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Even though the existence of intermediate-mass black holes (IMBHs, blackholes with masses ranging between $10^{2-4}\,M_{\odot}$) has not yet beencorroborated observationally, these objects are of high interest forastrophysics. Our understanding of the formation and evolution of supermassiveblack holes (SMBHs), as well as galaxy evolution modeling and cosmography woulddramatically change if an IMBH were to be observed. From a point of view oftraditional photon-based astronomy, {which relies on the monitoring ofinnermost stellar kinematics}, the {\em direct} detection of an IMBH seems tobe rather far in the future. However, the prospect of the detection andcharacterization of an IMBH has good chances in lower-frequencygravitational-wave (GW) astrophysics using ground-based detectors such as LIGO,Virgo and the future Einstein Telescope (ET). We present an analysis of thesignal of a system of a binary of IMBHs (BBH from now onwards) based on awaveform model obtained with numerical relativity simulations coupled withpost-Newtonian calculations at the highest available order. IMBH binaries withtotal masses between $200-20000\,M_\odot$ would produce significantsignal-to-noise ratios (SNRs) in advanced LIGO and Virgo and the ET. We havecomputed the expected event rate of IMBH binary coalescences for differentconfigurations of the binary, finding interesting values that depend on thespin of the IMBHs. The prospects for IMBH detection and characterization withground-based GW observatories would not only provide us with a robust test ofgeneral relativity, but would also corroborate the existence of these systems.Such detections should allow astrophysicists to probe the stellar environmentsof IMBHs and their formation processes.

Detection of IMBHs with ground-based gravitational wave observatories: A biography of a binary of black holes, from birth to death