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We use spectra observed with the integral-field spectrograph MUSE to revealthe central kinematics of the Galactic globular cluster Messier 80 (M80, NGC6093). Using observations obtained with the recently commissioned narrow-fieldmode of MUSE, we are able to analyse 932 stars in the central 7.5 arcsec by 7.5arcsec of the cluster for which no useful spectra previously existed. Meanradial velocities of individual stars derived from the spectra are compared topredictions from axisymmetric Jeans models, resulting in radial profiles of thevelocity dispersion, the rotation amplitude, and the mass-to-light ratio. Thenew data allow us to search for an intermediate-mass black hole (IMBH) in thecentre of the cluster. Our Jeans model finds two similarly probable solutionsaround different dynamical cluster centres. The first solution has a centreclose to the photometric estimates available in the literature and does notneed an IMBH to fit the observed kinematics. The second solution contains alocation of the cluster centre that is offset by about 2.4 arcsec from thefirst one and it needs an IMBH mass of $4600^{+1700}_{-1400}$ solar masses.N-body models support the existence of an IMBH in this cluster with a mass ofup to 6000 solar masses in this cluster, although models without an IMBHprovide a better fit to the observed surface brightness profile. They furtherindicate that the cluster has lost nearly all stellar-mass black holes. Wefurther discuss the detection of two potential high-velocity stars with radialvelocities of 80 to 90 km/s relative to the cluster mean.

Central kinematics of the Galactic globular cluster M80