Consistency of post-Newtonian waveforms with numerical relativity

Details Consistency of post-Newtonian waveforms with numerical relativity Consistency of post-Newtonian waveforms with numerical relativity

2006-12-04

arxiv.org/abs/gr-qc/0612024v2

Phys.Rev.Lett.99:181101,2007

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

Replaced with published version -- one figure removed, text and other figures updated for clarity of discussion

Scientific paper

10.1103/PhysRevLett.99.181101

General relativity predicts the gravitational wave signatures of coalescing binary black holes. Explicit waveform predictions for such systems, required for optimal analysis of observational data, have so far been achieved using the post-Newtonian (PN) approximation. The quality of this treatment is unclear, however, for the important late-inspiral portion. We derive late-inspiral waveforms via a complementary approach, direct numerical simulation of Einstein's equations. We compare waveform phasing from simulations of the last $\sim 14$ cycles of gravitational radiation from equal-mass, nonspinning black holes with the corresponding 2.5PN, 3PN, and 3.5PN orbital phasing. We find phasing agreement consistent with internal error estimates based on either approach, suggesting that PN waveforms for this system are effective until the last orbit prior to final merger.

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