Kavli Affiliate: Scott A. Hughes

| First 5 Authors: Halston Lim, Gaurav Khanna, Anuj Apte, Scott A. Hughes,

| Summary:

Using inspiral and plunge trajectories we construct with a generalized

Ori-Thorne algorithm, we use a time-domain black hole perturbation theory code

to compute the corresponding gravitational waves. The last cycles of these

waveforms are a superposition of Kerr quasinormal modes. In this paper, we

examine how the modes’ excitations vary as a function of source parameters,

such as the larger black hole’s spin and the geometry of the smaller body’s

inspiral and plunge. We find that the mixture of quasinormal modes that

characterize the final gravitational waves from a coalescence is entirely

determined by the spin $a$ of the larger black hole, an angle $I$ which

characterizes the misalignment of the orbital plane from the black hole’s spin

axis, a second angle $theta_{rm fin}$ which describes the location at which

the small body crosses the black hole’s event horizon, and the direction

sgn$(dottheta_{rm fin})$ of the body’s final motion. If these

large-mass-ratio results hold at less extreme mass ratios, then measuring

multiple ringdown modes of binary black hole coalescence gravitational waves

may provide important information about the source’s binary properties, such as

the misalignment of the orbit’s angular momentum with black hole spin. This may

be particularly useful for large mass binaries, for which the early inspiral

waves are out of the detectors’ most sensitive band.

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