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In the last five years, gravitational-wave astronomy has gone from a purelytheoretical field into a thriving experimental science. Many gravitational-wavesignals, emitted by stellar-mass binary black holes and binary neutron stars,have been detected, and many more are expected in the future. The observationof the gravitational-wave signals from these systems, and the characterizationof their sources, heavily relies on the precise models for the emittedgravitational waveforms. In this thesis, I present an updated version of thewaveform models for spinning binary black holes within the effective-one-bodyformalism. The novelty of the waveform models presented in this work is theinclusion of beyond-quadupolar terms in the waveforms emitted by spinningbinary black holes. I first construct the model in the simplified case of blackholes with spins aligned with the orbital angular momentum of the binary, thenI extend it to the case of generic spin orientations. The measurement of thesource properties of a binary system emitting gravitational waves requires tocompute $\mathcal{O}(10^7-10^9)$ different waveforms. Since the waveform modelsmentioned before can require $\mathcal{O}(1-10)$s to generate a singlewaveform, they can be difficult to use in data-analysis studies. To overcomethis obstacle, I use the reduced-order-modeling technique to develop a fasterversion of the waveform model for black holes with spins aligned to the orbitalangular momentum of the binary. The waveform models developed in this thesishave been used by the LIGO and Virgo collaborations for the inference of thesource parameters of the gravitational-wave signals detected during the secondand third observing runs (O2 and O3) of the LIGO and Virgo detectors. Here, Ipresent a study on the source properties of the signals GW170729 and GW190412,for which I have been directly involved in the analysis.

Multipolar gravitational waveforms for spinning binary black holes and their impact on source characterization