Gravitational waves emitted by black-hole binary systems have the highest
signal-to-noise ratio in LIGO and Virgo detectors when black-hole spins are
aligned with the orbital angular momentum and extremal. For such systems, we
extend the effective-one-body inspiral-merger-ringdown waveforms to generic
mass ratios and spins calibrating them to 38 numerical-relativity nonprecessing
waveforms produced by the SXS Collaboration. The numerical-relativity
simulations span mass ratios from 1 to 8, spin magnitudes up to 98% of
extremality, and last for 40 to 60 gravitational-wave cycles. When the total
mass of the binary is between 20Msun and 200Msun, the effective-one-body
nonprecessing (dominant mode) waveforms have overlaps above 99% (using the
advanced-LIGO design noise spectral density) with all of the 38 nonprecessing
numerical waveforms, when maximizing only on initial phase and time. This
implies a negligible loss in event rate due to modeling. Moreover, without
further calibration, we show that the precessing effective-one-body (dominant
mode) waveforms have overlaps above 97% with two very long, strongly precessing
numerical-relativity waveforms, when maximizing only on the initial phase and
time.

本研究针对黑洞二元系统发射的引力波，在黑洞自旋沿轨道角动量极值的方向对 LIGO 和 Virgo 探测器信噪比最高时，扩展了有效单体缠绕波形以涵盖通用质量比和自旋，将其与 SXS 协作组生成的 38 个数值相对论单向波形的校准。当二元系统的总质量在 20 至 200Msun 之间时，使用先进的 LIGO 设计噪声光谱密度，最大化初始相位和时间的重叠率高达 99％，说明模型对事件率的影响可以忽略不计。此外，研究还发现在不需要进一步校准的情况下，旋转效应有效单体峰值波形与两个强烈进动数值相对论波形的重叠率高达 97％。