Kavli Affiliate: Scott A. Hughes
| First 5 Authors: Christian E. A. Chapman-Bird, Lorenzo Speri, Zachary Nasipak, Ollie Burke, Michael L. Katz
| Summary:
Observations of gravitational-wave signals emitted by compact binary
inspirals provide unique insights into their properties, but their analysis
requires accurate and efficient waveform models. Intermediate- and
extreme-mass-ratio inspirals (I/EMRIs), with mass ratios $q gtrsim 10^2$, are
promising sources for future detectors such as the Laser Interferometer Space
Antenna (LISA). Modelling waveforms for these asymmetric-mass binaries is
challenging, entailing the tracking of many harmonic modes over thousands to
millions of cycles. The FastEMRIWaveforms (FEW) modelling framework addresses
this need, leveraging precomputation of mode data and interpolation to rapidly
compute adiabatic waveforms for eccentric inspirals into zero-spin black holes.
In this work, we extend FEW to model eccentric equatorial inspirals into black
holes with spin magnitudes $|a| leq 0.999$. Our model supports eccentricities
$e < 0.9$ and semi-latus recta $p < 200$, enabling the generation of
long-duration IMRI waveforms, and produces waveforms in $sim 100$ ms with
hardware acceleration. Characterising systematic errors, we estimate that our
model attains mismatches of $sim 10^{-5}$ (for LISA sensitivity) with respect
to error-free adiabatic waveforms over most of parameter space. We find that
kludge models introduce errors in signal-to-noise ratios (SNRs) as great as
$^{+60%}_{-40%}$ and induce marginal biases of up to $sim 1sigma$ in
parameter estimation. We show LISA’s horizon redshift for I/EMRI signals varies
significantly with $a$, reaching a redshift of $3$ ($15$) for EMRIs (IMRIs)
with only minor $(sim10%)$ dependence on $e$ for an SNR threshold of 20. For
signals with SNR $sim 50$, spin and eccentricity-at-plunge are measured with
uncertainties of $delta a sim 10^{-7}$ and $delta e_f sim 10^{-5}$. This
work advances the state-of-the-art in waveform generation for asymmetric-mass
binaries.
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