Gravitational-wave echoes from numerical-relativity waveforms via spacetime construction near merging compact objects
We propose a new approach toward reconstructing the late-time near-horizon geometry of merging binary black holes, and toward computing gravitational-wave echoes from exotic compact objects. A binary black-hole merger spacetime can be divided by a timelike hypersurface into a black-hole perturbation (BHP) region (in which the spacetime geometry can be approximated by homogeneous linear perturbations of the final Kerr black hole) and a nonlinear region. At late times, the boundary between the two regions is an infalling shell. The BHP region contains late-time gravitational waves emitted toward the future horizon, as well as those emitted toward future null infinity. In this region, by imposing no-ingoing-wave conditions at past null infinity and matching outgoing waves at future null infinity with waveforms computed from numerical relativity, we can obtain waves that travel toward the future horizon. In particular, the Newman-Penrose ψ₀ associated with the ingoing wave on the horizon is related to tidal deformations measured by fiducial observers floating above the horizon. We further determine the boundary of the BHP region on the future horizon by imposing that ψ₀ inside the BHP region can be faithfully represented by quasinormal modes. Using a physically motivated method to impose boundary conditions near the horizon and applying the so-called Boltzmann reflectivity, we compute the quasinormal modes of nonrotating exotic compact objects, as well as gravitational-wave echoes. We also investigate the detectability of these echoes in current and future detectors and prospects for parameter estimation.
© 2022 American Physical Society. (Received 7 March 2022; accepted 20 April 2022; published 5 May 2022) We thank Manu Srivastava, Shuo Xin, Rico K. L. Lo, and Ling Sun for the discussions. This work makes use of the Black Hole Perturbation Toolkit. The computations presented here were conducted on the Caltech High Performance Cluster, partially supported by a grant from the Gordon and Betty Moore Foundation. This work was supported by the Simons Foundation (Grant No. 568762), the Brinson Foundation, and the Sherman Fairchild Foundation, and by NSF Grants No. PHY-2011961, No. PHY-2011968, No. PHY-1836809, and No. OAC-1931266 at Caltech, and NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell.
Published - PhysRevD.105.104007.pdf
Accepted Version - 2203.03174.pdf