Where post-Newtonian and numerical-relativity waveforms meet

Details Where post-Newtonian and numerical-relativity waveforms meet Where post-Newtonian and numerical-relativity waveforms meet

2007-06-11

arxiv.org/abs/0706.1305v2

Phys.Rev.D77:044020,2008

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

14 pages, 18 figures. Modifications resulting from bug fixes in LAL, and extended analysis of numerical errors and phase agree

Scientific paper

10.1103/PhysRevD.77.044020

We analyze numerical-relativity (NR) waveforms that cover nine orbits (18 gravitational-wave cycles) before merger of an equal-mass system with low eccentricity, with numerical uncertainties of 0.25 radians in the phase and less than 2% in the amplitude; such accuracy allows a direct comparison with post-Newtonian (PN) waveforms. We focus on one of the PN approximants that has been proposed for use in gravitational-wave data analysis, the restricted 3.5PN ``TaylorT1'' waveforms, and compare these with a section of the numerical waveform from the second to the eighth orbit, which is about one and a half orbits before merger. This corresponds to a gravitational-wave frequency range of $M\omega = 0.0455$ to 0.1. Depending on the method of matching PN and NR waveforms, the accumulated phase disagreement over this frequency range can be within numerical uncertainty. Similar results are found in comparisons with an alternative PN approximant, 3PN ``TaylorT3''. The amplitude disagreement, on the other hand, is around 6%, but roughly constant for all 13 cycles that are compared, suggesting that only 4.5 orbits need be simulated to match PN and NR waves with the same accuracy as is possible with nine orbits. If, however, we model the amplitude up to 2.5PN order, the amplitude disagreement is roughly within numerical uncertainty up to about 11 cycles before merger.

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