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The detection of intermediate mass black holes in the centres of globularclusters is highly controversial, as complementary observational methods oftendeliver significantly different results. In order to understand thesediscrepancies, we develop a procedure to simulate integral field unit (IFU)observations of globular clusters: Simulating IFU Star Cluster Observations(SISCO). The input of our software are realistic dynamical models of globularclusters that are then converted in a spectral data cube. We apply SISCO toMonte Carlo cluster simulations from Downing et al. (2010), with a realisticnumber of stars and concentrations. Using independent realisations of a givensimulation we are able to quantify the stochasticity intrinsic to the problemof observing a partially resolved stellar population with integrated-lightspectroscopy. We show that the luminosity-weighted IFU observations can bestrongly biased by the presence of a few bright stars that introduce a scatterin the velocity dispersion measurements up to $\simeq$40% around the expectedvalue, preventing any sound assessment of the central kinematic and a sensibleinterpretation of the presence/absence of an intermediate mass black hole.Moreover, we illustrate that, in our mock IFU observations, the averagekinematic tracer has a mass of $\simeq$0.75 solar masses, only slightly lowerthan the mass of the typical stars examined in studies of resolvedline-of-sight velocities of giant stars. Finally, in order to recover unbiasedkinematic measurements we test different masking techniques that allow us toremove the spaxels dominated by bright stars, bringing the scatter down to alevel of only a few percent. The application of SISCO will allow to investigatestate-of-the-art simulations as realistic observations.

Understanding the central kinematics of globular clusters with simulated integrated-light IFU observations