Time-domain phenomenological multipolar waveforms for aligned-spin binary black holes in elliptical orbits
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| Autores principales: | , , , , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| _version_ | 1866914254007828480 |
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| author | Planas, Maria de Lluc Ramos-Buades, Antoni García-Quirós, Cecilio Estellés, Héctor Husa, Sascha Haney, Maria |
| author_facet | Planas, Maria de Lluc Ramos-Buades, Antoni García-Quirós, Cecilio Estellés, Héctor Husa, Sascha Haney, Maria |
| contents | We introduce IMRPhenomTEHM, a new phenomenological time-domain model for eccentric aligned-spin binary black holes. Building upon the accurate quasi-circular IMRPhenomTHM model, IMRPhenomTEHM integrates the eccentric post-Newtonian (PN) dynamics and introduces eccentric corrections into the waveform multipoles up to 3PN, including spin effects. The model incorporates the dominant (2, $\pm$2) spherical harmonic mode, as well as the subdominant modes (2, $\pm$1), (3, $\pm$3), (4, $\pm$4), and (5, $\pm$5), assuming the binary has circularized by the time of merger. This approach ensures a smooth transition to the non-eccentric limit, providing an accurate quasi-circular limit against the IMRPhenomTHM model. When comparing against 28 public eccentric numerical relativity simulations from the Simulating eXtreme Spacetimes catalog, IMRPhenomTEHM achieves lower than 2% unfaithfulness, confirming its accurate description without calibration to numerical relativity eccentric datasets. IMRPhenomTEHM provides a reliable description of the evolution of eccentric black hole binaries with aligned spins and eccentricities lower than $e=0.4$ at a frequency of 10 Hz, making it suitable for upcoming gravitational-wave observing runs. We validate the model's accuracy through parameter estimation studies, recovering injected parameters within 90% credible intervals for three numerical relativity eccentric simulations and reanalyzing GW150914 and GW190521, obtaining results consistent with the literature. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_13062 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Time-domain phenomenological multipolar waveforms for aligned-spin binary black holes in elliptical orbits Planas, Maria de Lluc Ramos-Buades, Antoni García-Quirós, Cecilio Estellés, Héctor Husa, Sascha Haney, Maria General Relativity and Quantum Cosmology We introduce IMRPhenomTEHM, a new phenomenological time-domain model for eccentric aligned-spin binary black holes. Building upon the accurate quasi-circular IMRPhenomTHM model, IMRPhenomTEHM integrates the eccentric post-Newtonian (PN) dynamics and introduces eccentric corrections into the waveform multipoles up to 3PN, including spin effects. The model incorporates the dominant (2, $\pm$2) spherical harmonic mode, as well as the subdominant modes (2, $\pm$1), (3, $\pm$3), (4, $\pm$4), and (5, $\pm$5), assuming the binary has circularized by the time of merger. This approach ensures a smooth transition to the non-eccentric limit, providing an accurate quasi-circular limit against the IMRPhenomTHM model. When comparing against 28 public eccentric numerical relativity simulations from the Simulating eXtreme Spacetimes catalog, IMRPhenomTEHM achieves lower than 2% unfaithfulness, confirming its accurate description without calibration to numerical relativity eccentric datasets. IMRPhenomTEHM provides a reliable description of the evolution of eccentric black hole binaries with aligned spins and eccentricities lower than $e=0.4$ at a frequency of 10 Hz, making it suitable for upcoming gravitational-wave observing runs. We validate the model's accuracy through parameter estimation studies, recovering injected parameters within 90% credible intervals for three numerical relativity eccentric simulations and reanalyzing GW150914 and GW190521, obtaining results consistent with the literature. |
| title | Time-domain phenomenological multipolar waveforms for aligned-spin binary black holes in elliptical orbits |
| topic | General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2503.13062 |