By combining high spatial resolution and wide-field spectroscopy performed , respectively , with SINFONI and FLAMES at the ESO/VLT we measured the radial velocities of more than 600 stars in the direction of NGC 6388 , a Galactic globular cluster which is suspected to host an intermediate-mass black hole . Approximately 55 % of the observed targets turned out to be cluster members . The cluster velocity dispersion has been derived from the radial velocity of individual stars : 52 measurements in the innermost 2 \arcsec , and 276 stars located between 18 \arcsec and 600 \arcsec . The velocity dispersion profile shows a central value of \sim 13 ~ { } { km~ { } s } ^ { -1 } , a flat behavior out to \sim 60 \arcsec and a decreasing trend outwards . The comparison with spherical and isotropic models shows that the observed density and velocity dispersion profiles are inconsistent with the presence of a central black hole more massive than \sim 2000 M _ { \odot } . These findings are at odds with recent results obtained from integrated light spectra , showing a velocity dispersion profile with a steep central cusp of 23 - 25 ~ { } { km~ { } s } ^ { -1 } at r < 2 \arcsec and suggesting the presence of a black hole with a mass of \sim 1.7 \times 10 ^ { 4 } M _ { \odot } ( 28 ) . We also found some evidence of systemic rotation with amplitude A _ { rot } \sim 8 ~ { } { km~ { } s } ^ { -1 } in the innermost 2 \arcsec ( 0.13 pc ) , decreasing to A _ { rot } = 3.2 ~ { } { km~ { } s } ^ { -1 } at 18 \arcsec < r < 160 \arcsec .