Large mass-ratio (3< q ≤ 10) inspiral-merger-ringdown model for eccentric binary black holes
Abstract
We present EccHybIMR22, a fully analytical Eccentric-Hybrid-Inspiral-Merger-Ringdown model for the quadrupole (ℓ=$2$, |m|=$2$ or simply the 22) mode. The model is obtained by smoothly attaching an eccentric-inspiral to a quasi-circular-merger-ringdown prescription and is trained on eccentric numerical relativity (NR) simulations with mass ratios q≤ 10. In particular, we focus on obtaining a model that is sensitive to large mass ratios (q>3). Leveraging the recent expansion of SXS catalog of NR simulations, we construct a set of 91 hybrids (obtained by combining waveforms from post-Newtonian (PN) theory with NR simulations) with a target low total mass limit (Mlow) of 20M⊙ at an averaged 22 mode frequency of 20Hz, inaccessible with existing NR simulations alone. Employing a little less than a third of these hybrids as targets, we construct EccHybIMR22 and recover 65% of the hybrids from the remaining set with mismatches smaller than ∼3% for a total mass of 40M⊙ (chosen arbitrarily) and orbital eccentricity e20Hz≲0.33 (e20Hz≲ 0.12) for mass ratios q≤3 (q>3). Furthermore, when tested against 175 SXS simulations, the model is able to recover nearly 80% of the simulations with similar mismatches for systems with 0≲ eNR20Hz≲ 0.3.
Related
- Learning Inspiral-Merger-Ringdown Waveforms from a Post-Newtonian Baseline
- Dissection of a merger-ringdown waveform in the small-mass-ratio limit
- Distinguishing lensing and precessional modulation in binary black-hole inspiral waveforms
- Resonance correction to time-dependent finite-size effects in Effective Field Theory of binary black hole inspiral
- Transformers with Physics-Informed Encodings and Simulation-Based Inference for Robust Detection of Eccentric Binary Black Holes in Pulsar Timing Array Data
BibTeX
@misc{manna2026large,
title = {{Large mass-ratio ($3< q \leq 10$) inspiral-merger-ringdown model for eccentric binary black holes}},
author = {Pratul Manna and Tamal RoyChowdhury and Chandra Kant Mishra},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.16958},
eprint = {2610.16958},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.16958},
}
RIS
TY - UNPB
TI - Large mass-ratio (3< q ≤ 10) inspiral-merger-ringdown model for eccentric binary black holes
AU - Pratul Manna
AU - Tamal RoyChowdhury
AU - Chandra Kant Mishra
PY - 2026
DA - 2026/10/12
PB - arXiv
DO - 10.48550/arxiv.2610.16958
UR - https://arxiv.org/abs/2610.16958
AB - We present EccHybIMR22, a fully analytical Eccentric-Hybrid-Inspiral-Merger-Ringdown model for the quadrupole (ℓ=$2$, |m|=$2$ or simply the 22) mode. The model is obtained by smoothly attaching an eccentric-inspiral to a quasi-circular-merger-ringdown prescription and is trained on eccentric numerical relativity (NR) simulations with mass ratios q≤ 10. In particular, we focus on obtaining a model that is sensitive to large mass ratios (q>3). Leveraging the recent expansion of SXS catalog of NR simulations, we construct a set of 91 hybrids (obtained by combining waveforms from post-Newtonian (PN) theory with NR simulations) with a target low total mass limit (M_low) of 20M_⊙ at an averaged 22 mode frequency of 20Hz, inaccessible with existing NR simulations alone. Employing a little less than a third of these hybrids as targets, we construct EccHybIMR22 and recover 65% of the hybrids from the remaining set with mismatches smaller than ∼3% for a total mass of 40M_⊙ (chosen arbitrarily) and orbital eccentricity e_20Hz≲0.33 (e_20Hz≲ 0.12) for mass ratios q≤3 (q>3). Furthermore, when tested against 175 SXS simulations, the model is able to recover nearly 80% of the simulations with similar mismatches for systems with 0≲ e^NR_20Hz≲ 0.3.
ER -