field and in clusters. The survey uses
globular clusters as intra- and inter-survey calibrators, deriving stellar
atmospheric parameters and abundances of a significant number of stars in
clusters, along with radial velocity determinations. We used precise radial
velocities of a large number of stars in seven globular clusters (NGC 1851, NGC
2808, NGC 4372, NGC 4833, NGC 5927, NGC 6752, and NGC 7078) to validate
pipeline results and to preliminarily investigate the cluster internal
kinematics. Radial velocity measurements were extracted from FLAMES/GIRAFFE
spectra processed by the survey pipeline as part of the second internal data
release of data products to ESO. We complemented our sample with ESO archival
data obtained with different instrument configurations. Reliable radial
velocity measurements for 1513 bona fide cluster star members were obtained in
total. We measured systemic rotation, estimated central velocity dispersions,
and present velocity dispersion profiles of all the selected clusters,
providing the first velocity dispersion curve and the first estimate of the
central velocity dispersion for the cluster NGC~5927. Finally, we explore the
possible link between cluster kinematics and other physical parameters. The
analysis we present here demonstrates that Gaia-ESO survey data are
sufficiently accurate to be used in studies of kinematics of stellar systems
and stellar populations in the Milky Way.
