http://arxiv.org/abs/2301.06630
We demonstrate how to quantify the frequency-domain amplitude and phase accuracy of waveform models, $\delta A$ and $\delta \phi$, in a form that could be marginalized over in gravitational-wave inference using techniques currently applied for quantifying calibration uncertainty. For concreteness, waveform uncertainties affecting neutron-star inspiral measurements are considered, and post-hoc error estimates from a variety of waveform models are made by comparing time-domain and frequency-domain analytic models with multiple-resolution numerical simulations. These waveform uncertainty estimates can be compared to GW170817 calibration envelopes or to Advanced LIGO and Virgo calibration goals. Signal-specific calibration and waveform uncertainties are compared to statistical fluctuations in gravitational-wave observatories, giving frequency-dependent modeling requirements for detectors such as Advanced LIGO Plus, Cosmic Explorer, or Einstein Telescope. Finally, the distribution of waveform error for GW170817 over the parameters of the low-spin posterior is computed from tidal models and compared to the constraints on $\delta \phi$ or $\delta A$ from GWTC-1 by Edelman et. al. In general, $\delta \phi$ and $\delta A$ can also be interpreted in terms of unmodeled astrophysical energy transfer within or from the source system.
J. Read
Wed, 18 Jan 23
124/133
Comments: 26 pages, 6 figures, submitted to CQG