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New gravitational waveform model for precessing binary neutron stars with double-spin effects

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arxiv 2311.15978 v2 pith:6CB27NRT submitted 2023-11-27 gr-qc astro-ph.HEastro-ph.IM

Marta Colleoni , Felip A. Ramis Vidal , Nathan K. Johnson-McDaniel , Tim Dietrich , Maria Haney , Geraint Pratten This is my paper · ORCID
classification gr-qcastro-ph.HEastro-ph.IM
keywords modelsbinaryneutronnrtidalv2effectsstarsincludingprecession
verification ladder T0 review T1 audit T2 compute T3 formal
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We present two new frequency-domain gravitational waveform models for the analysis of signals emitted by binary neutron star coalescences: IMRPhenomXAS_NRTidalv2 and IMRPhenomXP_NRTidalv2. Both models are available through the public algorithm library LALSuite and represent the first extensions of IMRPhenomX models including matter effects. We show here that these two models represent a significant advancement in efficiency and accuracy with respect to their phenomenological predecessors, IMRPhenomD_NRTidalv2 and IMRPhenomPv2_NRTidalv2. The computational efficiency of the new models is achieved through the application of the same multibanding technique previously applied to binary black hole models. Furthermore, IMRPhenomXP_NRTidalv2 implements a more accurate description of the precession dynamics, including double-spin effects and, optionally, matter effects in the twisting-up construction. The latter are available through an option to use a numerical integration of the post-Newtonian precession equations. We show that the new precession descriptions allow the model to better reproduce the phenomenology observed in numerical-relativity simulations of precessing binary neutron stars. Finally, we present some applications of the new models to Bayesian parameter estimation studies, including a reanalysis of GW170817 and a study of simulated observations using numerical relativity waveforms for nonprecessing binary neutron stars with highly spinning components. We find that in these cases the new models make a negligible difference in the results. Nevertheless, by virtue of the aforementioned improvements, the new models represent valuable tools for the study of future detections of coalescing binary neutron stars.

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Cited by 6 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Tidal contributions to the full gravitational waveform to the second-and-a-half post-Newtonian order

    gr-qc 2024-12 conditional novelty 7.0 of 10

    Tidal contributions to all gravitational waveform amplitude modes up to l=7 are derived to 2.5PN for quasi-circular non-spinning compact binaries, with flux and phasing provided at the same order.

  2. A pipeline to search for signatures of line-of-sight acceleration in gravitational wave signals produced by compact binary coalescences

    astro-ph.HE 2025-06 conditional novelty 6.0 of 10

    Line-of-sight acceleration phase corrections for gravitational waves are extended to aligned-spin and tidal binaries, and a pipeline with selection criteria is tested against several acceleration-mimicking effects.

  3. Improved post-Newtonian waveform model for inspiralling precessing-eccentric compact binaries

    gr-qc 2025-02 conditional novelty 6.0 of 10

    The paper presents pyEFPE, a validated and publicly available frequency-domain post-Newtonian waveform model for inspiralling precessing-eccentric compact binaries, with up to about a fifteen-fold speedup.

  4. Fast frequency-domain gravitational waveforms for precessing binaries with a new twist

    gr-qc 2024-12 conditional novelty 6.0 of 10

    IMRPhenomXPHM-SpinTaylor computes precession angles by numerically solving post-Newtonian spin equations in the frequency domain and improves match to numerical relativity from mean mismatch 6.3e-3 to 5.1e-3.

  5. Cosmological constraints and standard sirens forecasts for non-dynamical dark energy in Horndeski gravity

    astro-ph.CO 2026-08 conditional novelty 5.0 of 10

    Standard sirens from third-generation detectors could measure H0 to 0.21% in Extended Cuscuton models, but the forecast omits the modified GW luminosity distance.

  6. Upper Limits on the Isotropic Gravitational-Wave Background from the first part of LIGO, Virgo, and KAGRA's fourth Observing Run

    gr-qc 2025-08 accept novelty 4.0 of 10

    No gravitational-wave background is detected in O1-O4a data; the new CBC-spectrum limit Ω_GW(25 Hz) = 2.0×10^-9 (95%) is 1.7x tighter and remains roughly 2-3x above the GWTC-4-predicted astrophysical background of 0.9×10^-9.

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