  In the context of the ESO-VLT Multi-Instrument Kinematic Survey (MIKiS) of
Galactic globular clusters, here we present the line-of-sight velocity
dispersion profile of NGC 6440, a massive globular cluster located in the
Galactic bulge. By combining the data acquired with four different
spectrographs, we obtained the radial velocity of a sample of $\sim 1800$
individual stars distributed over the entire cluster extension, from
$\sim$0.1$"$ to 778$"$ from the center. Using a properly selected sample of
member stars with the most reliable radial velocity measures, we derived the
velocity dispersion profile up to 250$"$ from the center. The profile is well
described by the same King model that best fits the projected star density
distribution, with a constant inner plateau (at ${\sigma}_0 \sim $ 12 km
s$^{-1}$) and no evidence of a central cusp or other significant deviations.
Our data allowed to study the presence of rotation only in the innermost
regions of the cluster (r < 5$"$), revealing a well-defined pattern of ordered
rotation with a position angle of the rotation axis of $\sim$132 $\pm$ 2{\deg}
and an amplitude of $\sim$3 km s$^{-1}$ (corresponding to Vrot/${\sigma}_0
\sim$ 0.3). Also, a flattening of the system qualitatively consistent with the
rotation signal has been detected in the central region.
