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By combining high spatial resolution and wide-field spectroscopy performed,respectively, with SINFONI and FLAMES at the ESO/VLT we measured the radialvelocities of more than 600 stars in the direction of NGC 6388, a Galacticglobular cluster which is suspected to host an intermediate-mass black hole.Approximately 55% of the observed targets turned out to be cluster members. Thecluster velocity dispersion has been derived from the radial velocity ofindividual stars: 52 measurements in the innermost 2", and 276 stars locatedbetween 18" and 600". The velocity dispersion profile shows a central value of~13 km/s, a flat behavior out to ~60" and a decreasing trend outwards. Thecomparison with spherical and isotropic models shows that the observed densityand velocity dispersion profiles are inconsistent with the presence of acentral black hole more massive than ~2000 Msol. These findings are at oddswith recent results obtained from integrated light spectra, showing a velocitydispersion profile with a steep central cusp of 23-25 km/s at r<2" andsuggesting the presence of a black hole with a mass of 17,000 Msol (Lutzgendorfet al. 2011). We also found some evidence of systemic rotation with amplitudeArot ~8 km/s in the innermost 2" (0.13 pc), decreasing to Arot= 3.2 km/s at18"<r<160".

astrophysical journal/the astrophysical journal

The velocity dispersion profile of NGC 6388 from resolved-star  spectroscopy: no evidence of a central cusp and new constraints on the black  hole mass