We present a study of the kinematics of the remote globular cluster NGC 5694 based on GIRAFFE @ VLT medium resolution spectra .
A sample of 165 individual stars selected to lie on the Red Giant Branch in the cluster Color Magnitude Diagram was considered .
Using radial velocity and metallicity from Calcium triplet , we were able to select 83 bona-fide cluster members .
The addition of six previously known members leads to a total sample of 89 cluster giants with typical uncertainties \leq 1.0 km/s in their radial velocity estimates .
The sample covers a wide range of projected distances from the cluster center , from \sim 0.2 \arcmin to 6.5 \arcmin \simeq 23 half-light radii ( r _ { h } ) .
We find only very weak rotation , as typical of metal-poor globular clusters .
The velocity dispersion gently declines from a central value of \sigma = 6.1 km/s to \sigma \simeq 2.5 km/s at \sim 2 \arcmin \simeq 7.1 r _ { h } , then it remainins flat out to the next ( and last ) measured point of the dispersion profile , at \sim 4 \arcmin \simeq 14.0 r _ { h } , at odds with the predictions of isotropic King models .
We show that both isotropic single-mass non-collisional models and multi-mass anisotropic models can reproduce the observed surface brightness and velocity dispersion profiles .