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

Keitel, David; Forteza, Xisco Jiménez; Husa, Sascha; London, Lionel; Nagar, Alessandro; Bernuzzi, Sebastiano; Harms, Enno; Hannam, Mark; Khan, Sebastian; Pürrer, Michael; Pratten, Geraint; Chaurasia, Vivek

doi:https://doi.org/10.1103/PhysRevD.96.024006

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

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Keitel, David
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Pürrer, Michael
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Citation

Keitel, D., Forteza, X. J., Husa, S., London, L., Nagar, A., Bernuzzi, S., et al. (2017). The most powerful astrophysical events: gravitational-wave peak luminosity of binary black holes as predicted by numerical relativity. Physical Review D, 96: 024006. doi:https://doi.org/10.1103/PhysRevD.96.024006.

Cite as: https://hdl.handle.net/11858/00-001M-0000-002C-59AC-C

Abstract

For a brief moment, a binary black hole (BBH) merger can be the most powerful astrophysical event in the visible universe. Here we present a model fit for this gravitational-wave peak luminosity of nonprecessing quasicircular BBH systems as a function of the masses and spins of the component black holes, based on numerical relativity (NR) simulations and the hierarchical fitting approach introduced in [arXiv:1611.00332]. This fit improves over previous results in accuracy and parameter-space coverage and can be used to infer posterior distributions for the peak luminosity of future astrophysical signals like GW150914 and GW151226. The model is calibrated to the l<=6 modes of 378 nonprecessing NR simulations up to mass ratios of 18 and dimensionless spin magnitudes up to 0.995, and includes unequal-spin effects. We also constrain the fit to perturbative numerical results for large mass ratios. Studies of key contributions to the uncertainty in NR peak luminosities, such as (i) mode selection, (ii) finite resolution, (iii) finite extraction radius, and (iv) different methods for converting NR waveforms to luminosity, allow us to use NR simulations from four different codes as a homogeneous calibration set. This study of systematic fits to combined NR and large-mass-ratio data, including higher modes, also paves the way for improved inspiral-merger-ringdown waveform models.