A compact time-domain reduced order quadrature for gravitational wave inspirals with non-stationary noise
Abstract
We develop the first time-domain reduced order quadrature for gravitational waves in the early inspiral period, motivated by the need for dataset compression in the presence of gaps, uneven sampling, and dense covariance matrices. A single reduced basis with 1290 elements can represent inspirals from supermassive black hole binary sources with chirp masses between 107−1010 M⊙, but in the presence of non-stationary noise ∼ 12902 reduced order quadrature weights must be stored. We are able to reduce the stored weights by a factor of two by partitioning our parameter space by GW frequency, with relative waveform/likelihood accuracies remaining below 10−5/10−3 after partition. Finally, we point out that heterodyning can be combined with reduced order methods with no loss in accuracy. Our reduced order quadrature makes inspiral searches in the time domain feasible for both pulsar timing arrays and relative stellar astrometry.
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BibTeX
@misc{zhang2026compact,
title = {{A compact time-domain reduced order quadrature for gravitational wave inspirals with non-stationary noise}},
author = {Benjamin Zhang and Kris Pardo and Bence Bécsy},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.14130},
eprint = {2609.14130},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.14130},
}
RIS
TY - UNPB
TI - A compact time-domain reduced order quadrature for gravitational wave inspirals with non-stationary noise
AU - Benjamin Zhang
AU - Kris Pardo
AU - Bence Bécsy
PY - 2026
DA - 2026/09/12
PB - arXiv
DO - 10.48550/arxiv.2609.14130
UR - https://arxiv.org/abs/2609.14130
AB - We develop the first time-domain reduced order quadrature for gravitational waves in the early inspiral period, motivated by the need for dataset compression in the presence of gaps, uneven sampling, and dense covariance matrices. A single reduced basis with 1290 elements can represent inspirals from supermassive black hole binary sources with chirp masses between 10^7−10^10 M_⊙, but in the presence of non-stationary noise ∼ 1290^2 reduced order quadrature weights must be stored. We are able to reduce the stored weights by a factor of two by partitioning our parameter space by GW frequency, with relative waveform/likelihood accuracies remaining below 10^−5/10^−3 after partition. Finally, we point out that heterodyning can be combined with reduced order methods with no loss in accuracy. Our reduced order quadrature makes inspiral searches in the time domain feasible for both pulsar timing arrays and relative stellar astrometry.
ER -