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

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:10.1103/PhysRevD.96.024006.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-002C-59AC-C Version Permalink: http://hdl.handle.net/11858/00-001M-0000-002E-07E8-5
Genre: Journal Article

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 Creators:
Keitel, David1, Author              
Forteza, Xisco Jiménez, Author
Husa, Sascha, Author
London, Lionel, Author
Nagar, Alessandro, Author
Bernuzzi, Sebastiano, Author
Harms, Enno, Author
Hannam, Mark, Author
Khan, Sebastian2, Author              
Pürrer, Michael3, Author              
Pratten, Geraint, Author
Chaurasia, Vivek, Author
Affiliations:
1Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, escidoc:24010              
2Binary Merger Observations and Numerical Relativity, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, escidoc:2461691              
3Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:1933290              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 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.

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 Dates: 2016-12-302017
 Publication Status: Published in print
 Pages: 18 pages, 22 figures, 6 tables; data and example implementations as supplementary material
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 Rev. Method: -
 Identifiers: arXiv: 1612.09566
URI: http://arxiv.org/abs/1612.09566
DOI: 10.1103/PhysRevD.96.024006
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 96 Sequence Number: 024006 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: http://pubman.mpdl.mpg.de/cone/journals/resource/111088197762258