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Matching post-Newtonian and numerical relativity waveforms: systematic errors and a new phenomenological model for non-precessing black hole binaries

MPS-Authors
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Santamaria,  L.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Ohme,  F.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Dorband,  Nils
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Husa,  S.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Mösta,  P.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Pollney,  Denis
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Reisswig,  Christian
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Robinson,  E. L.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Seiler,  Jennifer
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Krishnan,  B.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Fulltext (public)

1005.3306
(Preprint), 4MB

prd064016.pdf
(Any fulltext), 3MB

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Citation

Santamaria, L., Ohme, F., Ajith, P., Bruegmann, B., Dorband, N., Hannam, M., et al. (2010). Matching post-Newtonian and numerical relativity waveforms: systematic errors and a new phenomenological model for non-precessing black hole binaries. Physical Review D., 82: 064016. doi:10.1103/PhysRevD.82.064016.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0012-BBAF-8
Abstract
We present a new phenomenological gravitational waveform model for the inspiral and coalescence of non-precessing spinning black hole binaries. Our approach is based on a frequency domain matching of post-Newtonian inspiral waveforms with numerical relativity based binary black hole coalescence waveforms. We quantify the various possible sources of systematic errors that arise in matching post-Newtonian and numerical relativity waveforms, and we use a matching criteria based on minimizing these errors; we find that the dominant source of errors are those in the post-Newtonian waveforms near the merger. An analytical formula for the dominant mode of the gravitational radiation of non-precessing black hole binaries is presented that captures the phenomenology of the hybrid waveforms. Its implementation in the current searches for gravitational waves should allow cross-checks of other inspiral-merger-ringdown waveform families and improve the reach of gravitational wave searches.