The internal dynamics of globular clusters is a fascinating subject. In the last few years, many advances in this field were made possible by increasingly large simulations and HST observations. Given this context, I will focus on the question whether intermediate-mass black holes are hosted by at least some Milky Way globular clusters. These objects, with masses of order 10^2 to 10^4 solar masses, are likely to affect the dynamics of the host cluster in an observable way. I will present a new method to fingerprint intermediate-mass black holes in globular clusters, based on the comparison of HST photometry and direct N-body simulations.