ESIGMAHM: an eccentric, spinning inspiral-merger-ringdown waveform model with higher modes for the detection and characterization of binary black holes

Paul, Kaushik, Maurya, Akash, Henry, Quentin, Sharma, Kartikey, Satheesh, Pranav, Divyajyoti, Divyajyoti ORCID: https://orcid.org/0000-0002-2787-1012, Kumar, Prayush and Mishra, Chandra Kant 2024. ESIGMAHM: an eccentric, spinning inspiral-merger-ringdown waveform model with higher modes for the detection and characterization of binary black holes. arXiv 2409 , 13866. 10.48550/arXiv.2409.13866

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Abstract

We present a time-domain inspiral-merger-ringdowm (IMR) waveform model ESIGMAHM constructed within a framework we named ESIGMA for coalescing binaries of spinning black holes on moderately eccentric orbits (Huerta et al. (2018) [Phys. Rev. D 97, 024031]). We now include the effect of black hole spins on the dynamics of eccentric binaries, as well as model sub-dominant waveform harmonics emitted by them. The inspiral evolution is described by a consistent combination of latest results from post-Newtonian theory, self-force, and black hole perturbation theory. We assume that these moderately eccentric binaries radiate away most of their orbital eccentricity before merger, and seamlessly connect the eccentric inspiral with a numerical relativity based surrogate waveform model for mergers of spinning binaries on quasi-circular orbits. We validate ESIGMAHM against eccentric Numerical Relativity simulations, and also against contemporary effective-one-body and phenomenological models in the quasi-circular limit. We find that ESIGMAHM achieves match values greater than 99% for quasi-circular spin-aligned binaries with mass ratios up to 8, and above 97% for non-spinning and spinning eccentric systems with small or positively aligned spins. Using IMRESIGMA, we quantify the impact of orbital eccentricity on GW signals, showing that next-generation detectors can detect eccentric sources up to 10% louder than quasi-circular ones. We also show that current templated LIGO-Virgo searches will lose more than 10% of optimal SNR for about 20% of all eccentric sources by using only quasi-circular waveform templates. The same will result in a 25% loss in detection rate for eccentric sources with mass ratios m1/m2≥4. Our results highlight the need for including eccentricity and higher-order modes in GW source models and searches for asymmetric eccentric BBH signals.

Item Type:	Working paper
Date Type:	Publication
Status:	Published
Schools:	Schools > Physics and Astronomy
Publisher:	Cornell University
ISSN:	2331-8422
Last Modified:	20 Jan 2026 09:41
URI:	https://orca.cardiff.ac.uk/id/eprint/172770

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