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Intermediate-mass black holes (IMBHs, 10^2-10^5 M_sun) fill the gap betweenstellar-mass black holes and supermassive black holes (SMBHs). Simulations haveshown that IMBHs may form in dense star clusters, and therefore may still bepresent in these smaller stellar systems. We investigate the Galactic globularcluster NGC 5286 for indications of a central IMBH using spectroscopic datafrom VLT/FLAMES, velocity measurements from the Rutgers Fabry Perot at CTIO,and photometric data from HST. We run analytic spherical and axisymmetric Jeansmodels with different central black-hole masses, anisotropy, mass-to-lightratio, and inclination. Further, we compare the data to a grid of N-bodysimulations without tidal field. Additionally, we use one N-body simulation tocheck the results of the spherical Jeans models for the total cluster mass.Both the Jeans models and the N-body simulations favor the presence of acentral black hole in NGC 5286 and our detection is at the 1- to 1.5-sigmalevel. From the spherical Jeans models we obtain a best fit with black-holemass M_BH=(1.5+-1.0)x10^3 M_sun. The error is the 68% confidence limit fromMonte Carlo simulations. Axisymmetric models give a consistent result. The bestfitting N-body model is found with a black hole of 0.9% of the total clustermass (4.38+-0.18)x10^5 M_sun, which results in an IMBH mass ofM_BH=(3.9+-2.0)x10^3 M_sun. Jeans models give lower values for the totalcluster mass. Our test of the Jeans models with N-body simulation data showsthat this discrepancy has two reasons: The influence of a radially varying M/Lprofile, and underestimation of the velocity dispersion as the measurements arelimited to bright stars. We conclude that detection of IMBHs in Galacticglobular clusters remains a challenging task unless their mass fractions areabove those found for SMBHs in nearby galaxies. [abridged]

Indication for an intermediate-mass black hole in the globular cluster NGC 5286 from kinematics