Analysis of late-time tails in spin-aligned eccentric binary black hole mergers

Abstract

We present a comprehensive analysis of late-time tails in gravitational radiation from merging spin-aligned eccentric binary black holes, using high-accuracy point-particle black hole perturbation theory simulations. We simulate the late-time evolution of 15 binary black hole mergers with mass ratio $q=1000$, dimensionless spins $\chi =[-0.9,-0.6,0.0,0.6,0.9]$ and eccentricity at the last stable orbit $e_{\mathrm{LSO}}=[0.8,0.9,0.95]$. We track the tail amplitudes and exponents up to a retarded time coordinate $t=9000M$ after merger for the six spin-weighted spherical harmonic modes $(2,1)$, $(2,2)$, $(3,2)$, $(3,3)$, $(4,3)$, and $(4,4)$ employing both frequentist and Bayesian approaches. We note that the tails are increasingly pronounced for binaries with high eccentricity $e_{\mathrm{LSO}}$ and large negative spin $\chi$. We find that the overall late-time exponents closely approach their predicted asymptotic values ($p=-\ell -4$ for Weyl curvature scalar ${\psi }_{4,\ell m}$ where $\ell$ is the spin-weighted spherical harmonic index), while estimates restricted to the latest portion of the data exactly recover them. We further verify numerically that modes with the same spherical index $\ell$ share identical tail exponents, while variations in $m$ do not affect the tail behavior. Our analysis framework is publicly available through the gwtails Python package.

17 pages, 10 figures; Follow-up of arXiv:2407.04682

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