Surrogate model for gravitational waveforms of spin-aligned binary black holes with eccentricities
Qianyun Yun, Wen-Biao Han, Xingyu Zhong, Carlos A. Benavides-Gallego
Abstract
A waveform model for the eccentric binary black holes named SEOBNRE has been used to analyze the LIGO-Virgo's gravitational wave data by several groups. The accuracy of this model has been validated by comparing it with numerical relativity. However, SEOBNRE is a time-domain model, and the efficiency for generating waveforms is a bottleneck in data analysis. To overcome this disadvantage, we offer a reduced-order surrogate model for eccentric binary black holes based on the SEOBNRE waveforms. This surrogate model (SEOBNRE_S) can simulate the complete inspiral-merger-ringdown waves with enough accuracy, covering eccentricities from 0 to 0.25 (0.1), and mass ratio from $1\ensuremath{\mathbin:}1$ to $5\ensuremath{\mathbin:}1$ ($2\ensuremath{\mathbin:}1$) for nonspinning (spinning) binaries. The speed of waveform generation is accelerated about ${10}^{2}--{10}^{3}$ times more than the original SEOBNRE model. Therefore SEOBNRE_S could be helpful in the analysis of LIGO data to find potential eccentricities.