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For a brief moment, a binary black hole (BBH) merger can be the most powerfulastrophysical event in the visible universe. Here we present a model fit forthis gravitational-wave peak luminosity of nonprecessing quasicircular BBHsystems as a function of the masses and spins of the component black holes,based on numerical relativity (NR) simulations and the hierarchical fittingapproach introduced by X. Jim\'enez-Forteza et al. [Phys. Rev. D 95, 064024(2017), arXiv:1611.00332]. This fit improves over previous results in accuracyand parameter-space coverage and can be used to infer posterior distributionsfor the peak luminosity of future astrophysical signals like GW150914 andGW151226. The model is calibrated to the l<=6 modes of 378 nonprecessing NRsimulations up to mass ratios of 18 and dimensionless spin magnitudes up to0.995, and includes unequal-spin effects. We also constrain the fit toperturbative numerical results for large mass ratios. Studies of keycontributions to the uncertainty in NR peak luminosities, such as (i) modeselection, (ii) finite resolution, (iii) finite extraction radius, and (iv)different methods for converting NR waveforms to luminosity, allow us to use NRsimulations from four different codes as a homogeneous calibration set. Thisstudy of systematic fits to combined NR and large-mass-ratio data, includinghigher modes, also paves the way for improved inspiral-merger-ringdown waveformmodels.

The most powerful astrophysical events: Gravitational-wave peak luminosity of binary black holes as predicted by numerical relativity