2024/04/08 by Alessandro Nagar, Rossella Gamba, Nagar, Alessandro +7 · 9 citations
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #Geophysics and Sensor Technology #Pulsars and Gravitational Waves Research
paper · pdf · doi:10.48550/arxiv.2404.05288
openalex publication_date 2024/04/08 · openalex created_date 2024/04/11 · openalex updated_date 2026/07/30
We present an updated version of the TEOBResumS-Dali effective-one-body (EOB) waveform model for spin aligned binaries on non-circularized orbits. Recently computed 4PN (nonspinning) terms are incorporated in the waveform and radiation reaction. The model is informed by a restricted sample (∼60) of spin-aligned, quasi-circular, Numerical Relativity (NR) simulations. In the quasi-circular limit, the model displays EOB/NR unfaithfulness F\rm max\rm EOBNR\lesssim 10-2 (with median~ 1.06× 10-3) (with Advanced LIGO noise and in the total mass range 10-200M_\odot) for the dominant ℓ=m=2 mode all over the 534 spin-aligned configurations available through the Simulating eXtreme Spacetime catalog of NR waveforms. Similar figures are also obtained with the 28 public eccentric SXS simulations and good compatibility between EOB and NR scattering angles is found. The quasi-circular limit of TEOBResumS-Dali is also found to be highly consistent with the TEOBResumS-GIOTTO quasi-circular model. We then systematically explore the importance of NR-tuning \it also the radiation reaction of the system. When this is done, the median of the distribution of quasi-circular F\rm max\rm EOBNR is lowered to 3.92× 10-4, though balanced by a tail up to ∼ 0.1 for large, positive spins. The same is true for the eccentric-inspiral datasets. We conclude that an improvement of the analytical description of the spin-dependent flux (and its interplay with the conservative part) is likely to be the cornerstone to lower the EOB/NR unfaithfulness below the 10-4 level all over the parameter space, thus grazing the current NR uncertainties as well as the expected needs for next generation of GW detector like Einstein Telescope.