Speaker
Description
The measurement of spin precession and orbital eccentricity in gravitational-wave signals is a key priority in GW astronomy as these effects provide unique insights into the astrophysical formation and evolution of compact binaries. Moreover, their neglect in waveform models can lead to significant biases in parameter estimation, searches, and tests of general relativity. But accurate and efficient modelling remains a significant challenge. In this talk, we present pyEFPE, a frequency-domain post-Newtonian waveform model for the inspiral of precessing-eccentric compact binaries. It improves upon previous models by introducing analytical expressions for the Fourier mode amplitudes, enhancing the numerical stability of the multiple scale analysis framework, and adding recently derived PN corrections. We also simplify the numerical implementation and introduce a scheme to interpolate the polarisation amplitudes to speedup waveform computations, making the model well-suited for data analysis applications. Comparing it to other waveform models in the quasicircular and eccentric, spin-aligned limits, we find very good agreement. When used to analyse simulated GW events, pyEFPE accurately recovers the signal parameters. While lacking some important physical effects, pyEFPE represents a significant step towards more complete waveform models, offering a flexible and efficient framework for future improvements.